NEWS

Was haben wir Menschen mit den Sternen gemeinsam? Menschen werden geboren, leben und sterben eines Tages – Sterne ebenso. Aber bei Sternen passiert alles über kosmologisch lange Zeitskalen und mit…

(1092)Long term neutron irradiation studies of square meter sized resistive strip micromegas detectors
  • Fabian Vogel,
  • Otmar Biebel,
  • Christoph Jagfeld,
  • Katrin Penski,
  • Maximilian Rinnagel
  • +2
  • Chrysostomos Valderanis,
  • Ralf Hertenberger
  • (less)
Nuclear Instruments and Methods in Physics Research A, 1045 (01/2023) doi:10.1016/j.nima.2022.167653
abstract + abstract -

Resistive strip Micromegas (MICRO-MEsh GAseous Structure) detectors provide even at square meter sizes a high spatial resolution for the reconstruction of Minimum Ionizing Particles (MIPs) like muons. Micromegas detectors consist of three parallel planar structures. A cathode, a grounded mesh and a segmented anode structure form the detector. Square meter sizes challenge the high-voltage stability during operation, especially when using the frequently used gas mixture of Ar:CO2 (93:7 vol%) with low quencher content. To improve the HV-stability and to enhance the discharge quenching different gas mixtures have been investigated. A very promising one has an 2% admixture of isobutane forming the ternary gas Ar:CO2:iC4H10 (93:5:2 vol%). Long term irradiation studies investigating both gas mixtures interrupted by cosmic muon tracking efficiency measurements have been performed by irradiation with neutrons and gammas from a 10 GBq Am-Be source for a period of two years. The comparison shows gain increase under Ar:CO2:iC4H10 and a considerably improved HV-stable operation of the detector. It is investigated for any performance deterioration for each of the two gas mixtures with focus on pulse-height and changes of efficiency.


(1091)The signature of large-scale turbulence driving on the structure of the interstellar medium
  • Colman,
  • T.,
  • Robitaille,
  • J.-F.,
  • Hennebelle
  • +19
  • P.,
  • Miville-Deschênes,
  • M.-A.,
  • Brucy,
  • N.,
  • Klessen,
  • R. S.,
  • Glover,
  • S. C. O.,
  • Soler,
  • J. D.,
  • Elia,
  • D.,
  • Traficante,
  • A.,
  • Molinari,
  • S.,
  • & Testi,
  • L
  • (less)
abstract + abstract -

The mechanisms that maintain turbulence in the interstellar medium (ISM) are still not identified. This work investigates how we can distinguish between two fundamental driving mechanisms: the accumulated effect of stellar feedback versus the energy injection from galactic scales. We perform a series of numerical simulations describing a stratified star-forming ISM subject to self-consistent stellar feedback. Large-scale external turbulent driving, of various intensities, is added to mimic galactic driving mechanisms. We analyse the resulting column density maps with a technique called Multi-scale non-Gaussian segmentation, which separates the coherent structures and the Gaussian background. This effectively discriminates between the various simulations and is a promising method to understand the ISM structure. In particular, the power spectrum of the coherent structures flattens above 60 pc when turbulence is driven only by stellar feedback. When large-scale driving is applied, the turn-over shifts to larger scales. A systematic comparison with the Large Magellanic Cloud (LMC) is then performed. Only 1 out of 25 regions has a coherent power spectrum that is consistent with the feedback-only simulation. A detailed study of the turn-over scale leads us to conclude that regular stellar feedback is not enough to explain the observed ISM structure on scales larger than 60 pc. Extreme feedback in the form of supergiant shells likely plays an important role but cannot explain all the regions of the LMC. If we assume ISM structure is generated by turbulence, another large-scale driving mechanism is needed to explain the entirety of the observations.

 


(1090)Shared Data and Algorithms for Deep Learning in Fundamental Physics
  • Lisa Benato,
  • Erik Buhmann,
  • Martin Erdmann,
  • Peter Fackeldey,
  • Jonas Glombitza
  • +8
  • Nikolai Hartmann,
  • Gregor Kasieczka,
  • William Korcari,
  • Thomas Kuhr,
  • Jan Steinheimer,
  • Horst Stöcker,
  • Tilman Plehn,
  • Kai Zhou
  • (less)
Computing and Software for Big Science, 6 (12/2022) doi:10.1007/s41781-022-00082-6
abstract + abstract -

We introduce a PYTHON package that provides simple and unified access to a collection of datasets from fundamental physics research—including particle physics, astroparticle physics, and hadron- and nuclear physics—for supervised machine learning studies. The datasets contain hadronic top quarks, cosmic-ray-induced air showers, phase transitions in hadronic matter, and generator-level histories. While public datasets from multiple fundamental physics disciplines already exist, the common interface and provided reference models simplify future work on cross-disciplinary machine learning and transfer learning in fundamental physics. We discuss the design and structure and line out how additional datasets can be submitted for inclusion. As showcase application, we present a simple yet flexible graph-based neural network architecture that can easily be applied to a wide range of supervised learning tasks. We show that our approach reaches performance close to dedicated methods on all datasets. To simplify adaptation for various problems, we provide easy-to-follow instructions on how graph-based representations of data structures, relevant for fundamental physics, can be constructed and provide code implementations for several of them. Implementations are also provided for our proposed method and all reference algorithms.


(1089)Clash of Titans: A MUSE dynamical study of the extreme cluster merger SPT-CL J0307-6225
  • D. Hernández-Lang,
  • A. Zenteno,
  • A. Diaz-Ocampo,
  • H. Cuevas,
  • J. Clancy
  • +21
  • P. H. Prado,
  • F. Aldás,
  • D. Pallero,
  • R. Monteiro-Oliveira,
  • F. A. Gómez,
  • Amelia Ramirez,
  • J. Wynter,
  • E. R. Carrasco,
  • G. K. T. Hau,
  • B. Stalder,
  • M. McDonald,
  • M. Bayliss,
  • B. Floyd,
  • G. Garmire,
  • A. Katzenberger,
  • K. J. Kim,
  • M. Klein,
  • G. Mahler,
  • J. L. Nilo Castellon,
  • A. Saro,
  • T. Somboonpanyakul
  • (less)
Monthly Notices of the Royal Astronomical Society, 517, p24 (12/2022) doi:10.1093/mnras/stac2480
abstract + abstract -

We present MUSE spectroscopy, Megacam imaging, and Chandra X-ray emission for SPT-CL J0307-6225, a $z = 0.58$ major merging galaxy cluster with a large BCG-SZ centroid separation and a highly disturbed X-ray morphology. The galaxy density distribution shows two main overdensities with separations of 0.144 and 0.017 arcmin to their respective BCGs. We characterize the central regions of the two colliding structures, namely 0307-6225N and 0307-6225S, finding velocity derived masses of M200, N = 2.44 ± 1.41 × 1014M and M200, S = 3.16 ± 1.88 × 1014M, with a line-of-sight velocity difference of |Δv| = 342 km s-1. The total dynamically derived mass is consistent with the SZ derived mass of 7.63 h$_{70}^{-1}$ ± 1.36 × 1014M. We model the merger using the Monte Carlo Merger Analysis Code, estimating a merging angle of 36$^{+14}_{-12}$ ° with respect to the plane of the sky. Comparing with simulations of a merging system with a mass ratio of 1:3, we find that the best scenario is that of an ongoing merger that began 0.96$^{+0.31}_{-0.18}$ Gyr ago. We also characterize the galaxy population using Hδ and [O II] λ3727 Å lines. We find that most of the emission-line galaxies belong to 0307-6225S, close to the X-ray peak position with a third of them corresponding to red-cluster sequence galaxies, and the rest to blue galaxies with velocities consistent with recent periods of accretion. Moreover, we suggest that 0307-6225S suffered a previous merger, evidenced through the two equally bright BCGs at the centre with a velocity difference of ~674 km s-1.


(1088)Taking off the edge - simultaneous filament and end core formation
  • S. Heigl,
  • E. Hoemann,
  • A. Burkert
Monthly Notices of the Royal Astronomical Society, 517, p9 (12/2022) doi:10.1093/mnras/stac3110
abstract + abstract -

Simulations of idealized star-forming filaments of finite length typically show core growth that is dominated by two cores forming at its respective end. The end cores form due to a strong increasing acceleration at the filament ends that leads to a sweep-up of material during the filament collapse along its axis. As this growth mode is typically faster than any other core formation mode in a filament, the end cores usually dominate in mass and density compared to other cores forming inside a filament. However, observations of star-forming filaments do not show this prevalence of cores at the filament ends. We explore a possible mechanism to slow the growth of the end cores using numerical simulations of simultaneous filament and embedded core formation, in our case a radially accreting filament forming in a finite converging flow. While such a set-up still leads to end cores, they soon begin to move inwards and a density gradient is formed outside of the cores by the continued accumulation of material. As a result, the outermost cores are no longer located at the exact ends of the filament and the density gradient softens the inward gravitational acceleration of the cores. Therefore, the two end cores do not grow as fast as expected and thus do not dominate over other core formation modes in the filament.


(1087)Fragmentation with discontinuous Galerkin schemes: non-linear fragmentation
  • Maxime Lombart,
  • Mark Hutchison,
  • Yueh-Ning Lee
Monthly Notices of the Royal Astronomical Society, 517, p16 (12/2022) doi:10.1093/mnras/stac2232
abstract + abstract -

Small grains play an essential role in astrophysical processes such as chemistry, radiative transfer, and gas/dust dynamics. The population of small grains is mainly maintained by the fragmentation process due to colliding grains. An accurate treatment of dust fragmentation is required in numerical modelling. However, current algorithms for solving fragmentation equation suffer from an overdiffusion in the conditions of 3D simulations. To tackle this challenge, we developed a discontinuous Galerkin scheme to solve efficiently the non-linear fragmentation equation with a limited number of dust bins.


(1086)A multisimulation study of relativistic SZ temperature scalings in galaxy clusters and groups
  • Elizabeth Lee,
  • Dhayaa Anbajagane,
  • Priyanka Singh,
  • Jens Chluba,
  • Daisuke Nagai
  • +4
  • Scott T. Kay,
  • Weiguang Cui,
  • Klaus Dolag,
  • Gustavo Yepes
  • (less)
Monthly Notices of the Royal Astronomical Society, 517, p22 (12/2022) doi:10.1093/mnras/stac2781
abstract + abstract -

The Sunyaev-Zeldovich (SZ) effect is a powerful tool in modern cosmology. With future observations promising ever improving SZ measurements, the relativistic corrections to the SZ signals from galaxy groups and clusters are increasingly relevant. As such, it is important to understand the differences between three temperature measures: (a) the average relativistic SZ (rSZ) temperature, (b) the mass-weighted temperature relevant for the thermal SZ (tSZ) effect, and (c) the X-ray spectroscopic temperature. In this work, we compare these cluster temperatures, as predicted by the BAHAMAS & MACSIS, ILLUSTRISTNG, MAGNETICUM, and THE THREE HUNDRED PROJECT simulations. Despite the wide range of simulation parameters, we find the SZ temperatures are consistent across the simulations. We estimate a $\simeq 10{{\ \rm per\ cent}}$ level correction from rSZ to clusters with Y ≃ 10-4 Mpc-2. Our analysis confirms a systematic offset between the three temperature measures; with the rSZ temperature $\simeq 20{{\ \rm per\ cent}}$ larger than the other measures, and diverging further at higher redshifts. We demonstrate that these measures depart from simple self-similar evolution and explore how they vary with the defined radius of haloes. We investigate how different feedback prescriptions and resolutions affect the observed temperatures, and discover the SZ temperatures are rather insensitive to these details. The agreement between simulations indicates an exciting avenue for observational and theoretical exploration, determining the extent of relativistic SZ corrections. We provide multiple simulation-based fits to the scaling relations for use in future SZ modelling.


(1085)The interplay between forming planets and photoevaporating discs I: forbidden line diagnostics
  • Michael L. Weber,
  • Barbara Ercolano,
  • Giovanni Picogna,
  • Christian Rab
Monthly Notices of the Royal Astronomical Society, 517, p15 (12/2022) doi:10.1093/mnras/stac2954
abstract + abstract -

Disc winds and planet formation are considered to be two of the most important mechanisms that drive the evolution and dispersal of protoplanetary discs and in turn define the environment in which planets form and evolve. While both have been studied extensively in the past, we combine them into one model by performing three-dimensional radiation-hydrodynamic simulations of giant planet hosting discs that are undergoing X-ray photoevaporation, with the goal to analyse the interactions between both mechanisms. In order to study the effect on observational diagnostics, we produce synthetic observations of commonly used wind-tracing forbidden emission lines with detailed radiative transfer and photoionization calculations. We find that a sufficiently massive giant planet carves a gap in the gas disc that is deep enough to affect the structure and kinematics of the pressure-driven photoevaporative wind significantly. This effect can be strong enough to be visible in the synthetic high-resolution observations of some of our wind diagnostic lines, such as the [O I] 6300 Å or [S II] 6730 Å lines. When the disc is observed at inclinations around 40° and higher, the spectral line profiles may exhibit a peak in the redshifted part of the spectrum, which cannot easily be explained by simple wind models alone. Moreover, massive planets can induce asymmetric substructures within the disc and the photoevaporative wind, giving rise to temporal variations of the line profiles that can be strong enough to be observable on time-scales of less than a quarter of the planet's orbital period.


(1084)Accuracy and precision of triaxial orbit models - II. Viewing angles, shape, and orbital structure
  • Stefano de Nicola,
  • Bianca Neureiter,
  • Jens Thomas,
  • Roberto P. Saglia,
  • Ralf Bender
Monthly Notices of the Royal Astronomical Society, 517, p14 (12/2022) doi:10.1093/mnras/stac2852
abstract + abstract -

We explore the potential of our novel triaxial modelling machinery in recovering the viewing angles, the shape, and the orbit distribution of galaxies by using a high-resolution N-body merger simulation. Our modelling technique includes several recent advancements. (i) Our new triaxial deprojection algorithm shape3d is able to significantly shrink the range of possible orientations of a triaxial galaxy and therefore to constrain its shape relying only on photometric information. It also allows to probe degeneracies, i.e. to recover different deprojections at the same assumed orientation. With this method we can constrain the intrinsic shape of the N-body simulation, i.e. the axis ratios p = b/a and q = c/a, with Δp and Δq ≲ 0.1 using only photometric information. The typical accuracy of the viewing angles reconstruction is 15°-20°. (ii) Our new triaxial Schwarzschild code smart exploits the full kinematic information contained in the entire non-parametric line-of-sight velocity distributions along with a 5D orbital sampling in phase space. (iii) We use a new generalized Akaike information criterion AICp to optimize the smoothing and to select the best-fitting model, avoiding potential biases in purely χ2-based approaches. With our deprojected densities, we recover the correct orbital structure and anisotropy parameter β with Δβ ≲ 0.1. These results are valid regardless of the tested orientation of the simulation and suggest that even despite the known intrinsic photometric and kinematic degeneracies the above described advanced methods make it possible to recover the shape and the orbital structure of triaxial bodies with unprecedented accuracy.


(1083)Fast radio bursts at the dawn of the 2020s
  • E. Petroff,
  • J. W. T. Hessels,
  • D. R. Lorimer
Astronomy and Astrophysics Review, 30 (12/2022) doi:10.1007/s00159-022-00139-w
abstract + abstract -

Since the discovery of the first fast radio burst (FRB) in 2007, and their confirmation as an abundant extragalactic population in 2013, the study of these sources has expanded at an incredible rate. In our 2019 review on the subject, we presented a growing, but still mysterious, population of FRBs—60 unique sources, 2 repeating FRBs, and only 1 identified host galaxy. However, in only a few short years, new observations and discoveries have given us a wealth of information about these sources. The total FRB population now stands at over 600 published sources, 24 repeaters, and 19 host galaxies. Higher time resolution data, sustained monitoring, and precision localisations have given us insight into repeaters, host galaxies, burst morphology, source activity, progenitor models, and the use of FRBs as cosmological probes. The recent detection of a bright FRB-like burst from the Galactic magnetar SGR 1935 + 2154 provides an important link between FRBs and magnetars. There also continue to be surprising discoveries, like periodic modulation of activity from repeaters and the localisation of one FRB source to a relatively nearby globular cluster associated with the M81 galaxy. In this review, we summarise the exciting observational results from the past few years. We also highlight their impact on our understanding of the FRB population and proposed progenitor models. We build on the introduction to FRBs in our earlier review, update our readers on recent results, and discuss interesting avenues for exploration as the field enters a new regime where hundreds to thousands of new FRBs will be discovered and reported each year.


(1082)Spatio-temporal distribution of shallow very-low-frequency earthquakes between December 2020 and January 2021 in Kumano-nada, Nankai subduction zone, detected by a permanent seafloor seismic network
  • Yojiro Yamamoto,
  • Keisuke Ariyoshi,
  • Shuichiro Yada,
  • Masaru Nakano,
  • Takane Hori
Earth, Planets and Space, 74 (12/2022) doi:10.1186/s40623-022-01573-x
abstract + abstract -

We estimate the hypocenter locations and the centroid moment tensor solutions of the shallow very-low-frequency earthquake (sVLFE) activity that occurred in the Kumano-nada region of the Nankai Trough megathrust zone in central Japan from December 2020 to January 2021. Using seafloor observation data, we examined the detailed spatio-temporal distribution of the sVLFE activity. During this episode, the activity area was within the vicinity in which the sVLFE activity has been observed in the past and can be divided into two major parts. The sVLFE activity started from the eastern side and remained there for the first 5 days and then migrated to the western side via secondary expansion. The eastern active area is located just below the outer ridge and coincides with the location where the paleo-Zenith Ridge subducted. The western activity area is centered between the outer wedge and the outer ridge with the primary active area being at the outer wedge. Comparing the activity in the eastern and western areas, the eastern side is more active, but the individual moment releases on this side are smaller than those on the western side. This may indicate a difference in the fluid pressure along the plate boundary between the eastern and western areas. After the second expansion of the active area, we observed several migration patterns within the expanded area with a faster velocity than those of the initial and second expansions. The direction of these migrations is opposite to that of the first and second expansions. This indicates that the fluid pressure and/or stress level in the sVLFE generation region changed with time within this episode. Furthermore, many waveforms with sVLFE characteristics were observed at only one or a few observation points near the trough axis in the middle to latter half of January 2021. This indicates the occurrence of small-scale sVLFEs in the vicinity of the trough axis at the end of this sVLFE episode.


(1081)The varied experience of undergraduate students during the transition to mandatory online chem lab during the initial lockdown of the COVID-19 pandemic
  • Joseph Watts,
  • Kent J. Crippen,
  • Corey Payne,
  • Lorelie Imperial,
  • Melanie Veige
Disciplinary and Interdisciplinary Science Education Research, 4 (12/2022) doi:10.1186/s43031-022-00055-0
abstract + abstract -

The radical global shift to online teaching that resulted from the initial lockdown of the COVID-19 pandemic forced many science educators into the predicament of translating courses, including teaching laboratories, that were based upon face-to-face or practical goals and conventions into ones that could be delivered online. We used this phenomenon at the scale of a research-intensive, land-grant public institution to understand the various ways that the switch was experienced by a large cohort of 702 undergraduate students taking General Chemistry Laboratory. Data was collected over 3 weeks with identical surveys involving four prompts for open-ended responses. Analysis involved sequential explanatory mixed methods where topic modeling, a machine learning technique, was used to identify 21 topics. As categories of experience, these topics were defined and further delineated into 52 dimensions by inductive coding with constant comparison. Reported strengths and positive implications tie predominantly to the topics of Time Management Across a Lab Activity and a Critique of Instruction. Consistent with other reports of teaching and learning during the pandemic, participants perceived Availability of the Teaching Assistant for Help as a positive implication. Perceptions of weakness were most associated with Having to Work Individually, the Hands On Experience, a Critique of Instruction, and Learning by Doing. Hands on Experience, which was interpreted as the lack thereof, was the only topic made up nearly entirely of weaknesses and negative implications. The topic of Learning by Doing was the topic of greatest occurrence, but was equally indicated as strengths, positive implication, weakness, and negative implication. Ramifications are drawn from the weaknesses indicated by students who identified as members of an underrepresented ethnic minority. The results serve as a reminder that the student experience must be the primary consideration for any educational endeavor and needs to continue as a principal point of emphasis for research and development for online science environments.


(1080)An ultralight geometry processing library for parallel mesh refinement
  • Bohan Wang,
  • Bo Chen,
  • Kaixin Yu,
  • Lijun Xie,
  • Jianjun Chen
Advances in Aeronautics, 4 (12/2022) doi:10.1186/s42774-021-00093-8
abstract + abstract -

In applications such as parallel mesh refinement, it remains a challenging issue to ensure the refined surface respects the original Computer-Aided Design (CAD) model accurately. In this paper, an ultralight geometry processing library is developed to resolve this issue effectively and efficiently. Here, we say the kernel is ultralight because it has a very small set of data-structures and algorithms by comparison with industrial-level geometry kernels. Within the library, a simplified surface boundary representation (B-rep) and a radial edge structure are developed respectively to depict the geometry model and the surface mesh, plus hash tables that record the connections between the geometry model and the surface mesh. Based on these data structures, a set of efficient algorithms are developed, which initializes the connection tables, projects a point back to the original geometry, etc. With these data-structure and algorithmic infrastructures set up, the callings of eight well-designed Application Programming Interfaces (APIs) are powerful enough to enable the parallel mesh refinement algorithm outputs a mesh respecting the input CAD model accurately. Numerical experiments will be finally presented to evaluate the performance of the overall parallel mesh refinement algorithm and the algorithms in relation with the developed library.


(1079)Influence of hydrothermal recharge on the evolution of eruption styles and hazards during the 2018-2019 activity at Kuchinoerabujima Volcano, Japan
  • Yusuke Minami,
  • Keiko Matsumoto,
  • Nobuo Geshi,
  • Hiroshi Shinohara
Earth, Planets and Space, 74 (12/2022) doi:10.1186/s40623-022-01580-y
abstract + abstract -

The activity of the 2018-2019 eruption of Kuchinoerabujima Volcano in Japan changed from continuous ejection of ash-laden plumes between October 21 and the middle of December, to intermittent explosive activity accompanied by several pyroclastic density currents until January 2019. To understand the behaviors of magma and hydrothermal fluid that controlled the eruptive sequence, we carried out component analysis, X-ray diffractometry, and leachate analysis for ash samples. The proportion of non-altered volcanic ash particles is ~ 15% in the earlier phase, then it decreased to less than 10% in the later explosive phase. Accordingly, the mineral assemblage of the volcanic ash samples changed from plagioclase-dominant to sulfate minerals-dominant. Concentration of SO42− and Cl/SO4 values of the ash-leachates decreased toward the later activity. These results indicate that the proportion of fresh volcanic rocks decreased and sulfuric acid fluid-derived sulfate minerals increased toward the later activities. Consequently, the 2018-2019 eruption at Kuchinoerabujima Volcano changed from magmatic activity to phreatomagmatic activity. Weak glowing of the crater was observed during the magmatic activity, indicating the volcanic conduit was hot enough to dry up the sub-volcanic hydrothermal system. The following phreatomagmatic activity indicates that the hydrothermal fluid recharged after the magmatic eruption phase. Recharge of the hydrothermal fluid likely caused the variation of the eruption style, and is a process that may control the evolution of hazards during future eruption scenarios at similar active volcanoes in Japan and worldwide.


(1078)Biological Stability of Water-Based Cutting Fluids: Progress and Application
  • Lizhi Tang,
  • Yanbin Zhang,
  • Changhe Li,
  • Zongming Zhou,
  • Xiaolin Nie
  • +9
  • Yun Chen,
  • Huajun Cao,
  • Bo Liu,
  • Naiqing Zhang,
  • Zafar Said,
  • Sujan Debnath,
  • Muhammad Jamil,
  • Hafiz Muhammad Ali,
  • Shubham Sharma
  • (less)
Chinese Journal of Mechanical Engineering, 35 (12/2022) doi:10.1186/s10033-021-00667-z
abstract + abstract -

The application of cutting fluid in the field of engineering manufacturing has a history of hundreds of years, and it plays a vital role in the processing efficiency and surface quality of parts. Among them, water-based cutting fluid accounts for more than 90% of the consumption of cutting fluid. However, long-term recycling of water-based cutting fluid could easily cause deterioration, and the breeding of bacteria could cause the cutting fluid to fail, increase manufacturing costs, and even endanger the health of workers. Traditional bactericides could improve the biological stability of cutting fluids, but they are toxic to the environment and do not conform to the development trend of low-carbon manufacturing. Low-carbon manufacturing is inevitable and the direction of sustainable manufacturing. The use of nanomaterials, transition metal complexes, and physical sterilization methods on the bacterial cell membrane and genetic material could effectively solve this problem. In this article, the mechanism of action of additives and microbial metabolites was first analyzed. Then, the denaturation mechanism of traditional bactericides on the target protein and the effect of sterilization efficiency were summarized. Further, the mechanism of nanomaterials disrupting cell membrane potential was discussed. The effects of lipophilicity and the atomic number of transition metal complexes on cell membrane penetration were also summarized, and the effects of ultraviolet rays and ozone on the destruction of bacterial genetic material were reviewed. In other words, the bactericidal performance, hazard, degradability, and economics of various sterilization methods were comprehensively evaluated, and the potential development direction of improving the biological stability of cutting fluid was proposed.


(1077)Recent Advances in Design Strategies and Multifunctionality of Flexible Electromagnetic Interference Shielding Materials
  • Junye Cheng,
  • Chuanbing Li,
  • Yingfei Xiong,
  • Huibin Zhang,
  • Hassan Raza
  • +7
  • Sana Ullah,
  • Jinyi Wu,
  • Guangping Zheng,
  • Qi Cao,
  • Deqing Zhang,
  • Qingbin Zheng,
  • Renchao Che
  • (less)
Nano-Micro Letters, 14 (12/2022) doi:10.1007/s40820-022-00823-7
abstract + abstract -

With rapid development of 5G communication technologies, electromagnetic interference (EMI) shielding for electronic devices has become an urgent demand in recent years, where the development of corresponding EMI shielding materials against detrimental electromagnetic radiation plays an essential role. Meanwhile, the EMI shielding materials with high flexibility and functional integrity are highly demanded for emerging shielding applications. Hitherto, a variety of flexible EMI shielding materials with lightweight and multifunctionalities have been developed. In this review, we not only introduce the recent development of flexible EMI shielding materials, but also elaborate the EMI shielding mechanisms and the index for "green EMI shielding" performance. In addition, the construction strategies for sophisticated multifunctionalities of flexible shielding materials are summarized. Finally, we propose several possible research directions for flexible EMI shielding materials in near future, which could be inspirational to the fast-growing next-generation flexible electronic devices with reliable and multipurpose protections as offered by EMI shielding materials.


(1076)Joint optimization of dynamic resource allocation and packet scheduling for virtual switches in cognitive internet of vehicles
  • Yang Wang,
  • Xiong Wang,
  • Zhuobin Huang,
  • Wei Li,
  • Shizhong Xu
EURASIP Journal on Applied Signal Processing, 2022 (12/2022) doi:10.1186/s13634-022-00862-7
abstract + abstract -

The rapidly evolving machine learning technologies have reshaped the transportation system and played an essential role in the Cognitive Internet of Vehicles (CIoV). Most of the cognitive services are computation-intensive or storage-intensive, and thus they are usually deployed in edge or cloud data centers. In today's data center networks, the virtual machines hosted in a server are connected to a virtual switch responsible for forwarding all packets for the cognitive services deployed on the virtual machines. Therefore, the virtual switches will become a performance bottleneck for cognitive services without an efficient resource allocation and data scheduling strategy. However, the highly dynamic characteristics of cognitive services make the resource allocation and packet scheduling problem for virtual switches surprisingly challenging. To guarantee the performance of cognitive services, we investigate the joint optimization problem of dynamic resource allocation and packet scheduling for virtual switches. We first model the joint optimization problem of dynamic resource allocation and packet scheduling for virtual switches as a mathematical optimization problem. Then, we analyze the problem with Lyapunov Optimization Framework and derive efficient optimization algorithms with performance tradeoff bounds. At last, we evaluate these algorithms on a testbed and a network-wide simulation platform. Experiment results show that our algorithms outperform other designs and meet the theoretical performance bound.


(1075)Electromagnetic counterparts to massive black-hole mergers
  • Tamara Bogdanović,
  • M. Coleman Miller,
  • Laura Blecha
Living Reviews in Relativity, 25 (12/2022) doi:10.1007/s41114-022-00037-8
abstract + abstract -

The next two decades are expected to open the door to the first coincident detections of electromagnetic (EM) and gravitational-wave (GW) signatures associated with massive black-hole (MBH) binaries heading for coalescence. These detections will launch a new era of multimessenger astrophysics by expanding this growing field to the low-frequency GW regime and will provide an unprecedented understanding of the evolution of MBHs and galaxies. They will also constitute fundamentally new probes of cosmology and would enable unique tests of gravity. The aim of this Living Review is to provide an introduction to this research topic by presenting a summary of key findings, physical processes and ideas pertaining to EM counterparts to MBH mergers as they are known at the time of this writing. We review current observational evidence for close MBH binaries, discuss relevant physical processes and timescales, and summarize the possible EM counterparts to GWs in the precursor, coalescence, and afterglow stages of a MBH merger. We also describe open questions and discuss future prospects in this dynamic and quick-paced research area.


(1074)Generalization enhancement of artificial neural network for turbulence closure by feature selection
  • Linyang Zhu,
  • Weiwei Zhang,
  • Guohua Tu
Advances in Aeronautics, 4 (12/2022) doi:10.1186/s42774-021-00088-5
abstract + abstract -

Feature selection targets for selecting relevant and useful features, and is a vital challenge in turbulence modeling by machine learning methods. In this paper, a new posterior feature selection method based on validation dataset is proposed, which is an efficient and universal method for complex systems including turbulence. Different from the priori feature importance ranking of the filter method and the exhaustive search for feature subset of the wrapper method, the proposed method ranks the features according to the model performance on the validation dataset, and generates the feature subsets in the order of feature importance. Using the features from the proposed method, a black-box model is built by artificial neural network (ANN) to reproduce the behavior of Spalart-Allmaras (S-A) turbulence model for high Reynolds number (Re) airfoil flows in aeronautical engineering. The results show that compared with the model without feature selection, the generalization ability of the model after feature selection is significantly improved. To some extent, it is also demonstrated that although the feature importance can be reflected by the model parameters during the training process, artificial feature selection is still very necessary.


(1073)Climate, vegetation and fire history during the past 18,000 years, recorded in high altitude lacustrine sediments on the Sanetti Plateau, Bale Mountains (Ethiopia)
  • Betelhem Mekonnen,
  • Bruno Glaser,
  • Roland Zech,
  • Michael Zech,
  • Frank Schlütz
  • +9
  • Robert Bussert,
  • Agerie Addis,
  • Graciela Gil-Romera,
  • Sileshi Nemomissa,
  • Tamrat Bekele,
  • Lucas Bittner,
  • Dawit Solomon,
  • Andreas Manhart,
  • Wolfgang Zech
  • (less)
Progress in Earth and Planetary Science, 9 (12/2022) doi:10.1186/s40645-022-00472-9
abstract + abstract -

Low-altitude lakes in eastern Africa have long been investigated and have provided valuable information about the Late Quaternary paleohydrological evolution, such as the African Humid Period. However, records often suffer from poor age control, resolution, and/or ambiguous proxy interpretation, and only little focus has been put on high-altitude regions despite their sensitivity to global, regional, and local climate change phenomena. Here we report on Last Glacial environmental fluctuations at about 4000 m asl on the Sanetti Plateau in the Bale Mountains (SE Ethiopia), based on biogeochemical and palynological analyses of laminated lacustrine sediments. After deglaciation at about 18 cal kyr BP, a steppe-like herb-rich grassland with maximum Chenopodiaceae/Amaranthaceae and Plantago existed. Between 16.6 and 15.7 cal kyr BP, conditions were dry with a desiccation layer at ~ 16.3 cal kyr BP, documenting a temporary phase of maximum aridity on the plateau. While that local event lasted for only a few decades, concentrations of various elements (e.g. Zr, HF, Nb, Nd, and Na) started to increase and reached a maximum at ~ 15.8-15.7 cal kyr BP. We interpret those elements to reflect allochthonous, aeolian dust input via dry northerly winds and increasingly arid conditions in the lowlands. We suggest an abrupt versus delayed response at high and low altitudes, respectively, in response to Northern Hemispheric cooling events (the Heinrich Event 1). The delayed response at low altitudes might be caused by slow negative vegetation and monsoon feedbacks that make the ecosystem somewhat resilient. At ~ 15.7 cal kyr BP, our record shows an abrupt onset of the African Humid Period, almost 1000 years before the onset of the Bølling-Allerød warming in the North-Atlantic region, and about 300 years earlier than in the Lake Tana region. Erica pollen increased significantly between 14.4 and 13.6 cal kyr BP in agreement with periodically wet and regionally warm conditions. Similarly, intense fire events, documented by increased black carbon, correlate with wet and warm environmental conditions that promote the growth of Erica shrubs. This allows to conclude that biomass and thus fuel availability is one important factor controlling fire events in the Bale Mountains.


(1072)Strong-field physics with nanospheres
  • Lennart Seiffert,
  • Sergey Zherebtsov,
  • Matthias F. Kling,
  • Thomas Fennel
Advances in Physics X, 7 (12/2022) doi:10.1080/23746149.2021.2010595
abstract + abstract -

When intense laser fields interact with nanoscale targets, strong-field physics meets plasmonic near-field enhancement and sub-wavelength localization of light. Photoemission spectra reflect the associated attosecond optical and electronic response and encode the collisional and collective dynamics of the solid. Nanospheres represent an ideal platform to explore the underlying attosecond nanophysics because of their particularly simple geometry. This review summarizes key results from the last decade and aims to provide the essential stepping stones for students and researchers to enter this field.


(1071)On the characterization of tidal ocean-dynamo signals in coastal magnetic observatories
  • Johannes Petereit,
  • Jan Saynisch-Wagner,
  • Achim Morschhauser,
  • Leonie Pick,
  • Maik Thomas
Earth, Planets and Space, 74 (12/2022) doi:10.1186/s40623-022-01610-9
abstract + abstract -

Periodic tidal ocean currents induce electric currents and, therefore, magnetic field signals that are observable using spaceborne and ground-based observation techniques. In theory, the signals can be used to monitor oceanic temperature and salinity variations. Tidal magnetic field amplitudes and phases have been extracted from magnetometer measurements in the past. However, due to uncertainties caused by a plentitude of influencing factors, the shape and temporal variation of these signals are only known to a limited extent. This study uses past extraction methods to characterize seasonal variations and long-term trends in the ten year magnetometer time series of three coastal island observatories. First, we assess data processing procedures used to prepare ground-based magnetometer observations for tidal ocean dynamo signal extraction to demonstrate that existing approaches, i.e., subtraction of core field models or first-order differencing, are unable to reliably remove low-frequency contributions. We hence propose low-frequency filtering using smoothing splines and demonstrate the advantages over the existing approaches. Second, we determine signal and side peak magnitudes of the M2 tide induced magnetic field signal by spectral analysis of the processed data. We find evidence for seasonal magnetic field signal variations of up to 25 % from the annual mean. Third, to characterize the long-term behavior of tidal ocean dynamo signal amplitudes and phases, we apply different signal extraction techniques to identify tidal ocean-dynamo signal amplitudes and phases in sub-series of the ten-year time series with incrementally increasing lengths. The analyses support three main findings: (1) trends cause signal amplitude changes of up to ≈1 nT and phase changes are in the order of O (10 ) within the observation period; (2) at least four years of data are needed to obtain reliable amplitude and phase values with the extraction methods used and (3) signal phases are a less dependent on the chosen extraction method than signal amplitudes.


(1070)Gain-controlled broadband tuneability in self-mode-locked Thulium-doped fibre laser
  • Dennis C. Kirsch,
  • Anastasia Bednyakova,
  • Petr Varak,
  • Pavel Honzatko,
  • Benoit Cadier
  • +4
  • Thierry Robin,
  • Andrei Fotiadi,
  • Pavel Peterka,
  • Maria Chernysheva
  • (less)
Communications Physics, 5 (12/2022) doi:10.1038/s42005-022-00989-x
abstract + abstract -

Ensuring self-driven mode-locking and broadband wavelength tuneability in all-fibre-integrated femtosecond laser sources enables a new level of their versatility and extends areas of their applications. Principle limitations for this are traditionally available ultrafast modulators and tuneability techniques. Here, we exploit Thulium-doped fibre to perform three roles in the cavity: laser gain, saturable absorber, and tuneability element via controlling its excitation level. We confirmed that Tm-doped fibre saturable absorption is defined by a reinforced quenching of Tm3+ pairs. As a result, we present both numerically and experimentally a highly stable sub-picosecond pulse generation with a ~90 nm tuneability range spanning from 1873 to 1962 nm via adjusting the cavity feedback. The maximum laser efficiency corresponds to 25% cavity feedback, enabling the highest output energy of 1 nJ in 600-fs solitons at 1877 nm. Overall, the presented laser system establishes a compact and straightforward approach for ultrafast generation, which can be translated to other fibre laser operation wavelengths.


(1069)The origin of galactic cosmic rays
  • Siming Liu,
  • Houdun Zeng,
  • Yuliang Xin,
  • Yiran Zhang
Reviews of Modern Plasma Physics, 6 (12/2022) doi:10.1007/s41614-022-00080-6
abstract + abstract -

Thanks to advances in γ -ray astronomy and precise measurements of cosmic ray (CR) properties, the last decade has witnessed significant progresses in our understanding of the origin of Galactic CRs. In particular, GeV CRs have been associated with supernova remnants (SNRs) with soft γ -ray spectra, while there is evidence of efficient TeV CR acceleration in SNRs with hard γ -ray spectra. Nevertheless, no ultra-high-energy (>50 TeV) γ -ray emission has been detected from shocks of SNRs, implying their limited contributions to PeV CR fluxes. Most ultra-high-energy γ -ray sources detected so far can be associated with pulsar wind nebulae (PWNe), that are known PeV electron/positron accelerators. Their contributions to PeV CRs are still a matter of debate. The Galactic center region and some star clusters, on the other hand, are known sources of PeV CRs. Detailed modelings of CR spectra and anisotropy show that the supernova that gave rise to the Geminga pulsar may have significant contributions to TeV CR fluxes, and PeV CRs should have significant contributions from source(s) in the direction of the Galactic center.


(1068)Quantum Floquet engineering with an exactly solvable tight-binding chain in a cavity
  • Christian J. Eckhardt,
  • Giacomo Passetti,
  • Moustafa Othman,
  • Christoph Karrasch,
  • Fabio Cavaliere
  • +2
  • Michael A. Sentef,
  • Dante M. Kennes
  • (less)
Communications Physics, 5 (12/2022) doi:10.1038/s42005-022-00880-9
abstract + abstract -

Recent experimental advances enable the manipulation of quantum matter by exploiting the quantum nature of light. However, paradigmatic exactly solvable models, such as the Dicke, Rabi or Jaynes-Cummings models for quantum-optical systems, are scarce in the corresponding solid-state, quantum materials context. Focusing on the long-wavelength limit for the light, here, we provide such an exactly solvable model given by a tight-binding chain coupled to a single cavity mode via a quantized version of the Peierls substitution. We show that perturbative expansions in the light-matter coupling have to be taken with care and can easily lead to a false superradiant phase. Furthermore, we provide an analytical expression for the groundstate in the thermodynamic limit, in which the cavity photons are squeezed by the light-matter coupling. In addition, we derive analytical expressions for the electronic single-particle spectral function and optical conductivity. We unveil quantum Floquet engineering signatures in these dynamical response functions, such as analogs to dynamical localization and replica side bands, complementing paradigmatic classical Floquet engineering results. Strikingly, the Drude weight in the optical conductivity of the electrons is partially suppressed by the presence of a single cavity mode through an induced electron-electron interaction.


(1067)HR-LCMS assisted phytochemical screening and an assessment of anticancer activity of Sargassum Squarrossum and Dictyota Dichotoma using in vitro and molecular docking approaches
  • Mohini Salunke,
  • Balaji Wakure,
  • Pravin Wakte
Journal of Molecular Structure, 1270 (12/2022) doi:10.1016/j.molstruc.2022.133833
abstract + abstract -

The research in the area of marine bioactives have substantially improved in the last few decades. The identified marine algae namely Sargassum squarrossum and Dictyota dichotoma were subjected to phytochemical profiling using the most sophisticated High-resolution-LCMS, 1H NMR and revealed the presence of many bioactive compounds.

In vitro MTT tests on lung and breast cancer cells revealed that the DCM fractions of Sargassum squarrossum and Dictyota dichotoma have anticancer characteristics, and they also demonstrated significant dose-dependant cytotoxicity on tumour cell lines. In MCF7 cells, the IC50 values for Sargassum squarrossum and Dictyota dichotoma were 139.51 μg/ml and 241.89 μg/ml whereas in A549 the cell line, the IC 50 values for the DCM fractions of Sargassum squarrossum and Dictyota dichotoma were 95.37 μg/ml and 92.09 μg/ml, respectively. Sargassum squarrossum shows potent anticancer activity in MCF7 and A549 whereas Dictyota dichotoma has potent anticancer activity in A549 and moderate activity in MCF7 cell lines.

The most prevalent enzymes VEGFR-2 and AXL tyrosine kinase, contribute to the development of cancer. A computational method was used to confirm the anticancer effects of the newly identified compounds targeting the above enzymes. According to the molecular docking studies, most of the detected compounds from marine algae were selectively interacting with AXL and VEGFR receptors with good binding affinity scores. The current work demonstrated the phytochemical assessment of marine algae and showed the ability of marine natural products to provide unique metabolites with significant biological activity.


(1066)A Comparison of CPU and GPU Implementations for the LHCb Experiment Run 3 Trigger
  • R. Aaij,
  • M. Adinolfi,
  • S. Aiola,
  • S. Akar,
  • J. Albrecht
  • +156
  • M. Alexander,
  • S. Amato,
  • Y. Amhis,
  • F. Archilli,
  • M. Bala,
  • G. Bassi,
  • L. Bian,
  • M. P. Blago,
  • T. Boettcher,
  • A. Boldyrev,
  • S. Borghi,
  • A. Brea Rodriguez,
  • L. Calefice,
  • M. Calvo Gomez,
  • D. H. Cámpora Pérez,
  • A. Cardini,
  • M. Cattaneo,
  • V. Chobanova,
  • G. Ciezarek,
  • X. Cid Vidal,
  • J. L. Cobbledick,
  • J. A. B. Coelho,
  • T. Colombo,
  • A. Contu,
  • B. Couturier,
  • D. C. Craik,
  • R. Currie,
  • P. d'Argent,
  • M. De Cian,
  • D. Derkach,
  • F. Dordei,
  • M. Dorigo,
  • L. Dufour,
  • P. Durante,
  • A. Dziurda,
  • A. Dzyuba,
  • S. Easo,
  • S. Esen,
  • P. Fernandez Declara,
  • S. Filippov,
  • C. Fitzpatrick,
  • M. Frank,
  • P. Gandini,
  • V. V. Gligorov,
  • E. Golobardes,
  • G. Graziani,
  • L. Grillo,
  • P. A. Günther,
  • S. Hansmann-Menzemer,
  • A. M. Hennequin,
  • L. Henry,
  • D. Hill,
  • S. E. Hollitt,
  • J. Hu,
  • W. Hulsbergen,
  • R. J. Hunter,
  • M. Hushchyn,
  • B. K. Jashal,
  • C. R. Jones,
  • S. Klaver,
  • K. Klimaszewski,
  • R. Kopecna,
  • W. Krzemien,
  • M. Kucharczyk,
  • R. Lane,
  • F. Lazzari,
  • R. Le Gac,
  • P. Li,
  • J. H. Lopes,
  • M. Lucio Martinez,
  • A. Lupato,
  • O. Lupton,
  • X. Lyu,
  • F. Machefert,
  • O. Madejczyk,
  • S. Malde,
  • J. F. Marchand,
  • S. Mariani,
  • C. Marin Benito,
  • D. Martinez Santos,
  • F. Martinez Vidal,
  • R. Matev,
  • M. Mazurek,
  • B. Mitreska,
  • D. S. Mitzel,
  • M. J. Morello,
  • H. Mu,
  • P. Muzzetto,
  • P. Naik,
  • M. Needham,
  • N. Neri,
  • N. Neufeld,
  • N. S. Nolte,
  • D. O'Hanlon,
  • A. Oyanguren,
  • M. Pepe Altarelli,
  • S. Petrucci,
  • M. Petruzzo,
  • L. Pica,
  • F. Pisani,
  • A. Piucci,
  • F. Polci,
  • A. Poluektov,
  • E. Polycarpo,
  • C. Prouve,
  • G. Punzi,
  • R. Quagliani,
  • R. I. Rabadan Trejo,
  • M. Ramos Pernas,
  • M. S. Rangel,
  • F. Ratnikov,
  • G. Raven,
  • F. Reiss,
  • V. Renaudin,
  • P. Robbe,
  • A. Ryzhikov,
  • M. Santimaria,
  • M. Saur,
  • M. Schiller,
  • R. Schwemmer,
  • B. Sciascia,
  • A. Solomin,
  • F. Suljik,
  • N. Skidmore,
  • M. D. Sokoloff,
  • P. Spradlin,
  • M. Stahl,
  • S. Stahl,
  • H. Stevens,
  • L. Sun,
  • A. Szabelski,
  • T. Szumlak,
  • M. Szymanski,
  • D. Y. Tou,
  • G. Tuci,
  • A. Usachov,
  • N. Valls Canudas,
  • R. Vazquez Gomez,
  • S. Vecchi,
  • M. Vesterinen,
  • X. Vilasis-Cardona,
  • D. Vom Bruch,
  • Z. Wang,
  • T. Wojton,
  • M. Whitehead,
  • M. Williams,
  • M. Witek,
  • Y. Xie,
  • A. Xu,
  • H. Yin,
  • M. Zdybal,
  • O. Zenaiev,
  • D. Zhang,
  • L. Zhang,
  • X. Zhu,
  • LHCb Collaboration
  • (less)
Computing and Software for Big Science, 6 (12/2022) doi:10.1007/s41781-021-00070-2
abstract + abstract -

The Large Hadron Collider beauty (LHCb) experiment at CERN is undergoing an upgrade in preparation for the Run 3 data collection period at the Large Hadron Collider (LHC). As part of this upgrade, the trigger is moving to a full software implementation operating at the LHC bunch crossing rate. We present an evaluation of a CPU-based and a GPU-based implementation of the first stage of the high-level trigger. After a detailed comparison, both options are found to be viable. This document summarizes the performance and implementation details of these options, the outcome of which has led to the choice of the GPU-based implementation as the baseline.


(1065)New horizons for fundamental physics with LISA
  • K. G. Arun,
  • Enis Belgacem,
  • Robert Benkel,
  • Laura Bernard,
  • Emanuele Berti
  • +136
  • Gianfranco Bertone,
  • Marc Besancon,
  • Diego Blas,
  • Christian G. Böhmer,
  • Richard Brito,
  • Gianluca Calcagni,
  • Alejandro Cardenas-Avendaño,
  • Katy Clough,
  • Marco Crisostomi,
  • Valerio De Luca,
  • Daniela Doneva,
  • Stephanie Escoffier,
  • José María Ezquiaga,
  • Pedro G. Ferreira,
  • Pierre Fleury,
  • Stefano Foffa,
  • Gabriele Franciolini,
  • Noemi Frusciante,
  • Juan García-Bellido,
  • Carlos Herdeiro,
  • Thomas Hertog,
  • Tanja Hinderer,
  • Philippe Jetzer,
  • Lucas Lombriser,
  • Elisa Maggio,
  • Michele Maggiore,
  • Michele Mancarella,
  • Andrea Maselli,
  • Sourabh Nampalliwar,
  • David Nichols,
  • Maria Okounkova,
  • Paolo Pani,
  • Vasileios Paschalidis,
  • Alvise Raccanelli,
  • Lisa Randall,
  • Sébastien Renaux-Petel,
  • Antonio Riotto,
  • Milton Ruiz,
  • Alexander Saffer,
  • Mairi Sakellariadou,
  • Ippocratis D. Saltas,
  • B. S. Sathyaprakash,
  • Lijing Shao,
  • Carlos F. Sopuerta,
  • Thomas P. Sotiriou,
  • Nikolaos Stergioulas,
  • Nicola Tamanini,
  • Filippo Vernizzi,
  • Helvi Witek,
  • Kinwah Wu,
  • Kent Yagi,
  • Stoytcho Yazadjiev,
  • Nicolás Yunes,
  • Miguel Zilhão,
  • Niayesh Afshordi,
  • Marie-Christine Angonin,
  • Vishal Baibhav,
  • Enrico Barausse,
  • Tiago Barreiro,
  • Nicola Bartolo,
  • Nicola Bellomo,
  • Ido Ben-Dayan,
  • Eric A. Bergshoeff,
  • Sebastiano Bernuzzi,
  • Daniele Bertacca,
  • Swetha Bhagwat,
  • Béatrice Bonga,
  • Lior M. Burko,
  • Geoffrey Compére,
  • Giulia Cusin,
  • Antonio da Silva,
  • Saurya Das,
  • Claudia de Rham,
  • Kyriakos Destounis,
  • Ema Dimastrogiovanni,
  • Francisco Duque,
  • Richard Easther,
  • Hontas Farmer,
  • Matteo Fasiello,
  • Stanislav Fisenko,
  • Kwinten Fransen,
  • Jörg Frauendiener,
  • Jonathan Gair,
  • László Árpád Gergely,
  • Davide Gerosa,
  • Leonardo Gualtieri,
  • Wen-Biao Han,
  • Aurelien Hees,
  • Thomas Helfer,
  • Jörg Hennig,
  • Alexander C. Jenkins,
  • Eric Kajfasz,
  • Nemanja Kaloper,
  • Vladimír Karas,
  • Bradley J. Kavanagh,
  • Sergei A. Klioner,
  • Savvas M. Koushiappas,
  • Macarena Lagos,
  • Christophe Le Poncin-Lafitte,
  • Francisco S. N. Lobo,
  • Charalampos Markakis,
  • Prado Martín-Moruno,
  • C. J. A. P. Martins,
  • Sabino Matarrese,
  • Daniel R. Mayerson,
  • José P. Mimoso,
  • Johannes Noller,
  • Nelson J. Nunes,
  • Roberto Oliveri,
  • Giorgio Orlando,
  • George Pappas,
  • Igor Pikovski,
  • Luigi Pilo,
  • Jiří Podolský,
  • Geraint Pratten,
  • Tomislav Prokopec,
  • Hong Qi,
  • Saeed Rastgoo,
  • Angelo Ricciardone,
  • Rocco Rollo,
  • Diego Rubiera-Garcia,
  • Olga Sergijenko,
  • Stuart Shapiro,
  • Deirdre Shoemaker,
  • Alessandro Spallicci,
  • Oleksandr Stashko,
  • Leo C. Stein,
  • Gianmassimo Tasinato,
  • Andrew J. Tolley,
  • Elias C. Vagenas,
  • Stefan Vandoren,
  • Daniele Vernieri,
  • Rodrigo Vicente,
  • Toby Wiseman,
  • Valery I. Zhdanov,
  • Miguel Zumalacárregui
  • (less)
Living Reviews in Relativity, 25 (12/2022) doi:10.1007/s41114-022-00036-9
abstract + abstract -

The Laser Interferometer Space Antenna (LISA) has the potential to reveal wonders about the fundamental theory of nature at play in the extreme gravity regime, where the gravitational interaction is both strong and dynamical. In this white paper, the Fundamental Physics Working Group of the LISA Consortium summarizes the current topics in fundamental physics where LISA observations of gravitational waves can be expected to provide key input. We provide the briefest of reviews to then delineate avenues for future research directions and to discuss connections between this working group, other working groups and the consortium work package teams. These connections must be developed for LISA to live up to its science potential in these areas.


(1064)Transition state theory characterizes thin film macrospin dynamics driven by an oscillatory magnetic field: Inertial effects
  • Michael Maihöfer,
  • Johannes Reiff,
  • Jörg Main,
  • Rigoberto Hernandez
Communications in Nonlinear Science and Numerical Simulations, 115 (12/2022) doi:10.1016/j.cnsns.2022.106764
abstract + abstract -

Understanding the magnetization switching process in ferromagnetic thin films is essential for many technological applications. We investigate the effects of periodic driving via magnetic fields on a macrospin system under explicit consideration of inertial dynamics. This is usually achieved by extending the Landau-Lifshitz-Gilbert equation with a term including the second time derivative of the magnetization. The dynamics of the magnetization switching can then be characterized by its switching rate. We apply methods from transition state theory for driven systems to resolve the rate of magnetization switching in this general case. In doing so, we find that magnetization exhibits resonance-like behavior under certain driving conditions, and it can be affected strongly by the system's relaxation rate.


(1063)Direct observation of significant hot carrier cooling suppression in a two-dimensional silicon phononic crystal
  • Wensheng Yan,
  • Liyuan Long,
  • Yue Zang,
  • Gaoyuan Yang,
  • Guijie Liang
npj Asia Materials, 14 (12/2022) doi:10.1038/s41427-022-00397-1
abstract + abstract -

Finding hot carrier cooling suppression in new material structures is fundamentally important for developing promising technological applications. These phenomenona have not been reported for crystalline silicon phononic crystals. Herein, we experimentally design two-dimensional (2D) silicon samples consisting of airy hole arrays in a crystalline silicon matrix. For reference, the determined hot carrier cooling times were 0.45 ps and 0.37 ps, respectively, at probe wavelengths of 1080 nm and 1100 nm. Surprisingly, when the 2D structured silicon possessed the properties of a phononic crystal, significant suppression of hot carrier cooling was observed. In these cases, the observed hot carrier cooling times were as long as 15.9 ps and 10.7 ps at probe wavelengths of 1080 nm and 1100 nm, respectively, indicating prolongation by orders of magnitude. This remarkable enhancement was also observed with other probe wavelengths. The present work presents experimental evidence for hot carrier cooling suppression in 2D silicon phononic crystals and opens opportunities for promising applications.


(1062)Emulating the impact of additional proton-proton interactions in the ATLAS simulation by presampling sets of inelastic Monte Carlo events
  • G. Aad,
  • B. Abbott,
  • D. C. Abbott,
  • A. Abed Abud,
  • K. Abeling
  • +2846
  • D. K. Abhayasinghe,
  • S. H. Abidi,
  • O. S. Abouzeid,
  • N. L. Abraham,
  • H. Abramowicz,
  • H. Abreu,
  • Y. Abulaiti,
  • A. C. Abusleme Hoffman,
  • B. S. Acharya,
  • B. Achkar,
  • L. Adam,
  • C. Adam Bourdarios,
  • L. Adamczyk,
  • L. Adamek,
  • J. Adelman,
  • A. Adiguzel,
  • S. Adorni,
  • T. Adye,
  • A. A. Affolder,
  • Y. Afik,
  • C. Agapopoulou,
  • M. N. Agaras,
  • A. Aggarwal,
  • C. Agheorghiesei,
  • J. A. Aguilar-Saavedra,
  • A. Ahmad,
  • F. Ahmadov,
  • W. S. Ahmed,
  • X. Ai,
  • G. Aielli,
  • S. Akatsuka,
  • M. Akbiyik,
  • T. P. A. Åkesson,
  • E. Akilli,
  • A. V. Akimov,
  • K. Al Khoury,
  • G. L. Alberghi,
  • J. Albert,
  • M. J. Alconada Verzini,
  • S. Alderweireldt,
  • M. Aleksa,
  • I. N. Aleksandrov,
  • C. Alexa,
  • T. Alexopoulos,
  • A. Alfonsi,
  • F. Alfonsi,
  • M. Alhroob,
  • B. Ali,
  • S. Ali,
  • M. Aliev,
  • G. Alimonti,
  • C. Allaire,
  • B. M. M. Allbrooke,
  • P. P. Allport,
  • A. Aloisio,
  • F. Alonso,
  • C. Alpigiani,
  • E. Alunno Camelia,
  • M. Alvarez Estevez,
  • M. G. Alviggi,
  • Y. Amaral Coutinho,
  • A. Ambler,
  • L. Ambroz,
  • C. Amelung,
  • D. Amidei,
  • S. P. Amor Dos Santos,
  • S. Amoroso,
  • C. S. Amrouche,
  • C. Anastopoulos,
  • N. Andari,
  • T. Andeen,
  • J. K. Anders,
  • S. Y. Andrean,
  • A. Andreazza,
  • V. Andrei,
  • C. R. Anelli,
  • S. Angelidakis,
  • A. Angerami,
  • A. V. Anisenkov,
  • A. Annovi,
  • C. Antel,
  • M. T. Anthony,
  • E. Antipov,
  • M. Antonelli,
  • D. J. A. Antrim,
  • F. Anulli,
  • M. Aoki,
  • J. A. Aparisi Pozo,
  • M. A. Aparo,
  • L. Aperio Bella,
  • N. Aranzabal,
  • V. Araujo Ferraz,
  • C. Arcangeletti,
  • A. T. H. Arce,
  • J. -F. Arguin,
  • S. Argyropoulos,
  • J. -H. Arling,
  • A. J. Armbruster,
  • A. Armstrong,
  • O. Arnaez,
  • H. Arnold,
  • Z. P. Arrubarrena Tame,
  • G. Artoni,
  • H. Asada,
  • K. Asai,
  • S. Asai,
  • N. A. Asbah,
  • E. M. Asimakopoulou,
  • L. Asquith,
  • J. Assahsah,
  • K. Assamagan,
  • R. Astalos,
  • R. J. Atkin,
  • M. Atkinson,
  • N. B. Atlay,
  • H. Atmani,
  • P. A. Atmasiddha,
  • K. Augsten,
  • V. A. Austrup,
  • G. Avolio,
  • M. K. Ayoub,
  • G. Azuelos,
  • D. Babal,
  • H. Bachacou,
  • K. Bachas,
  • F. Backman,
  • P. Bagnaia,
  • H. Bahrasemani,
  • A. J. Bailey,
  • V. R. Bailey,
  • J. T. Baines,
  • C. Bakalis,
  • O. K. Baker,
  • P. J. Bakker,
  • E. Bakos,
  • D. Bakshi Gupta,
  • S. Balaji,
  • R. Balasubramanian,
  • E. M. Baldin,
  • P. Balek,
  • F. Balli,
  • W. K. Balunas,
  • J. Balz,
  • E. Banas,
  • M. Bandieramonte,
  • A. Bandyopadhyay,
  • L. Barak,
  • W. M. Barbe,
  • E. L. Barberio,
  • D. Barberis,
  • M. Barbero,
  • G. Barbour,
  • K. N. Barends,
  • T. Barillari,
  • M. -S. Barisits,
  • J. Barkeloo,
  • T. Barklow,
  • B. M. Barnett,
  • R. M. Barnett,
  • Z. Barnovska-Blenessy,
  • A. Baroncelli,
  • G. Barone,
  • A. J. Barr,
  • L. Barranco Navarro,
  • F. Barreiro,
  • J. Barreiro Guimarães da Costa,
  • U. Barron,
  • S. Barsov,
  • F. Bartels,
  • R. Bartoldus,
  • G. Bartolini,
  • A. E. Barton,
  • P. Bartos,
  • A. Basalaev,
  • A. Basan,
  • A. Bassalat,
  • M. J. Basso,
  • C. R. Basson,
  • R. L. Bates,
  • S. Batlamous,
  • J. R. Batley,
  • B. Batool,
  • M. Battaglia,
  • M. Bauce,
  • F. Bauer,
  • P. Bauer,
  • H. S. Bawa,
  • A. Bayirli,
  • J. B. Beacham,
  • T. Beau,
  • P. H. Beauchemin,
  • F. Becherer,
  • P. Bechtle,
  • H. P. Beck,
  • K. Becker,
  • C. Becot,
  • A. J. Beddall,
  • V. A. Bednyakov,
  • C. P. Bee,
  • T. A. Beermann,
  • M. Begalli,
  • M. Begel,
  • A. Behera,
  • J. K. Behr,
  • J. F. Beirer,
  • F. Beisiegel,
  • M. Belfkir,
  • G. Bella,
  • L. Bellagamba,
  • A. Bellerive,
  • P. Bellos,
  • K. Beloborodov,
  • K. Belotskiy,
  • N. L. Belyaev,
  • D. Benchekroun,
  • N. Benekos,
  • Y. Benhammou,
  • D. P. Benjamin,
  • M. Benoit,
  • J. R. Bensinger,
  • S. Bentvelsen,
  • L. Beresford,
  • M. Beretta,
  • D. Berge,
  • E. Bergeaas Kuutmann,
  • N. Berger,
  • B. Bergmann,
  • L. J. Bergsten,
  • J. Beringer,
  • S. Berlendis,
  • G. Bernardi,
  • C. Bernius,
  • F. U. Bernlochner,
  • T. Berry,
  • P. Berta,
  • A. Berthold,
  • I. A. Bertram,
  • O. Bessidskaia Bylund,
  • S. Bethke,
  • A. Betti,
  • A. J. Bevan,
  • S. Bhatta,
  • D. S. Bhattacharya,
  • P. Bhattarai,
  • V. S. Bhopatkar,
  • R. Bi,
  • R. M. Bianchi,
  • O. Biebel,
  • R. Bielski,
  • K. Bierwagen,
  • N. V. Biesuz,
  • M. Biglietti,
  • T. R. V. Billoud,
  • M. Bindi,
  • A. Bingul,
  • C. Bini,
  • S. Biondi,
  • C. J. Birch-Sykes,
  • M. Birman,
  • T. Bisanz,
  • J. P. Biswal,
  • D. Biswas,
  • A. Bitadze,
  • C. Bittrich,
  • K. Bjørke,
  • T. Blazek,
  • I. Bloch,
  • C. Blocker,
  • A. Blue,
  • U. Blumenschein,
  • G. J. Bobbink,
  • V. S. Bobrovnikov,
  • D. Bogavac,
  • A. G. Bogdanchikov,
  • C. Bohm,
  • V. Boisvert,
  • P. Bokan,
  • T. Bold,
  • M. Bomben,
  • M. Bona,
  • J. S. Bonilla,
  • M. Boonekamp,
  • C. D. Booth,
  • A. G. Borbély,
  • H. M. Borecka-Bielska,
  • L. S. Borgna,
  • G. Borissov,
  • D. Bortoletto,
  • D. Boscherini,
  • M. Bosman,
  • J. D. Bossio Sola,
  • K. Bouaouda,
  • J. Boudreau,
  • E. V. Bouhova-Thacker,
  • D. Boumediene,
  • R. Bouquet,
  • A. Boveia,
  • J. Boyd,
  • D. Boye,
  • I. R. Boyko,
  • A. J. Bozson,
  • J. Bracinik,
  • N. Brahimi,
  • G. Brandt,
  • O. Brandt,
  • F. Braren,
  • B. Brau,
  • J. E. Brau,
  • W. D. Breaden Madden,
  • K. Brendlinger,
  • R. Brener,
  • L. Brenner,
  • R. Brenner,
  • S. Bressler,
  • B. Brickwedde,
  • D. L. Briglin,
  • D. Britton,
  • D. Britzger,
  • I. Brock,
  • R. Brock,
  • G. Brooijmans,
  • W. K. Brooks,
  • E. Brost,
  • P. A. Bruckman de Renstrom,
  • B. Brüers,
  • D. Bruncko,
  • A. Bruni,
  • G. Bruni,
  • M. Bruschi,
  • N. Bruscino,
  • L. Bryngemark,
  • T. Buanes,
  • Q. Buat,
  • P. Buchholz,
  • A. G. Buckley,
  • I. A. Budagov,
  • M. K. Bugge,
  • O. Bulekov,
  • B. A. Bullard,
  • T. J. Burch,
  • S. Burdin,
  • C. D. Burgard,
  • A. M. Burger,
  • B. Burghgrave,
  • J. T. P. Burr,
  • C. D. Burton,
  • J. C. Burzynski,
  • V. Büscher,
  • E. Buschmann,
  • P. J. Bussey,
  • J. M. Butler,
  • C. M. Buttar,
  • J. M. Butterworth,
  • W. Buttinger,
  • C. J. Buxo Vazquez,
  • A. R. Buzykaev,
  • G. Cabras,
  • S. Cabrera Urbán,
  • D. Caforio,
  • H. Cai,
  • V. M. M. Cairo,
  • O. Cakir,
  • N. Calace,
  • P. Calafiura,
  • G. Calderini,
  • P. Calfayan,
  • G. Callea,
  • L. P. Caloba,
  • A. Caltabiano,
  • S. Calvente Lopez,
  • D. Calvet,
  • S. Calvet,
  • T. P. Calvet,
  • M. Calvetti,
  • R. Camacho Toro,
  • S. Camarda,
  • D. Camarero Munoz,
  • P. Camarri,
  • M. T. Camerlingo,
  • D. Cameron,
  • C. Camincher,
  • M. Campanelli,
  • A. Camplani,
  • V. Canale,
  • A. Canesse,
  • M. Cano Bret,
  • J. Cantero,
  • Y. Cao,
  • M. Capua,
  • R. Cardarelli,
  • F. Cardillo,
  • G. Carducci,
  • T. Carli,
  • G. Carlino,
  • B. T. Carlson,
  • E. M. Carlson,
  • L. Carminati,
  • M. Carnesale,
  • R. M. D. Carney,
  • S. Caron,
  • E. Carquin,
  • S. Carrá,
  • G. Carratta,
  • J. W. S. Carter,
  • T. M. Carter,
  • M. P. Casado,
  • A. F. Casha,
  • E. G. Castiglia,
  • F. L. Castillo,
  • L. Castillo Garcia,
  • V. Castillo Gimenez,
  • N. F. Castro,
  • A. Catinaccio,
  • J. R. Catmore,
  • A. Cattai,
  • V. Cavaliere,
  • V. Cavasinni,
  • E. Celebi,
  • F. Celli,
  • K. Cerny,
  • A. S. Cerqueira,
  • A. Cerri,
  • L. Cerrito,
  • F. Cerutti,
  • A. Cervelli,
  • S. A. Cetin,
  • Z. Chadi,
  • D. Chakraborty,
  • M. Chala,
  • J. Chan,
  • W. S. Chan,
  • W. Y. Chan,
  • J. D. Chapman,
  • B. Chargeishvili,
  • D. G. Charlton,
  • T. P. Charman,
  • M. Chatterjee,
  • C. C. Chau,
  • S. Chekanov,
  • S. V. Chekulaev,
  • G. A. Chelkov,
  • B. Chen,
  • C. Chen,
  • C. H. Chen,
  • H. Chen,
  • H. Chen,
  • J. Chen,
  • J. Chen,
  • J. Chen,
  • S. Chen,
  • S. J. Chen,
  • X. Chen,
  • Y. Chen,
  • Y. -H. Chen,
  • C. L. Cheng,
  • H. C. Cheng,
  • H. J. Cheng,
  • A. Cheplakov,
  • E. Cheremushkina,
  • R. Cherkaoui El Moursli,
  • E. Cheu,
  • K. Cheung,
  • L. Chevalier,
  • V. Chiarella,
  • G. Chiarelli,
  • G. Chiodini,
  • A. S. Chisholm,
  • A. Chitan,
  • I. Chiu,
  • Y. H. Chiu,
  • M. V. Chizhov,
  • K. Choi,
  • A. R. Chomont,
  • Y. Chou,
  • Y. S. Chow,
  • L. D. Christopher,
  • M. C. Chu,
  • X. Chu,
  • J. Chudoba,
  • J. J. Chwastowski,
  • D. Cieri,
  • K. M. Ciesla,
  • V. Cindro,
  • I. A. Cioarǎ,
  • A. Ciocio,
  • F. Cirotto,
  • Z. H. Citron,
  • M. Citterio,
  • D. A. Ciubotaru,
  • B. M. Ciungu,
  • A. Clark,
  • P. J. Clark,
  • S. E. Clawson,
  • C. Clement,
  • L. Clissa,
  • Y. Coadou,
  • M. Cobal,
  • A. Coccaro,
  • J. Cochran,
  • R. Coelho Lopes de Sa,
  • S. Coelli,
  • H. Cohen,
  • A. E. C. Coimbra,
  • B. Cole,
  • J. Collot,
  • P. Conde Muiño,
  • S. H. Connell,
  • I. A. Connelly,
  • F. Conventi,
  • A. M. Cooper-Sarkar,
  • F. Cormier,
  • L. D. Corpe,
  • M. Corradi,
  • E. E. Corrigan,
  • F. Corriveau,
  • M. J. Costa,
  • F. Costanza,
  • D. Costanzo,
  • G. Cowan,
  • J. W. Cowley,
  • J. Crane,
  • K. Cranmer,
  • R. A. Creager,
  • S. Crépé-Renaudin,
  • F. Crescioli,
  • M. Cristinziani,
  • M. Cristoforetti,
  • V. Croft,
  • G. Crosetti,
  • A. Cueto,
  • T. Cuhadar Donszelmann,
  • H. Cui,
  • A. R. Cukierman,
  • W. R. Cunningham,
  • S. Czekierda,
  • P. Czodrowski,
  • M. M. Czurylo,
  • M. J. da Cunha Sargedas de Sousa,
  • J. V. da Fonseca Pinto,
  • C. da Via,
  • W. Dabrowski,
  • T. Dado,
  • S. Dahbi,
  • T. Dai,
  • C. Dallapiccola,
  • M. Dam,
  • G. D'Amen,
  • V. D'Amico,
  • J. Damp,
  • J. R. Dandoy,
  • M. F. Daneri,
  • M. Danninger,
  • V. Dao,
  • G. Darbo,
  • A. Dattagupta,
  • S. D'Auria,
  • C. David,
  • T. Davidek,
  • D. R. Davis,
  • I. Dawson,
  • K. de,
  • R. de Asmundis,
  • M. de Beurs,
  • S. de Castro,
  • N. de Groot,
  • P. de Jong,
  • H. de la Torre,
  • A. de Maria,
  • D. de Pedis,
  • A. de Salvo,
  • U. de Sanctis,
  • M. de Santis,
  • A. de Santo,
  • J. B. de Vivie de Regie,
  • D. V. Dedovich,
  • J. Degens,
  • A. M. Deiana,
  • J. Del Peso,
  • Y. Delabat Diaz,
  • F. Deliot,
  • C. M. Delitzsch,
  • M. Della Pietra,
  • D. Della Volpe,
  • A. Dell'Acqua,
  • L. Dell'Asta,
  • M. Delmastro,
  • C. Delporte,
  • P. A. Delsart,
  • S. Demers,
  • M. Demichev,
  • G. Demontigny,
  • S. P. Denisov,
  • L. D'Eramo,
  • D. Derendarz,
  • J. E. Derkaoui,
  • F. Derue,
  • P. Dervan,
  • K. Desch,
  • K. Dette,
  • C. Deutsch,
  • P. O. Deviveiros,
  • F. A. di Bello,
  • A. di Ciaccio,
  • L. di Ciaccio,
  • C. di Donato,
  • A. di Girolamo,
  • G. di Gregorio,
  • A. di Luca,
  • B. di Micco,
  • R. di Nardo,
  • C. Diaconu,
  • F. A. Dias,
  • T. Dias Do Vale,
  • M. A. Diaz,
  • F. G. Diaz Capriles,
  • J. Dickinson,
  • M. Didenko,
  • E. B. Diehl,
  • J. Dietrich,
  • S. Díez Cornell,
  • C. Diez Pardos,
  • A. Dimitrievska,
  • W. Ding,
  • J. Dingfelder,
  • S. J. Dittmeier,
  • F. Dittus,
  • F. Djama,
  • T. Djobava,
  • J. I. Djuvsland,
  • M. A. B. Do Vale,
  • M. Dobre,
  • D. Dodsworth,
  • C. Doglioni,
  • J. Dolejsi,
  • Z. Dolezal,
  • M. Donadelli,
  • B. Dong,
  • J. Donini,
  • A. D'Onofrio,
  • M. D'Onofrio,
  • J. Dopke,
  • A. Doria,
  • M. T. Dova,
  • A. T. Doyle,
  • E. Drechsler,
  • E. Dreyer,
  • T. Dreyer,
  • A. S. Drobac,
  • D. Du,
  • T. A. Du Pree,
  • Y. Duan,
  • F. Dubinin,
  • M. Dubovsky,
  • A. Dubreuil,
  • E. Duchovni,
  • G. Duckeck,
  • O. A. Ducu,
  • D. Duda,
  • A. Dudarev,
  • A. C. Dudder,
  • M. D'Uffizi,
  • L. Duflot,
  • M. Dührssen,
  • C. Dülsen,
  • M. Dumancic,
  • A. E. Dumitriu,
  • M. Dunford,
  • S. Dungs,
  • A. Duperrin,
  • H. Duran Yildiz,
  • M. Düren,
  • A. Durglishvili,
  • B. Dutta,
  • D. Duvnjak,
  • G. I. Dyckes,
  • M. Dyndal,
  • S. Dysch,
  • B. S. Dziedzic,
  • B. Eckerova,
  • M. G. Eggleston,
  • L. F. Ehrke,
  • T. Eifert,
  • G. Eigen,
  • K. Einsweiler,
  • T. Ekelof,
  • H. El Jarrari,
  • A. El Moussaouy,
  • V. Ellajosyula,
  • M. Ellert,
  • F. Ellinghaus,
  • A. A. Elliot,
  • N. Ellis,
  • J. Elmsheuser,
  • M. Elsing,
  • D. Emeliyanov,
  • A. Emerman,
  • Y. Enari,
  • J. Erdmann,
  • A. Ereditato,
  • P. A. Erland,
  • M. Errenst,
  • M. Escalier,
  • C. Escobar,
  • O. Estrada Pastor,
  • E. Etzion,
  • G. Evans,
  • H. Evans,
  • M. O. Evans,
  • A. Ezhilov,
  • F. Fabbri,
  • L. Fabbri,
  • V. Fabiani,
  • G. Facini,
  • R. M. Fakhrutdinov,
  • S. Falciano,
  • P. J. Falke,
  • S. Falke,
  • J. Faltova,
  • Y. Fang,
  • Y. Fang,
  • G. Fanourakis,
  • M. Fanti,
  • M. Faraj,
  • A. Farbin,
  • A. Farilla,
  • E. M. Farina,
  • T. Farooque,
  • S. M. Farrington,
  • P. Farthouat,
  • F. Fassi,
  • D. Fassouliotis,
  • M. Faucci Giannelli,
  • W. J. Fawcett,
  • L. Fayard,
  • O. L. Fedin,
  • A. Fehr,
  • M. Feickert,
  • L. Feligioni,
  • A. Fell,
  • C. Feng,
  • M. Feng,
  • M. J. Fenton,
  • A. B. Fenyuk,
  • S. W. Ferguson,
  • J. Ferrando,
  • A. Ferrari,
  • P. Ferrari,
  • R. Ferrari,
  • D. Ferrere,
  • C. Ferretti,
  • F. Fiedler,
  • A. Filipčič,
  • F. Filthaut,
  • K. D. Finelli,
  • M. C. N. Fiolhais,
  • L. Fiorini,
  • F. Fischer,
  • J. Fischer,
  • W. C. Fisher,
  • T. Fitschen,
  • I. Fleck,
  • P. Fleischmann,
  • T. Flick,
  • B. M. Flierl,
  • L. Flores,
  • L. R. Flores Castillo,
  • F. M. Follega,
  • N. Fomin,
  • J. H. Foo,
  • G. T. Forcolin,
  • B. C. Forland,
  • A. Formica,
  • F. A. Förster,
  • A. C. Forti,
  • E. Fortin,
  • M. G. Foti,
  • D. Fournier,
  • H. Fox,
  • P. Francavilla,
  • S. Francescato,
  • M. Franchini,
  • S. Franchino,
  • D. Francis,
  • L. Franco,
  • L. Franconi,
  • M. Franklin,
  • G. Frattari,
  • P. M. Freeman,
  • B. Freund,
  • W. S. Freund,
  • E. M. Freundlich,
  • D. C. Frizzell,
  • D. Froidevaux,
  • J. A. Frost,
  • Y. Fu,
  • M. Fujimoto,
  • E. Fullana Torregrosa,
  • T. Fusayasu,
  • J. Fuster,
  • A. Gabrielli,
  • A. Gabrielli,
  • P. Gadow,
  • G. Gagliardi,
  • L. G. Gagnon,
  • G. E. Gallardo,
  • E. J. Gallas,
  • B. J. Gallop,
  • R. Gamboa Goni,
  • K. K. Gan,
  • S. Ganguly,
  • J. Gao,
  • Y. Gao,
  • Y. S. Gao,
  • F. M. Garay Walls,
  • C. García,
  • J. E. García Navarro,
  • J. A. García Pascual,
  • M. Garcia-Sciveres,
  • R. W. Gardner,
  • S. Gargiulo,
  • C. A. Garner,
  • V. Garonne,
  • S. J. Gasiorowski,
  • P. Gaspar,
  • G. Gaudio,
  • P. Gauzzi,
  • I. L. Gavrilenko,
  • A. Gavrilyuk,
  • C. Gay,
  • G. Gaycken,
  • E. N. Gazis,
  • A. A. Geanta,
  • C. M. Gee,
  • C. N. P. Gee,
  • J. Geisen,
  • M. Geisen,
  • C. Gemme,
  • M. H. Genest,
  • C. Geng,
  • S. Gentile,
  • S. George,
  • T. Geralis,
  • L. O. Gerlach,
  • P. Gessinger-Befurt,
  • G. Gessner,
  • M. Ghasemi Bostanabad,
  • M. Ghneimat,
  • A. Ghosh,
  • A. Ghosh,
  • B. Giacobbe,
  • S. Giagu,
  • N. Giangiacomi,
  • P. Giannetti,
  • A. Giannini,
  • S. M. Gibson,
  • M. Gignac,
  • D. T. Gil,
  • B. J. Gilbert,
  • D. Gillberg,
  • G. Gilles,
  • N. E. K. Gillwald,
  • D. M. Gingrich,
  • M. P. Giordani,
  • P. F. Giraud,
  • G. Giugliarelli,
  • D. Giugni,
  • F. Giuli,
  • S. Gkaitatzis,
  • I. Gkialas,
  • E. L. Gkougkousis,
  • P. Gkountoumis,
  • L. K. Gladilin,
  • C. Glasman,
  • G. R. Gledhill,
  • I. Gnesi,
  • M. Goblirsch-Kolb,
  • D. Godin,
  • S. Goldfarb,
  • T. Golling,
  • D. Golubkov,
  • A. Gomes,
  • R. Goncalves Gama,
  • R. Gonçalo,
  • G. Gonella,
  • L. Gonella,
  • A. Gongadze,
  • F. Gonnella,
  • J. L. Gonski,
  • S. González de La Hoz,
  • S. Gonzalez Fernandez,
  • R. Gonzalez Lopez,
  • C. Gonzalez Renteria,
  • R. Gonzalez Suarez,
  • S. Gonzalez-Sevilla,
  • G. R. Gonzalvo Rodriguez,
  • L. Goossens,
  • N. A. Gorasia,
  • P. A. Gorbounov,
  • H. A. Gordon,
  • B. Gorini,
  • E. Gorini,
  • A. Gorišek,
  • A. T. Goshaw,
  • M. I. Gostkin,
  • C. A. Gottardo,
  • M. Gouighri,
  • A. G. Goussiou,
  • N. Govender,
  • C. Goy,
  • I. Grabowska-Bold,
  • E. Gramstad,
  • S. Grancagnolo,
  • M. Grandi,
  • V. Gratchev,
  • P. M. Gravila,
  • F. G. Gravili,
  • C. Gray,
  • H. M. Gray,
  • C. Grefe,
  • I. M. Gregor,
  • P. Grenier,
  • K. Grevtsov,
  • C. Grieco,
  • N. A. Grieser,
  • A. A. Grillo,
  • K. Grimm,
  • S. Grinstein,
  • J. -F. Grivaz,
  • S. Groh,
  • E. Gross,
  • J. Grosse-Knetter,
  • Z. J. Grout,
  • C. Grud,
  • A. Grummer,
  • J. C. Grundy,
  • L. Guan,
  • W. Guan,
  • C. Gubbels,
  • J. Guenther,
  • J. G. R. Guerrero Rojas,
  • F. Guescini,
  • D. Guest,
  • R. Gugel,
  • A. Guida,
  • T. Guillemin,
  • S. Guindon,
  • J. Guo,
  • L. Guo,
  • Y. Guo,
  • Z. Guo,
  • R. Gupta,
  • S. Gurbuz,
  • G. Gustavino,
  • M. Guth,
  • P. Gutierrez,
  • L. F. Gutierrez Zagazeta,
  • C. Gutschow,
  • C. Guyot,
  • C. Gwenlan,
  • C. B. Gwilliam,
  • E. S. Haaland,
  • A. Haas,
  • M. H. Habedank,
  • C. Haber,
  • H. K. Hadavand,
  • A. Hadef,
  • M. Haleem,
  • J. Haley,
  • J. J. Hall,
  • G. Halladjian,
  • G. D. Hallewell,
  • K. Hamano,
  • H. Hamdaoui,
  • M. Hamer,
  • G. N. Hamity,
  • K. Han,
  • L. Han,
  • L. Han,
  • S. Han,
  • Y. F. Han,
  • K. Hanagaki,
  • M. Hance,
  • M. D. Hank,
  • R. Hankache,
  • E. Hansen,
  • J. B. Hansen,
  • J. D. Hansen,
  • M. C. Hansen,
  • P. H. Hansen,
  • E. C. Hanson,
  • K. Hara,
  • T. Harenberg,
  • S. Harkusha,
  • P. F. Harrison,
  • N. M. Hartman,
  • N. M. Hartmann,
  • Y. Hasegawa,
  • A. Hasib,
  • S. Hassani,
  • S. Haug,
  • R. Hauser,
  • M. Havranek,
  • C. M. Hawkes,
  • R. J. Hawkings,
  • S. Hayashida,
  • D. Hayden,
  • C. Hayes,
  • R. L. Hayes,
  • C. P. Hays,
  • J. M. Hays,
  • H. S. Hayward,
  • S. J. Haywood,
  • F. He,
  • Y. He,
  • Y. He,
  • M. P. Heath,
  • V. Hedberg,
  • A. L. Heggelund,
  • N. D. Hehir,
  • C. Heidegger,
  • K. K. Heidegger,
  • W. D. Heidorn,
  • J. Heilman,
  • S. Heim,
  • T. Heim,
  • B. Heinemann,
  • J. G. Heinlein,
  • J. J. Heinrich,
  • L. Heinrich,
  • J. Hejbal,
  • L. Helary,
  • A. Held,
  • S. Hellesund,
  • C. M. Helling,
  • S. Hellman,
  • C. Helsens,
  • R. C. W. Henderson,
  • L. Henkelmann,
  • A. M. Henriques Correia,
  • H. Herde,
  • Y. Hernández Jiménez,
  • H. Herr,
  • M. G. Herrmann,
  • T. Herrmann,
  • G. Herten,
  • R. Hertenberger,
  • L. Hervas,
  • N. P. Hessey,
  • H. Hibi,
  • S. Higashino,
  • E. Higón-Rodriguez,
  • K. Hildebrand,
  • K. K. Hill,
  • K. H. Hiller,
  • S. J. Hillier,
  • M. Hils,
  • I. Hinchliffe,
  • F. Hinterkeuser,
  • M. Hirose,
  • S. Hirose,
  • D. Hirschbuehl,
  • B. Hiti,
  • O. Hladik,
  • J. Hobbs,
  • R. Hobincu,
  • N. Hod,
  • M. C. Hodgkinson,
  • A. Hoecker,
  • D. Hohn,
  • T. Holm,
  • T. R. Holmes,
  • M. Holzbock,
  • L. B. A. H. Hommels,
  • T. M. Hong,
  • J. C. Honig,
  • A. Hönle,
  • B. H. Hooberman,
  • W. H. Hopkins,
  • Y. Horii,
  • P. Horn,
  • L. A. Horyn,
  • S. Hou,
  • J. Howarth,
  • J. Hoya,
  • M. Hrabovsky,
  • A. Hrynevich,
  • T. Hryn'ova,
  • P. J. Hsu,
  • S. -C. Hsu,
  • Q. Hu,
  • S. Hu,
  • Y. F. Hu,
  • D. P. Huang,
  • X. Huang,
  • Y. Huang,
  • Y. Huang,
  • Z. Hubacek,
  • F. Hubaut,
  • M. Huebner,
  • F. Huegging,
  • T. B. Huffman,
  • M. Huhtinen,
  • R. Hulsken,
  • R. F. H. Hunter,
  • N. Huseynov,
  • J. Huston,
  • J. Huth,
  • R. Hyneman,
  • S. Hyrych,
  • G. Iacobucci,
  • G. Iakovidis,
  • I. Ibragimov,
  • L. Iconomidou-Fayard,
  • P. Iengo,
  • R. Ignazzi,
  • R. Iguchi,
  • T. Iizawa,
  • Y. Ikegami,
  • N. Ilic,
  • H. Imam,
  • G. Introzzi,
  • M. Iodice,
  • K. Iordanidou,
  • V. Ippolito,
  • M. Ishino,
  • W. Islam,
  • C. Issever,
  • S. Istin,
  • J. M. Iturbe Ponce,
  • R. Iuppa,
  • A. Ivina,
  • J. M. Izen,
  • V. Izzo,
  • P. Jacka,
  • P. Jackson,
  • R. M. Jacobs,
  • B. P. Jaeger,
  • G. Jäkel,
  • K. B. Jakobi,
  • K. Jakobs,
  • T. Jakoubek,
  • J. Jamieson,
  • K. W. Janas,
  • P. A. Janus,
  • G. Jarlskog,
  • A. E. Jaspan,
  • N. Javadov,
  • T. Javå¯Rek,
  • M. Javurkova,
  • F. Jeanneau,
  • L. Jeanty,
  • J. Jejelava,
  • P. Jenni,
  • S. Jézéquel,
  • J. Jia,
  • Z. Jia,
  • Y. Jiang,
  • S. Jiggins,
  • F. A. Jimenez Morales,
  • J. Jimenez Pena,
  • S. Jin,
  • A. Jinaru,
  • O. Jinnouchi,
  • H. Jivan,
  • P. Johansson,
  • K. A. Johns,
  • C. A. Johnson,
  • E. Jones,
  • R. W. L. Jones,
  • T. J. Jones,
  • J. Jovicevic,
  • X. Ju,
  • J. J. Junggeburth,
  • A. Juste Rozas,
  • A. Kaczmarska,
  • M. Kado,
  • H. Kagan,
  • M. Kagan,
  • A. Kahn,
  • C. Kahra,
  • T. Kaji,
  • E. Kajomovitz,
  • C. W. Kalderon,
  • A. Kaluza,
  • A. Kamenshchikov,
  • M. Kaneda,
  • N. J. Kang,
  • S. Kang,
  • Y. Kano,
  • J. Kanzaki,
  • D. Kar,
  • K. Karava,
  • M. J. Kareem,
  • I. Karkanias,
  • S. N. Karpov,
  • Z. M. Karpova,
  • V. Kartvelishvili,
  • A. N. Karyukhin,
  • E. Kasimi,
  • C. Kato,
  • J. Katzy,
  • K. Kawade,
  • K. Kawagoe,
  • T. Kawaguchi,
  • T. Kawamoto,
  • G. Kawamura,
  • E. F. Kay,
  • F. I. Kaya,
  • S. Kazakos,
  • V. F. Kazanin,
  • Y. Ke,
  • J. M. Keaveney,
  • R. Keeler,
  • J. S. Keller,
  • D. Kelsey,
  • J. J. Kempster,
  • J. Kendrick,
  • K. E. Kennedy,
  • O. Kepka,
  • S. Kersten,
  • B. P. Kerševan,
  • S. Ketabchi Haghighat,
  • F. Khalil-Zada,
  • M. Khandoga,
  • A. Khanov,
  • A. G. Kharlamov,
  • T. Kharlamova,
  • E. E. Khoda,
  • T. J. Khoo,
  • G. Khoriauli,
  • E. Khramov,
  • J. Khubua,
  • S. Kido,
  • M. Kiehn,
  • A. Kilgallon,
  • E. Kim,
  • Y. K. Kim,
  • N. Kimura,
  • A. Kirchhoff,
  • D. Kirchmeier,
  • J. Kirk,
  • A. E. Kiryunin,
  • T. Kishimoto,
  • D. P. Kisliuk,
  • V. Kitali,
  • C. Kitsaki,
  • O. Kivernyk,
  • T. Klapdor-Kleingrothaus,
  • M. Klassen,
  • C. Klein,
  • L. Klein,
  • M. H. Klein,
  • M. Klein,
  • U. Klein,
  • P. Klimek,
  • A. Klimentov,
  • F. Klimpel,
  • T. Klingl,
  • T. Klioutchnikova,
  • F. F. Klitzner,
  • P. Kluit,
  • S. Kluth,
  • E. Kneringer,
  • A. Knue,
  • D. Kobayashi,
  • M. Kobel,
  • M. Kocian,
  • T. Kodama,
  • P. Kodys,
  • D. M. Koeck,
  • P. T. Koenig,
  • T. Koffas,
  • N. M. Köhler,
  • M. Kolb,
  • I. Koletsou,
  • T. Komarek,
  • K. Köneke,
  • A. X. Y. Kong,
  • T. Kono,
  • V. Konstantinides,
  • N. Konstantinidis,
  • B. Konya,
  • R. Kopeliansky,
  • S. Koperny,
  • K. Korcyl,
  • K. Kordas,
  • G. Koren,
  • A. Korn,
  • S. Korn,
  • I. Korolkov,
  • E. V. Korolkova,
  • N. Korotkova,
  • O. Kortner,
  • S. Kortner,
  • V. V. Kostyukhin,
  • A. Kotsokechagia,
  • A. Kotwal,
  • A. Koulouris,
  • A. Kourkoumeli-Charalampidi,
  • C. Kourkoumelis,
  • E. Kourlitis,
  • R. Kowalewski,
  • W. Kozanecki,
  • A. S. Kozhin,
  • V. A. Kramarenko,
  • G. Kramberger,
  • D. Krasnopevtsev,
  • M. W. Krasny,
  • A. Krasznahorkay,
  • J. A. Kremer,
  • J. Kretzschmar,
  • K. Kreul,
  • P. Krieger,
  • F. Krieter,
  • S. Krishnamurthy,
  • A. Krishnan,
  • M. Krivos,
  • K. Krizka,
  • K. Kroeninger,
  • H. Kroha,
  • J. Kroll,
  • J. Kroll,
  • K. S. Krowpman,
  • U. Kruchonak,
  • H. Krüger,
  • N. Krumnack,
  • M. C. Kruse,
  • J. A. Krzysiak,
  • A. Kubota,
  • O. Kuchinskaia,
  • S. Kuday,
  • D. Kuechler,
  • J. T. Kuechler,
  • S. Kuehn,
  • T. Kuhl,
  • V. Kukhtin,
  • Y. Kulchitsky,
  • S. Kuleshov,
  • M. Kumar,
  • M. Kuna,
  • A. Kupco,
  • T. Kupfer,
  • O. Kuprash,
  • H. Kurashige,
  • L. L. Kurchaninov,
  • Y. A. Kurochkin,
  • A. Kurova,
  • M. G. Kurth,
  • E. S. Kuwertz,
  • M. Kuze,
  • A. K. Kvam,
  • J. Kvita,
  • T. Kwan,
  • C. Lacasta,
  • F. Lacava,
  • D. P. J. Lack,
  • H. Lacker,
  • D. Lacour,
  • E. Ladygin,
  • R. Lafaye,
  • B. Laforge,
  • T. Lagouri,
  • S. Lai,
  • I. K. Lakomiec,
  • J. E. Lambert,
  • S. Lammers,
  • W. Lampl,
  • C. Lampoudis,
  • E. Lançon,
  • U. Landgraf,
  • M. P. J. Landon,
  • V. S. Lang,
  • J. C. Lange,
  • R. J. Langenberg,
  • A. J. Lankford,
  • F. Lanni,
  • K. Lantzsch,
  • A. Lanza,
  • A. Lapertosa,
  • J. F. Laporte,
  • T. Lari,
  • F. Lasagni Manghi,
  • M. Lassnig,
  • V. Latonova,
  • T. S. Lau,
  • A. Laudrain,
  • A. Laurier,
  • M. Lavorgna,
  • S. D. Lawlor,
  • M. Lazzaroni,
  • B. Le,
  • A. Lebedev,
  • M. Leblanc,
  • T. Lecompte,
  • F. Ledroit-Guillon,
  • A. C. A. Lee,
  • C. A. Lee,
  • G. R. Lee,
  • L. Lee,
  • S. C. Lee,
  • S. Lee,
  • L. L. Leeuw,
  • B. Lefebvre,
  • H. P. Lefebvre,
  • M. Lefebvre,
  • C. Leggett,
  • K. Lehmann,
  • N. Lehmann,
  • G. Lehmann Miotto,
  • W. A. Leight,
  • A. Leisos,
  • M. A. L. Leite,
  • C. E. Leitgeb,
  • R. Leitner,
  • K. J. C. Leney,
  • T. Lenz,
  • S. Leone,
  • C. Leonidopoulos,
  • A. Leopold,
  • C. Leroy,
  • R. Les,
  • C. G. Lester,
  • M. Levchenko,
  • J. Levêque,
  • D. Levin,
  • L. J. Levinson,
  • D. J. Lewis,
  • B. Li,
  • B. Li,
  • C. -Q. Li,
  • F. Li,
  • H. Li,
  • H. Li,
  • J. Li,
  • K. Li,
  • L. Li,
  • M. Li,
  • Q. Y. Li,
  • S. Li,
  • X. Li,
  • Y. Li,
  • Z. Li,
  • Z. Li,
  • Z. Li,
  • Z. Li,
  • Z. Liang,
  • M. Liberatore,
  • B. Liberti,
  • K. Lie,
  • C. Y. Lin,
  • K. Lin,
  • R. A. Linck,
  • R. E. Lindley,
  • J. H. Lindon,
  • A. Linss,
  • A. L. Lionti,
  • E. Lipeles,
  • A. Lipniacka,
  • T. M. Liss,
  • A. Lister,
  • J. D. Little,
  • B. Liu,
  • B. X. Liu,
  • J. B. Liu,
  • J. K. K. Liu,
  • K. Liu,
  • M. Liu,
  • M. Y. Liu,
  • P. Liu,
  • X. Liu,
  • Y. Liu,
  • Y. Liu,
  • Y. L. Liu,
  • Y. W. Liu,
  • M. Livan,
  • A. Lleres,
  • J. Llorente Merino,
  • S. L. Lloyd,
  • E. M. Lobodzinska,
  • P. Loch,
  • S. Loffredo,
  • T. Lohse,
  • K. Lohwasser,
  • M. Lokajicek,
  • J. D. Long,
  • R. E. Long,
  • I. Longarini,
  • L. Longo,
  • R. Longo,
  • I. Lopez Paz,
  • A. Lopez Solis,
  • J. Lorenz,
  • N. Lorenzo Martinez,
  • A. M. Lory,
  • A. Lösle,
  • X. Lou,
  • X. Lou,
  • A. Lounis,
  • J. Love,
  • P. A. Love,
  • J. J. Lozano Bahilo,
  • G. Lu,
  • M. Lu,
  • S. Lu,
  • Y. J. Lu,
  • H. J. Lubatti,
  • C. Luci,
  • F. L. Lucio Alves,
  • A. Lucotte,
  • F. Luehring,
  • I. Luise,
  • L. Luminari,
  • B. Lund-Jensen,
  • N. A. Luongo,
  • M. S. Lutz,
  • D. Lynn,
  • H. Lyons,
  • R. Lysak,
  • E. Lytken,
  • F. Lyu,
  • V. Lyubushkin,
  • T. Lyubushkina,
  • H. Ma,
  • L. L. Ma,
  • Y. Ma,
  • D. M. Mac Donell,
  • G. Maccarrone,
  • C. M. MacDonald,
  • J. C. MacDonald,
  • J. Machado Miguens,
  • R. Madar,
  • W. F. Mader,
  • M. Madugoda Ralalage Don,
  • N. Madysa,
  • J. Maeda,
  • T. Maeno,
  • M. Maerker,
  • V. Magerl,
  • J. Magro,
  • D. J. Mahon,
  • C. Maidantchik,
  • A. Maio,
  • K. Maj,
  • O. Majersky,
  • S. Majewski,
  • N. Makovec,
  • B. Malaescu,
  • Pa. Malecki,
  • V. P. Maleev,
  • F. Malek,
  • D. Malito,
  • U. Mallik,
  • C. Malone,
  • S. Maltezos,
  • S. Malyukov,
  • J. Mamuzic,
  • G. Mancini,
  • J. P. Mandalia,
  • I. Mandić,
  • L. Manhaes de Andrade Filho,
  • I. M. Maniatis,
  • M. Manisha,
  • J. Manjarres Ramos,
  • K. H. Mankinen,
  • A. Mann,
  • A. Manousos,
  • B. Mansoulie,
  • I. Manthos,
  • S. Manzoni,
  • A. Marantis,
  • L. Marchese,
  • G. Marchiori,
  • M. Marcisovsky,
  • L. Marcoccia,
  • C. Marcon,
  • M. Marjanovic,
  • Z. Marshall,
  • M. U. F. Martensson,
  • S. Marti-Garcia,
  • T. A. Martin,
  • V. J. Martin,
  • B. Martin Dit Latour,
  • L. Martinelli,
  • M. Martinez,
  • P. Martinez Agullo,
  • V. I. Martinez Outschoorn,
  • S. Martin-Haugh,
  • V. S. Martoiu,
  • A. C. Martyniuk,
  • A. Marzin,
  • S. R. Maschek,
  • L. Masetti,
  • T. Mashimo,
  • R. Mashinistov,
  • J. Masik,
  • A. L. Maslennikov,
  • L. Massa,
  • P. Massarotti,
  • P. Mastrandrea,
  • A. Mastroberardino,
  • T. Masubuchi,
  • D. Matakias,
  • T. Mathisen,
  • A. Matic,
  • N. Matsuzawa,
  • J. Maurer,
  • B. Maček,
  • D. A. Maximov,
  • R. Mazini,
  • I. Maznas,
  • S. M. Mazza,
  • C. Mc Ginn,
  • J. P. Mc Gowan,
  • S. P. Mc Kee,
  • T. G. McCarthy,
  • W. P. McCormack,
  • E. F. McDonald,
  • A. E. McDougall,
  • J. A. McFayden,
  • G. McHedlidze,
  • M. A. McKay,
  • K. D. McLean,
  • S. J. McMahon,
  • P. C. McNamara,
  • R. A. McPherson,
  • J. E. Mdhluli,
  • Z. A. Meadows,
  • S. Meehan,
  • T. Megy,
  • S. Mehlhase,
  • A. Mehta,
  • B. Meirose,
  • D. Melini,
  • B. R. Mellado Garcia,
  • F. Meloni,
  • A. Melzer,
  • E. D. Mendes Gouveia,
  • A. M. Mendes Jacques da Costa,
  • H. Y. Meng,
  • L. Meng,
  • S. Menke,
  • E. Meoni,
  • S. A. M. Merkt,
  • C. Merlassino,
  • P. Mermod,
  • L. Merola,
  • C. Meroni,
  • G. Merz,
  • O. Meshkov,
  • J. K. R. Meshreki,
  • J. Metcalfe,
  • A. S. Mete,
  • C. Meyer,
  • J. -P. Meyer,
  • M. Michetti,
  • R. P. Middleton,
  • L. Mijović,
  • G. Mikenberg,
  • M. Mikestikova,
  • M. Mikuž,
  • H. Mildner,
  • A. Milic,
  • C. D. Milke,
  • D. W. Miller,
  • L. S. Miller,
  • A. Milov,
  • D. A. Milstead,
  • A. A. Minaenko,
  • I. A. Minashvili,
  • L. Mince,
  • A. I. Mincer,
  • B. Mindur,
  • M. Mineev,
  • Y. Minegishi,
  • Y. Mino,
  • L. M. Mir,
  • M. Miralles Lopez,
  • M. Mironova,
  • T. Mitani,
  • V. A. Mitsou,
  • M. Mittal,
  • O. Miu,
  • A. Miucci,
  • P. S. Miyagawa,
  • A. Mizukami,
  • J. U. Mjörnmark,
  • T. Mkrtchyan,
  • M. Mlynarikova,
  • T. Moa,
  • S. Mobius,
  • K. Mochizuki,
  • P. Moder,
  • P. Mogg,
  • S. Mohapatra,
  • G. Mokgatitswane,
  • B. Mondal,
  • S. Mondal,
  • K. Mönig,
  • E. Monnier,
  • A. Montalbano,
  • J. Montejo Berlingen,
  • M. Montella,
  • F. Monticelli,
  • N. Morange,
  • A. L. Moreira de Carvalho,
  • M. Moreno Llácer,
  • C. Moreno Martinez,
  • P. Morettini,
  • M. Morgenstern,
  • S. Morgenstern,
  • D. Mori,
  • M. Morii,
  • M. Morinaga,
  • V. Morisbak,
  • A. K. Morley,
  • A. P. Morris,
  • L. Morvaj,
  • P. Moschovakos,
  • B. Moser,
  • M. Mosidze,
  • T. Moskalets,
  • P. Moskvitina,
  • J. Moss,
  • E. J. W. Moyse,
  • S. Muanza,
  • J. Mueller,
  • D. Muenstermann,
  • G. A. Mullier,
  • J. J. Mullin,
  • D. P. Mungo,
  • J. L. Munoz Martinez,
  • F. J. Munoz Sanchez,
  • P. Murin,
  • W. J. Murray,
  • A. Murrone,
  • J. M. Muse,
  • M. Muškinja,
  • C. Mwewa,
  • A. G. Myagkov,
  • A. A. Myers,
  • G. Myers,
  • J. Myers,
  • M. Myska,
  • B. P. Nachman,
  • O. Nackenhorst,
  • A. Nag Nag,
  • K. Nagai,
  • K. Nagano,
  • J. L. Nagle,
  • E. Nagy,
  • A. M. Nairz,
  • Y. Nakahama,
  • K. Nakamura,
  • H. Nanjo,
  • F. Napolitano,
  • R. F. Naranjo Garcia,
  • R. Narayan,
  • I. Naryshkin,
  • M. Naseri,
  • T. Naumann,
  • G. Navarro,
  • J. Navarro-Gonzalez,
  • P. Y. Nechaeva,
  • F. Nechansky,
  • T. J. Neep,
  • A. Negri,
  • M. Negrini,
  • C. Nellist,
  • C. Nelson,
  • K. Nelson,
  • M. E. Nelson,
  • S. Nemecek,
  • M. Nessi,
  • M. S. Neubauer,
  • F. Neuhaus,
  • M. Neumann,
  • R. Newhouse,
  • P. R. Newman,
  • C. W. Ng,
  • Y. S. Ng,
  • Y. W. Y. Ng,
  • B. Ngair,
  • H. D. N. Nguyen,
  • T. Nguyen Manh,
  • E. Nibigira,
  • R. B. Nickerson,
  • R. Nicolaidou,
  • D. S. Nielsen,
  • J. Nielsen,
  • M. Niemeyer,
  • N. Nikiforou,
  • V. Nikolaenko,
  • I. Nikolic-Audit,
  • K. Nikolopoulos,
  • P. Nilsson,
  • H. R. Nindhito,
  • A. Nisati,
  • N. Nishu,
  • R. Nisius,
  • T. Nitta,
  • T. Nobe,
  • D. L. Noel,
  • Y. Noguchi,
  • I. Nomidis,
  • M. A. Nomura,
  • R. R. B. Norisam,
  • J. Novak,
  • T. Novak,
  • O. Novgorodova,
  • R. Novotny,
  • L. Nozka,
  • K. Ntekas,
  • E. Nurse,
  • F. G. Oakham,
  • J. Ocariz,
  • A. Ochi,
  • I. Ochoa,
  • J. P. Ochoa-Ricoux,
  • K. O'Connor,
  • S. Oda,
  • S. Odaka,
  • S. Oerdek,
  • A. Ogrodnik,
  • A. Oh,
  • C. C. Ohm,
  • H. Oide,
  • R. Oishi,
  • M. L. Ojeda,
  • Y. Okazaki,
  • M. W. O'Keefe,
  • Y. Okumura,
  • A. Olariu,
  • L. F. Oleiro Seabra,
  • S. A. Olivares Pino,
  • D. Oliveira Damazio,
  • D. Oliveira Goncalves,
  • J. L. Oliver,
  • M. J. R. Olsson,
  • A. Olszewski,
  • J. Olszowska,
  • Ö. O. Ïncel,
  • D. C. O'Neil,
  • A. P. O'Neill,
  • A. Onofre,
  • P. U. E. Onyisi,
  • H. Oppen,
  • R. G. Oreamuno Madriz,
  • M. J. Oreglia,
  • G. E. Orellana,
  • D. Orestano,
  • N. Orlando,
  • R. S. Orr,
  • V. O'Shea,
  • R. Ospanov,
  • G. Otero Y. Garzon,
  • H. Otono,
  • P. S. Ott,
  • G. J. Ottino,
  • M. Ouchrif,
  • J. Ouellette,
  • F. Ould-Saada,
  • A. Ouraou,
  • Q. Ouyang,
  • M. Owen,
  • R. E. Owen,
  • V. E. Ozcan,
  • N. Ozturk,
  • J. Pacalt,
  • H. A. Pacey,
  • K. Pachal,
  • A. Pacheco Pages,
  • C. Padilla Aranda,
  • S. Pagan Griso,
  • G. Palacino,
  • S. Palazzo,
  • S. Palestini,
  • M. Palka,
  • P. Palni,
  • D. K. Panchal,
  • C. E. Pandini,
  • J. G. Panduro Vazquez,
  • P. Pani,
  • G. Panizzo,
  • L. Paolozzi,
  • C. Papadatos,
  • S. Parajuli,
  • A. Paramonov,
  • C. Paraskevopoulos,
  • D. Paredes Hernandez,
  • S. R. Paredes Saenz,
  • B. Parida,
  • T. H. Park,
  • A. J. Parker,
  • M. A. Parker,
  • F. Parodi,
  • E. W. Parrish,
  • J. A. Parsons,
  • U. Parzefall,
  • L. Pascual Dominguez,
  • V. R. Pascuzzi,
  • J. M. P. Pasner,
  • F. Pasquali,
  • E. Pasqualucci,
  • S. Passaggio,
  • F. Pastore,
  • P. Pasuwan,
  • J. R. Pater,
  • A. Pathak,
  • J. Patton,
  • T. Pauly,
  • J. Pearkes,
  • M. Pedersen,
  • L. Pedraza Diaz,
  • R. Pedro,
  • T. Peiffer,
  • S. V. Peleganchuk,
  • O. Penc,
  • C. Peng,
  • H. Peng,
  • M. Penzin,
  • B. S. Peralva,
  • M. M. Perego,
  • A. P. Pereira Peixoto,
  • L. Pereira Sanchez,
  • D. V. Perepelitsa,
  • E. Perez Codina,
  • M. Perganti,
  • L. Perini,
  • H. Pernegger,
  • S. Perrella,
  • A. Perrevoort,
  • K. Peters,
  • R. F. Y. Peters,
  • B. A. Petersen,
  • T. C. Petersen,
  • E. Petit,
  • V. Petousis,
  • C. Petridou,
  • P. Petroff,
  • F. Petrucci,
  • M. Pettee,
  • N. E. Pettersson,
  • K. Petukhova,
  • A. Peyaud,
  • R. Pezoa,
  • L. Pezzotti,
  • G. Pezzullo,
  • T. Pham,
  • P. W. Phillips,
  • M. W. Phipps,
  • G. Piacquadio,
  • E. Pianori,
  • A. Picazio,
  • R. Piegaia,
  • D. Pietreanu,
  • J. E. Pilcher,
  • A. D. Pilkington,
  • M. Pinamonti,
  • J. L. Pinfold,
  • C. Pitman Donaldson,
  • D. A. Pizzi,
  • L. Pizzimento,
  • A. Pizzini,
  • M. -A. Pleier,
  • V. Plesanovs,
  • V. Pleskot,
  • E. Plotnikova,
  • P. Podberezko,
  • R. Poettgen,
  • R. Poggi,
  • L. Poggioli,
  • I. Pogrebnyak,
  • D. Pohl,
  • I. Pokharel,
  • G. Polesello,
  • A. Poley,
  • A. Policicchio,
  • R. Polifka,
  • A. Polini,
  • C. S. Pollard,
  • V. Polychronakos,
  • D. Ponomarenko,
  • L. Pontecorvo,
  • S. Popa,
  • G. A. Popeneciu,
  • L. Portales,
  • D. M. Portillo Quintero,
  • S. Pospisil,
  • P. Postolache,
  • K. Potamianos,
  • I. N. Potrap,
  • C. J. Potter,
  • H. Potti,
  • T. Poulsen,
  • J. Poveda,
  • T. D. Powell,
  • G. Pownall,
  • M. E. Pozo Astigarraga,
  • A. Prades Ibanez,
  • P. Pralavorio,
  • M. M. Prapa,
  • S. Prell,
  • D. Price,
  • M. Primavera,
  • M. L. Proffitt,
  • N. Proklova,
  • K. Prokofiev,
  • F. Prokoshin,
  • S. Protopopescu,
  • J. Proudfoot,
  • M. Przybycien,
  • D. Pudzha,
  • P. Puzo,
  • D. Pyatiizbyantseva,
  • J. Qian,
  • Y. Qin,
  • A. Quadt,
  • M. Queitsch-Maitland,
  • G. Rabanal Bolanos,
  • F. Ragusa,
  • G. Rahal,
  • J. A. Raine,
  • S. Rajagopalan,
  • K. Ran,
  • D. F. Rassloff,
  • D. M. Rauch,
  • S. Rave,
  • B. Ravina,
  • I. Ravinovich,
  • M. Raymond,
  • A. L. Read,
  • N. P. Readioff,
  • M. Reale,
  • D. M. Rebuzzi,
  • G. Redlinger,
  • K. Reeves,
  • D. Reikher,
  • A. Reiss,
  • A. Rej,
  • C. Rembser,
  • A. Renardi,
  • M. Renda,
  • M. B. Rendel,
  • A. G. Rennie,
  • S. Resconi,
  • E. D. Resseguie,
  • S. Rettie,
  • B. Reynolds,
  • E. Reynolds,
  • M. Rezaei Estabragh,
  • O. L. Rezanova,
  • P. Reznicek,
  • E. Ricci,
  • R. Richter,
  • S. Richter,
  • E. Richter-Was,
  • M. Ridel,
  • P. Rieck,
  • O. Rifki,
  • M. Rijssenbeek,
  • A. Rimoldi,
  • M. Rimoldi,
  • L. Rinaldi,
  • T. T. Rinn,
  • G. Ripellino,
  • I. Riu,
  • P. Rivadeneira,
  • J. C. Rivera Vergara,
  • F. Rizatdinova,
  • E. Rizvi,
  • C. Rizzi,
  • S. H. Robertson,
  • M. Robin,
  • D. Robinson,
  • C. M. Robles Gajardo,
  • M. Robles Manzano,
  • A. Robson,
  • A. Rocchi,
  • C. Roda,
  • S. Rodriguez Bosca,
  • A. Rodriguez Rodriguez,
  • A. M. Rodríguez Vera,
  • S. Roe,
  • J. Roggel,
  • O. Røhne,
  • R. A. Rojas,
  • B. Roland,
  • C. P. A. Roland,
  • J. Roloff,
  • A. Romaniouk,
  • M. Romano,
  • N. Rompotis,
  • M. Ronzani,
  • L. Roos,
  • S. Rosati,
  • G. Rosin,
  • B. J. Rosser,
  • E. Rossi,
  • E. Rossi,
  • E. Rossi,
  • L. P. Rossi,
  • L. Rossini,
  • R. Rosten,
  • M. Rotaru,
  • B. Rottler,
  • D. Rousseau,
  • G. Rovelli,
  • A. Roy,
  • A. Rozanov,
  • Y. Rozen,
  • X. Ruan,
  • A. J. Ruby,
  • T. A. Ruggeri,
  • F. Rühr,
  • A. Ruiz-Martinez,
  • A. Rummler,
  • Z. Rurikova,
  • N. A. Rusakovich,
  • H. L. Russell,
  • L. Rustige,
  • J. P. Rutherfoord,
  • E. M. Rüttinger,
  • M. Rybar,
  • E. B. Rye,
  • A. Ryzhov,
  • J. A. Sabater Iglesias,
  • P. Sabatini,
  • L. Sabetta,
  • H. F. -W. Sadrozinski,
  • R. Sadykov,
  • F. Safai Tehrani,
  • B. Safarzadeh Samani,
  • M. Safdari,
  • P. Saha,
  • S. Saha,
  • M. Sahinsoy,
  • A. Sahu,
  • M. Saimpert,
  • M. Saito,
  • T. Saito,
  • D. Salamani,
  • G. Salamanna,
  • A. Salnikov,
  • J. Salt,
  • A. Salvador Salas,
  • D. Salvatore,
  • F. Salvatore,
  • A. Salzburger,
  • D. Sammel,
  • D. Sampsonidis,
  • D. Sampsonidou,
  • J. Sánchez,
  • A. Sanchez Pineda,
  • H. Sandaker,
  • C. O. Sander,
  • I. G. Sanderswood,
  • M. Sandhoff,
  • C. Sandoval,
  • D. P. C. Sankey,
  • M. Sannino,
  • Y. Sano,
  • A. Sansoni,
  • C. Santoni,
  • H. Santos,
  • S. N. Santpur,
  • A. Santra,
  • K. A. Saoucha,
  • A. Sapronov,
  • J. G. Saraiva,
  • O. Sasaki,
  • K. Sato,
  • F. Sauerburger,
  • E. Sauvan,
  • P. Savard,
  • R. Sawada,
  • C. Sawyer,
  • L. Sawyer,
  • I. Sayago Galvan,
  • C. Sbarra,
  • A. Sbrizzi,
  • T. Scanlon,
  • J. Schaarschmidt,
  • P. Schacht,
  • D. Schaefer,
  • L. Schaefer,
  • U. Schäfer,
  • A. C. Schaffer,
  • D. Schaile,
  • R. D. Schamberger,
  • E. Schanet,
  • C. Scharf,
  • N. Scharmberg,
  • V. A. Schegelsky,
  • D. Scheirich,
  • F. Schenck,
  • M. Schernau,
  • C. Schiavi,
  • L. K. Schildgen,
  • Z. M. Schillaci,
  • E. J. Schioppa,
  • M. Schioppa,
  • K. E. Schleicher,
  • S. Schlenker,
  • K. Schmieden,
  • C. Schmitt,
  • S. Schmitt,
  • L. Schoeffel,
  • A. Schoening,
  • P. G. Scholer,
  • E. Schopf,
  • M. Schott,
  • J. Schovancova,
  • S. Schramm,
  • F. Schroeder,
  • A. Schulte,
  • H. -C. Schultz-Coulon,
  • M. Schumacher,
  • B. A. Schumm,
  • Ph. Schune,
  • A. Schwartzman,
  • T. A. Schwarz,
  • Ph. Schwemling,
  • R. Schwienhorst,
  • A. Sciandra,
  • G. Sciolla,
  • F. Scuri,
  • F. Scutti,
  • C. D. Sebastiani,
  • K. Sedlaczek,
  • P. Seema,
  • S. C. Seidel,
  • A. Seiden,
  • B. D. Seidlitz,
  • T. Seiss,
  • C. Seitz,
  • J. M. Seixas,
  • G. Sekhniaidze,
  • S. J. Sekula,
  • L. P. Selem,
  • N. Semprini-Cesari,
  • S. Sen,
  • C. Serfon,
  • L. Serin,
  • L. Serkin,
  • M. Sessa,
  • H. Severini,
  • S. Sevova,
  • F. Sforza,
  • A. Sfyrla,
  • E. Shabalina,
  • J. D. Shahinian,
  • N. W. Shaikh,
  • D. Shaked Renous,
  • L. Y. Shan,
  • M. Shapiro,
  • A. Sharma,
  • A. S. Sharma,
  • P. B. Shatalov,
  • K. Shaw,
  • S. M. Shaw,
  • M. Shehade,
  • Y. Shen,
  • P. Sherwood,
  • L. Shi,
  • C. O. Shimmin,
  • Y. Shimogama,
  • M. Shimojima,
  • J. D. Shinner,
  • I. P. J. Shipsey,
  • S. Shirabe,
  • M. Shiyakova,
  • J. Shlomi,
  • M. J. Shochet,
  • J. Shojaii,
  • D. R. Shope,
  • S. Shrestha,
  • E. M. Shrif,
  • M. J. Shroff,
  • E. Shulga,
  • P. Sicho,
  • A. M. Sickles,
  • E. Sideras Haddad,
  • O. Sidiropoulou,
  • A. Sidoti,
  • F. Siegert,
  • Dj. Sijacki,
  • M. V. Silva Oliveira,
  • S. B. Silverstein,
  • S. Simion,
  • R. Simoniello,
  • S. Simsek,
  • P. Sinervo,
  • V. Sinetckii,
  • S. Singh,
  • S. Sinha,
  • M. Sioli,
  • I. Siral,
  • S. Yu. Sivoklokov,
  • J. Sjölin,
  • A. Skaf,
  • E. Skorda,
  • P. Skubic,
  • M. Slawinska,
  • K. Sliwa,
  • V. Smakhtin,
  • B. H. Smart,
  • J. Smiesko,
  • S. Yu. Smirnov,
  • Y. Smirnov,
  • L. N. Smirnova,
  • O. Smirnova,
  • E. A. Smith,
  • H. A. Smith,
  • M. Smizanska,
  • K. Smolek,
  • A. Smykiewicz,
  • A. A. Snesarev,
  • H. L. Snoek,
  • I. M. Snyder,
  • S. Snyder,
  • R. Sobie,
  • A. Soffer,
  • A. Søgaard,
  • F. Sohns,
  • C. A. Solans Sanchez,
  • E. Yu. Soldatov,
  • U. Soldevila,
  • A. A. Solodkov,
  • S. Solomon,
  • A. Soloshenko,
  • O. V. Solovyanov,
  • V. Solovyev,
  • P. Sommer,
  • H. Son,
  • A. Sonay,
  • W. Y. Song,
  • A. Sopczak,
  • A. L. Sopio,
  • F. Sopkova,
  • S. Sottocornola,
  • R. Soualah,
  • A. M. Soukharev,
  • Z. Soumaimi,
  • D. South,
  • S. Spagnolo,
  • M. Spalla,
  • M. Spangenberg,
  • F. Spanò,
  • D. Sperlich,
  • T. M. Spieker,
  • G. Spigo,
  • M. Spina,
  • D. P. Spiteri,
  • M. Spousta,
  • A. Stabile,
  • B. L. Stamas,
  • R. Stamen,
  • M. Stamenkovic,
  • A. Stampekis,
  • E. Stanecka,
  • B. Stanislaus,
  • M. M. Stanitzki,
  • M. Stankaityte,
  • B. Stapf,
  • E. A. Starchenko,
  • G. H. Stark,
  • J. Stark,
  • P. Staroba,
  • P. Starovoitov,
  • S. Stärz,
  • R. Staszewski,
  • G. Stavropoulos,
  • P. Steinberg,
  • A. L. Steinhebel,
  • B. Stelzer,
  • H. J. Stelzer,
  • O. Stelzer-Chilton,
  • H. Stenzel,
  • T. J. Stevenson,
  • G. A. Stewart,
  • M. C. Stockton,
  • G. Stoicea,
  • M. Stolarski,
  • S. Stonjek,
  • A. Straessner,
  • J. Strandberg,
  • S. Strandberg,
  • M. Strauss,
  • T. Strebler,
  • P. Strizenec,
  • R. Ströhmer,
  • D. M. Strom,
  • L. R. Strom,
  • R. Stroynowski,
  • A. Strubig,
  • S. A. Stucci,
  • B. Stugu,
  • J. Stupak,
  • N. A. Styles,
  • D. Su,
  • W. Su,
  • X. Su,
  • N. B. Suarez,
  • V. V. Sulin,
  • M. J. Sullivan,
  • D. M. S. Sultan,
  • S. Sultansoy,
  • T. Sumida,
  • S. Sun,
  • S. Sun,
  • X. Sun,
  • C. J. E. Suster,
  • M. R. Sutton,
  • M. Svatos,
  • M. Swiatlowski,
  • S. P. Swift,
  • T. Swirski,
  • A. Sydorenko,
  • I. Sykora,
  • M. Sykora,
  • T. Sykora,
  • D. Ta,
  • K. Tackmann,
  • A. Taffard,
  • R. Tafirout,
  • E. Tagiev,
  • R. H. M. Taibah,
  • R. Takashima,
  • K. Takeda,
  • T. Takeshita,
  • E. P. Takeva,
  • Y. Takubo,
  • M. Talby,
  • A. A. Talyshev,
  • K. C. Tam,
  • N. M. Tamir,
  • J. Tanaka,
  • R. Tanaka,
  • S. Tapia Araya,
  • S. Tapprogge,
  • A. Tarek Abouelfadl Mohamed,
  • S. Tarem,
  • K. Tariq,
  • G. Tarna,
  • G. F. Tartarelli,
  • P. Tas,
  • M. Tasevsky,
  • E. Tassi,
  • G. Tateno,
  • Y. Tayalati,
  • G. N. Taylor,
  • W. Taylor,
  • H. Teagle,
  • A. S. Tee,
  • R. Teixeira de Lima,
  • P. Teixeira-Dias,
  • H. Ten Kate,
  • J. J. Teoh,
  • K. Terashi,
  • J. Terron,
  • S. Terzo,
  • M. Testa,
  • R. J. Teuscher,
  • N. Themistokleous,
  • T. Theveneaux-Pelzer,
  • D. W. Thomas,
  • J. P. Thomas,
  • E. A. Thompson,
  • P. D. Thompson,
  • E. Thomson,
  • E. J. Thorpe,
  • V. O. Tikhomirov,
  • Yu. A. Tikhonov,
  • S. Timoshenko,
  • P. Tipton,
  • S. Tisserant,
  • S. H. Tlou,
  • A. Tnourji,
  • K. Todome,
  • S. Todorova-Nova,
  • S. Todt,
  • J. Tojo,
  • S. Tokár,
  • K. Tokushuku,
  • E. Tolley,
  • R. Tombs,
  • M. Tomoto,
  • L. Tompkins,
  • P. Tornambe,
  • E. Torrence,
  • H. Torres,
  • E. Torró Pastor,
  • M. Toscani,
  • C. Tosciri,
  • J. Toth,
  • D. R. Tovey,
  • A. Traeet,
  • C. J. Treado,
  • T. Trefzger,
  • A. Tricoli,
  • I. M. Trigger,
  • S. Trincaz-Duvoid,
  • D. A. Trischuk,
  • W. Trischuk,
  • B. Trocmé,
  • A. Trofymov,
  • C. Troncon,
  • F. Trovato,
  • L. Truong,
  • M. Trzebinski,
  • A. Trzupek,
  • F. Tsai,
  • P. V. Tsiareshka,
  • A. Tsirigotis,
  • V. Tsiskaridze,
  • E. G. Tskhadadze,
  • M. Tsopoulou,
  • I. I. Tsukerman,
  • V. Tsulaia,
  • S. Tsuno,
  • D. Tsybychev,
  • Y. Tu,
  • A. Tudorache,
  • V. Tudorache,
  • A. N. Tuna,
  • S. Turchikhin,
  • D. Turgeman,
  • I. Turk Cakir,
  • R. J. Turner,
  • R. Turra,
  • P. M. Tuts,
  • S. Tzamarias,
  • P. Tzanis,
  • E. Tzovara,
  • K. Uchida,
  • F. Ukegawa,
  • G. Unal,
  • M. Unal,
  • A. Undrus,
  • G. Unel,
  • F. C. Ungaro,
  • K. Uno,
  • J. Urban,
  • P. Urquijo,
  • G. Usai,
  • Z. Uysal,
  • V. Vacek,
  • B. Vachon,
  • K. O. H. Vadla,
  • T. Vafeiadis,
  • C. Valderanis,
  • E. Valdes Santurio,
  • M. Valente,
  • S. Valentinetti,
  • A. Valero,
  • L. Valéry,
  • R. A. Vallance,
  • A. Vallier,
  • J. A. Valls Ferrer,
  • T. R. Van Daalen,
  • P. Van Gemmeren,
  • S. Van Stroud,
  • I. Van Vulpen,
  • M. Vanadia,
  • W. Vandelli,
  • M. Vandenbroucke,
  • E. R. Vandewall,
  • D. Vannicola,
  • R. Vari,
  • E. W. Varnes,
  • C. Varni,
  • T. Varol,
  • D. Varouchas,
  • K. E. Varvell,
  • M. E. Vasile,
  • L. Vaslin,
  • G. A. Vasquez,
  • F. Vazeille,
  • D. Vazquez Furelos,
  • T. Vazquez Schroeder,
  • J. Veatch,
  • V. Vecchio,
  • M. J. Veen,
  • L. M. Veloce,
  • F. Veloso,
  • S. Veneziano,
  • A. Ventura,
  • A. Verbytskyi,
  • M. Verducci,
  • C. Vergis,
  • W. Verkerke,
  • A. T. Vermeulen,
  • J. C. Vermeulen,
  • C. Vernieri,
  • P. J. Verschuuren,
  • M. L. Vesterbacka,
  • M. C. Vetterli,
  • N. Viaux Maira,
  • T. Vickey,
  • O. E. Vickey Boeriu,
  • G. H. A. Viehhauser,
  • L. Vigani,
  • M. Villa,
  • M. Villaplana Perez,
  • E. M. Villhauer,
  • E. Vilucchi,
  • M. G. Vincter,
  • G. S. Virdee,
  • A. Vishwakarma,
  • C. Vittori,
  • I. Vivarelli,
  • V. Vladimirov,
  • M. Vogel,
  • P. Vokac,
  • J. Von Ahnen,
  • S. E. Von Buddenbrock,
  • E. Von Toerne,
  • V. Vorobel,
  • K. Vorobev,
  • M. Vos,
  • J. H. Vossebeld,
  • M. Vozak,
  • N. Vranjes,
  • M. Vranjes Milosavljevic,
  • V. Vrba,
  • M. Vreeswijk,
  • N. K. Vu,
  • R. Vuillermet,
  • I. Vukotic,
  • S. Wada,
  • C. Wagner,
  • P. Wagner,
  • W. Wagner,
  • S. Wahdan,
  • H. Wahlberg,
  • R. Wakasa,
  • V. M. Walbrecht,
  • J. Walder,
  • R. Walker,
  • S. D. Walker,
  • W. Walkowiak,
  • V. Wallangen,
  • A. M. Wang,
  • A. Z. Wang,
  • C. Wang,
  • C. Wang,
  • H. Wang,
  • J. Wang,
  • P. Wang,
  • R. -J. Wang,
  • R. Wang,
  • R. Wang,
  • S. M. Wang,
  • S. Wang,
  • T. Wang,
  • W. T. Wang,
  • W. X. Wang,
  • Y. Wang,
  • Z. Wang,
  • C. Wanotayaroj,
  • A. Warburton,
  • C. P. Ward,
  • R. J. Ward,
  • N. Warrack,
  • A. T. Watson,
  • M. F. Watson,
  • G. Watts,
  • B. M. Waugh,
  • A. F. Webb,
  • C. Weber,
  • M. S. Weber,
  • S. A. Weber,
  • S. M. Weber,
  • C. Wei,
  • Y. Wei,
  • A. R. Weidberg,
  • J. Weingarten,
  • M. Weirich,
  • C. Weiser,
  • P. S. Wells,
  • T. Wenaus,
  • B. Wendland,
  • T. Wengler,
  • S. Wenig,
  • N. Wermes,
  • M. Wessels,
  • T. D. Weston,
  • K. Whalen,
  • A. M. Wharton,
  • A. S. White,
  • A. White,
  • M. J. White,
  • D. Whiteson,
  • W. Wiedenmann,
  • C. Wiel,
  • M. Wielers,
  • N. Wieseotte,
  • C. Wiglesworth,
  • L. A. M. Wiik-Fuchs,
  • H. G. Wilkens,
  • L. J. Wilkins,
  • D. M. Williams,
  • H. H. Williams,
  • S. Williams,
  • S. Willocq,
  • P. J. Windischhofer,
  • I. Wingerter-Seez,
  • F. Winklmeier,
  • B. T. Winter,
  • M. Wittgen,
  • M. Wobisch,
  • A. Wolf,
  • R. Wölker,
  • J. Wollrath,
  • M. W. Wolter,
  • H. Wolters,
  • V. W. S. Wong,
  • A. F. Wongel,
  • N. L. Woods,
  • S. D. Worm,
  • B. K. Wosiek,
  • K. W. Woźniak,
  • K. Wraight,
  • J. Wu,
  • S. L. Wu,
  • X. Wu,
  • Y. Wu,
  • Z. Wu,
  • J. Wuerzinger,
  • T. R. Wyatt,
  • B. M. Wynne,
  • S. Xella,
  • J. Xiang,
  • X. Xiao,
  • X. Xie,
  • I. Xiotidis,
  • D. Xu,
  • H. Xu,
  • H. Xu,
  • L. Xu,
  • R. Xu,
  • T. Xu,
  • W. Xu,
  • Y. Xu,
  • Z. Xu,
  • Z. Xu,
  • B. Yabsley,
  • S. Yacoob,
  • D. P. Yallup,
  • N. Yamaguchi,
  • Y. Yamaguchi,
  • M. Yamatani,
  • H. Yamauchi,
  • T. Yamazaki,
  • Y. Yamazaki,
  • J. Yan,
  • Z. Yan,
  • H. J. Yang,
  • H. T. Yang,
  • S. Yang,
  • T. Yang,
  • X. Yang,
  • X. Yang,
  • Y. Yang,
  • Z. Yang,
  • W. -M. Yao,
  • Y. C. Yap,
  • H. Ye,
  • J. Ye,
  • S. Ye,
  • I. Yeletskikh,
  • M. R. Yexley,
  • P. Yin,
  • K. Yorita,
  • K. Yoshihara,
  • C. J. S. Young,
  • C. Young,
  • R. Yuan,
  • X. Yue,
  • M. Zaazoua,
  • B. Zabinski,
  • G. Zacharis,
  • E. Zaffaroni,
  • J. Zahreddine,
  • A. M. Zaitsev,
  • T. Zakareishvili,
  • N. Zakharchuk,
  • S. Zambito,
  • D. Zanzi,
  • S. V. Zeißner,
  • C. Zeitnitz,
  • G. Zemaityte,
  • J. C. Zeng,
  • O. Zenin,
  • T. Ženiš,
  • S. Zenz,
  • S. Zerradi,
  • D. Zerwas,
  • M. Zgubič,
  • B. Zhang,
  • D. F. Zhang,
  • G. Zhang,
  • J. Zhang,
  • K. Zhang,
  • L. Zhang,
  • L. Zhang,
  • M. Zhang,
  • R. Zhang,
  • S. Zhang,
  • X. Zhang,
  • X. Zhang,
  • Z. Zhang,
  • P. Zhao,
  • Y. Zhao,
  • Z. Zhao,
  • A. Zhemchugov,
  • Z. Zheng,
  • D. Zhong,
  • B. Zhou,
  • C. Zhou,
  • H. Zhou,
  • M. Zhou,
  • N. Zhou,
  • Y. Zhou,
  • C. G. Zhu,
  • C. Zhu,
  • H. L. Zhu,
  • H. Zhu,
  • J. Zhu,
  • Y. Zhu,
  • X. Zhuang,
  • K. Zhukov,
  • V. Zhulanov,
  • D. Zieminska,
  • N. I. Zimine,
  • S. Zimmermann,
  • Z. Zinonos,
  • M. Ziolkowski,
  • L. Živković,
  • A. Zoccoli,
  • K. Zoch,
  • T. G. Zorbas,
  • R. Zou,
  • W. Zou,
  • L. Zwalinski,
  • Atlas Collaboration
  • (less)
Computing and Software for Big Science, 6 (12/2022) doi:10.1007/s41781-021-00062-2
abstract + abstract -

The accurate simulation of additional interactions at the ATLAS experiment for the analysis of proton-proton collisions delivered by the Large Hadron Collider presents a significant challenge to the computing resources. During the LHC Run 2 (2015-2018), there were up to 70 inelastic interactions per bunch crossing, which need to be accounted for in Monte Carlo (MC) production. In this document, a new method to account for these additional interactions in the simulation chain is described. Instead of sampling the inelastic interactions and adding their energy deposits to a hard-scatter interaction one-by-one, the inelastic interactions are presampled, independent of the hard scatter, and stored as combined events. Consequently, for each hard-scatter interaction, only one such presampled event needs to be added as part of the simulation chain. For the Run 2 simulation chain, with an average of 35 interactions per bunch crossing, this new method provides a substantial reduction in MC production CPU needs of around 20%, while reproducing the properties of the reconstructed quantities relevant for physics analyses with good accuracy.


(1061)Coexisting Z-type charge and bond order in metallic NaRu<SUB>2</SUB>O<SUB>4</SUB>
  • Arvind Kumar Yogi,
  • Alexander Yaresko,
  • C. I. Sathish,
  • Hasung Sim,
  • Daisuke Morikawa
  • +5
  • Juergen Nuss,
  • Kenji Tsuda,
  • Yukio. Noda,
  • Daniel I. Khomskii,
  • Je-Geun Park
  • (less)
Communications Materials, 3 (12/2022) doi:10.1038/s43246-022-00224-8
abstract + abstract -

How particular bonds form in quantum materials has been a long-standing puzzle. Two key concepts dealing with charge degrees of freedom are dimerization (forming metal-metal bonds) and charge ordering. Since the 1930s, these two concepts have been frequently invoked to explain numerous exciting quantum materials, typically insulators. Here we report dimerization and charge ordering within the dimers coexisting in metallic NaRu2O4. By combining high-resolution x-ray diffraction studies and theoretical calculations, we demonstrate that this unique phenomenon occurs through a new type of bonding, which we call Z-type ordering. The low-temperature superstructure has strong dimerization in legs of zigzag ladders, with short dimers in legs connected by short zigzag bonds, forming Z-shape clusters: simultaneously, site-centered charge ordering also appears. Our results demonstrate the yet unknown flexibility of quantum materials with the intricate interplay among orbital, charge, and lattice degrees of freedom.


(1060)B-meson decay into a proton and dark antibaryon from QCD light-cone sum rules
  • Alexander Khodjamirian,
  • Marcel Wald
Physics Letters B, 834 (11/2022) doi:10.1016/j.physletb.2022.137434
abstract + abstract -

The recently developed B-Mesogenesis scenario predicts decays of B mesons into a baryon and hypothetical dark antibaryon Ψ. We suggest a method to calculate the amplitude of the simplest exclusive decay mode B+ → pΨ. Considering two models of B-Mesogenesis, we obtain the B → p hadronic matrix elements by applying QCD light-cone sum rules with the proton light-cone distribution amplitudes. We estimate the B+ → pΨ decay width as a function of the mass and effective coupling of the dark antibaryon.


(1059)Primordial dusty rings and episodic outbursts in protoplanetary discs
  • Kundan Kadam,
  • Eduard Vorobyov,
  • Shantanu Basu
Monthly Notices of the Royal Astronomical Society, 516, p21 (11/2022) doi:10.1093/mnras/stac2455
abstract + abstract -

We investigate the formation and evolution of 'primordial' dusty rings occurring in the inner regions of protoplanetary discs, with the help of long-term, coupled dust-gas, magnetohydrodynamic simulations. The simulations are global and start from the collapse phase of the parent cloud core, while the dead zone is calculated via an adaptive α formulation by taking into account the local ionization balance. The evolution of the dusty component includes its growth and back reaction on to the gas. Previously, using simulations with only a gas component, we showed that dynamical rings form at the inner edge of the dead zone. We find that when dust evolution, as well as magnetic field evolution in the flux-freezing limit are included, the dusty rings formed are more numerous and span a larger radial extent in the inner disc, while the dead zone is more robust and persists for a much longer time. We show that these dynamical rings concentrate enough dust mass to become streaming unstable, which should result in a rapid planetesimal formation even in the embedded phases of the system. The episodic outbursts caused by the magnetorotational instability have a significant impact on the evolution of the rings. The outbursts drain the inner disc of grown dust, however, the period between bursts is sufficiently long for the planetesimal growth via streaming instability. The dust mass contained within the rings is large enough to ultimately produce planetary systems with the core accretion scenario. The low-mass systems rarely undergo outbursts, and, thus, the conditions around such stars can be especially conducive for planet formation.


(1058)Onboard performance of the level 1 trigger of the mini-EUSO telescope
  • M. Battisti,
  • D. Barghini,
  • A. Belov,
  • M. Bertaina,
  • F. Bisconti
  • +28
  • K. Bolmgren,
  • G. Cambiè,
  • F. Capel,
  • M. Casolino,
  • T. Ebisuzaki,
  • F. Fenu,
  • M. A. Franceschi,
  • C. Fuglesang,
  • A. Golzio,
  • P. Gorodetzki,
  • F. Kajino,
  • P. Klimov,
  • M. Manfrin,
  • L. Marcelli,
  • W. Marszał,
  • H. Miyamoto,
  • T. Napolitano,
  • E. Parizot,
  • P. Picozza,
  • L. W. Piotrowski,
  • Z. Plebaniak,
  • G. Prévôt,
  • E. Reali,
  • M. Ricci,
  • N. Sakaki,
  • K. Shinozaki,
  • J. Szabelski,
  • Y. Takizawa
  • (less)
Advances in Space Research, 70, p17 (11/2022) doi:10.1016/j.asr.2022.07.077
abstract + abstract -

The Mini-EUSO telescope was launched for the International Space Station on August 22nd , 2019 to observe from the ISS orbit (∼ 400 km altitude) various phenomena occurring in the Earth's atmosphere through a UV-transparent window located in the Russian Zvezda Module. Mini-EUSO is based on a set of two Fresnel lenses of 25 cm diameter each and a focal plane of 48 × 48 pixels, for a total field of view of 44 ° . Until July 2021, Mini-EUSO performed a total of 41 data acquisition sessions, obtaining UV images of the Earth in the 290 nm - 430 nm band with temporal and spatial resolution on ground of 2.5 μs and 6.3 × 6.3 km2, respectively. The data acquisition was performed with a 2.5 μs sampling rate, using a dedicated trigger looking for signals with a typical duration of tens of μs.

In the present paper the analysis of the performance of the 2.5 μs trigger logic is presented, with a focus on the method used for the analysis and the categories of triggered events. The expected functioning of the trigger logic has been confirmed, with the trigger rate on spurious events that remains within the requirements in nominal background conditions. The trigger logic detected several different phenomena, including lightning strikes, elves, ground-based flashers and events with EAS-like characteristics.


(1057)Ammonia in the interstellar medium of a starbursting disc at z = 2.6
  • M. J. Doherty,
  • J. E. Geach,
  • R. J. Ivison,
  • K. M. Menten,
  • A. M. Jacob
  • +2
Monthly Notices of the Royal Astronomical Society, 517 (11/2022) doi:10.1093/mnrasl/slac111
abstract + abstract -

We report the detection of the ground state rotational emission of ammonia, ortho-NH3 (JK = 10 → 00) in a gravitationally lensed intrinsically hyperluminous star-bursting galaxy at z = 2.6. The integrated line profile is consistent with other molecular and atomic emission lines which have resolved kinematics well modelled by a 5 kpc-diameter rotating disc. This implies that the gas responsible for NH3 emission is broadly tracing the global molecular reservoir, but likely distributed in pockets of high density (n ≳ 5 × 104 cm-3). With a luminosity of 2.8 × 106 L, the NH3 emission represents 2.5 × 10-7 of the total infrared luminosity of the galaxy, comparable to the ratio observed in the Kleinmann-Low nebula in Orion and consistent with sites of massive star formation in the Milky Way. If $L_{\rm NH_3}/L_{\rm IR}$ serves as a proxy for the 'mode' of star formation, this hints that the nature of star formation in extreme starbursts in the early Universe is similar to that of Galactic star-forming regions, with a large fraction of the cold interstellar medium in this state, plausibly driven by a storm of violent disc instabilities in the gas-dominated disc. This supports the 'full of Orions' picture of star formation in the most extreme galaxies seen close to the peak epoch of stellar mass assembly.


(1056)SN 2019ewu: A Peculiar Supernova with Early Strong Carbon and Weak Oxygen Features from a New Sample of Young SN Ic Spectra
  • Marc Williamson,
  • Christian Vogl,
  • Maryam Modjaz,
  • Wolfgang Kerzendorf,
  • Jaladh Singhal
  • +15
  • Teresa Boland,
  • Jamison Burke,
  • Zhihao Chen,
  • Daichi Hiramatsu,
  • Lluis Galbany,
  • Estefania Padilla Gonzalez,
  • D. Andrew Howell,
  • Saurabh W. Jha,
  • Lindsey A. Kwok,
  • Curtis McCully,
  • Megan Newsome,
  • Craig Pellegrino,
  • Jeonghee Rho,
  • Giacomo Terreran,
  • Xiaofeng Wang
  • (less)
arXiv e-prints (11/2022) e-Print:2211.04482
abstract + abstract -

With the advent of high cadence, all-sky automated surveys, supernovae (SNe) are now discovered closer than ever to their dates of explosion. However, young pre-maximum light follow-up spectra of Type Ic supernovae (SNe Ic), probably arising from the most stripped massive stars, remain rare despite their importance. In this paper we present a set of 49 optical spectra observed with the Las Cumbres Observatory through the Global Supernova Project for 6 SNe Ic, including a total of 17 pre-maximum spectra, of which 8 are observed more than a week before V-band maximum light. This dataset increases the total number of publicly available pre-maximum light SN Ic spectra by 25% and we provide publicly available SNID templates that will significantly aid in the fast identification of young SNe Ic in the future. We present detailed analysis of these spectra, including Fe II 5169 velocity measurements, O I 7774 line strengths, and continuum shapes. We compare our results to published samples of stripped supernovae in the literature and find one SN in our sample that stands out. SN 2019ewu has a unique combination of features for a SN Ic: an extremely blue continuum, high absorption velocities, a P-cygni shaped feature almost 2 weeks before maximum light that TARDIS radiative transfer modeling attributes to C II rather than H$\alpha$, and weak or non-existent O I 7774 absorption feature until maximum light.


(1055)Can neutron star mergers alone explain the r-process enrichment of the Milky Way?
  • Chiaki Kobayashi,
  • Ilya Mandel,
  • Krzysztof Belczynski,
  • Stephane Goriely,
  • Thomas H. Janka
  • +7
  • Oliver Just,
  • Ashley J. Ruiter,
  • Dany Van Beveren,
  • Matthias U. Kruckow,
  • Max M. Briel,
  • Jan J. Eldridge,
  • Elizabeth Stanway
  • (less)
arXiv e-prints (11/2022) e-Print:2211.04964
abstract + abstract -

Comparing Galactic chemical evolution models to the observed elemental abundances in the Milky Way, we show that neutron star mergers can be a leading r-process site only if such mergers have very short delay times and/or beneficial masses of the compact objects at low metallicities. Namely, black hole-neutron star mergers, depending on the black-hole spins, can play an important role in the early chemical enrichment of the Milky Way. We also show that none of the binary population synthesis models used in this paper, i.e., COMPAS, StarTrack, Brussels, ComBinE, and BPASS, can currently reproduce the elemental abundance observations. The predictions are problematic not only for neutron star mergers, but also for Type Ia supernovae, which may point to shortcomings in binary evolution models.


(1054)A Neural Network Subgrid Model of the Early Stages of Planet Formation
  • Thomas Pfeil,
  • Miles Cranmer,
  • Shirley Ho,
  • Philip J. Armitage,
  • Tilman Birnstiel
  • +1
arXiv e-prints (11/2022) e-Print:2211.04160
abstract + abstract -

Planet formation is a multi-scale process in which the coagulation of $\mathrm{\mu m}$-sized dust grains in protoplanetary disks is strongly influenced by the hydrodynamic processes on scales of astronomical units ($\approx 1.5\times 10^8 \,\mathrm{km}$). Studies are therefore dependent on subgrid models to emulate the micro physics of dust coagulation on top of a large scale hydrodynamic simulation. Numerical simulations which include the relevant physical effects are complex and computationally expensive. Here, we present a fast and accurate learned effective model for dust coagulation, trained on data from high resolution numerical coagulation simulations. Our model captures details of the dust coagulation process that were so far not tractable with other dust coagulation prescriptions with similar computational efficiency.


(1053)STRIDES: Automated uniform models for 30 quadruply imaged quasars
  • T. Schmidt,
  • T. Treu,
  • S. Birrer,
  • A. J. Shajib,
  • C. Lemon
  • +67
  • M. Millon,
  • D. Sluse,
  • A. Agnello,
  • T. Anguita,
  • M. W. Auger-Williams,
  • R. G. McMahon,
  • V. Motta,
  • P. Schechter,
  • C. Spiniello,
  • I. Kayo,
  • F. Courbin,
  • S. Ertl,
  • C. D. Fassnacht,
  • J. A. Frieman,
  • A. More,
  • S. Schuldt,
  • S. H. Suyu,
  • M. Aguena,
  • F. Andrade-Oliveira,
  • J. Annis,
  • D. Bacon,
  • E. Bertin,
  • D. Brooks,
  • D. L. Burke,
  • A. Carnero Rosell,
  • M. Carrasco Kind,
  • J. Carretero,
  • C. Conselice,
  • M. Costanzi,
  • L. N. da Costa,
  • M. E. S. Pereira,
  • J. De Vicente,
  • S. Desai,
  • P. Doel,
  • S. Everett,
  • I. Ferrero,
  • D. Friedel,
  • J. García-Bellido,
  • E. Gaztanaga,
  • D. Gruen,
  • R. A. Gruendl,
  • J. Gschwend,
  • G. Gutierrez,
  • S. R. Hinton,
  • D. L. Hollowood,
  • K. Honscheid,
  • D. J. James,
  • K. Kuehn,
  • O. Lahav,
  • F. Menanteau,
  • R. Miquel,
  • A. Palmese,
  • F. Paz-Chinchón,
  • A. Pieres,
  • A. A. Plazas Malagón,
  • J. Prat,
  • M. Rodriguez-Monroy,
  • A. K. Romer,
  • E. Sanchez,
  • V. Scarpine,
  • I. Sevilla-Noarbe,
  • M. Smith,
  • E. Suchyta,
  • G. Tarle,
  • C. To,
  • T. N. Varga,
  • DES Collaboration
  • (less)
Monthly Notices of the Royal Astronomical Society (11/2022) doi:10.1093/mnras/stac2235
abstract + abstract -

Gravitational time delays provide a powerful one step measurement of H0, independent of all other probes. One key ingredient in time delay cosmography are high accuracy lens models. Those are currently expensive to obtain, both, in terms of computing and investigator time (105 - 6 CPU hours and ~0.5-1 year, respectively). Major improvements in modeling speed are therefore necessary to exploit the large number of lenses that are forecast to be discovered over the current decade. In order to bypass this roadblock, we develop an automated modeling pipeline and apply it to a sample of 31 lens systems, observed by the Hubble Space Telescope in multiple bands. Our automated pipeline can derive models for 30/31 lenses with few hours of human time and <100 CPU hours of computing time for a typical system. For each lens, we provide measurements of key parameters and predictions of magnification as well as time delays for the multiple images. We characterize the cosmography-readiness of our models using the stability of differences in Fermat potential (proportional to time delay) w.r.t. modeling choices. We find that for 10/30 lenses our models are cosmography or nearly cosmography grade (<3 per cent and 3-5 per cent variations). For 6/30 lenses the models are close to cosmography grade (5-10 per cent). These results utilize informative priors and will need to be confirmed by further analysis. However, they are also likely to improve by extending the pipeline modeling sequence and options. In conclusion, we show that uniform cosmography grade modeling of large strong lens samples is within reach.


(1052)Perfecting one-loop BCJ numerators in SYM and supergravity
  • Alex Edison,
  • Song He,
  • Henrik Johansson,
  • Oliver Schlotterer,
  • Fei Teng
  • +1
arXiv e-prints (11/2022) e-Print:2211.00638
abstract + abstract -

We take a major step towards computing $D$-dimensional one-loop amplitudes in general gauge theories, compatible with the principles of unitarity and the color-kinematics duality. For $n$-point amplitudes with either supersymmetry multiplets or generic non-supersymmetric matter in the loop, simple all-multiplicity expressions are obtained for the maximal cuts of kinematic numerators of $n$-gon diagrams. At $n=6,7$ points with maximal supersymmetry, we extend the cubic-diagram numerators to encode all contact terms, and thus solve the long-standing problem of \emph{simultaneously} realizing the following properties: color-kinematics duality, manifest locality, optimal power counting of loop momenta, quadratic rather than linearized Feynman propagators, compatibility with double copy as well as all graph symmetries. Color-kinematics dual representations with similar properties are presented in the half-maximally supersymmetric case at $n=4,5$ points. The resulting gauge-theory integrands and their supergravity counterparts obtained from the double copy are checked to reproduce the expected ultraviolet divergences.


(1051)Rapid Formation of Massive Planetary Cores in a Pressure Bump
  • Tommy Chi Ho Lau,
  • Joanna Drążkowska,
  • Sebastian M. Stammler,
  • Tilman Birnstiel,
  • Cornelis P. Dullemond
arXiv e-prints (11/2022) e-Print:2211.04497
abstract + abstract -

Models of planetary core growth by either planetesimal or pebble accretion are traditionally disconnected from the models of dust evolution and formation of the first gravitationally-bound planetesimals. The state-of-the-art models typically start with massive planetary cores already present. We aim to study the formation and growth of planetary cores in a pressure bump, motivated by the annular structures observed in protoplanetary disks, starting with sub-micron-sized dust grains. We connect the models of dust coagulation and drift, planetesimal formation in the streaming instability, gravitational interactions between planetesimals, pebble accretion, and planet migration, into one uniform framework. We find that planetesimals forming early at the massive end of the size distribution grow quickly dominantly by pebble accretion. These few massive bodies grow on the timescales of ~100 000 years and stir the planetesimals formed later preventing the emergence of further planetary cores. Additionally, a migration trap occurs allowing for retention of the growing cores. Pressure bumps are favourable locations for the emergence and rapid growth of planetary cores by pebble accretion as the dust density and grain size are increased and the pebble accretion onset mass is reduced compared to a smooth-disk model.


(1050)QuantumFDTD -- A computational framework for the relativistic Schrödinger equation
  • Rafael L. Delgado,
  • Sebastian Steinbeißer,
  • Michael Strickland,
  • Johannes H. Weber
arXiv e-prints (11/2022) e-Print:2211.10185
abstract + abstract -

We extend the publicly available quantumfdtd code. It was originally intended for solving the time-independent three-dimensional Schrödinger equation via the finite-difference time-domain (FDTD) method and for extracting the ground, first, and second excited states. We (a) include the case of the relativistic Schrödinger equation and (b) add two optimized FFT-based kinetic energy terms for the non-relativistic case. All the three new kinetic terms are computed using Fast Fourier Transform (FFT). We release the resulting code as version 3 of quantumfdtd. Finally, the code now supports arbitrary external file-based potentials and the option to project out distinct parity eigenstates from the solutions. Our goal is quark models used for phenomenological descriptions of QCD bound states, described by the three-dimensional Schrödinger equation. However, we target any field where solving either the non-relativistic or the relativistic three-dimensional Schrödinger equation is required.


(1049)Towards an electrostatic storage ring for fundamental physics measurements
  • Chiara Brandenstein,
  • Stefan Stelzl,
  • Erwin Gutsmiedl,
  • Wolfgang Schott,
  • Andreas Weiler
  • +1
arXiv e-prints (11/2022) e-Print:2211.08439
abstract + abstract -

We describe a new table-top electrostatic storage ring concept for $30$ keV polarized ions at frozen spin condition. The device will ultimately be capable of measuring magnetic fields with a resolution of 10$^{-21}$ T with sub-mHz bandwidth. With the possibility to store different kinds of ions or ionic molecules and access to prepare and probe states of the systems using lasers and SQUIDs, it can be used to search for electric dipole moments (EDMs) of electrons and nucleons, as well as axion-like particle dark matter and dark photon dark matter. Its sensitivity potential stems from several hours of storage time, comparably long spin coherence times, and the possibility to trap up to 10$^9$ particles in bunches with possibly different state preparations for differential measurements. As a dark matter experiment, it is most sensitive in the mass range of 10$^{-10}$ to 10$^{-19}$ eV, where it can potentially probe couplings orders of magnitude below current and proposed laboratory experiments.


(1048)LensWatch: I. Resolved HST Observations and Constraints on the Strongly-Lensed Type Ia Supernova 2022qmx ("SN Zwicky")
  • J. D. R. Pierel,
  • N. Arendse,
  • S. Ertl,
  • X. Huang,
  • L. A. Moustakas
  • +37
  • S. Schuldt,
  • A. J. Shajib,
  • Y. Shu,
  • S. Birrer,
  • M. Bronikowski,
  • J. Hjorth,
  • S. H. Suyu,
  • S. Agarwal,
  • A. Agnello,
  • A. S. Bolton,
  • S. Chakrabarti,
  • C. Cold,
  • F. Courbin,
  • J. M. Della Costa,
  • S. Dhawan,
  • M. Engesser,
  • O. D. Fox,
  • C. Gall,
  • S. Gomez,
  • A. Goobar,
  • C. Jimenez,
  • J. Johansson,
  • G. Li,
  • R. Marques-Chaves,
  • S. Mao,
  • P. A. Mazzali,
  • I. Perez-Fournon,
  • T. Petrushevska,
  • F. Poidevin,
  • A. Rest,
  • W. Sheu,
  • R. Shirley,
  • E. Silver,
  • C. Storfer,
  • T. Treu,
  • R. Wojtak,
  • Y. Zenati
  • (less)
arXiv e-prints (11/2022) e-Print:2211.03772
abstract + abstract -

Supernovae (SNe) that have been multiply-imaged by gravitational lensing are rare and powerful probes for cosmology. Each detection is an opportunity to develop the critical tools and methodologies needed as the sample of lensed SNe increases by orders of magnitude with the upcoming Vera C. Rubin Observatory and Nancy Grace Roman Space Telescope. The latest such discovery is of the quadruply-imaged Type Ia SN 2022qmx (aka, "SN Zwicky"; Goobar et al. 2022) at z = 0.3544. SN Zwicky was discovered by the Zwicky Transient Facility (ZTF) in spatially unresolved data. Here we present follow-up Hubble Space Telescope observations of SN Zwicky, the first from the multi-cycle "LensWatch" program (www.lenswatch.org). We measure photometry for each of the four images of SN Zwicky, which are resolved in three WFC3/UVIS filters (F475W, F625W, F814W) but unresolved with WFC3/IR F160W, and produce an analysis of the lensing system using a variety of independent lens modeling methods. We find consistency between time delays estimated with the single epoch of HST photometry and the lens model predictions constrained through the multiple image positions, with both inferring time delays of <1 day. Our lens models converge to an Einstein radius of (0.168+0.009-0.005)", the smallest yet seen in a lensed SN. The "standard candle" nature of SN Zwicky provides magnification estimates independent of the lens modeling that are brighter by ~1.5 mag and ~0.8 mag for two of the four images, suggesting significant microlensing and/or additional substructure beyond the flexibility of our image-position mass models.


(1047)White dwarfs as a probe of light QCD axions
  • Reuven Balkin,
  • Javi Serra,
  • Konstantin Springmann,
  • Stefan Stelzl,
  • Andreas Weiler
arXiv e-prints (11/2022) e-Print:2211.02661
abstract + abstract -

We study the effects of light QCD axions on the stellar configuration of white dwarfs. At finite baryon density, the non-derivative coupling of the axion to nucleons displaces the axion from its in-vacuum minimum which implies a reduction of the nucleon mass. This dramatically alters the composition of stellar remnants. In particular, the modifications of the mass-radius relationship of white dwarfs allow us to probe large regions of unexplored axion parameter space without requiring it to be a significant fraction of dark matter.


(1046)Novel approaches in hadron spectroscopy
  • Miguel Albaladejo,
  • Łukasz Bibrzycki,
  • Sebastian M. Dawid,
  • César Fernández-Ramírez,
  • Sergi Gonzàlez-Solís
  • +13
  • Astrid N. Hiller Blin,
  • Andrew W. Jackura,
  • Vincent Mathieu,
  • Mikhail Mikhasenko,
  • Victor I. Mokeev,
  • Emilie Passemar,
  • Alessandro Pilloni,
  • Arkaitz Rodas,
  • Jorge A. Silva-Castro,
  • Wyatt A. Smith,
  • Adam P. Szczepaniak,
  • Daniel Winney,
  • (Joint Physics Analysis Center)
  • (less)
Progress in Particle and Nuclear Physics, 127 (11/2022) doi:10.1016/j.ppnp.2022.103981
abstract + abstract -

The last two decades have witnessed the discovery of a myriad of new and unexpected hadrons. The future holds more surprises for us, thanks to new-generation experiments. Understanding the signals and determining the properties of the states requires a parallel theoretical effort. To make full use of available and forthcoming data, a careful amplitude modeling is required, together with a sound treatment of the statistical uncertainties, and a systematic survey of the model dependencies. We review the contributions made by the Joint Physics Analysis Center to the field of hadron spectroscopy.


(1045)Beam functions for $N$-jettiness at N$^3$LO in perturbative QCD
  • Daniel Baranowski,
  • Arnd Behring,
  • Kirill Melnikov,
  • Lorenzo Tancredi,
  • Christopher Wever
arXiv e-prints (11/2022) e-Print:2211.05722
abstract + abstract -

We present a calculation of all matching coefficients for $N$-jettiness beam functions at next-to-next-to-next-to-leading order (N$^3$LO) in perturbative quantum chromodynamics (QCD). Our computation is performed starting from the respective collinear splitting kernels, which we integrate using the axial gauge. We use reverse unitarity to map the relevant phase-space integrals to loop integrals, which allows us to employ multi-loop techniques including integration-by-parts identities and differential equations. We find a canonical basis and use an algorithm to establish non-trivial partial fraction relations among the resulting master integrals, which allows us to reduce their number substantially. By use of regularity conditions, we express all necessary boundary constants in terms of an independent set, which we compute by direct integration of the corresponding integrals in the soft limit. In this way, we provide an entirely independent calculation of the matching coefficients which were previously computed in arXiv:2006.03056.


(1044)Towards an automated data cleaning with deep learning in CRESST
  • G. Angloher,
  • S. Banik,
  • D. Bartolot,
  • G. Benato,
  • A. Bento
  • +60
  • A. Bertolini,
  • R. Breier,
  • C. Bucci,
  • J. Burkhart,
  • L. Canonica,
  • A. D'Addabbo,
  • S. Di Lorenzo,
  • L. Einfalt,
  • A. Erb,
  • F. v. Feilitzsch,
  • N. Ferreiro Iachellini,
  • S. Fichtinger,
  • D. Fuchs,
  • A. Fuss,
  • A. Garai,
  • V. M. Ghete,
  • S. Gerster,
  • P. Gorla,
  • P. V. Guillaumon,
  • S. Gupta,
  • D. Hauff,
  • M. Ješkovský,
  • J. Jochum,
  • M. Kaznacheeva,
  • A. Kinast,
  • H. Kluck,
  • H. Kraus,
  • M. Lackner,
  • A. Langenkämper,
  • M. Mancuso,
  • L. Marini,
  • L. Meyer,
  • V. Mokina,
  • A. Nilima,
  • M. Olmi,
  • T. Ortmann,
  • C. Pagliarone,
  • L. Pattavina,
  • F. Petricca,
  • W. Potzel,
  • P. Povinec,
  • F. Pröbst,
  • F. Pucci,
  • F. Reindl,
  • D. Rizvanovic,
  • J. Rothe,
  • K. Schäffner,
  • J. Schieck,
  • D. Schmiedmayer,
  • S. Schönert,
  • C. Schwertner,
  • M. Stahlberg,
  • L. Stodolsky,
  • C. Strandhagen,
  • R. Strauss,
  • I. Usherov,
  • F. Wagner,
  • M. Willers,
  • V. Zema,
  • W. Waltenberger
  • (less)
arXiv e-prints (11/2022) e-Print:2211.00564
abstract + abstract -

The CRESST experiment employs cryogenic calorimeters for the sensitive measurement of nuclear recoils induced by dark matter particles. The recorded signals need to undergo a careful cleaning process to avoid wrongly reconstructed recoil energies caused by pile-up and read-out artefacts. We frame this process as a time series classification task and propose to automate it with neural networks. With a data set of over one million labeled records from 68 detectors, recorded between 2013 and 2019 by CRESST, we test the capability of four commonly used neural network architectures to learn the data cleaning task. Our best performing model achieves a balanced accuracy of 0.932 on our test set. We show on an exemplary detector that about half of the wrongly predicted events are in fact wrongly labeled events, and a large share of the remaining ones have a context-dependent ground truth. We furthermore evaluate the recall and selectivity of our classifiers with simulated data. The results confirm that the trained classifiers are well suited for the data cleaning task.


(1043)Cosmic nucleosynthesis: A multi-messenger challenge
  • Roland Diehl,
  • Andreas J. Korn,
  • Bruno Leibundgut,
  • Maria Lugaro,
  • Anton Wallner
Progress in Particle and Nuclear Physics, 127 (11/2022) doi:10.1016/j.ppnp.2022.103983
abstract + abstract -

The origins of the elements and isotopes of cosmic material is a critical aspect of understanding the evolution of the universe. Nucleosynthesis typically requires physical conditions of high temperatures and densities. These are found in the Big Bang, in the interiors of stars, and in explosions with their compressional shocks and high neutrino and neutron fluxes. Many different tools are available to disentangle the composition of cosmic matter, in material of extraterrestrial origins such as cosmic rays, meteorites, stardust grains, lunar and terrestrial sediments, and through astronomical observations across the electromagnetic spectrum. Understanding cosmic abundances and their evolution requires combining such measurements with approaches of astrophysical, nuclear theories and laboratory experiments, and exploiting additional cosmic messengers, such as neutrinos and gravitational waves. Recent years have seen significant progress in almost all these fields; they are presented in this review.

The Sun and the solar system are our reference system for abundances of elements and isotopes. Many direct and indirect methods are employed to establish a refined abundance record from the time when the Sun and the Earth were formed. Indications for nucleosynthesis in the local environment when the Sun was formed are derived from meteoritic material and inclusion of radioactive atoms in deep-sea sediments. Spectroscopy at many wavelengths and the neutrino flux from the hydrogen fusion processes in the Sun have established a refined model of how the nuclear energy production shapes stars. Models are required to explore nuclear fusion of heavier elements. These stellar evolution calculations have been confirmed by observations of nucleosynthesis products in the ejecta of stars and supernovae, as captured by stardust grains and by characteristic lines in spectra seen from these objects. One of the successes has been to directly observe γ rays from radioactive material synthesised in stellar explosions, which fully support the astrophysical models. Another has been the observation of radioactive afterglow and characteristic heavy-element spectrum from a neutron-star merger, confirming the neutron rich environments encountered in such rare explosions. The ejecta material captured by Earth over millions of years in sediments and identified through characteristic radio-isotopes suggests that nearby nucleosynthesis occurred in recent history, with further indications for sites of specific nucleosynthesis. Together with stardust and diffuse γ rays from radioactive ejecta, these help to piece together how cosmic materials are transported in interstellar space and re-cycled into and between generations of stars. Our description of cosmic compositional evolution needs such observational support, as it rests on several assumptions that appear challenged by recent recognition of violent events being common during evolution of a galaxy. This overview presents the flow of cosmic matter and the various sites of nucleosynthesis, as understood from combining many techniques and observations, towards the current knowledge of how the universe is enriched with elements.


(1042)Compact jets dominate the continuum emission in low-luminosity active galactic nuclei
  • J. A. Fernández-Ontiveros,
  • X. López-López,
  • A. Prieto
arXiv e-prints (11/2022) e-Print:2211.09828
abstract + abstract -

The disappearance of the accretion disc in low-luminosity active galactic nuclei (LLAGN) leaves behind a faint optical nuclear continuum whose nature has been largely debated, mainly due to serious observational limitations in the IR to UV range. We combine multi-wavelength sub-arcsecond resolution observations -- able to isolate the genuine nuclear continuum -- with nebular lines in the mid-IR, to indirectly probe the shape of the extreme UV continuum. We found that 8 of the nearest prototype LLAGN are compatible with pure compact jet emission (self-absorbed synchrotron plus the associated self-Compton component) over more than ten orders of magnitude in frequency. When compared with typical radio galaxies, the LLAGN continua show two peculiarities: $i)$ a very steep spectral slope in the IR-to-optical/UV range ($-3.7 < \alpha_0 < -1.3$; $F_\nu \propto \nu^{\alpha_0}$); and $ii)$ a very high turnover frequency ($0.2-30\, \rm{THz}$; $1.3\,\rm{mm}-10\,\rm{\mu m}$). These attributes can be explained if the synchrotron continuum is mainly dominated by thermalised particles at the jet base or corona with considerably high temperatures, whereas only a small fraction of the energy ($\sim 20\%$) would be distributed along the high-energy power-law tail of accelerated particles. On the other hand, the nebular gas excitation in LLAGN is in agreement with photo-ionisation from inverse Compton radiation ($\alpha_{\rm x} \sim -0.7$), which would dominate the nuclear continuum shortwards of $\sim 3000$ Å. Our results suggest that the LLAGN continuum can be dominated at all wavelengths by undeveloped jets, powered by a thermalised particle distribution, similar to the behaviour observed in compact jets of quiescent black hole X-ray binaries. This has important implications in the context of galaxy evolution, since LLAGN may represent a major but underestimated source of kinetic feedback in galaxies.


(1041)Impact of half-wave plate systematics on the measurement of cosmic birefringence from CMB polarization
  • Marta Monelli,
  • Eiichiro Komatsu,
  • Alexandre E. Adler,
  • Matteo Billi,
  • Paolo Campeti
  • +4
  • Nadia Dachlythra,
  • Adriaan J. Duivenvoorden,
  • Jon E. Gudmundsson,
  • Martin Reinecke
  • (less)
arXiv e-prints (11/2022) e-Print:2211.05685
abstract + abstract -

Polarization of the cosmic microwave background (CMB) can probe new parity-violating physics such as cosmic birefringence (CB), which requires exquisite control over instrumental systematics. The non-idealities of the half-wave plate (HWP) represent a source of systematics when used as a polarization modulator. We study their impact on the CMB angular power spectra, which is partially degenerate with CB and miscalibration of the polarization angle. We use full-sky beam convolution simulations including HWP to generate mock noiseless time-ordered data, process them through a bin averaging map-maker, and calculate the power spectra including $TB$ and $EB$ correlations. We also derive analytical formulae which accurately model the observed spectra. For our choice of HWP parameters, the HWP-induced angle amounts to a few degrees, which could be misinterpreted as CB. Accurate knowledge of the HWP is required to mitigate this. Our simulation and analytical formulae will be useful for deriving requirements for the accuracy of HWP calibration.


(1040)Is the star formation rate in $z\sim 6$ quasars overestimated?
  • Fabio Di Mascia,
  • Stefano Carniani,
  • Simona Gallerani,
  • Fabio Vito,
  • Andrea Pallottini
  • +2
  • Andrea Ferrara,
  • Milena Valentini
  • (less)
arXiv e-prints (11/2022) e-Print:2211.05790
abstract + abstract -

The large total infrared (TIR) luminosities ($L_{\rm TIR} \gtrsim 10^{12}~L_\odot$) observed in $z \sim 6$ quasars are generally converted into high star formation rates ($SFR \gtrsim 10^2~M_\odot$ yr$^{-1}$) of their host galaxies. However, these estimates rely on the assumption that dust heating is dominated by stellar radiation, neglecting the contribution from the central Active Galactic Nuclei (AGN). We test the validity of this assumption by combining cosmological hydrodynamic simulations with radiative transfer calculations. We find that, when AGN radiation is included in the simulations, the mass (luminosity)-weighted dust temperature in the host galaxies increases from $T\approx 50$ K ($T \approx 70$ K) to $T\approx 80$ K ($T\approx 200$ K), suggesting that AGN effectively heat the bulk of dust in the host galaxy. We compute the AGN-host galaxy $SFR$ from the synthetic spectral energy distribution by using standard $SFR - L_{\rm TIR}$ relations, and compare the results with the "true" values in the simulations. We find that the $SFR$ is overestimated by a factor of $\approx 3$ ($\gtrsim 10$) for AGN bolometric luminosities of $L_{\rm bol} \approx 10^{12}~L_\odot$ ($\gtrsim 10^{13}~ L_\odot$), implying that the star formation rates of $z\sim 6$ quasars can be overestimated by over an order of magnitude.


(1039)MGLenS: Modified gravity weak lensing simulations for emulation-based cosmological inference
  • Joachim Harnois-Déraps,
  • Cesar Hernandez-Aguayo,
  • Carolina Cuesta-Lazaro,
  • Christian Arnold,
  • Baojiu Li
  • +2
  • Christopher T. Davies,
  • Yan-Chuan Cai
  • (less)
arXiv e-prints (11/2022) e-Print:2211.05779
abstract + abstract -

We present MGLenS, a large series of modified gravity lensing simulations tailored for cosmic shear data analyses and forecasts in which cosmological and modified gravity parameters are varied simultaneously. Based on the FORGE and BRIDGE $N$-body simulation suites presented in companion papers, we construct 500,000 deg$^2$ of mock Stage-IV lensing data, sampling a pair of 4-dimensional volumes designed for the training of emulators. We validate the accuracy of MGLenS with inference analyses based on the lensing power spectrum exploiting our implementation of $f(R)$ and nDGP theoretical predictions within the cosmoSIS cosmological inference package. A Fisher analysis reveals that the vast majority of the constraining power from such a survey comes from the highest redshift galaxies alone. We further find from a full likelihood sampling that cosmic shear can achieve 95% CL constraints on the modified gravity parameters of log$_{10}\left[ f_{R_0}\right] < -5.24$ and log$_{10}\left[ H_0 r_c\right] > -0.05$, after marginalising over intrinsic alignments of galaxies and including scales up to $\ell=5000$. Such a survey setup could in fact detect with more than $3\sigma$ confidence $f(R)$ values larger than $3 \times 10^{-6}$ and $H_0 r_c$ smaller than 1.0. Scale cuts at $\ell=3000$ reduce the degeneracy breaking between $S_8$ and the modified gravity parameters, while photometric redshift uncertainty seem to play a subdominant role in our error budget. We finally explore the consequences of analysing data with the wrong gravity model, and report the catastrophic biases for a number of possible scenarios. The Stage-IV MGLenS simulations, the FORGE and BRIDGE emulators and the cosmoSIS interface modules will be made publicly available upon journal acceptance.


(1038)Testing the galaxy collision induced formation scenario for the trail of dark matter deficient galaxies with the susceptibility of globular clusters to the tidal force
  • Go Ogiya,
  • Frank C. van den Bosch,
  • Andreas Burkert,
  • Xi Kang
arXiv e-prints (11/2022) e-Print:2211.05993
abstract + abstract -

It has been suggested that a trail of diffuse galaxies, including two dark matter deficient galaxies (DMDGs), in the vicinity of NGC1052 formed because of a high-speed collision between two gas-rich dwarf galaxies, one bound to NGC1052 and the other one on an unbound orbit. The collision compresses the gas reservoirs of the colliding galaxies, which in turn triggers a burst of star formation. In contrast, the dark matter and pre-existing stars in the progenitor galaxies pass through it. Since the high pressures in the compressed gas are conducive to the formation of massive globular clusters (GCs), this scenario can explain the formation of DMDGs with large populations of massive GCs, consistent with the observations of NGC1052-DF2 (DF2) and NGC1052-DF4. A potential difficulty with this `mini bullet cluster' scenario is that the observed spatial distributions of GCs in DMDGs are extended. GCs experience dynamical friction causing their orbits to decay with time. Consequently, their distribution at formation should have been even more extended than that observed at present. Using a semi-analytic model, we show that the observed positions and velocities of the GCs in DF2 imply that they must have formed at a radial distance of 5-10kpc from the center of DF2. However, as we demonstrate, the scenario is difficult to reconcile with the fact that the strong tidal forces from NGC1052 strip the extendedly distributed GCs from DF2, requiring 33-59 massive GCs to form at the collision to explain observations.


(1037)PANDORA project: photo-nuclear reactions below $A=60$
  • A. Tamii,
  • L. Pellegri,
  • P. -A. Söderström,
  • D. Allard,
  • S. Goriely
  • +76
  • T. Inakura,
  • E. Khan,
  • E. Kido,
  • M. Kimura,
  • E. Litvinova,
  • S. Nagataki,
  • P. von Neumann-Cosel,
  • N. Pietralla,
  • N. Shimizu,
  • N. Tsoneva,
  • Y. Utsuno,
  • S. Adachi,
  • P. Adsley,
  • A. Bahini,
  • D. Balabanski,
  • B. Baret,
  • J. A. C. Bekker,
  • S. D. Binda,
  • E. Boicu,
  • A. Bracco,
  • I. Brandherm,
  • M. Brezeanu,
  • J. W. Brummer,
  • F. Camera,
  • F. C. L. Crespi,
  • R. Dalal,
  • L. M. Donaldson,
  • Y. Fujikawa,
  • T. Furuno,
  • H. Haoning,
  • Y. Honda,
  • A. Gavrilescu,
  • A. Inoue,
  • J. Isaak,
  • H. Jivan,
  • P. M. Jones,
  • S. Jongile,
  • O. Just,
  • T. Kawabata,
  • T. Khumalo,
  • J. Kiener,
  • J. Kleemann,
  • N. Kobayashi,
  • Y. Koshio,
  • A. Kuşoğlu,
  • K. C. W. Li,
  • K. L. Malatji,
  • R. E. Molaeng,
  • H. Motoki,
  • M. Murata,
  • A. A. Netshiya,
  • R. Neveling,
  • R. Niina,
  • S. Okamoto,
  • S. Ota,
  • O. Papst,
  • E. Parizot,
  • T. Petruse,
  • M. S. Reen,
  • P. Ring,
  • K. Sakanashi,
  • E. Sideras-Haddad,
  • S. Siem,
  • M. Spall,
  • T. Suda,
  • T. Sudo,
  • Y. Taniguchi,
  • V. Tatischeff,
  • H. Utsunomiya,
  • H. Wang,
  • V. Werner,
  • H. Wibowo,
  • M. Wiedeking,
  • O. Wieland,
  • Y. Xu,
  • Z. H. Yang
  • (less)
arXiv e-prints (11/2022) e-Print:2211.03986
abstract + abstract -

Photo-nuclear reactions of light nuclei below a mass of $A=60$ are studied experimentally and theoretically by the PANDORA (Photo-Absorption of Nuclei and Decay Observation for Reactions in Astrophysics) project. Two experimental methods, virtual-photon excitation by proton scattering and real-photo absorption by a high-brilliance gamma-ray beam produced by laser Compton scattering, will be applied to measure the photo-absorption cross sections and the decay branching ratio of each decay channel as a function of the photon energy. Several nuclear models, e.g. anti-symmetrized molecular dynamics, mean-field type models, a large-scale shell model, and ab initio models, will be employed to predict the photo-nuclear reactions. The uncertainty in the model predictions will be evaluated from the discrepancies between the model predictions and the experimental data. The data and the predictions will be implemented in a general reaction calculation code TALYS . The results will be applied to the simulation of the photo-disintegration process of ultra-high-energy cosmic rays in inter-galactic propagation.


(1036)Modelling photo-evaporation in planet forming discs
  • Barbara Ercolano,
  • Giovanni Picogna
arXiv e-prints (11/2022) e-Print:2211.10130
abstract + abstract -

Planets are born from the gas and dust discs surrounding young stars. Energetic radiation from the central star can drive thermal outflows from the discs atmospheres, strongly affecting the evolution of the discs and the nascent planetary system. In this context several numerical models of varying complexity have been developed to study the process of disc photoevaporation from their central stars. We describe the numerical techniques, the results and the predictivity of current models and identify observational tests to constrain them.


(1035)The short ionizing photon mean free path at z = 6 in Cosmic Dawn III, a new fully coupled radiation-hydrodynamical simulation of the Epoch of Reionization
  • Joseph S. W. Lewis,
  • Pierre Ocvirk,
  • Jenny G. Sorce,
  • Yohan Dubois,
  • Dominique Aubert
  • +11
  • Luke Conaboy,
  • Paul R. Shapiro,
  • Taha Dawoodbhoy,
  • Romain Teyssier,
  • Gustavo Yepes,
  • Stefan Gottlöber,
  • Yann Rasera,
  • Kyungjin Ahn,
  • Ilian T. Iliev,
  • Hyunbae Park,
  • Émilie Thélie
  • (less)
Monthly Notices of the Royal Astronomical Society, 516, p9 (11/2022) doi:10.1093/mnras/stac2383
abstract + abstract -

Recent determinations of the mean free path of ionizing photons (mfp) in the intergalactic medium (IGM) at z = 6 are lower than many theoretical predictions. In order to gain insight, we investigate the evolution of the mfp in our new massive fully coupled radiation-hydrodynamics cosmological simulation of reionization: Cosmic Dawn III (CoDa III). CoDa III's scale ($\rm 94^3 \, cMpc^3$) and resolution ($\rm 8192^3$ grid) make it particularly suitable to study the IGM during reionization. The simulation was performed with RAMSES-CUDATON on Summit, and used 13 1072 processors coupled to 24 576 GPUs, making it the largest reionization simulation, and largest ever RAMSES simulation. A superior agreement with global constraints on reionization is obtained in CoDa III over Cosmic Dawn II (CoDa II), especially for the evolution of the neutral hydrogen fraction and the cosmic photoionization rate, thanks to an improved calibration, later end of reionization (z = 5.6), and higher spatial resolution. Analysing the mfp, we find that CoDa III reproduces the most recent observations very well, from z = 6 to z = 4.6. We show that the distribution of the mfp in CoDa III is bimodal, with short (neutral) and long (ionized) mfp modes, due to the patchiness of reionization and the coexistence of neutral versus ionized regions during reionization. The neutral mode peaks at sub-kpc to kpc scales of mfp, while the ionized mode peak evolves from 0.1 Mpc h-1 at z = 7 to ~10 Mpc h-1 at z = 5.2. Computing the mfp as the average of the ionized mode provides the best match to the recent observational determinations. The distribution reduces to a single neutral (ionized) mode at z > 13 (z < 5).


(1034)Seismic source analysis of two anomalous earthquakes in Northern Chile
  • Carlos Tassara,
  • Simone Cesca,
  • Matthew Miller,
  • José Ángel López-Comino,
  • Christian Sippl
  • +2
  • Joaquín Cortés-Aranda,
  • Bernd Schurr
  • (less)
Journal of South American Earth Sciences, 119 (11/2022) doi:10.1016/j.jsames.2022.103948
abstract + abstract -

Northern Chile is a seismically very active region driven by subduction of the Nazca plate beneath the South American plate. Anomalous focal mechanisms were reported by international agencies for two recent earthquakes with magnitudes larger than Mw 6. The September 11, 2020, Mw 6.2 Loa River earthquake occurred in the forearc under the Coastal Cordillera and had a strike-slip mechanism, while most common regional seismicity is characterised by NS-oriented, trench-parallel, thrust mechanisms, consistent with the subduction geometry. The June 3, 2020, Mw 6.8 San Pedro de Atacama earthquake occurred at intermediate depth with a normal faulting mechanism. In this case, the anomalous behavior involves the NW-SE striking of the focal mechanism, which deviate from the typical NS orientation in the region. In this study we reconstruct the rupture geometry for these two earthquakes by means of moment tensor inversion, rupture directivity analysis and aftershock distribution. Seismological results are discussed in the frame of the spatial and temporal distribution of local seismicity, which are analyzed using clustering techniques. Our results show that both earthquakes reveal the activation of seismogenic structures in the continental crust or within the subducting oceanic crust close to the subduction interface. The Loa River earthquake occurred at the base of the continental crust, at the contact with the slab. This finding highlights the role of seismicity associated with crustal faults in the South American plate, which poses a secondary seismic hazard for the region, alongside the seismicity directly associated with the subduction zone. The San Pedro de Atacama earthquake, in turn, occurred within the subducting slab. Its anomalous mechanism may indicate a local anomaly in the geometry of the subducting slab.


(1033)Testing the key role of the stellar mass-halo mass relation in galaxy merger rates and morphologies via DECODE, a novel Discrete statistical sEmi-empiriCal mODEl
  • Hao Fu,
  • Francesco Shankar,
  • Mohammadreza Ayromlou,
  • Max Dickson,
  • Ioanna Koutsouridou
  • +17
  • Yetli Rosas-Guevara,
  • Christopher Marsden,
  • Kristina Brocklebank,
  • Mariangela Bernardi,
  • Nikolaos Shiamtanis,
  • Joseph Williams,
  • Lorenzo Zanisi,
  • Viola Allevato,
  • Lumen Boco,
  • Silvia Bonoli,
  • Andrea Cattaneo,
  • Paola Dimauro,
  • Fangzhou Jiang,
  • Andrea Lapi,
  • Nicola Menci,
  • Stefani Petropoulou,
  • Carolin Villforth
  • (less)
Monthly Notices of the Royal Astronomical Society, 516, p28 (11/2022) doi:10.1093/mnras/stac2205
abstract + abstract -

The relative roles of mergers and star formation in regulating galaxy growth are still a matter of intense debate. We here present our DECODE, a new Discrete statistical sEmi-empiriCal mODEl specifically designed to predict rapidly and efficiently, in a full cosmological context, galaxy assembly, and merger histories for any given input stellar mass-halo mass (SMHM) relation. DECODE generates object-by-object dark matter merger trees (hence discrete) from accurate subhalo mass and infall redshift probability functions (hence statistical) for all subhaloes, including those residing within other subhaloes, with virtually no resolution limits on mass or volume. Merger trees are then converted into galaxy assembly histories via an input, redshift-dependent SMHM relation, which is highly sensitive to the significant systematics in the galaxy stellar mass function and on its evolution with cosmic time. DECODE can accurately reproduce the predicted mean galaxy merger rates and assembly histories of hydrodynamic simulations and semi-analytical models, when adopting in input their SMHM relations. In this work, we use DECODE to prove that only SMHM relations implied by stellar mass functions characterized by large abundances of massive galaxies and significant redshift evolution, at least at $M_\star \gtrsim 10^{11} \, \mathrm{M}_\odot$, can simultaneously reproduce the local abundances of satellite galaxies, the galaxy (major merger) pairs since z ~ 3, and the growth of Brightest Cluster Galaxies. The same models can also reproduce the local fraction of elliptical galaxies, on the assumption that these are strictly formed by major mergers, but not the full bulge-to-disc ratio distributions, which require additional processes.


(1032)The MADPSZ catalogue of Planck clusters over the DES region: extending to lower mass and higher redshift
  • D. Hernández-Lang,
  • J. J. Mohr,
  • M. Klein,
  • S. Grandis,
  • J. -B. Melin
  • +56
  • P. Tarrío,
  • M. Arnaud,
  • G. W. Pratt,
  • T. M. C. Abbott,
  • M. Aguena,
  • O. Alves,
  • F. Andrade-Oliveira,
  • D. Bacon,
  • E. Bertin,
  • D. Brooks,
  • D. L. Burke,
  • A. Carnero Rosell,
  • M. Carrasco Kind,
  • J. Carretero,
  • F. J. Castander,
  • M. Costanzi,
  • L. N. da Costa,
  • M. E. S. Pereira,
  • S. Desai,
  • H. T. Diehl,
  • P. Doel,
  • S. Everett,
  • I. Ferrero,
  • B. Flaugher,
  • J. Frieman,
  • J. García-Bellido,
  • D. Gruen,
  • R. A. Gruendl,
  • J. Gschwend,
  • G. Gutierrez,
  • S. R. Hinton,
  • D. L. Hollowood,
  • K. Honscheid,
  • D. J. James,
  • K. Kuehn,
  • N. Kuropatkin,
  • O. Lahav,
  • C. Lidman,
  • P. Melchior,
  • J. Mena-Fernández,
  • F. Menanteau,
  • R. Miquel,
  • A. Palmese,
  • F. Paz-Chinchón,
  • A. Pieres,
  • A. A. Plazas Malagón,
  • M. Raveri,
  • M. Rodriguez-Monroy,
  • A. K. Romer,
  • V. Scarpine,
  • I. Sevilla-Noarbe,
  • M. Smith,
  • E. Suchyta,
  • G. Tarle,
  • D. Thomas,
  • N. Weaverdyck
  • (less)
arXiv e-prints (10/2022) e-Print:2210.04666
abstract + abstract -

We present the first systematic follow-up of Planck Sunyaev-Zeldovich effect (SZE) selected candidates down to signal-to-noise (S/N) of 3 over the 5000 deg$^2$ covered by the Dark Energy Survey. Using the MCMF cluster confirmation algorithm, we identify optical counterparts, determine photometric redshifts and richnesses and assign a parameter, $f_{\rm cont}$, that reflects the probability that each SZE-optical pairing represents a real cluster rather than a random superposition of physically unassociated systems. The new MADPSZ cluster catalogue consists of 1092 MCMF confirmed clusters and has a purity of 85%. We present the properties of subsamples of the MADPSZ catalogue that have purities ranging from 90% to 97.5%, depending on the adopted $f_{\rm cont}$ threshold. $M_{500}$ halo mass estimates, redshifts, richnesses, and optical centers are presented for all MADPSZ clusters. The MADPSZ catalogue adds 828 previously unknown Planck identified clusters over the DES footprint and provides redshifts for an additional 50 previously published Planck selected clusters with S/N>4.5. Using the subsample with spectroscopic redshifts, we demonstrate excellent cluster photo-$z$ performance with an RMS scatter in $\Delta z/(1+z)$ of 0.47%. Our MCMF based analysis allows us to infer the contamination fraction of the initial S/N>3 Planck selected candidate list, which is 50%. We present a method of estimating the completeness of the MADPSZ cluster sample and $f_{\rm cont}$ selected subsamples. In comparison to the previously published Planck cluster catalogues. this new S/N $>$ 3 MCMF confirmed cluster catalogue populates the lower mass regime at all redshifts and includes clusters up to z$\sim$1.3.


(1031)The Loop Momentum Amplituhedron
  • Livia Ferro,
  • Tomasz Lukowski
arXiv e-prints (10/2022) e-Print:2210.01127
abstract + abstract -

In this paper we focus on scattering amplitudes in maximally supersymmetric Yang-Mills theory and define a long sought-after geometry, the loop momentum amplituhedron, which we conjecture to encode tree and (the integrands of) loop amplitudes in spinor helicity variables. Motivated by the structure of amplitude singularities, we define an extended positive space, which enhances the Grassmannian space featuring at tree level, and a map which associates to each of its points tree-level kinematic variables and loop momenta. The image of this map is the loop momentum amplituhedron. Importantly, our formulation provides a global definition of the loop momenta. We conjecture that for all multiplicities and helicity sectors, there exists a canonical logarithmic differential form defined on this space, and provide its explicit form in a few examples.


(1030)Modified gravity approaches to the cosmological constant problem
  • The FADE Collaboration,
  • Heliudson Bernardo,
  • Benjamin Bose,
  • Guilherme Franzmann,
  • Steffen Hagstotz
  • +3
  • Yutong He,
  • Aliki Litsa,
  • Florian Niedermann
  • (less)
arXiv e-prints (10/2022) e-Print:2210.06810
abstract + abstract -

The cosmological constant and its phenomenology remain among the greatest puzzles in theoretical physics. We review how modifications of Einstein's general relativity could alleviate the different problems associated with it that result from the interplay of classical gravity and quantum field theory. We introduce a modern and concise language to describe the problems associated with its phenomenology, and inspect no-go theorems and their loopholes to motivate the approaches discussed here. Constrained gravity approaches exploit minimal departures from general relativity; massive gravity introduces mass to the graviton; Horndeski theories lead to the breaking of translational invariance of the vacuum; and models with extra dimensions change the symmetries of the vacuum. We also review screening mechanisms that have to be present in some of these theories if they aim to recover the success of general relativity on small scales as well. Finally, we summarise the statuses of these models in their attempt to solve the different cosmological constant problems while being able to account for current astrophysical and cosmological observations.


(1029)Pushing forward jet substructure measurements in heavy-ion collisions
  • Daniel Pablos,
  • Alba Soto-Ontoso
arXiv e-prints (10/2022) e-Print:2210.07901
abstract + abstract -

Energetic jets that traverse the quark-gluon plasma created in heavy-ion collisions serve as excellent probes to study this new state of deconfined QCD matter. Presently, however, our ability to achieve a crisp theoretical interpretation of the crescent number of jet observables measured in experiments is hampered by the presence of selection biases. The aim of this work is to minimise those selection biases associated to the modification of the quark- vs. gluon-initiated jet fraction in order to assess the presence of other medium-induced effects, namely color decoherence, by exploring the rapidity dependence of jet substructure observables. So far, all jet substructure measurements at mid-rapidity have shown that heavy-ion jets are narrower than vacuum jets. We show both analytically and with Monte Carlo simulations that if the narrowing effect persists at forward rapidities, where the quark-initiated jet fraction is greatly increased, this could serve as an unambiguous experimental observation of color decoherence dynamics in heavy-ion collisions.


(1028)Monitoring accretion rate variability in the Orion Nebula Cluster with the Wendelstein Wide Field Imager
  • S. Flaischlen,
  • T. Preibisch,
  • M. Kluge,
  • C. F. Manara,
  • B. Ercolano
Astronomy and Astrophysics, 666, p12 (10/2022) doi:10.1051/0004-6361/202142630
abstract + abstract -

Context. The understanding of the accretion process has a central role in the understanding of star and planet formation.
Aims: We aim to test how accretion variability influences previous correlation analyses of the relation between X-ray activity and accretion rates, which is important for understanding the evolution of circumstellar disks and disk photoevaporation.
Methods: We monitored accreting stars in the Orion Nebula Cluster from November 24, 2014, until February 17, 2019, for 42 epochs with the Wendelstein Wide Field Imager in the Sloan Digital Sky Survey u'g'r' filters on the 2 m Fraunhofer Telescope on Mount Wendelstein. Mass accretion rates were determined from the measured ultraviolet excess. The influence of the mass accretion rate variability on the relation between X-ray luminosities and mass accretion rates was analyzed statistically.
Results: We find a typical interquartile range of ∼0.3 dex for the mass accretion rate variability on timescales from weeks to ∼2 yr. The variability has likely no significant influence on a correlation analysis of the X-ray luminosity and the mass accretion rate observed at different times when the sample size is large enough.
Conclusions: The observed anticorrelation between the X-ray luminosity and the mass accretion rate predicted by models of photoevaporation-starved accretion is likely not due to a bias introduced by different observing times.

Full Tables 1-3 and reduced data are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/666/A55


(1027)Enhancing Searches for Heavy QCD Axions via Dimuon Final States
  • Raymond T. Co,
  • Soubhik Kumar,
  • Zhen Liu
arXiv e-prints (10/2022) e-Print:2210.02462
abstract + abstract -

Heavy QCD axions are well-motivated extensions of the QCD axion that address the quality problem while still solving the strong CP problem. Owing to the gluon coupling, critical for solving the strong CP problem, these axions can be produced in significant numbers in beam dump and collider environments for axion decay constants as large as PeV, relevant for addressing the axion quality problem. In addition, if these axions have leptonic couplings, they can give rise to long-lived decay into lepton pairs, in particular, dominantly into muons above the dimuon threshold and below the GeV scale in a broad class of axion models. Considering existing constraints, primarily from rare meson decays, we demonstrate that current and future neutrino facilities and long-lived particle searches have the potential to probe significant parts of the heavy QCD axion parameter space via dimuon final states.


(1026)Mapping gas around massive galaxies: cross-correlation of DES Y3 galaxies and Compton-$y$-maps from SPT and Planck
  • J. Sánchez,
  • Y. Omori,
  • C. Chang,
  • L. E. Bleem,
  • T. Crawford
  • +122
  • A. Drlica-Wagner,
  • S. Raghunathan,
  • G. Zacharegkas,
  • T. M. C. Abbott,
  • M. Aguena,
  • A. Alarcon,
  • S. Allam,
  • O. Alves,
  • A. Amon,
  • S. Avila,
  • E. Baxter,
  • K. Bechtol,
  • B. A. Benson,
  • G. M. Bernstein,
  • E. Bertin,
  • S. Bocquet,
  • D. Brooks,
  • D. L. Burke,
  • A. Campos,
  • J. E. Carlstrom,
  • A. Carnero Rosell,
  • M. Carrasco Kind,
  • J. Carretero,
  • F. J. Castander,
  • R. Cawthon,
  • C. L. Chang,
  • A. Chen,
  • A. Choi,
  • R. Chown,
  • M. Costanzi,
  • A. T. Crites,
  • M. Crocce,
  • L. N. da Costa,
  • M. E. S. Pereira,
  • T. de Haan,
  • J. De Vicente,
  • J. DeRose,
  • S. Desai,
  • H. T. Diehl,
  • M. A. Dobbs,
  • S. Dodelson,
  • P. Doel,
  • J. Elvin-Poole,
  • W. Everett,
  • S. Everett,
  • I. Ferrero,
  • B. Flaugher,
  • P. Fosalba,
  • J. Frieman,
  • J. García-Bellido,
  • M. Gatti,
  • E. M. George,
  • D. W. Gerdes,
  • G. Giannini,
  • D. Gruen,
  • R. A. Gruendl,
  • J. Gschwend,
  • G. Gutierrez,
  • N. W. Halverson,
  • S. R. Hinton,
  • G. P. Holder,
  • D. L. Hollowood,
  • W. L. Holzapfel,
  • K. Honscheid,
  • J. D. Hrubes,
  • D. J. James,
  • L. Knox,
  • K. Kuehn,
  • N. Kuropatkin,
  • O. Lahav,
  • A. T. Lee,
  • D. Luong-Van,
  • N. MacCrann,
  • J. L. Marshall,
  • J. McCullough,
  • J. J. McMahon,
  • P. Melchior,
  • J. Mena-Fernández,
  • F. Menanteau,
  • R. Miquel,
  • L. Mocanu,
  • J. J. Mohr,
  • J. Muir,
  • J. Myles,
  • T. Natoli,
  • S. Padin,
  • A. Palmese,
  • S. Pandey,
  • F. Paz-Chinchón,
  • A. Pieres,
  • A. A. Plazas Malagón,
  • A. Porredon,
  • C. Pryke,
  • M. Raveri,
  • C. L. Reichardt,
  • M. Rodriguez-Monroy,
  • A. J. Ross,
  • J. E. Ruhl,
  • E. Rykoff,
  • C. Sánchez,
  • E. Sanchez,
  • V. Scarpine,
  • K. K. Schaffer,
  • I. Sevilla-Noarbe,
  • E. Sheldon,
  • E. Shirokoff,
  • M. Smith,
  • M. Soares-Santos,
  • Z. Staniszewski,
  • A. A. Stark,
  • E. Suchyta,
  • M. E. C. Swanson,
  • G. Tarle,
  • D. Thomas,
  • M. A. Troxel,
  • D. L. Tucker,
  • J. D. Vieira,
  • M. Vincenzi,
  • N. Weaverdyck,
  • R. Williamson,
  • B. Yanny,
  • B. Yin
  • (less)
arXiv e-prints (10/2022) e-Print:2210.08633
abstract + abstract -

We cross-correlate positions of galaxies measured in data from the first three years of the Dark Energy Survey with Compton-$y$-maps generated using data from the South Pole Telescope (SPT) and the {\it Planck} mission. We model this cross-correlation measurement together with the galaxy auto-correlation to constrain the distribution of gas in the Universe. We measure the hydrostatic mass bias or, equivalently, the mean halo bias-weighted electron pressure $\langle b_{h}P_{e}\rangle$, using large-scale information. We find $\langle b_{h}P_{e}\rangle$ to be $[0.16^{+0.03}_{-0.04},0.28^{+0.04}_{-0.05},0.45^{+0.06}_{-0.10},0.54^{+0.08}_{-0.07},0.61^{+0.08}_{-0.06},0.63^{+0.07}_{-0.08}]$ meV cm$^{-3}$ at redshifts $z \sim [0.30, 0.46, 0.62,0.77, 0.89, 0.97]$. These values are consistent with previous work where measurements exist in the redshift range. We also constrain the mean gas profile using small-scale information, enabled by the high-resolution of the SPT data. We compare our measurements to different parametrized profiles based on the cosmo-OWLS hydrodynamical simulations. We find that our data are consistent with the simulation that assumes an AGN heating temperature of $10^{8.5}$K but are incompatible with the model that assumes an AGN heating temperature of $10^{8.0}$K. These comparisons indicate that the data prefer a higher value of electron pressure than the simulations within $r_{500c}$ of the galaxies' halos.


(1025)ALMACAL IX: multi-band ALMA survey for dusty star-forming galaxies and the resolved fractions of the cosmic infrared background
  • Jianhang Chen,
  • R. J. Ivison,
  • Martin A. Zwaan,
  • Ian Smail,
  • Anne Klitsch
  • +6
  • Céline Péroux,
  • Gergö Popping,
  • Andrew D. Biggs,
  • Roland Szakacs,
  • Aleksandra Hamanowicz,
  • Claudia Lagos
  • (less)
arXiv e-prints (10/2022) e-Print:2210.09329
abstract + abstract -

Wide, deep, blind continuum surveys at submillimetre/millimetre (submm/mm) wavelengths are required to provide a full inventory of the dusty, distant Universe. However, conducting such surveys to the necessary depth, with sub-arcsec angular resolution, is prohibitively time-consuming, even for the most advanced submm/mm telescopes. Here, we report the most recent results from the ALMACAL project, which exploits the 'free' calibration data from the Atacama Large Millimetre/submillimetre Array (ALMA) to map the lines of sight towards and beyond the ALMA calibrators. ALMACAL has now covered 1,001 calibrators, with a total sky coverage around 0.3 deg2, distributed across the sky accessible from the Atacama desert, and has accumulated more than 1,000h of integration. The depth reached by combining multiple visits to each field makes ALMACAL capable of searching for faint, dusty, star-forming galaxies (DSFGs), with detections at multiple frequencies to constrain the emission mechanism. Based on the most up-to-date ALMACAL database, we report the detection of 186 DSFGs with flux densities down to S870um ~ 0.2mJy, comparable with existing ALMA large surveys but less susceptible to cosmic variance. We report the number counts at five wavelengths between 870um and 3mm, in ALMA bands 3, 4, 5, 6 and 7, providing a benchmark for models of galaxy formation and evolution. By integrating the observed number counts and the best-fitting functions, we also present the resolved fraction of the cosmic infrared background (CIB) and the CIB spectral shape. Combining existing surveys, ALMA has currently resolved about half of the CIB in the submm/mm regime.


(1024)Beyond $\Lambda$CDM constraints from the full shape clustering measurements from BOSS and eBOSS
  • Agne Semenaite,
  • Ariel G. Sánchez,
  • Andrea Pezzotta,
  • Jiamin Hou,
  • Alexander Eggemeier
  • +5
  • Martin Crocce,
  • Cheng Zhao,
  • Joel R. Brownstein,
  • Graziano Rossi,
  • Donald P. Schneider
  • (less)
arXiv e-prints (10/2022) e-Print:2210.07304
abstract + abstract -

We analyse the full shape of anisotropic clustering measurements from the extended Baryon Oscillation Spectroscopic survey (eBOSS) quasar sample together with the combined galaxy sample from the Baryon Oscillation Spectroscopic Survey (BOSS). We obtain constraints on the cosmological parameters independent of the Hubble parameter $h$ for the extensions of the $\Lambda$CDM models, focusing on cosmologies with free dark energy equation of state parameter $w$. We combine the clustering constraints with those from the latest CMB data from Planck to obtain joint constraints for these cosmologies for $w$ and the additional extension parameters - its time evolution $w_{\rm{a}}$, the physical curvature density $\omega_{K}$ and the neutrino mass sum $\sum m_{\nu}$. Our joint constraints are consistent with flat $\Lambda$CDM cosmological model within 68\% confidence limits. We demonstrate that the Planck data are able to place tight constraints on the clustering amplitude today, $\sigma_{12}$, in cosmologies with varying $w$ and present the first constraints for the clustering amplitude for such cosmologies, which is found to be slightly higher than the $\Lambda$CDM value. Additionally, we show that when we vary $w$ and allow for non-flat cosmologies and the physical curvature density is used, Planck prefers a curved universe at $4\sigma$ significance, which is $\sim2\sigma$ higher than when using the relative curvature density $\Omega_{\rm{K}}$. Finally, when $w$ is varied freely, clustering provides only a modest improvement (of 0.021 eV) on the upper limit of $\sum m_{\nu}$.


(1023)Evidence for past interaction with an asymmetric circumstellar shell in the young SNR Cassiopeia A
  • S. Orlando,
  • A. Wongwathanarat,
  • H. -T. Janka,
  • M. Miceli,
  • S. Nagataki
  • +6
  • M. Ono,
  • F. Bocchino,
  • J. Vink,
  • D. Milisavljevic,
  • D. J. Patnaude,
  • G. Peres
  • (less)
Astronomy and Astrophysics, 666, p19 (10/2022) doi:10.1051/0004-6361/202243258
abstract + abstract -

Context. Observations of the supernova remnant (SNR) Cassiopeia A (Cas A) show significant asymmetries in the reverse shock that cannot be explained by models describing a remnant expanding through a spherically symmetric wind of the progenitor star.
Aims: We investigate whether a past interaction of Cas A with a massive asymmetric shell of the circumstellar medium can account for the observed asymmetries of the reverse shock.
Methods: We performed three-dimensional (3D) (magneto)-hydrodynamic simulations that describe the remnant evolution from the SN explosion to its interaction with a massive circumstellar shell. The initial conditions (soon after the shock breakout at the stellar surface) are provided by a 3D neutrino-driven SN model whose morphology closely resembles Cas A and the SNR simulations cover ≈2000 yr of evolution. We explored the parameter space of the shell, searching for a set of parameters able to produce an inward-moving reverse shock in the western hemisphere of the remnant at the age of ≈350 yr, analogous to that observed in Cas A.
Results: The interaction of the remnant with the shell can produce asymmetries resembling those observed in the reverse shock if the shell was asymmetric with the densest portion in the (blueshifted) nearside to the northwest (NW). According to our favorite model, the shell was thin (thickness σ ≈ 0.02 pc) with a radius rsh ≈ 1.5 pc from the center of the explosion. The reverse shock shows the following asymmetries at the age of Cas A: (i) it moves inward in the observer frame in the NW region, while it moves outward in most other regions; (ii) the geometric center of the reverse shock is offset to the NW by ≈0.1 pc from the geometric center of the forward shock; and (iii) the reverse shock in the NW region has enhanced nonthermal emission because, there, the ejecta enter the reverse shock with a higher relative velocity (between 4000 and 7000 km s−1) than in other regions (below 2000 km s−1).
Conclusions: The large-scale asymmetries observed in the reverse shock of Cas A can be interpreted as signatures of the interaction of the remnant with an asymmetric dense circumstellar shell that occurred between ≈180 and ≈240 yr after the SN event. We suggest that the shell was, most likely, the result of a massive eruption from the progenitor star that occurred between 104 and 105 yr prior to core-collapse. We estimate a total mass of the shell of the order of 2 M.


(1022)BIFROST: simulating compact subsystems in star clusters using a hierarchical fourth-order forward symplectic integrator code
  • Antti Rantala,
  • Thorsten Naab,
  • Francesco Paolo Rizzuto,
  • Matias Mannerkoski,
  • Christian Partmann
  • +1
arXiv e-prints (10/2022) e-Print:2210.02472
abstract + abstract -

We present BIFROST, an extended version of the GPU-accelerated hierarchical fourth-order forward symplectic integrator code FROST. BIFROST (BInaries in FROST) can efficiently evolve collisional stellar systems with arbitrary binary fractions up to $f_\mathrm{bin}=100\%$ by using secular and regularised integration for binaries, triples, multiple systems or small clusters around black holes within the fourth-order forward integrator framework. Post-Newtonian (PN) terms up to order PN3.5 are included in the equations of motion of compact subsystems with optional three-body and spin-dependent terms. PN1.0 terms for interactions with black holes are computed everywhere in the simulation domain. The code has several merger criteria (gravitational-wave inspirals, tidal disruption events and stellar and compact object collisions) with the addition of relativistic recoil kicks for compact object mergers. We show that for systems with $N$ particles the scaling of the code remains good up to $N_\mathrm{GPU} \sim 40\times N / 10^6$ GPUs and that the increasing binary fractions up to 100 per cent hardly increase the code running time (less than a factor $\sim 1.5$). We also validate the numerical accuracy of BIFROST by presenting a number of star clusters simulations the most extreme ones including a core collapse and a merger of two intermediate mass black holes with a relativistic recoil kick.


(1021)Exploring the cosmological synergy between galaxy cluster and cosmic void number counts
  • Davide Pelliciari,
  • Sofia Contarini,
  • Federico Marulli,
  • Lauro Moscardini,
  • Carlo Giocoli
  • +2
  • Giorgio Francesco Lesci,
  • Klaus Dolag
  • (less)
arXiv e-prints (10/2022) e-Print:2210.07248
abstract + abstract -

Galaxy clusters and cosmic voids are the most extreme objects of our Universe in terms of mass and size, tracing two opposite sides of the large-scale matter density field. By studying their abundance as a function of their mass and radius, respectively, i.e. the halo mass function (HMF) and void size function (VSF), it is possible to achieve fundamental constraints on the cosmological model. While the HMF has already been extensively exploited providing robust constraints on the main cosmological model parameters (e.g. $\Omega_{\rm m}$, $\sigma_8$ and $S_8$), the VSF is still emerging as a viable and effective cosmological probe. Given the expected complementarity of these statistics, in this work we aim at estimating the costraining power deriving from their combination. To achieve this goal, we exploit realistic mock samples of galaxy clusters and voids extracted from state-of-the-art large hydrodynamical simulations, in the redshift range $0.2 \leq z \leq 1$. We perform an accurate calibration of the free parameters of the HMF and VSF models, needed to take into account the differences between the types of mass tracers used in this work and those considered in previous literature analyses. Then, we obtain constraints on $\Omega_{\rm m}$ and $\sigma_8$ by performing a Bayesian Markov Chain Monte Carlo analysis. We find that cluster and void counts represent powerful independent and complementary probes to test the cosmological framework. In particular, we found that the constraining power of the HMF on $\Omega_{\rm m}$ and $\sigma_8$ improves drastically with the VSF contribution, increasing the $S_8$ constraint precision by a factor of about $60\%$.


(1020)The interplay between forming planets and photo-evaporating discs I: Forbidden line diagnostics
  • Michael L. Weber,
  • Barbara Ercolano,
  • Giovanni Picogna,
  • Christian Rab
arXiv e-prints (10/2022) e-Print:2210.06097
abstract + abstract -

Disc winds and planet formation are considered to be two of the most important mechanisms that drive the evolution and dispersal of protoplanetary discs and in turn define the environment in which planets form and evolve. While both have been studied extensively in the past, we combine them into one model by performing three-dimensional radiation-hydrodynamic simulations of giant planet hosting discs that are undergoing X-ray photo-evaporation, with the goal to analyse the interactions between both mechanisms. In order to study the effect on observational diagnostics, we produce synthetic observations of commonly used wind-tracing forbidden emission lines with detailed radiative transfer and photo-ionisation calculations. We find that a sufficiently massive giant planet carves a gap in the gas disc that is deep enough to affect the structure and kinematics of the pressure-driven photo-evaporative wind significantly. This effect can be strong enough to be visible in the synthetic high-resolution observations of some of our wind diagnostic lines, such as the [OI] 6300 Å or [SII] 6730 Å lines. When the disc is observed at inclinations around 40° and higher, the spectral line profiles may exhibit a peak in the redshifted part of the spectrum, which cannot easily be explained by simple wind models alone. Moreover, massive planets can induce asymmetric substructures within the disc and the photo-evaporative wind, giving rise to temporal variations of the line profiles that can be strong enough to be observable on timescales of less than a quarter of the planet's orbital period.


(1019)Soft-Collinear Gravity and Soft Theorems
  • Martin Beneke,
  • Patrick Hager,
  • Robert Szafron
arXiv e-prints (10/2022) e-Print:2210.09336
abstract + abstract -

This chapter reviews the construction of ``soft-collinear gravity'', the effective field theory which describes the interaction of collinear and soft gravitons with matter (and themselves), to all orders in the soft-collinear power expansion, focusing on the essential concepts. Among them are an emergent soft background gauge symmetry, which lives on the light-like trajectories of energetic particles and allows for a manifestly gauge-invariant representation of the interactions in terms of a soft covariant derivative and the soft Riemann tensor, and a systematic treatment of collinear interactions, which are absent at leading power in gravity. The gravitational soft theorems are derived from soft-collinear gravity at the Lagrangian level. The symmetries of the effective theory provide a transparent explanation of why soft graviton emission is universal to sub-sub-leading power, but gauge boson emission is not and suggest a physical interpretation of the form of the universal soft factors in terms of the charges corresponding to the soft symmetries. The power counting of soft-collinear gravity further provides an understanding of the structure of loop corrections to the soft theorems.


(1018)Multi-messenger characterization of Mrk 501 during historically low X-ray and $\gamma$-ray activity
  • H. Abe,
  • S. Abe,
  • V. A. Acciari,
  • I. Agudo,
  • T. Aniello
  • +319
  • S. Ansoldi,
  • L. A. Antonelli,
  • A. Arbet Engels,
  • C. Arcaro,
  • M. Artero,
  • K. Asano,
  • D. Baack,
  • A. Babić,
  • A. Baquero,
  • U. Barres de Almeida,
  • J. A. Barrio,
  • I. Batković,
  • J. Baxter,
  • J. Becerra González,
  • W. Bednarek,
  • E. Bernardini,
  • M. Bernardos,
  • A. Berti,
  • J. Besenrieder,
  • W. Bhattacharyya,
  • C. Bigongiari,
  • A. Biland,
  • O. Blanch,
  • G. Bonnoli,
  • Ž. Bošnjak,
  • I. Burelli,
  • G. Busetto,
  • R. Carosi,
  • M. Carretero-Castrillo,
  • A. J. Castro-Tirado,
  • G. Ceribella,
  • Y. Chai,
  • A. Chilingarian,
  • S. Cikota,
  • E. Colombo,
  • J. L. Contreras,
  • J. Cortina,
  • S. Covino,
  • G. D'Amico,
  • V. D'Elia,
  • P. Da Vela,
  • F. Dazzi,
  • A. De Angelis,
  • B. De Lotto,
  • A. Del Popolo,
  • M. Delfino,
  • J. Delgado,
  • C. Delgado Mendez,
  • D. Depaoli,
  • F. Di Pierro,
  • L. Di Venere,
  • E. Do Souto Espiñeira,
  • D. Dominis Prester,
  • A. Donini,
  • D. Dorner,
  • M. Doro,
  • D. Elsaesser,
  • G. Emery,
  • J. Escudero,
  • V. Fallah Ramazani,
  • L. Fariña,
  • A. Fattorini,
  • L. Foffano,
  • L. Font,
  • C. Fruck,
  • S. Fukami,
  • Y. Fukazawa,
  • R. J. García López,
  • M. Garczarczyk,
  • S. Gasparyan,
  • M. Gaug,
  • J. G. Giesbrecht Paiva,
  • N. Giglietto,
  • F. Giordano,
  • P. Gliwny,
  • N. Godinović,
  • R. Grau,
  • D. Green,
  • J. G. Green,
  • D. Hadasch,
  • A. Hahn,
  • T. Hassan,
  • L. Heckmann,
  • J. Herrera,
  • D. Hrupec,
  • M. Hütten,
  • R. Imazawa,
  • T. Inada,
  • R. Iotov,
  • K. Ishio,
  • I. Jiménez Martínez,
  • J. Jormanainen,
  • D. Kerszberg,
  • Y. Kobayashi,
  • H. Kubo,
  • J. Kushida,
  • A. Lamastra,
  • D. Lelas,
  • F. Leone,
  • E. Lindfors,
  • L. Linhoff,
  • S. Lombardi,
  • F. Longo,
  • R. López-Coto,
  • M. López-Moya,
  • A. López-Oramas,
  • S. Loporchio,
  • A. Lorini,
  • E. Lyard,
  • B. Machado de Oliveira Fraga,
  • P. Majumdar,
  • M. Makariev,
  • G. Maneva,
  • N. Mang,
  • M. Manganaro,
  • S. Mangano,
  • K. Mannheim,
  • M. Mariotti,
  • M. Martínez,
  • A. Mas-Aguilars,
  • D. Mazin,
  • S. Menchiari,
  • S. Mender,
  • S. Mićanović,
  • D. Miceli,
  • T. Miener,
  • J. M. Miranda,
  • R. Mirzoyan,
  • E. Molina,
  • H. A. Mondal,
  • A. Moralejo,
  • D. Morcuende,
  • V. Moreno,
  • T. Nakamori,
  • C. Nanci,
  • L. Nava,
  • V. Neustroev,
  • M. Nievas Rosillo,
  • C. Nigro,
  • K. Nilsson,
  • K. Nishijima,
  • T. Njoh Ekoume,
  • K. Noda,
  • S. Nozaki,
  • Y. Ohtani,
  • T. Oka,
  • A. Okumura,
  • J. Otero-Santos,
  • S. Paiano,
  • M. Palatiello,
  • D. Paneque,
  • R. Paoletti,
  • J. M. Paredes,
  • L. Pavletić,
  • M. Persic,
  • M. Pihet,
  • G. Pirola,
  • F. Podobnik,
  • P. G. Prada Moroni,
  • E. Prandini,
  • G. Principe,
  • C. Priyadarshi,
  • W. Rhode,
  • M. Ribó,
  • J. Rico,
  • C. Righi,
  • A. Rugliancich,
  • N. Sahakyan,
  • T. Saito,
  • S. Sakurai,
  • K. Satalecka,
  • F. G. Saturni,
  • B. Schleicher,
  • K. Schmidt,
  • F. Schmuckermaier,
  • J. L. Schubert,
  • T. Schweizer,
  • J. Sitarek,
  • V. Sliusar,
  • D. Sobczynska,
  • A. Spolon,
  • A. Stamerra,
  • J. Strišković,
  • D. Strom,
  • M. Strzys,
  • Y. Suda,
  • T. Surić,
  • H. Tajima,
  • M. Takahashi,
  • R. Takeishi,
  • F. Tavecchio,
  • P. Temnikov,
  • K. Terauchi,
  • T. Terzić,
  • M. Teshima,
  • L. Tosti,
  • S. Truzzi,
  • A. Tutone,
  • S. Ubach,
  • J. van Scherpenberg,
  • M. Vazquez Acosta,
  • S. Ventura,
  • V. Verguilov,
  • I. Viale,
  • C. F. Vigorito,
  • V. Vitale,
  • I. Vovk,
  • R. Walter,
  • M. Will,
  • C. Wunderlich,
  • T. Yamamoto,
  • D. Zarić,
  • Other groups,
  • collaborations,
  • :,
  • M. Cerruti,
  • J. A. Acosta-Pulido,
  • G. Apolonio,
  • R. Bachev,
  • M. Baloković,
  • E. Benítez,
  • I. Björklund,
  • V. Bozhilov,
  • L. F. Brown,
  • A. Bugg,
  • W. Carbonell,
  • M. I. Carnerero,
  • D. Carosati,
  • C. Casadio,
  • W. Chamani,
  • W. P. Chen,
  • R. A. Chigladze,
  • G. Damljanovic,
  • K. Epps,
  • A. Erkenov,
  • M. Feige,
  • J. Finke,
  • A. Fuentes,
  • K. Gazeas,
  • M. Giroletti,
  • T. S. Grishina,
  • A. C. Gupta,
  • M. A. Gurwell,
  • E. Heidemann,
  • D. Hiriart,
  • W. J. Hou,
  • T. Hovatta,
  • S. Ibryamov,
  • M. D. Joner,
  • S. G. Jorstad,
  • J. Kania,
  • S. Kiehlmann,
  • G. N. Kimeridze,
  • E. N. Kopatskaya,
  • M. Kopp,
  • M. Korte,
  • B. Kotas,
  • S. Koyama,
  • J. A. Kramer,
  • L. Kunkel,
  • S. O. Kurtanidze,
  • O. M. Kurtanidze,
  • A. Lähteenmäki,
  • J. M. López,
  • V. M. Larionov,
  • E. G. Larionova,
  • L. V. Larionova,
  • C. Leto,
  • C. Lorey,
  • R. Mújica,
  • G. M. Madejski,
  • N. Marchili,
  • A. P. Marscher,
  • M. Minev,
  • A. Modaressi,
  • D. A. Morozova,
  • T. Mufakharov,
  • I. Myserlis,
  • A. A. Nikiforova,
  • M. G. Nikolashvili,
  • E. Ovcharov,
  • M. Perri,
  • C. M. Raiteri,
  • A. C. S. Readhead,
  • A. Reimer,
  • D. Reinhart,
  • S. Righini,
  • K. Rosenlehner,
  • A. C. Sadun,
  • S. S. Savchenko,
  • A. Scherbantin,
  • L. Schneider,
  • K. Schoch,
  • D. Seifert,
  • E. Semkov,
  • L. A. Sigua,
  • C. Singh,
  • P. Sola,
  • Y. Sotnikova,
  • M. Spencer,
  • R. Steineke,
  • M. Stojanovic,
  • A. Strigachev,
  • M. Tornikoski,
  • E. Traianou,
  • A. Tramacere,
  • Yu. V. Troitskaya,
  • I. S. Troitskiy,
  • J. B. Trump,
  • A. Tsai,
  • A. Valcheva,
  • A. A. Vasilyev,
  • F. Verrecchia,
  • M. Villata,
  • O. Vince,
  • K. Vrontaki,
  • Z. R. Weaver,
  • E. Zaharieva,
  • N. Zottmann
  • (less)
arXiv e-prints (10/2022) e-Print:2210.02547
abstract + abstract -

We study the broadband emission of the TeV blazar Mrk501 using multi-wavelength (MWL) observations from 2017 to 2020 performed with a multitude of instruments, involving, among others, MAGIC, Fermi-LAT, NuSTAR, Swift, GASP-WEBT, and OVRO. During this period, Mrk501 showed an extremely low broadband activity, which may help to unravel its baseline emission. Despite the low activity, significant flux variations are detected at all wavebands, with the highest variations occurring at X-rays and VHE $\gamma$-rays. A significant correlation (>3$\sigma$) between X-rays and VHE $\gamma$-rays is measured, supporting leptonic scenarios to explain the variable parts of the spectral energy distribution (SED), also during low activity states. Extending our data set to 12-years (from 2008 to 2020), we find significant correlations between X-rays and HE $\gamma$-rays, indicating, for the first time, a common physical origin driving the variability between these two bands. We additionally find a correlation between HE $\gamma$-rays and radio, with the radio emission lagging the HE $\gamma$-ray emission by more than 100 days. This is consistent with the $\gamma$-ray emission zone being located upstream of the radio-bright regions of the Mrk501 jet. Furthermore, Mrk501 showed a historically low activity in both X-rays and VHE $\gamma$-rays from mid-2017 to mid-2019 with a stable VHE flux (>2TeV) of 5% the emission of the Crab Nebula. The broadband SED of this 2-year long low-state, the potential baseline emission of Mrk501, can be adequately characterized with a one-zone leptonic model, and with (lepto)-hadronic models that fulfill the neutrino flux constraints from IceCube. We explore the time evolution of the SED towards the historically low-state, revealing that the stable baseline emission may be ascribed to a standing shock, and the variable emission to an additional expanding or traveling shock.


(1017)Why Cosmic Voids Matter: Nonlinear Structure &amp; Linear Dynamics
  • Nico Schuster,
  • Nico Hamaus,
  • Klaus Dolag,
  • Jochen Weller
arXiv e-prints (10/2022) e-Print:2210.02457
abstract + abstract -

We use the Magneticum suite of state-of-the-art hydrodynamical simulations to identify cosmic voids based on the watershed technique and investigate their most fundamental properties across different resolutions in mass and scale. This encompasses the distributions of void sizes, shapes, and content, as well as their radial density and velocity profiles traced by the distribution of cold dark matter particles and halos. We also study the impact of various tracer properties, such as their sparsity and mass, and the influence of void merging on these summary statistics. Our results reveal that all of the analyzed void properties are physically related to each other and describe universal characteristics that are largely independent of tracer type and resolution. Most notably, we find that the motion of tracers around void centers is perfectly consistent with linear dynamics, both for individual, as well as stacked voids. Despite the large range of scales accessible in our simulations, we are unable to identify the occurrence of nonlinear dynamics even inside voids of only a few Mpc in size. This suggests voids to be among the most pristine probes of cosmology down to scales that are commonly referred to as highly nonlinear in the field of large-scale structure.


(1016)Landau and leading singularities in arbitrary space-time dimensions
  • Wojciech Flieger,
  • William J. Torres Bobadilla
arXiv e-prints (10/2022) e-Print:2210.09872
abstract + abstract -

Using the decomposition of the $D$-dimensional space-time into parallel and perpendicular subspaces, we study and prove a connection between Landau and leading singularities for $N$-point one-loop Feynman integrals by applying multi-dimensional theory of residues. We show that if $D=N$ and $D=N+1$, the leading singularity corresponds to the inverse of the square root of the leading Landau singularity of the first and second type, respectively. We make use of this outcome to systematically provide differential equations of Feynman integrals in canonical forms and the extension of the connection of these singularities at multi-loop level by exploiting the loop-by-loop approach. Illustrative examples with the calculation of Landau and leading singularities are provided to supplement our results.


(1015)Perturbation theory with dispersion and higher cumulants: non-linear regime
  • Mathias Garny,
  • Dominik Laxhuber,
  • Roman Scoccimarro
arXiv e-prints (10/2022) e-Print:2210.08089
abstract + abstract -

We present non-linear solutions of Vlasov Perturbation Theory (VPT), describing gravitational clustering of collisionless dark matter with dispersion and higher cumulants induced by orbit crossing. We show that VPT can be cast into a form that is formally analogous to standard perturbation theory (SPT), but including additional perturbation variables, non-linear interactions, and a more complex propagation. VPT non-linear kernels have a crucial decoupling property: for fixed total momentum, the kernels becomes strongly suppressed when any of the individual momenta cross the dispersion scale into the non-linear regime. This screening of UV modes allows us to compute non-linear corrections to power spectra even for cosmologies with very blue power-law input spectra, for which SPT diverges. We compare predictions for the density and velocity divergence power spectra as well as the bispectrum at one-loop order to N-body results in a scaling universe with spectral indices $-1\leq n_s\leq +2$. We find a good agreement up to the non-linear scale for all cases, with a reach that increases with the spectral index $n_s$. We discuss the generation of vorticity as well as vector and tensor modes of the velocity dispersion, showing that neglecting vorticity when including dispersion would lead to a violation of momentum conservation. We verify momentum conservation when including vorticity, and compute the vorticity power spectrum at two-loop order, necessary to recover the correct large-scale limit with slope $n_w=2$. Comparing to our N-body measurements confirms the cross-over from $k^4$ to $k^2$ scaling on large scales. Our results provide a proof-of-principle that perturbative techniques for dark matter clustering can be systematically improved based on the known underlying collisionless dynamics.


(1014)Robustness of cosmic birefringence measurement against Galactic foreground emission and instrumental systematics
  • P. Diego-Palazuelos,
  • E. Martínez-González,
  • P. Vielva,
  • R. B. Barreiro,
  • M. Tristram
  • +9
  • E. de la Hoz,
  • J. R. Eskilt,
  • Y. Minami,
  • R. M. Sullivan,
  • A. J. Banday,
  • K. M. Górski,
  • R. Keskitalo,
  • E. Komatsu,
  • D. Scott
  • (less)
arXiv e-prints (10/2022) e-Print:2210.07655
abstract + abstract -

The polarization of the cosmic microwave background (CMB) can be used to search for parity-violating processes like that predicted by a Chern-Simons coupling to a light pseudoscalar field. Such an interaction rotates $E$ modes into $B$ modes in the observed CMB signal by an effect known as cosmic birefringence. Even though isotropic birefringence can be confused with the rotation produced by a miscalibration of the detectors' polarization angles the degeneracy between both effects is broken when Galactic foreground emission is used as a calibrator. In this work, we use realistic simulations of the High-Frequency Instrument of the Planck mission to test the impact that Galactic foreground emission and instrumental systematics have on the recent birefringence measurements obtained through this technique. Our results demonstrate the robustness of the methodology against the miscalibration of polarization angles and other systematic effects, like intensity-to-polarization leakage, beam leakage, or cross-polarization effects. However, our estimator is sensitive to the $EB$ correlation of polarized foreground emission. Here we propose to correct the bias induced by dust $EB$ by modeling the foreground signal with templates produced in Bayesian component-separation analyses that fit parametric models to CMB data. Acknowledging the limitations of currently available dust templates like that of the Commander sky model, high-precision CMB data and a characterization of dust beyond the modified blackbody paradigm are needed to obtain a definitive measurement of cosmic birefringence in the future.


(1013)Perturbation theory with dispersion and higher cumulants: framework and linear theory
  • Mathias Garny,
  • Dominik Laxhuber,
  • Roman Scoccimarro
arXiv e-prints (10/2022) e-Print:2210.08088
abstract + abstract -

The standard perturbation theory (SPT) approach to gravitational clustering is based on a fluid approximation of the underlying Vlasov-Poisson dynamics, taking only the zeroth and first cumulant of the phase-space distribution function into account (density and velocity fields). This assumption breaks down when dark matter particle orbits cross and leads to well-known problems, e.g. an anomalously large backreaction of small-scale modes onto larger scales that compromises predictivity. We extend SPT by incorporating second and higher cumulants generated by orbit crossing. For collisionless matter, their equations of motion are completely fixed by the Vlasov-Poisson system, and thus we refer to this approach as Vlasov Perturbation Theory (VPT). Even cumulants develop a background value, and they enter the hierarchy of coupled equations for the fluctuations. The background values are in turn sourced by power spectra of the fluctuations. The latter can be brought into a form that is formally analogous to SPT, but with an extended set of variables and linear as well as non-linear terms, that we derive explicitly. In this paper, we focus on linear solutions, which are far richer than in SPT, showing that modes that cross the dispersion scale set by the second cumulant are highly suppressed. We derive stability conditions on the background values of even cumulants from the requirement that exponential instabilities be absent. We also compute the expected magnitude of averaged higher cumulants for various halo models and show that they satisfy the stability conditions. Finally, we derive self-consistent solutions of perturbations and background values for a scaling universe and study the convergence of the cumulant expansion. The VPT framework provides a conceptually straightforward and deterministic extension of SPT that accounts for the decoupling of small-scale modes.


(1012)Indirect upper limits on $\ell_i\to\ell_j\gamma\gamma$ from $\ell_i\to\ell_j\gamma$
  • Fabiola Fortuna,
  • Alejandro Ibarra,
  • Xabier Marcano,
  • Marcela Marín,
  • Pablo Roig
arXiv e-prints (10/2022) e-Print:2210.05703
abstract + abstract -

We perform an effective field theory analysis to correlate the charged lepton flavor violating processes $\ell_i\to\ell_j\gamma\gamma$ and $\ell_i\to\ell_j\gamma$. Using the current upper bounds on the rate for $\ell_i\to\ell_j\gamma$, we derive model-independent upper limits on the rates for $\ell_i\to\ell_j\gamma\gamma$. Our indirect limits are about three orders of magnitude stronger than the direct bounds from current searches for $\mu\to e\gamma\gamma$, and four orders of magnitude better than current bounds for $\tau\to\ell\gamma\gamma$. We also stress the relevance of Belle II or a Super Tau Charm Facility to discover the rare decay $\tau\to\ell\gamma\gamma$.


(1011)The MADPSZ catalogue of Planck clusters over the DES region: extending to lower mass and higher redshift
  • D. Hernández-Lang,
  • J.J. Mohr,
  • M. Klein,
  • S. Grandis,
  • J.-B. Melin
  • +56
  • P. Tarrío,
  • M. Arnaud,
  • G.W. Pratt,
  • T.M.C. Abbott,
  • M. Aguena,
  • O. Alves,
  • F. Andrade-Oliveira,
  • D. Bacon,
  • E. Bertin,
  • D. Brooks,
  • D.L. Burke,
  • A. Carnero Rosell,
  • M. Carrasco Kind,
  • J. Carretero,
  • F.J. Castander,
  • M. Costanzi,
  • L.N. da Costa,
  • M.E.S. Pereira,
  • S. Desai,
  • H.T. Diehl,
  • P. Doel,
  • S. Everett,
  • I. Ferrero,
  • B. Flaugher,
  • J. Frieman,
  • J. García-Bellido,
  • D. Gruen,
  • R.A. Gruendl,
  • J. Gschwend,
  • G. Gutierrez,
  • S.R. Hinton,
  • D.L. Hollowood,
  • K. Honscheid,
  • D.J. James,
  • K. Kuehn,
  • N. Kuropatkin,
  • O. Lahav,
  • C. Lidman,
  • P. Melchior,
  • J. Mena-Fernández,
  • F. Menanteau,
  • R. Miquel,
  • A. Palmese,
  • F. Paz-Chinchón,
  • A. Pieres,
  • A.A. Plazas Malagón,
  • M. Raveri,
  • M. Rodriguez-Monroy,
  • A.K. Romer,
  • V. Scarpine,
  • I. Sevilla-Noarbe,
  • M. Smith,
  • E. Suchyta,
  • G. Tarle,
  • D. Thomas,
  • N. Weaverdyck
  • (less)
(10/2022) e-Print:2210.04666
abstract + abstract -

We present the first systematic follow-up of Planck Sunyaev-Zeldovich effect (SZE) selected candidates down to signal-to-noise (S/N) of 3 over the 5000 deg$^2$ covered by the Dark Energy Survey. Using the MCMF cluster confirmation algorithm, we identify optical counterparts, determine photometric redshifts and richnesses and assign a parameter, $f_{\rm cont}$, that reflects the probability that each SZE-optical pairing represents a real cluster rather than a random superposition of physically unassociated systems. The new MADPSZ cluster catalogue consists of 1092 MCMF confirmed clusters and has a purity of 85%. We present the properties of subsamples of the MADPSZ catalogue that have purities ranging from 90% to 97.5%, depending on the adopted $f_{\rm cont}$ threshold. $M_{500}$ halo mass estimates, redshifts, richnesses, and optical centers are presented for all MADPSZ clusters. The MADPSZ catalogue adds 828 previously unknown Planck identified clusters over the DES footprint and provides redshifts for an additional 50 previously published Planck selected clusters with S/N>4.5. Using the subsample with spectroscopic redshifts, we demonstrate excellent cluster photo-$z$ performance with an RMS scatter in $\Delta z/(1+z)$ of 0.47%. Our MCMF based analysis allows us to infer the contamination fraction of the initial S/N>3 Planck selected candidate list, which is 50%. We present a method of estimating the completeness of the MADPSZ cluster sample and $f_{\rm cont}$ selected subsamples. In comparison to the previously published Planck cluster catalogues. this new S/N $>$ 3 MCMF confirmed cluster catalogue populates the lower mass regime at all redshifts and includes clusters up to z$\sim$1.3.


(1010)Why Cosmic Voids Matter: Nonlinear Structure & Linear Dynamics
  • Nico Schuster,
  • Nico Hamaus,
  • Klaus Dolag,
  • Jochen Weller
(10/2022) e-Print:2210.02457
abstract + abstract -

We use the Magneticum suite of state-of-the-art hydrodynamical simulations to identify cosmic voids based on the watershed technique and investigate their most fundamental properties across different resolutions in mass and scale. This encompasses the distributions of void sizes, shapes, and content, as well as their radial density and velocity profiles traced by the distribution of cold dark matter particles and halos. We also study the impact of various tracer properties, such as their sparsity and mass, and the influence of void merging on these summary statistics. Our results reveal that all of the analyzed void properties are physically related to each other and describe universal characteristics that are largely independent of tracer type and resolution. Most notably, we find that the motion of tracers around void centers is perfectly consistent with linear dynamics, both for individual, as well as stacked voids. Despite the large range of scales accessible in our simulations, we are unable to identify the occurrence of nonlinear dynamics even inside voids of only a few Mpc in size. This suggests voids to be among the most pristine probes of cosmology down to scales that are commonly referred to as highly nonlinear in the field of large-scale structure.


(1009)Forecasting cosmological parameter constraints using multiple sparsity measurements as tracers of the mass profiles of dark matter haloes
  • P. S. Corasaniti,
  • A. M. C. Le Brun,
  • T. R. G. Richardson,
  • Y. Rasera,
  • S. Ettori
  • +2
Monthly Notices of the Royal Astronomical Society, 516, p16 (10/2022) doi:10.1093/mnras/stac2196
abstract + abstract -

The dark matter halo sparsity, i.e. the ratio between spherical halo masses enclosing two different overdensities, provides a non-parametric proxy of the halo mass distribution that has been shown to be a sensitive probe of the cosmological imprint encoded in the mass profile of haloes hosting galaxy clusters. Mass estimations at several overdensities would allow for multiple sparsity measurements, which can potentially retrieve the entirety of the cosmological information imprinted on the halo profile. Here, we investigate the impact of multiple sparsity measurements on the cosmological model parameter inference. For this purpose, we analyse N-body halo catalogues from the Raygal and M2Csims simulations and evaluate the correlations among six different sparsities from spherical overdensity halo masses at Δ = 200, 500, 1000, and 2500 (in units of the critical density). Remarkably, sparsities associated to distinct halo mass shells are not highly correlated. This is not the case for sparsities obtained using halo masses estimated from the Navarro-Frenk-White (NFW) best-fitting profile, which artificially correlates different sparsities to order one. This implies that there is additional information in the mass profile beyond the NFW parametrization and that it can be exploited with multiple sparsities. In particular, from a likelihood analysis of synthetic average sparsity data, we show that cosmological parameter constraints significantly improve when increasing the number of sparsity combinations, though the constraints saturate beyond four sparsity estimates. We forecast constraints for the CHEX-MATE cluster sample and find that systematic mass bias errors mildly impact the parameter inference, though more studies are needed in this direction.


(1008)The MillenniumTNG Project: High-precision predictions for matter clustering and halo statistics
  • César Hernández-Aguayo,
  • Volker Springel,
  • Rüdiger Pakmor,
  • Monica Barrera,
  • Fulvio Ferlito
  • +7
  • Simon D. M. White,
  • Lars Hernquist,
  • Boryana Hadzhiyska,
  • Ana Maria Delgado,
  • Rahul Kannan,
  • Sownak Bose,
  • Carlos Frenk
  • (less)
arXiv e-prints (10/2022) e-Print:2210.10059
abstract + abstract -

Cosmological inference with large galaxy surveys requires theoretical models that combine precise predictions for large-scale structure with robust and flexible galaxy formation modelling throughout a sufficiently large cosmic volume. Here, we introduce the MillenniumTNG (MTNG) project which combines the hydrodynamical galaxy formation model of IllustrisTNG with the large volume of the Millennium simulation. Our largest hydrodynamic simulation, covering (500 Mpc/h)^3 = (740 Mpc)^3, is complemented by a suite of dark-matter-only simulations with up to 4320^3 dark matter particles (a mass resolution of 1.32 x 10^8 Msun/h) using the fixed-and-paired technique to reduce large-scale cosmic variance. The hydro simulation adds 4320^3 gas cells, achieving a baryonic mass resolution of 2 x 10^7 Msun/h. High time-resolution merger trees and direct lightcone outputs facilitate the construction of a new generation of semi-analytic galaxy formation models that can be calibrated against both the hydro simulation and observation, and then applied to even larger volumes - MTNG includes a flagship simulation with 1.1 trillion dark matter particles and massive neutrinos in a volume of (3000 Mpc)^3. In this introductory analysis we carry out convergence tests on basic measures of non-linear clustering such as the matter power spectrum, the halo mass function and halo clustering, and we compare simulation predictions to those from current cosmological emulators. We also use our simulations to study matter and halo statistics, such as halo bias and clustering at the baryonic acoustic oscillation scale. Finally we measure the impact of baryonic physics on the matter and halo distributions.


(1007)The MillenniumTNG Project: Inferring cosmology from galaxy clustering with accelerated N-body scaling and subhalo abundance matching
  • Sergio Contreras,
  • Raul E. Angulo,
  • Volker Springel,
  • Simon D. M. White,
  • Boryana Hadzhiyska
  • +9
  • Lars Hernquist,
  • Rüdiger Pakmor,
  • Rahul Kannan,
  • César Hernández-Aguayo,
  • Monica Barrera,
  • Fulvio Ferlito,
  • Ana Maria Delgado,
  • Sownak Bose,
  • Carlos Frenk
  • (less)
arXiv e-prints (10/2022) e-Print:2210.10075
abstract + abstract -

We introduce a novel technique for constraining cosmological parameters and galaxy assembly bias using non-linear redshift-space clustering of galaxies. We scale cosmological N-body simulations and insert galaxies with the SubHalo Abundance Matching extended (SHAMe) empirical model to generate over 175,000 clustering measurements spanning all relevant cosmological and SHAMe parameter values. We then build an emulator capable of reproducing the projected galaxy correlation function at the monopole, quadrupole and hexadecapole level for separations between $0.1\,h^{-1}{\rm Mpc}$ and $25\,h^{-1}{\rm Mpc}$. We test this approach by using the emulator and Monte Carlo Markov Chain (MCMC) inference to jointly estimate cosmology and assembly bias parameters both for the MTNG740 hydrodynamic simulation and for a semi-analytical galaxy formation model (SAM) built on the MTNG740-DM dark matter-only simulation, obtaining unbiased results for all cosmological parameters. For instance, for MTNG740 and a galaxy number density of $n\sim 0.01 h^{3}{\rm Mpc}^{-3}$, we obtain $\sigma_{8}=0.799^{+0.039}_{-0.044}$ ($\sigma_{8,{\rm MTNG}} =$ 0.8159), and $\Omega_\mathrm{M}h^2= 0.138^{+ 0.025}_{- 0.018}$ ($\Omega_{\mathrm{M}} h^2_{\rm MTNG} =$ 0.142). For fixed Hubble parameter ($h$), the constraint becomes $\Omega_\mathrm{M}h^2= 0.137^{+ 0.011}_{- 0.012}$. Our method performs similarly well for the SAM and for other tested sample densities. We almost always recover the true amount of galaxy assembly bias within one sigma. The best constraints are obtained when scales smaller than $2\,h^{-1}{\rm Mpc}$ are included, as well as when at least the projected correlation function and the monopole are incorporated. These methods offer a powerful way to constrain cosmological parameters using galaxy surveys.


(1006)Endpoint factorization and next-to-leading power resummation of gluon thrust
  • M. Beneke,
  • M. Garny,
  • S. Jaskiewicz,
  • J. Strohm,
  • R. Szafron
  • +2
Loops and Legs in Quantum Field Theory (10/2022)
abstract + abstract -

Endpoint divergences in the convolution integrals appearing in next-to-leading-power factorization theorems prevent a straightforward application of standard methods to resum large logarithmic power-suppressed corrections in collider physics. We study the power-suppressed configuration of the thrust distribution in the two-jet region, where a gluon-initiated jet recoils against a quark-antiquark pair. With the aid of operatorial endpoint factorization conditions, we derive a factorization formula where the individual terms are free from endpoint divergences and can be written in terms of renormalized hard, (anti) collinear, and soft functions in four dimensions. This framework enables us to perform the first resummation of the endpoint-divergent SCET$_{\rm I}$ observables at the leading logarithmic accuracy using exclusively renormalization-group methods.


(1005)The MillenniumTNG Project: An improved two-halo model for the galaxy-halo connection of red and blue galaxies
  • Boryana Hadzhiyska,
  • Daniel Eisenstein,
  • Lars Hernquist,
  • Rüdiger Pakmor,
  • Sownak Bose
  • +9
  • Ana Maria Delgado,
  • Sergio Contreras,
  • Rahul Kannan,
  • Simon D. M. White,
  • Volker Springel,
  • Carlos Frenk,
  • César Hernández-Aguayo,
  • Fulvio Ferlito,
  • Monica Barrera
  • (less)
arXiv e-prints (10/2022) e-Print:2210.10072
abstract + abstract -

Approximate methods to populate dark matter halos with galaxies are of great utility to large galaxy surveys. However, the limitations of simple halo occupation models (HODs) preclude a full use of small-scale galaxy clustering data and call for more sophisticated models. We study two galaxy populations, luminous red galaxies (LRGs) and star-forming emission-line galaxies (ELGs), at two epochs, $z=1$ and $z=0$, in the large volume, high-resolution hydrodynamical simulation of the MillenniumTNG project. In a partner study we concentrated on the small-scale, one-halo regime down to $r\sim 0.1{\rm Mpc}/h$, while here we focus on modeling galaxy assembly bias in the two-halo regime, $r\gtrsim 1{\rm Mpc}/h$. Interestingly, the ELG signal exhibits scale dependence out to relatively large scales ($r\sim 20{\rm Mpc}/h$), implying that the linear bias approximation for this tracer is invalid on these scales, contrary to common assumptions. The 10-15\% discrepancy present in the standard halo model prescription is only reconciled when we augment our halo occupation model with a dependence on extrinsic halo properties ("shear" being the best-performing one) rather than intrinsic ones (e.g., concentration, peak mass). We argue that this fact constitutes evidence for two-halo galaxy conformity. Including tertiary assembly bias (i.e. a property beyond mass and "shear") is not an essential requirement for reconciling the galaxy assembly bias signal of LRGs, but the combination of external and internal properties is beneficial for recovering ELG the clustering. We find that centrals in low-mass haloes dominate the assembly bias signal of both populations. Finally, we explore the predictions of our model for higher-order statistics such as nearest-neighbor counts. The latter supplies additional information about galaxy assembly bias and can be used to break degeneracies between halo model parameters.


(1004)Systematic parametrization of the leading B-meson light-cone distribution amplitude
  • Thorsten Feldmann,
  • Philip Lüghausen,
  • Danny van Dyk
Journal of High Energy Physics, 2022 (10/2022) doi:10.1007/JHEP10(2022)162
abstract + abstract -

We propose a parametrization of the leading B-meson light-cone distribution amplitude (LCDA) in heavy-quark effective theory (HQET). In position space, it uses a conformal transformation that yields a systematic Taylor expansion and an integral bound, which enables control of the truncation error. Our parametrization further produces compact analytical expressions for a variety of derived quantities. At a given reference scale, our momentum-space parametrization corresponds to an expansion in associated Laguerre polynomials, which turn into confluent hypergeometric functions 1F1 under renormalization-group evolution at one-loop accuracy. Our approach thus allows a straightforward and transparent implementation of a variety of phenomenological constraints, regardless of their origin. Moreover, we can include theoretical information on the Taylor coefficients by using the local operator product expansion. We showcase the versatility of the parametrization in a series of phenomenological pseudo-fits.


(1003)Lower-than-expected flare temperatures for TRAPPIST-1
  • A. J. Maas,
  • E. Ilin,
  • M. Oshagh,
  • E. Pallé,
  • H. Parviainen
  • +10
  • K. Molaverdikhani,
  • A. Quirrenbach,
  • E. Esparza-Borges,
  • F. Murgas,
  • V. J. S. Béjar,
  • N. Narita,
  • A. Fukui,
  • C. -L. Lin,
  • M. Mori,
  • P. Klagyivik
  • (less)
arXiv e-prints (10/2022) e-Print:2210.11103
abstract + abstract -

Although high energetic radiation from flares is a potential threat to exoplanet atmospheres and may lead to surface sterilization, it might also provide the extra energy for low-mass stars needed to trigger and sustain prebiotic chemistry. We investigate two flares on TRAPPIST-1, an ultra-cool dwarf star that hosts seven exoplanets of which three lie within its habitable zone. The flares are detected in all four passbands of the MuSCAT2 allowing a determination of their temperatures and bolometric energies. We analyzed the light curves of the MuSCAT1 and MuSCAT2 instruments obtained between 2016 and 2021 in $g,r,i,z_\mathrm{s}$-filters. We conducted an automated flare search and visually confirmed possible flare events. We studied the temperature evolution, the global temperature, and the peak temperature of both flares. For the first time we infer effective black body temperatures of flares that occurred on TRAPPIST-1. The black body temperatures for the two TRAPPIST-1 flares derived from the SED are consistent with $T_\mathrm{SED} = 7940_{-390}^{+430}$K and $T_\mathrm{SED} = 6030_{-270}^{+300}$K. The flare black body temperatures at the peak are also calculated from the peak SED yielding $T_\mathrm{SEDp} = 13620_{-1220}^{1520}$K and $T_\mathrm{SEDp} = 8290_{-550}^{+660}$K. We show that for the ultra-cool M-dwarf TRAPPIST-1 the flare black body temperatures associated with the total continuum emission are lower and not consistent with the usually adopted assumption of 9000-10000 K. This could imply different and faster cooling mechanisms. Further multi-color observations are needed to investigate whether or not our observations are a general characteristic of ultra-cool M-dwarfs. This would have significant implications for the habitability of exoplanets around these stars because the UV surface flux is likely to be overestimated by the models with higher flare temperatures.


(1002)Spin fields for the spinning particle
  • E. Boffo,
  • I. Sachs
Journal of High Energy Physics, 2022 (10/2022) doi:10.1007/JHEP10(2022)117
abstract + abstract -

We propose an analogue of spin fields for the relativistic RNS-particle in 4 dimensions, in order to describe Ramond-Ramond states as "two-particle" excitations on the world line. On a natural representation space we identify a differential whose cohomology agrees with RR-fields equations. We then discuss the non-linear theory encoded in deformations of the latter by background fields. We also formulate a sigma model for this spin field from which we recover the RNS-formulation by imposing suitable constraints.


(1001)Toward a population synthesis of disks and planets. I. Evolution of dust with entrainment in winds and radiation pressure
  • R. Burn,
  • A. Emsenhuber,
  • J. Weder,
  • O. Völkel,
  • H. Klahr
  • +3
  • T. Birnstiel,
  • B. Ercolano,
  • C. Mordasini
  • (less)
Astronomy and Astrophysics, 666, p15 (10/2022) doi:10.1051/0004-6361/202243262
abstract + abstract -

Context. Millimeter astronomy provides valuable information on the birthplaces of planetary systems. In order to compare theoretical models with observations, the dust component has to be carefully calculated.
Aims: Here, we aim to study the effects of dust entrainment in photoevaporative winds, and the ejection and drag of dust due to the effects caused by radiation from the central star.
Methods: We improved and extended the existing implementation of a two-population dust and pebble description in the global Bern/Heidelberg planet formation and evolution model. Modern prescriptions for photoevaporative winds were used and we accounted for settling and advection of dust when calculating entrainment rates. In order to prepare for future population studies with varying conditions, we explored a wide range of disk, photoevaporation, and dust parameters.
Results: If dust can grow to pebble sizes, that is, if they are resistant to fragmentation or turbulence is weak, drift dominates and the entrained mass is small but larger than under the assumption of no vertical advection of grains with the gas flow. For the case of fragile dust shattering at velocities of 1m s−1 - as indicated in laboratory experiments -, an order of magnitude more dust is entrained, which becomes the main dust removal process. Radiation pressure effects disperse massive, dusty disks on timescales of a few hundred Myr.
Conclusions: These results highlight the importance of dust entrainment in winds as a solid-mass removal process. Furthermore, this model extension lays the foundations for future statistical studies of the formation of planets in their birth environment.


(1000)The phase structure of cosmic ray driven outflows in stream fed disc galaxies
  • Nicolas Peschken,
  • Michał Hanasz,
  • Thorsten Naab,
  • Dominik Wóltański,
  • Artur Gawryszczak
arXiv e-prints (10/2022) e-Print:2210.17328
abstract + abstract -

Feeding with gas in streams is predicted to be an important galaxy growth mechanism. Using an idealised setup, we study the impact of stream feeding (with 10$^7$ M$_{\odot}$ Myr$^{-1}$ rate) on the star formation and outflows of disc galaxies with $\sim$10$^{11}$ M$_{\odot}$ baryonic mass. The magneto-hydrodynamical simulations are carried out with the PIERNIK code and include star formation, feedback from supernova, and cosmic ray advection and diffusion. We find that stream accretion enhances galactic star formation. Lower angular momentum streams result in more compact discs, higher star formation rates and stronger outflows. In agreement with previous studies, models including cosmic rays launch stronger outflows travelling much further into the galactic halo. Cosmic ray supported outflows are also cooler than supernova only driven outflows. With cosmic rays, the star formation is suppressed and the thermal pressure is reduced. We find evidence for two distinct outflow phases. The warm outflows have high angular momentum and stay close to the galactic disc, while the hot outflow phase has low angular momentum and escapes from the centre deep into the halo. Cosmic rays can therefore have a strong impact on galaxy evolution by removing low angular momentum, possibly metal enriched gas from the disc and injecting it into the circumgalactic medium.


(999)ALMACAL IX: Multi-band ALMA survey for dusty star-forming galaxies and the resolved fractions of the cosmic infrared background
  • Jianhang Chen,
  • R. J. Ivison,
  • Martin A. Zwaan,
  • Ian Smail,
  • Anne Klitsch
  • +6
  • Céline Péroux,
  • Gergö Popping,
  • Andrew D. Biggs,
  • Roland Szakacs,
  • Aleksandra Hamanowicz,
  • Claudia Lagos
  • (less)
Monthly Notices of the Royal Astronomical Society (10/2022) doi:10.1093/mnras/stac2989
abstract + abstract -

Wide, deep, blind continuum surveys at submillimetre/millimetre (submm/mm) wavelengths are required to provide a full inventory of the dusty, distant Universe. However, conducting such surveys to the necessary depth, with sub-arcsec angular resolution, is prohibitively time-consuming, even for the most advanced submm/mm telescopes. Here, we report the most recent results from the ALMACAL project, which exploits the 'free' calibration data from the Atacama Large Millimetre/submillimetre Array (ALMA) to map the lines of sight towards and beyond the ALMA calibrators. ALMACAL has now covered 1,001 calibrators, with a total sky coverage around 0.3 deg2, distributed across the sky accessible from the Atacama desert, and has accumulated more than 1,000 h of integration. The depth reached by combining multiple visits to each field makes ALMACAL capable of searching for faint, dusty, star-forming galaxies (DSFGs), with detections at multiple frequencies to constrain the emission mechanism. Based on the most up-to-date ALMACAL database, we report the detection of 186 DSFGs with flux densities down to S870μm ~ 0.2 mJy, comparable with existing ALMA large surveys but less susceptible to cosmic variance. We report the number counts at five wavelengths between 870 μm and 3 mm, in ALMA bands 3, 4, 5, 6 and 7, providing a benchmark for models of galaxy formation and evolution. By integrating the observed number counts and the best-fitting functions, we also present the resolved fraction of the cosmic infrared background (CIB) and the CIB spectral shape. Combining existing surveys, ALMA has currently resolved about half of the CIB in the submm/mm regime.


(998)Cosmic voids as cosmological laboratories
  • Carlos Mauricio Correa
arXiv e-prints (10/2022) e-Print:2210.17459
abstract + abstract -

Cosmic voids are promising cosmological laboratories for studying the dark energy phenomenon and alternative gravity theories. They are receiving special attention nowadays in view of the new generation of galaxy spectroscopic surveys, which are covering an unprecedented volume and redshift range. There are two primary statistics in void studies: (i) the void size function, which characterises the abundance of voids, and (ii) the void-galaxy cross-correlation function, which contains information about the density and velocity fields in these regions. However, it is necessary a complete description of the effects of geometrical (Alcock-Paczynski effect, AP) and dynamical (Kaiser effect, RSD) distortions around voids in order to design reliable cosmological tests based on these statistics. Observational measurements show prominent anisotropic patterns that lead to biased cosmological constraints if they are not properly modelled. This thesis addresses this problematic by presenting a theoretical and statistical framework based on dynamical and cosmological foundations capable of describing all the underlying effects involved: the expansion effect (t-RSD), the off-centring effect (v-RSD), the AP-volume effect and the ellipticity effect (e-RSD). These effects can be understood by studying the mapping of voids between real and redshift space. In this way, we lay the foundations for a proper modelling of the aforementioned statistics. In addition, we present a new cosmological test based on two perpendicular projections of the correlation function. The method is fiducial-cosmology free, which allows us to effectively break any possible degeneracy between the cosmological parameters involved. Moreover, it allows us to significantly reduce the number of mock catalogues needed to estimate covariances.


(997)Razor-thin dust layers in protoplanetary disks: Limits on the vertical shear instability
  • C. P. Dullemond,
  • A. Ziampras,
  • D. Ostertag,
  • C. Dominik
arXiv e-prints (10/2022) e-Print:2210.13413
abstract + abstract -

Context: Recent observations with the Atacama Large Millimeter Array (ALMA) have shown that the large dust aggregates observed at millimeter wavelengths settle to the midplane into a remarkably thin layer. Aims: We intend to find out if the geometric thinness of these layers is evidence against the vertical shear instability (VSI) operating in these disks. Methods: We performed hydrodynamic simulations of a protoplanetary disk with a locally isothermal equation of state, and let the VSI fully develop. We sprinkled dust particles and followed their motion as they got stirred up by the VSI. We determined for which grain size the layer becomes geometrically thin enough to be consistent with ALMA observations. We then verified if, with these grain sizes, it is still possible to generate a moderately optically thick layer at millimeter wavelengths, as observations appear to indicate. Results: We found that even very large dust aggregates with Stokes numbers close to unity get stirred up to relatively large heights above the midplane by the VSI, which is in conflict with the observed geometric thinness. For grains so large that the Stokes number exceeds unity, the layer can be made to remain thin, but we show that it is hard to make dust layers optically thick at ALMA wavelengths (e.g., tau(1.3mm)>=1) with such large dust aggregates. Conclusions: We conclude that protoplanetary disks with geometrically thin midplane dust layers cannot be VSI unstable, at least not down to the disk midplane. Explanations for the inhibition of the VSI include a reduced dust-to-gas ratio of the small dust grains that are responsible for the radiative cooling of the disk. A reduction of small grains by a factor of between 10 and 100 is sufficient to quench the VSI. Such a reduction is plausible in dust growth models, and still consistent with observations at optical and infrared wavelengths.


(996)Inclusive production of $J/\psi$, $\psi(2S)$, and $\Upsilon$ states in pNRQCD
  • Nora Brambilla,
  • Hee Sok Chung,
  • Antonio Vairo,
  • Xiang-Peng Wang
arXiv e-prints (10/2022) e-Print:2210.17345
abstract + abstract -

Under some assumptions on the hierarchy of relevant energy scales, we compute the nonrelativistic QCD (NRQCD) long-distance matrix elements (LDMEs) for inclusive production of $J/\psi$, $\psi(2S)$, and $\Upsilon$ states based on the potential NRQCD (pNRQCD) effective field theory. Based on the pNRQCD formalism, we obtain expressions for the LDMEs in terms of the quarkonium wavefunctions at the origin and universal gluonic correlators, which do not depend on the heavy quark flavor or the radial excitation. This greatly reduces the number of nonperturbative unknowns and substantially enhances the predictive power of the nonrelativistic effective field theory formalism. We obtain improved determinations of the LDMEs for $J/\psi$, $\psi(2S)$, and $\Upsilon$ states thanks to the universality of the gluonic correlators, and obtain phenomenological results for cross sections and polarizations at large transverse momentum that agree well with measurements at the LHC.


(995)Strong lensing time-delay cosmography in the 2020s
  • T. Treu,
  • S. H. Suyu,
  • P. J. Marshall
arXiv e-prints (10/2022) e-Print:2210.15794
abstract + abstract -

Multiply imaged time-variable sources can be used to measure absolute distances as a function of redshifts and thus determine cosmological parameters, chiefly the Hubble Constant H$_0$. In the two decades up to 2020, through a number of observational and conceptual breakthroughs, this so-called time-delay cosmography has reached a precision sufficient to be an important independent voice in the current ``Hubble tension'' debate between early- and late-universe determinations of H$_0$. The 2020s promise to deliver major advances in time-delay cosmography, owing to the large number of lenses to be discovered by new and upcoming surveys and the vastly improved capabilities for follow-up and analysis. In this review -- after a brief summary of the foundations of the method and recent advances -- we outline the opportunities for the decade and the challenges that will need to be overcome in order to meet the goal of the determination of H$_0$ from time-delay cosmography with 1\% precision and accuracy.


(994)The MillenniumTNG Project: Refining the one-halo model of red and blue galaxies at different redshifts
  • Boryana Hadzhiyska,
  • Lars Hernquist,
  • Daniel Eisenstein,
  • Ana Maria Delgado,
  • Sownak Bose
  • +9
  • Rahul Kannan,
  • Rüdiger Pakmor,
  • Volker Springel,
  • Sergio Contreras,
  • Monica Barrera,
  • Fulvio Ferlito,
  • César Hernández-Aguayo,
  • Simon D. M. White,
  • Carlos Frenk
  • (less)
arXiv e-prints (10/2022) e-Print:2210.10068
abstract + abstract -

Luminous red galaxies (LRGs) and blue star-forming emission-line galaxies (ELGs) are key tracers of large-scale structure used by cosmological surveys. Theoretical predictions for such data are often done via simplistic models for the galaxy-halo connection. In this work, we use the large, high-fidelity hydrodynamical simulation of the MillenniumTNG project (MTNG) to inform a new phenomenological approach for obtaining an accurate and flexible galaxy-halo model on small scales. Our aim is to study LRGs and ELGs at two distinct epochs, $z = 1$ and $z = 0$, and recover their clustering down to very small scales, $r \sim 0.1 \ {\rm Mpc}/h$, i.e. the one-halo regime, while a companion paper extends this to a two-halo model for larger distances. The occupation statistics of ELGs in MTNG inform us that: (1) the satellite occupations exhibit a slightly super-Poisson distribution, contrary to commonly made assumptions, and (2) that haloes containing at least one ELG satellite are twice as likely to host a central ELG. We propose simple recipes for modeling these effects, each of which calls for the addition of a single free parameter to simpler halo occupation models. To construct a reliable satellite population model, we explore the LRG and ELG satellite radial and velocity distributions and compare them with those of subhalos and particles in the simulation. We find that ELGs are anisotropically distributed within halos, which together with our occupation results provides strong evidence for cooperative galaxy formation (manifesting itself as one-halo galaxy conformity); i.e.~galaxies with similar properties form in close proximity to each other. Our refined galaxy-halo model represents a useful improvement of commonly used analysis tools and thus can be of help to increase the constraining power of large-scale structure surveys.


(993)The MillenniumTNG Project: Semi-analytic galaxy formation models on the past lightcone
  • Monica Barrera,
  • Volker Springel,
  • Simon White,
  • César Hernández-Aguayo,
  • Lars Hernquist
  • +7
  • Carlos Frenk,
  • Rüdiger Pakmor,
  • Fulvio Ferlito,
  • Boryana Hadzhiyska,
  • Ana Maria Delgado,
  • Rahul Kannan,
  • Sownak Bose
  • (less)
arXiv e-prints (10/2022) e-Print:2210.10419
abstract + abstract -

Upcoming large galaxy surveys will subject the standard cosmological model, $\Lambda$CDM, to new precision tests. These can be tightened considerably if theoretical models of galaxy formation are available that can predict galaxy clustering and galaxy-galaxy lensing on the full range of measurable scales throughout volumes as large as those of the surveys and with sufficient flexibility that uncertain aspects of the underlying astrophysics can be marginalised over. This, in particular, requires mock galaxy catalogues in large cosmological volumes that can be directly compared to observation, and can be optimised empirically by Monte Carlo Markov Chains or other similar schemes to eliminate or estimate astrophysical parameters related to galaxy formation when constraining cosmology. Semi-analytic galaxy formation methods implemented on top of cosmological dark matter simulations offer a computationally efficient approach to construct physically based and flexibly parametrised galaxy formation models, and as such they are more potent than still faster, but purely empirical models. Here we introduce an updated methodology for the semi-analytic L-GALAXIES code, allowing it to be applied to simulations of the new MillenniumTNG project, producing galaxies directly on fully continuous past lightcones, potentially over the full sky, out to high redshift, and for all galaxies more massive than $\sim 10^8\,{\rm M}_\odot$. We investigate the numerical convergence of the resulting predictions, and study the projected galaxy clustering signals of different samples. The new methodology can be viewed as an important step towards more faithful forward-modelling of observational data, helping to reduce systematic distortions in the comparison of theory to observations.


(992)The MillenniumTNG Project: The hydrodynamical full physics simulation and a first look at its galaxy clusters
  • Ruediger Pakmor,
  • Volker Springel,
  • Jonathan P. Coles,
  • Thomas Guillet,
  • Christoph Pfrommer
  • +10
  • Sownak Bose,
  • Monica Barrera,
  • Ana Maria Delgado,
  • Fulvio Ferlito,
  • Carlos Frenk,
  • Boryana Hadzhiyska,
  • César Hernández-Aguayo,
  • Lars Hernquist,
  • Rahul Kannan,
  • Simon D. M. White
  • (less)
arXiv e-prints (10/2022) e-Print:2210.10060
abstract + abstract -

Cosmological simulations are an important theoretical pillar for understanding nonlinear structure formation in our Universe and for relating it to observations on large scales. In several papers, we introduce our MillenniumTNG (MTNG) project that provides a comprehensive set of high-resolution, large volume simulations of cosmic structure formation aiming to better understand physical processes on large scales and to help interpreting upcoming large-scale galaxy surveys. We here focus on the full physics box MTNG740 that computes a volume of $(740\,\mathrm{Mpc})^3$ with a baryonic mass resolution of $3.1\times~10^7\,\mathrm{M_\odot}$ using \textsc{arepo} with $80.6$~billion cells and the IllustrisTNG galaxy formation model. We verify that the galaxy properties produced by MTNG740 are consistent with the TNG simulations, including more recent observations. We focus on galaxy clusters and analyse cluster scaling relations and radial profiles. We show that both are broadly consistent with various observational constraints. We demonstrate that the SZ-signal on a deep lightcone is consistent with Planck limits. Finally, we compare MTNG740 clusters with galaxy clusters found in Planck and the SDSS-8 RedMaPPer richness catalogue in observational space, finding very good agreement as well. However, {\it simultaneously} matching cluster masses, richness, and Compton-$y$ requires us to assume that the SZ mass estimates for Planck clusters are underestimated by $0.2$~dex on average. Thanks to its unprecedented volume for a high-resolution hydrodynamical calculation, the MTNG740 simulation offers rich possibilities to study baryons in galaxies, galaxy clusters, and in large scale structure, and in particular their impact on upcoming large cosmological surveys.


(991)The MillenniumTNG Project: The large-scale clustering of galaxies
  • Sownak Bose,
  • Boryana Hadzhiyska,
  • Monica Barrera,
  • Ana Maria Delgado,
  • Fulvio Ferlito
  • +7
  • Carlos Frenk,
  • César Hernández-Aguayo,
  • Lars Hernquist,
  • Rahul Kannan,
  • Rüdiger Pakmor,
  • Volker Springel,
  • Simon D. M. White
  • (less)
arXiv e-prints (10/2022) e-Print:2210.10065
abstract + abstract -

Modern redshift surveys are tasked with mapping out the galaxy distribution over enormous distance scales. Existing hydrodynamical simulations, however, do not reach the volumes needed to match upcoming surveys. We present results for the clustering of galaxies using a new, large volume hydrodynamical simulation as part of the MillenniumTNG (MTNG) project. With a computational volume that is $\approx15$ times larger than the next largest such simulation currently available, we show that MTNG is able to accurately reproduce the observed clustering of galaxies as a function of stellar mass. When separated by colour, there are some discrepancies with respect to the observed population, which can be attributed to the quenching of satellite galaxies in our model. We combine MTNG galaxies with those generated using a semi-analytic model to emulate the sample selection of luminous red galaxies (LRGs) and emission line galaxies (ELGs), and show that although the bias of these populations is approximately (but not exactly) constant on scales larger than $\approx10$ Mpc, there is significant scale-dependent bias on smaller scales. The amplitude of this effect varies between the two galaxy types, and also between the semi-analytic model and MTNG. We show that this is related to the distribution of haloes hosting LRGs and ELGs. Using mock SDSS-like catalogues generated on MTNG lightcones, we demonstrate the existence of prominent baryonic acoustic features in the large-scale galaxy clustering. We also demonstrate the presence of realistic redshift space distortions in our mocks, finding excellent agreement with the multipoles of the redshift-space clustering measured in SDSS data.


(990)TOI-1468: A system of two transiting planets, a super-Earth and a mini-Neptune, on opposite sides of the radius valley
  • P. Chaturvedi,
  • P. Bluhm,
  • E. Nagel,
  • A. P. Hatzes,
  • G. Morello
  • +65
  • M. Brady,
  • J. Korth,
  • K. Molaverdikhani,
  • D. Kossakowski,
  • J. A. Caballero,
  • E. W. Guenther,
  • E. Pallé,
  • N. Espinoza,
  • A. Seifahrt,
  • N. Lodieu,
  • C. Cifuentes,
  • E. Furlan,
  • P. J. Amado,
  • T. Barclay,
  • J. Bean,
  • V. J. S. Béjar,
  • G. Bergond,
  • A. W. Boyle,
  • D. Ciardi,
  • K. A. Collins,
  • K. I. Collins,
  • E. Esparza-Borges,
  • A. Fukui,
  • C. L. Gnilka,
  • R. Goeke,
  • P. Guerra,
  • Th. Henning,
  • E. Herrero,
  • S. B. Howell,
  • S. V. Jeffers,
  • J. M. Jenkins,
  • E. L. N. Jensen,
  • D. Kasper,
  • T. Kodama,
  • D. W. Latham,
  • M. J. López-González,
  • R. Luque,
  • D. Montes,
  • J. C. Morales,
  • M. Mori,
  • F. Murgas,
  • N. Narita,
  • G. Nowak,
  • H. Parviainen,
  • V. M. Passegger,
  • A. Quirrenbach,
  • S. Reffert,
  • A. Reiners,
  • I. Ribas,
  • G. R. Ricker,
  • E. Rodriguez,
  • C. Rodríguez-López,
  • M. Schlecker,
  • R. P. Schwarz,
  • A. Schweitzer,
  • S. Seager,
  • G. Stefánsson,
  • C. Stockdale,
  • L. Tal-Or,
  • J. D. Twicken,
  • S. Vanaverbeke,
  • G. Wang,
  • D. Watanabe,
  • J. N. Winn,
  • M. Zechmeister
  • (less)
Astronomy and Astrophysics, 666, p25 (10/2022) doi:10.1051/0004-6361/202244056
abstract + abstract -

We report the discovery and characterization of two small transiting planets orbiting the bright M3.0V star TOI-1468 (LSPM J0106+1913), whose transit signals were detected in the photometric time series in three sectors of the TESS mission. We confirm the planetary nature of both of them using precise radial velocity measurements from the CARMENES and MAROON-X spectrographs, and supplement them with ground-based transit photometry. A joint analysis of all these data reveals that the shorter-period planet, TOI-1468 b (Pb = 1.88 d), has a planetary mass of Mb = 3.21 ± 0.24M and a radius of Rb = 1.280−0.039+0.038 R, resulting in a density of ρb = 8.39−0.92+1.05 g cm−3, which is consistent with a mostly rocky composition. For the outer planet, TOI-1468 c (Pc = 15.53 d), we derive a mass of Mc = 6.64−0.68+0.67 M,aradius of Rc = 2.06 ± 0.04 R, and a bulk density of ρc = 2.00−0.19+0.21 g cm−3, which corresponds to a rocky core composition with a H/He gas envelope. These planets are located on opposite sides of the radius valley, making our system an interesting discovery as there are only a handful of other systems with the same properties. This discovery can further help determine a more precise location of the radius valley for small planets around M dwarfs and, therefore, shed more light on planet formation and evolution scenarios.

Radial velocities and photometry are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/666/A155


(989)Time-Delay Cosmography: Measuring the Hubble Constant and other cosmological parameters with strong gravitational lensing
  • S. Birrer,
  • M. Millon,
  • D. Sluse,
  • A. J. Shajib,
  • F. Courbin
  • +3
  • L. V. E. Koopmans,
  • S. H. Suyu,
  • T. Treu
  • (less)
arXiv e-prints (10/2022) e-Print:2210.10833
abstract + abstract -

Multiply lensed sources experience a relative time delay in the arrival of photons. This effect can be used to measure absolute distances and the Hubble constant ($H_0$) and is known as time-delay cosmography. The methodology is independent of the local distance ladder and early-universe physics and provides a precise and competitive measurement of $H_0$. With upcoming observatories, time-delay cosmography can provide a 1% precision measurement of $H_0$ and can decisively shed light on the current reported 'Hubble tension'. This paper presents the theoretical background and the current techniques applied for time-delay cosmographic studies and the measurement of the Hubble constant. The paper describes the challenges and systematics in the different components of the analysis and strategies to mitigate them. The current measurements are discussed in context and the opportunities with the anticipated data sets in the future are laid out.


(988)Super-sample covariance of the power spectrum, bispectrum, halos, voids, and their cross-covariances
  • Adrian E. Bayer,
  • Jia Liu,
  • Ryo Terasawa,
  • Alexandre Barreira,
  • Yici Zhong
  • +1
arXiv e-prints (10/2022) e-Print:2210.15647
abstract + abstract -

We study the effect of super-sample covariance (SSC) on the power spectrum and higher-order statistics: bispectrum, halo mass function, and void size function. We also investigate the effect of SSC on the cross-covariance between the statistics. We consider both the matter and halo fields. Higher-order statistics of the large-scale structure contain additional cosmological information beyond the power spectrum and are a powerful tool to constrain cosmology. They are a promising probe for ongoing and upcoming high precision cosmological surveys such as DESI, PFS, Rubin Observatory LSST, Euclid, SPHEREx, SKA, and Roman Space Telescope. Cosmological simulations used in modeling and validating these statistics often have sizes that are much smaller than the observed Universe. Density fluctuations on scales larger than the simulation box, known as super-sample modes, are not captured by the simulations and in turn can lead to inaccuracies in the covariance matrix. We compare the covariance measured using simulation boxes containing super-sample modes to those without. We also compare with the Separate Universe approach. We find that while the power spectrum, bispectrum and halo mass function show significant scale- or mass-dependent SSC, the void size function shows relatively small SSC. We also find significant SSC contributions to the cross-covariances between the different statistics, implying that future joint-analyses will need to carefully take into consideration the effect of SSC.


(987)The MillenniumTNG Project: The galaxy population at $z\geq 8$
  • Rahul Kannan,
  • Volker Springel,
  • Lars Hernquist,
  • Rüdiger Pakmor,
  • Ana Maria Delgado
  • +9
  • Boryana Hadzhiyska,
  • César Hernández-Aguayo,
  • Monica Barrera,
  • Fulvio Ferlito,
  • Sownak Bose,
  • Simon White,
  • Carlos Frenk,
  • Aaron Smith,
  • Enrico Garaldi
  • (less)
arXiv e-prints (10/2022) e-Print:2210.10066
abstract + abstract -

The early release science results from the $\textit{James Webb Space Telescope (JWST)}$ have yielded an unexpected abundance of high-redshift luminous galaxies that seems to be in tension with current theories of galaxy formation. However, it is currently difficult to draw definitive conclusions form these results as the sources have not yet been spectroscopically confirmed. It is in any case important to establish baseline predictions from current state-of-the-art galaxy formation models that can be compared and contrasted with these new measurements. In this work, we use the new large-volume ($L_\mathrm{box}\sim 740 \, \mathrm{cMpc}$) hydrodynamic simulation of the MillenniumTNG project to make predictions for the high-redshift ($z\gtrsim8$) galaxy population and compare them to recent $\textit{JWST}$ observations. We show that the simulated galaxy population is broadly consistent with observations until $z\sim10$. From $z\approx10-12$, the observations indicate a preference for a galaxy population that is largely dust-free, but is still consistent with the simulations. Beyond $z\gtrsim12$, however, our simulation results underpredict the abundance of luminous galaxies and their star-formation rates by almost an order of magnitude. This indicates either an incomplete understanding of the new $\textit{JWST}$ data or a need for more sophisticated galaxy formation models that account for additional physical processes such as Population~III stars, variable stellar initial mass functions, or even deviations from the standard $\Lambda$CDM model. We emphasise that any new process invoked to explain this tension should only significantly influence the galaxy population beyond $z\gtrsim10$, while leaving the successful galaxy formation predictions of the fiducial model intact below this redshift.


(986)Interpreting molecular hydrogen and atomic oxygen line emission of T Tauri disks with photoevaporative disk-wind models
  • Ch. Rab,
  • M. Weber,
  • T. Grassi,
  • B. Ercolano,
  • G. Picogna
  • +4
  • P. Caselli,
  • W. -F. Thi,
  • I. Kamp,
  • P. Woitke
  • (less)
arXiv e-prints (10/2022) e-Print:2210.15486
abstract + abstract -

Winds in protoplanetary disks play an important role in their evolution and dispersal. However, what physical process is driving the winds is still unclear (i.e. magnetically vs thermally driven), and can only be understood by directly confronting theoretical models with observational data. We use hydrodynamic photoevaporative disk-wind models and post-process them with a thermo-chemical model to produce synthetic observables for the o-H$_2$ at 2.12 micron and [OI] at 0.63 micron spectral lines and directly compare the results to a sample of observations. Our photoevaporative disk-wind model is consistent with the observed signatures of the blueshifted narrow low-velocity component (NLVC), which is usually associated with slow disk winds, for both tracers. Only for one out of seven targets that show blueshifted NLVCs does the photoevaporative model fail to explain the observed line kinematics. Our results also indicate that interpreting spectral line profiles by simple methods, such as the thin-disk approximation, to determine the line emitting region can yield misleading conclusions. The photoevaporative disk-wind models are largely consistent with the studied observational data set, but it is not possible to clearly discriminate between different wind-driving mechanisms. Further improvements to the models, such as consistent modelling of the dynamics and chemistry and detailed modelling of individual targets would be beneficial. Furthermore, a direct comparison of magnetically driven disk-wind models to the observational data set is necessary in order to determine whether or not spatially unresolved observations of multiple wind tracers are sufficient to discriminate between theoretical models.


(985)Cosmological simulations with rare and frequent dark matter self-interactions
  • Moritz S. Fischer,
  • Marcus Brüggen,
  • Kai Schmidt-Hoberg,
  • Klaus Dolag,
  • Felix Kahlhoefer
  • +2
  • Antonio Ragagnin,
  • Andrew Robertson
  • (less)
Monthly Notices of the Royal Astronomical Society, 516, p18 (10/2022) doi:10.1093/mnras/stac2207
abstract + abstract -

Dark matter (DM) with self-interactions is a promising solution for the small-scale problems of the standard cosmological model. Here we perform the first cosmological simulation of frequent DM self-interactions, corresponding to small-angle DM scatterings. The focus of our analysis lies in finding and understanding differences to the traditionally assumed rare DM (large-angle) self-scatterings. For this purpose, we compute the distribution of DM densities, the matter power spectrum, the two-point correlation function, and the halo and subhalo mass functions. Furthermore, we investigate the density profiles of the DM haloes and their shapes. We find that overall large-angle and small-angle scatterings behave fairly similarly with a few exceptions. In particular, the number of satellites is considerably suppressed for frequent compared to rare self-interactions with the same cross-section. Overall, we observe that while differences between the two cases may be difficult to establish using a single measure, the degeneracy may be broken through a combination of multiple ones. For instance, the combination of satellite counts with halo density or shape profiles could allow discriminating between rare and frequent self-interactions. As a by-product of our analysis, we provide - for the first time - upper limits on the cross-section for frequent self-interactions.


(984)Arp 58 and Arp 68: two M 51-type systems
  • Anatoly V. Zasov,
  • Anna S. Saburova,
  • Oleg V. Egorov,
  • Vsevolod Yu Lander,
  • Dmitry I. Makarov
Monthly Notices of the Royal Astronomical Society, 516, p12 (10/2022) doi:10.1093/mnras/stac2165
abstract + abstract -

We study two M 51-type systems Arp 68 and Arp 58, which strongly differ by their stellar masses, gas content, and environment. Long-slit spectral observations obtained at the Russian 6-m telescope were used to trace the distributions of a line-of-sight (LOS) velocity and a gas-phase oxygen abundance along the spectral cuts. Two systems are compared by their observed properties. We found a very strong large-scale non-circular motion of gas in both systems and a kpc-size saw-edged velocity profile along the tidal spiral arm of Arp 68, probably caused by the gas outflow due to the stellar feedback. A deep decrease of LOS velocity is also found in the 'hinge' region in Arp 58, where the inner spiral arm transforms into the tidal spiral arm, which was predicted earlier for M 51-type galaxies. Local sites of star formation and the satellites are compared with the evolutionary models at the colour-colour diagrams. Unlike the spiral galaxy Arp 58, the main galaxy in Arp 68 system is experiencing an ongoing burst of star formation. Gas-phase metallicity estimates show that Arp 58 has a higher metal abundance and reveals a shallow negative radial gradient of the gas-phase oxygen abundance. The emission gas in Arp 68 has noticeably lower metallicity than it is expected for a given luminosity of this galaxy, which may be connected with its space position in the local void.


(983)Convective mesoscale turbulence at very low Prandtl numbers
  • Ambrish Pandey,
  • Dmitry Krasnov,
  • Katepalli R. Sreenivasan,
  • Jörg Schumacher
Journal of Fluid Mechanics, 948 (10/2022) doi:10.1017/jfm.2022.694
abstract + abstract -

Horizontally extended turbulent convection, termed mesoscale convection in natural systems, remains a challenge to investigate in both experiments and simulations. This is particularly so for very low molecular Prandtl numbers, such as occur in stellar convection and in the Earth's outer core. The present study reports three-dimensional direct numerical simulations of turbulent Rayleigh–Bénard convection in square boxes of side length $L$ and height $H$ with the aspect ratio $\varGamma =L/H$ of 25, for Prandtl numbers that span almost 4 orders of magnitude, $10^{-3}\le Pr \le 7$ , and Rayleigh numbers $10^5 \le Ra \le 10^7$ , obtained by massively parallel computations on grids of up to $5.36\times 10^{11}$ points. The low end of this $Pr$ -range cannot be accessed in controlled laboratory measurements. We report the essential properties of the flow and their trends with the Rayleigh and Prandtl numbers, in particular, the global transport of momentum and heat – the latter decomposed into convective and diffusive contributions – across the convection layer, mean vertical profiles of the temperature and temperature fluctuations and the kinetic energy and thermal dissipation rates. We also explore the degree to which the turbulence in the bulk of the convection layer resembles classical homogeneous and isotropic turbulence in terms of spectra, increment moments and dissipative anomaly, and find close similarities. Finally, we show that a characteristic scale of the order of the mesoscale seems to saturate to a wavelength of $\lambda \gtrsim 3H$ for $Pr\lesssim 0.005$ . We briefly discuss possible implications of these results for the development of subgrid-scale parameterization of turbulent convection.


(982)Science Requirements and Detector Concepts for the Electron-Ion Collider. EIC Yellow Report
  • R. Abdul Khalek,
  • A. Accardi,
  • J. Adam,
  • D. Adamiak,
  • W. Akers
  • +410
  • M. Albaladejo,
  • A. Al-bataineh,
  • M. G. Alexeev,
  • F. Ameli,
  • P. Antonioli,
  • N. Armesto,
  • W. R. Armstrong,
  • M. Arratia,
  • J. Arrington,
  • A. Asaturyan,
  • M. Asai,
  • E. C. Aschenauer,
  • S. Aune,
  • H. Avagyan,
  • C. Ayerbe Gayoso,
  • B. Azmoun,
  • A. Bacchetta,
  • M. D. Baker,
  • F. Barbosa,
  • L. Barion,
  • K. N. Barish,
  • P. C. Barry,
  • M. Battaglieri,
  • A. Bazilevsky,
  • N. K. Behera,
  • F. Benmokhtar,
  • V. V. Berdnikov,
  • J. C. Bernauer,
  • V. Bertone,
  • S. Bhattacharya,
  • C. Bissolotti,
  • D. Boer,
  • M. Boglione,
  • M. Bondì,
  • P. Boora,
  • I. Borsa,
  • F. Bossù,
  • G. Bozzi,
  • J. D. Brandenburg,
  • N. Brei,
  • A. Bressan,
  • W. K. Brooks,
  • S. Bufalino,
  • M. H. S. Bukhari,
  • V. Burkert,
  • N. H. Buttimore,
  • A. Camsonne,
  • A. Celentano,
  • F. G. Celiberto,
  • W. Chang,
  • C. Chatterjee,
  • K. Chen,
  • T. Chetry,
  • T. Chiarusi,
  • Y. -T. Chien,
  • M. Chiosso,
  • X. Chu,
  • E. Chudakov,
  • G. Cicala,
  • E. Cisbani,
  • I. C. Cloet,
  • C. Cocuzza,
  • P. L. Cole,
  • D. Colella,
  • J. L. Collins,
  • M. Constantinou,
  • M. Contalbrigo,
  • G. Contin,
  • R. Corliss,
  • W. Cosyn,
  • A. Courtoy,
  • J. Crafts,
  • R. Cruz-Torres,
  • R. C. Cuevas,
  • U. D'Alesio,
  • S. Dalla Torre,
  • D. Das,
  • S. S. Dasgupta,
  • C. Da Silva,
  • W. Deconinck,
  • M. Defurne,
  • W. DeGraw,
  • K. Dehmelt,
  • A. Del Dotto,
  • F. Delcarro,
  • A. Deshpande,
  • W. Detmold,
  • R. De Vita,
  • M. Diefenthaler,
  • C. Dilks,
  • D. U. Dixit,
  • S. Dulat,
  • A. Dumitru,
  • R. Dupré,
  • J. M. Durham,
  • M. G. Echevarria,
  • L. El Fassi,
  • D. Elia,
  • R. Ent,
  • R. Esha,
  • J. J. Ethier,
  • O. Evdokimov,
  • K. O. Eyser,
  • C. Fanelli,
  • R. Fatemi,
  • S. Fazio,
  • C. Fernandez-Ramirez,
  • M. Finger,
  • M. Finger,
  • D. Fitzgerald,
  • C. Flore,
  • T. Frederico,
  • I. Friščić,
  • S. Fucini,
  • S. Furletov,
  • Y. Furletova,
  • C. Gal,
  • L. Gamberg,
  • H. Gao,
  • P. Garg,
  • D. Gaskell,
  • K. Gates,
  • M. B. Gay Ducati,
  • M. Gericke,
  • G. Gil Da Silveira,
  • F. -X. Girod,
  • D. I. Glazier,
  • K. Gnanvo,
  • V. P. Goncalves,
  • L. Gonella,
  • J. O. Gonzalez Hernandez,
  • Y. Goto,
  • F. Grancagnolo,
  • L. C. Greiner,
  • W. Guryn,
  • V. Guzey,
  • Y. Hatta,
  • M. Hattawy,
  • F. Hauenstein,
  • X. He,
  • T. K. Hemmick,
  • O. Hen,
  • G. Heyes,
  • D. W. Higinbotham,
  • A. N. Hiller Blin,
  • T. J. Hobbs,
  • M. Hohlmann,
  • T. Horn,
  • T. -J. Hou,
  • J. Huang,
  • Q. Huang,
  • G. M. Huber,
  • C. E. Hyde,
  • G. Iakovidis,
  • Y. Ilieva,
  • B. V. Jacak,
  • P. M. Jacobs,
  • M. Jadhav,
  • Z. Janoska,
  • A. Jentsch,
  • T. Jezo,
  • X. Jing,
  • P. G. Jones,
  • K. Joo,
  • S. Joosten,
  • V. Kafka,
  • N. Kalantarians,
  • G. Kalicy,
  • D. Kang,
  • Z. B. Kang,
  • K. Kauder,
  • S. J. D. Kay,
  • C. E. Keppel,
  • J. Kim,
  • A. Kiselev,
  • M. Klasen,
  • S. Klein,
  • H. T. Klest,
  • O. Korchak,
  • A. Kostina,
  • P. Kotko,
  • Y. V. Kovchegov,
  • M. Krelina,
  • S. Kuleshov,
  • S. Kumano,
  • K. S. Kumar,
  • R. Kumar,
  • L. Kumar,
  • K. Kumerički,
  • A. Kusina,
  • K. Kutak,
  • Y. S. Lai,
  • K. Lalwani,
  • T. Lappi,
  • J. Lauret,
  • M. Lavinsky,
  • D. Lawrence,
  • D. Lednicky,
  • C. Lee,
  • K. Lee,
  • S. H. Lee,
  • S. Levorato,
  • H. Li,
  • S. Li,
  • W. Li,
  • X. Li,
  • X. Li,
  • W. B. Li,
  • T. Ligonzo,
  • H. Liu,
  • M. X. Liu,
  • X. Liu,
  • S. Liuti,
  • N. Liyanage,
  • C. Lorcé,
  • Z. Lu,
  • G. Lucero,
  • N. S. Lukow,
  • E. Lunghi,
  • R. Majka,
  • Y. Makris,
  • I. Mandjavidze,
  • S. Mantry,
  • H. Mäntysaari,
  • F. Marhauser,
  • P. Markowitz,
  • L. Marsicano,
  • A. Mastroserio,
  • V. Mathieu,
  • Y. Mehtar-Tani,
  • W. Melnitchouk,
  • L. Mendez,
  • A. Metz,
  • Z. -E. Meziani,
  • C. Mezrag,
  • M. Mihovilovič,
  • R. Milner,
  • M. Mirazita,
  • H. Mkrtchyan,
  • A. Mkrtchyan,
  • V. Mochalov,
  • V. Moiseev,
  • M. M. Mondal,
  • A. Morreale,
  • D. Morrison,
  • L. Motyka,
  • H. Moutarde,
  • C. Muñoz Camacho,
  • F. Murgia,
  • M. J. Murray,
  • P. Musico,
  • P. Nadel-Turonski,
  • P. M. Nadolsky,
  • J. Nam,
  • P. R. Newman,
  • D. Neyret,
  • D. Nguyen,
  • E. R. Nocera,
  • F. Noferini,
  • F. Noto,
  • A. S. Nunes,
  • V. A. Okorokov,
  • F. Olness,
  • J. D. Osborn,
  • B. S. Page,
  • S. Park,
  • A. Parker,
  • K. Paschke,
  • B. Pasquini,
  • H. Paukkunen,
  • S. Paul,
  • C. Pecar,
  • I. L. Pegg,
  • C. Pellegrino,
  • C. Peng,
  • L. Pentchev,
  • R. Perrino,
  • F. Petriello,
  • R. Petti,
  • A. Pilloni,
  • C. Pinkenburg,
  • B. Pire,
  • C. Pisano,
  • D. Pitonyak,
  • A. A. Poblaguev,
  • T. Polakovic,
  • M. Posik,
  • M. Potekhin,
  • R. Preghenella,
  • S. Preins,
  • A. Prokudin,
  • P. Pujahari,
  • M. L. Purschke,
  • J. R. Pybus,
  • M. Radici,
  • R. Rajput-Ghoshal,
  • P. E. Reimer,
  • M. Rinaldi,
  • F. Ringer,
  • C. D. Roberts,
  • S. Rodini,
  • J. Rojo,
  • D. Romanov,
  • P. Rossi,
  • E. Santopinto,
  • M. Sarsour,
  • R. Sassot,
  • N. Sato,
  • B. Schenke,
  • W. B. Schmidke,
  • I. Schmidt,
  • A. Schmidt,
  • B. Schmookler,
  • G. Schnell,
  • P. Schweitzer,
  • J. Schwiening,
  • I. Scimemi,
  • S. Scopetta,
  • J. Segovia,
  • R. Seidl,
  • S. Sekula,
  • K. Semenov-Tian-Shanskiy,
  • D. Y. Shao,
  • N. Sherrill,
  • E. Sichtermann,
  • M. Siddikov,
  • A. Signori,
  • B. K. Singh,
  • S. Širca,
  • K. Slifer,
  • W. Slominski,
  • D. Sokhan,
  • W. E. Sondheim,
  • Y. Song,
  • O. Soto,
  • H. Spiesberger,
  • A. M. Stasto,
  • P. Stepanov,
  • G. Sterman,
  • J. R. Stevens,
  • I. W. Stewart,
  • I. Strakovsky,
  • M. Strikman,
  • M. Sturm,
  • M. L. Stutzman,
  • M. Sullivan,
  • B. Surrow,
  • P. Svihra,
  • S. Syritsyn,
  • A. Szczepaniak,
  • P. Sznajder,
  • H. Szumila-Vance,
  • L. Szymanowski,
  • A. S. Tadepalli,
  • J. D. Tapia Takaki,
  • G. F. Tassielli,
  • J. Terry,
  • F. Tessarotto,
  • K. Tezgin,
  • L. Tomasek,
  • F. Torales Acosta,
  • P. Tribedy,
  • A. Tricoli,
  • Triloki,
  • S. Tripathi,
  • R. L. Trotta,
  • O. D. Tsai,
  • Z. Tu,
  • C. Tuvè,
  • T. Ullrich,
  • M. Ungaro,
  • G. M. Urciuoli,
  • A. Valentini,
  • P. Vancura,
  • M. Vandenbroucke,
  • C. Van Hulse,
  • G. Varner,
  • R. Venugopalan,
  • I. Vitev,
  • A. Vladimirov,
  • G. Volpe,
  • A. Vossen,
  • E. Voutier,
  • J. Wagner,
  • S. Wallon,
  • H. Wang,
  • Q. Wang,
  • X. Wang,
  • S. Y. Wei,
  • C. Weiss,
  • T. Wenaus,
  • H. Wennlöf,
  • N. Wickramaarachchi,
  • A. Wikramanayake,
  • D. Winney,
  • C. P. Wong,
  • C. Woody,
  • L. Xia,
  • B. W. Xiao,
  • J. Xie,
  • H. Xing,
  • Q. H. Xu,
  • J. Zhang,
  • S. Zhang,
  • Z. Zhang,
  • Z. W. Zhao,
  • Y. X. Zhao,
  • L. Zheng,
  • Y. Zhou,
  • P. Zurita
  • (less)
Nuclear Physics A, 1026 (10/2022) doi:10.1016/j.nuclphysa.2022.122447
abstract + abstract -

This report describes the physics case, the resulting detector requirements, and the evolving detector concepts for the experimental program at the Electron-Ion Collider (EIC). The EIC will be a powerful new high-luminosity facility in the United States with the capability to collide high-energy electron beams with high-energy proton and ion beams, providing access to those regions in the nucleon and nuclei where their structure is dominated by gluons. Moreover, polarized beams in the EIC will give unprecedented access to the spatial and spin structure of the proton, neutron, and light ions. The studies leading to this document were commissioned and organized by the EIC User Group with the objective of advancing the state and detail of the physics program and developing detector concepts that meet the emerging requirements in preparation for the realization of the EIC. The effort aims to provide the basis for further development of concepts for experimental equipment best suited for the science needs, including the importance of two complementary detectors and interaction regions.

This report consists of three volumes. Volume I is an executive summary of our findings and developed concepts. In Volume II we describe studies of a wide range of physics measurements and the emerging requirements on detector acceptance and performance. Volume III discusses general-purpose detector concepts and the underlying technologies to meet the physics requirements. These considerations will form the basis for a world-class experimental program that aims to increase our understanding of the fundamental structure of all visible matter.


(981)Milky Way-like galaxies: stellar population properties of dynamically defined discs, bulges and stellar haloes
  • Sara Ortega-Martinez,
  • Aura Obreja,
  • Rosa Dominguez-Tenreiro,
  • Susana E. Pedrosa,
  • Yetli Rosas-Guevara
  • +1
Monthly Notices of the Royal Astronomical Society, 516, p19 (10/2022) doi:10.1093/mnras/stac2033
abstract + abstract -

The formation of galaxies can be understood in terms of the assembly patterns of each type of galactic component. To perform this kind of analysis, it is necessary to define some criteria to separate those components. Decomposition methods based on dynamical properties are more physically motivated than photometry-based ones. We use the unsupervised Gaussian Mixture model of galactic structure finder to extract the components of a sub-sample of galaxies with Milky Way-like masses from the EAGLE simulations. A clustering in the space of first- and second-order dynamical moments of all identified substructures reveals five types of galaxy components: thin and thick discs, stellar haloes, bulges and spheroids. We analyse the dynamical, morphological and stellar population (SP) properties of these five component types, exploring to what extent these properties correlate with each other, and how much they depend on the total galaxy stellar and dark matter halo masses. All galaxies contain a bulge, a stellar halo and a disc. In total, 60 per cent of objects host two discs (thin and thick), and 68 per cent host also a spheroid. The dynamical disc-to-total ratio does not depend on stellar mass, but the median rotational velocities of the two discs do. Thin discs are well separated in stellar ages, [Fe/H] and α-enhancement from the three dispersion-dominated components, while thick discs are in between. Except for thin discs, all components show correlations among their SP properties: older ages mean lower metallicities and larger α-enhancement. Finally, we quantify the weak dependence of SP properties on each component's dynamics.


(980)External or internal companion exciting the spiral arms in CQ Tau?
  • Iain Hammond,
  • Valentin Christiaens,
  • Daniel J. Price,
  • Maria Giulia Ubeira-Gabellini,
  • Jennifer Baird
  • +7
  • Josh Calcino,
  • Myriam Benisty,
  • Giuseppe Lodato,
  • Leonardo Testi,
  • Christophe Pinte,
  • Claudia Toci,
  • Davide Fedele
  • (less)
Monthly Notices of the Royal Astronomical Society, 515, p13 (10/2022) doi:10.1093/mnras/stac2119
abstract + abstract -

We present new high-contrast images in near-infrared wavelengths (λc = 1.04, 1.24, 1.62, 2.18, and 3.78 μm) of the young variable star CQ Tau, aiming to constrain the presence of companions in the protoplanetary disc. We reached a Ks-band contrast of 14 mag with SPHERE/IRDIS at separations greater than 0${_{.}^{\prime\prime}}$4 from the star. Our mass sensitivity curve rules out giant planets above 4 MJup immediately outside the spiral arms at ~60 au and above 2-3 MJup beyond 100 au to 5σ confidence assuming hot-start models. We do, however, detect four spiral arms, a double-arc and evidence for shadows in scattered light cast by a misaligned inner disc. Our observations may be explained by an unseen close-in companion on an inclined and eccentric orbit. Such a hypothesis would also account for the disc CO cavity and disturbed kinematics.


(979)Beyond-mean-field approaches for nuclear neutrinoless double beta decay in the standard mechanism
  • J. M. Yao,
  • J. Meng,
  • Y. F. Niu,
  • P. Ring
Progress in Particle and Nuclear Physics, 126 (09/2022) doi:10.1016/j.ppnp.2022.103965
abstract + abstract -

Nuclear weak decays provide important probes to fundamental symmetries in nature. A precise description of these processes in atomic nuclei requires comprehensive knowledge on both the strong and weak interactions in the nuclear medium and on the dynamics of quantum many-body systems. In particular, an observation of the hypothetical double beta decay without emission of neutrinos (0 νββ) would unambiguously demonstrate the Majorana nature of neutrinos and the existence of the lepton-number-violation process. It would also provide unique information on the ordering and absolute scale of neutrino masses. The next-generation tonne-scale experiments with sensitivity up to 1028 years after a few years of running will probably provide a definite answer to these fundamental questions based on our current knowledge on the nuclear matrix element (NME), the precise determination of which is a challenge to nuclear theory. Beyond-mean-field approaches have been frequently adapted for the study of nuclear structure and decay throughout the nuclear chart for several decades. In this review, we summarize the status of beyond-mean-field calculations of the NMEs of 0 νββ decay assuming the standard mechanism of an exchange of light Majorana neutrinos. The challenges and prospects in the extension and application of beyond-mean-field approaches for 0 νββ decay are discussed.


(978)Strong Supernova 1987A Constraints on Bosons Decaying to Neutrinos
  • Damiano F. G. Fiorillo,
  • Georg G. Raffelt,
  • Edoardo Vitagliano
arXiv e-prints (09/2022) e-Print:2209.11773
abstract + abstract -

Majoron-like bosons would emerge from a supernova (SN) core by neutrino coalescence of the form $\nu\nu\to\phi$ and $\bar\nu\bar\nu\to\phi$ with 100 MeV-range energies. Subsequent decays to (anti)neutrinos of all flavors provide a flux component with energies much larger than the usual flux from the "neutrino sphere." The absence of 100 MeV-range events in the Kamiokande II and IMB signal of SN 1987A implies that $\lesssim0.03$ of the total energy was thus emitted and provides the strongest constraint on the majoron-neutrino coupling of $g\lesssim 10^{-9}\,{\rm MeV}/m_\phi$ for $100~{\rm eV}\lesssim m_\phi\lesssim100~{\rm MeV}$. It is straightforward to extend our new argument to other hypothetical feebly interacting particles.


(977)A multi-simulation study of relativistic SZ temperature scalings in galaxy clusters and groups
  • Elizabeth Lee,
  • Dhayaa Anbajagane,
  • Priyanka Singh,
  • Jens Chluba,
  • Daisuke Nagai
  • +4
  • Scott T. Kay,
  • Weiguang Cui,
  • Klaus Dolag,
  • Gustavo Yepes
  • (less)
Monthly Notices of the Royal Astronomical Society (09/2022) doi:10.1093/mnras/stac2781
abstract + abstract -

The Sunyaev-Zeldovich (SZ) effect is a powerful tool in modern cosmology. With future observations promising ever improving SZ measurements, the relativistic corrections to the SZ signals from galaxy groups and clusters are increasingly relevant. As such, it is important to understand the differences between three temperature measures: (a) the average relativistic SZ (rSZ) temperature, (b) the mass-weighted temperature relevant for the thermal SZ (tSZ) effect, and (c) the X-ray spectroscopic temperature. In this work, we compare these cluster temperatures, as predicted by the BAHAMAS & MACSIS, ILLUSTRISTNG, MAGNETICUM, and THE THREE HUNDRED PROJECT simulations. Despite the wide range of simulation parameters, we find the SZ temperatures are consistent across the simulations. We estimate a $\simeq 10{{\ \rm per\ cent}}$ level correction from rSZ to clusters with Y ≃ 10-4 Mpc-2. Our analysis confirms a systematic offset between the three temperature measures; with the rSZ temperature $\simeq 20{{\ \rm per\ cent}}$ larger than the other measures, and diverging further at higher redshifts. We demonstrate that these measures depart from simple self-similar evolution and explore how they vary with the defined radius of haloes. We investigate how different feedback prescriptions and resolutions affect the observed temperatures, and discover the SZ temperatures are rather insensitive to these details. The agreement between simulations indicates an exciting avenue for observational and theoretical exploration, determining the extent of relativistic SZ corrections. We provide multiple simulation-based fits to the scaling relations for use in future SZ modelling.


(976)Neutrino Fast Flavor Pendulum. Part 2: Collisional Damping
  • Ian Padilla-Gay,
  • Irene Tamborra,
  • Georg G. Raffelt
arXiv e-prints (09/2022) e-Print:2209.11235
abstract + abstract -

In compact astrophysical objects, the neutrino density can be so high that neutrino-neutrino refraction can lead to fast flavor conversion of the kind $\nu_e \bar\nu_e \leftrightarrow \nu_x \bar\nu_x$ with $x=\mu,\tau$, depending on the neutrino angle distribution. Previously, we have shown that in a homogeneous, axisymmetric two-flavor system, these collective solutions evolve in analogy to a gyroscopic pendulum. In flavor space, its deviation from the weak-interaction direction is quantified by a variable $\cos\vartheta$ that moves between $+1$ and $\cos\vartheta_{\rm min}$, the latter following from a linear mode analysis. As a next step, we include collisional damping of flavor coherence, assuming a common damping rate $\Gamma$ for all modes. Empirically we find that the damped pendular motion reaches an asymptotic level of pair conversion $f=A+(1-A)\cos\vartheta_{\rm min}$ (numerically $A\simeq 0.370$) that does not depend on details of the angular distribution (except for fixing $\cos\vartheta_{\rm min}$), the initial seed, nor $\Gamma$. On the other hand, even a small asymmetry between the neutrino and antineutrino damping rates strongly changes this picture and can even enable flavor instabilities in otherwise stable systems. Furthermore, we establish a formal connection with a stationary and inhomogeneous neutrino ensemble, showing that our findings also apply to this system.


(975)Vacuum stability and scalar masses in the superweak extension of the standard model
  • Zoltán Péli,
  • Zoltán Trócsányi
Physical Review D, 106 (09/2022) doi:10.1103/PhysRevD.106.055045
abstract + abstract -

We study the allowed parameter space of the scalar sector in the superweak extension of the standard model (SM). The allowed region is defined by the following conditions: (i) stability of the vacuum, (ii) perturbativity up to the Planck scale, and (iii) the pole mass of the Higgs boson falling into its experimentally measured range. We employ renormalization group equations and quantum corrections at two-loop accuracy. We study the dependence on the Yukawa couplings of the sterile neutrinos at selected values. We also check the exclusion limit set by the precise measurement of the mass of the W boson. Our method for constraining the parameter space using two-loop predictions can also be applied to simpler models such as the singlet scalar extension of the SM in a straightforward way.


(974)Effective field theory of Stückelberg vector bosons
  • Graham D. Kribs,
  • Gabriel Lee,
  • Adam Martin
Physical Review D, 106 (09/2022) doi:10.1103/PhysRevD.106.055020
abstract + abstract -

We explore the effective field theory of a vector field Xμ that has a Stückelberg mass. The absence of a gauge symmetry for Xμ implies Lorentz-invariant operators are constructed directly from Xμ. Beyond the kinetic and mass terms, allowed interactions at the renormalizable level include XμXμHH , (XμXμ)2, and Xμjμ, where jμ is a global current of the SM or of a hidden sector. We show that all of these interactions lead to scattering amplitudes that grow with powers of √{s }/mX, except for the case of Xμjμ where jμ is a nonanomalous global current. The latter is well known when X is identified as a dark photon coupled to the electromagnetic current, often written equivalently as kinetic mixing between X and the photon. The power counting for the energy growth of the scattering amplitudes is facilitated by isolating the longitudinal enhancement. We examine in detail the interaction with an anomalous global vector current Xμjanomμ, carefully isolating the finite contribution to the fermion triangle diagram. We calculate the longitudinally-enhanced observables Z →X γ (when mX<mZ), f f ¯→X γ , and Z γ →Z γ when X couples to the baryon number current. Introducing a "fake" gauge-invariance by writing Xμ=Aμ-∂μπ /mX, the would-be gauge anomaly associated with Aμjanomμ is canceled by janomμμπ /mX; this is the four-dimensional Green-Schwarz anomaly-cancellation mechanism at work. Our analysis demonstrates there is a much larger set of possible interactions that an EFT with a Stückelberg vector field can have, revealing scattering amplitudes that grow with energy. The growth of these amplitudes can be tamed by a dark Higgs sector, but this requires dark Higgs boson interactions (and reintroduces fine-tuning in the dark Higgs sector) that can be separated from X interactions only in the limit g ≪1 .


(973)The metallicity and distance of NGC 2403 from blue supergiants
  • Fabio Bresolin,
  • Rolf-Peter Kudritzki,
  • Miguel A. Urbaneja
arXiv e-prints (09/2022) e-Print:2209.13135
abstract + abstract -

We present the first quantitative spectral analysis of blue supergiant stars in the nearby galaxy NGC 2403. Out of a sample of 47 targets observed with the LRIS spectrograph at the Keck I telescope we have extracted 16 B- and A-type supergiants for which we have data of sufficient quality to carry out a comparison with model spectra of evolved massive stars and infer the stellar parameters. The radial metallicity gradient of NGC 2403 that we derive has a slope of -0.14 (+/- 0.05) dex/r_e, and is in accordance with the analysis of H II region oxygen abundances. We present evidence that the stellar metallicities that we obtain in extragalactic systems in general agree with the nebular abundances based on the analysis of the auroral lines, over more than one order of magnitude in metallicity. Adopting the known relation between stellar parameters and intrinsic luminosity we find a distance modulus m-M = 27.38 +/- 0.08 mag. While this can be brought into agreement with Cepheid-based determinations, it is 0.14 mag short of the value measured from the tip of the red giant branch. We update the mass-metallicity relation secured from chemical abundance studies of stars in resolved star-forming galaxies.


(972)Probing Axions via Light Circular Polarization and Event Horizon Telescope
  • Soroush Shakeri,
  • Fazlollah Hajkarim
arXiv e-prints (09/2022) e-Print:2209.13572
abstract + abstract -

The impact of axion-like particles on the light polarization around the horizon of suppermassive black hole (SMBH) is discussed in the light of the latest polarization measurement of the Event Horizon Telescope (EHT). We investigate different sources of the polarization due to axion interaction with photons and the magnetic field of SMBH. These can modify the linear and circular polarization parameters of the emitted light. We have shown that a significant circular polarization can be produced via the photon scattering from the background magnetic field with axions as off-shell particles. This can further constrain the parameter space of ultralight axion-like particles and their couplings with photons. The future precise measurements of circular polarization can probe the features of ultralight axions in the near vicinity of SMBH.


(971)Revisiting constraints on WIMPs around primordial black holes
  • Estanis Utrilla Ginés,
  • Olga Mena,
  • Samuel J. Witte
Physical Review D, 106 (09/2022) doi:10.1103/PhysRevD.106.063538
abstract + abstract -

While primordial black holes (PBHs) with masses MPBH≳10-11 M cannot comprise the entirety of dark matter, the existence of even a small population of these objects can have profound astrophysical consequences. A subdominant population of PBHs will efficiently accrete dark matter particles before matter-radiation equality, giving rise to high-density dark matter spikes. We consider here the scenario in which dark matter is comprised primarily of weakly interacting massive particles (WIMPs) with a small subdominant contribution coming from PBHs, and revisit the constraints on the annihilation of WIMPs in these spikes using observations of the isotropic gamma-ray background (IGRB) and the cosmic microwave background (CMB), for a range of WIMP masses, annihilation channels, cross sections, and PBH mass functions. We find that the constraints derived using the IGRB have been significantly overestimated (in some cases by many orders of magnitude), and that limits obtained using observations of the CMB are typically stronger than, or comparable to, those coming from the IGRB. Importantly, we show that ∼O (M) PBHs can still contribute significantly to the dark matter density for sufficiently low WIMP masses and p-wave annihilation cross sections.


(970)A detailed analysis of the Gl 486 planetary system
  • J. A. Caballero,
  • E. González-Álvarez,
  • M. Brady,
  • T. Trifonov,
  • T. G. Ellis
  • +62
  • C. Dorn,
  • C. Cifuentes,
  • K. Molaverdikhani,
  • J. L. Bean,
  • T. Boyajian,
  • E. Rodríguez,
  • J. Sanz-Forcada,
  • M. R. Zapatero Osorio,
  • C. Abia,
  • P. J. Amado,
  • N. Anugu,
  • V. J. S. Béjar,
  • C. L. Davies,
  • S. Dreizler,
  • F. Dubois,
  • J. Ennis,
  • N. Espinoza,
  • C. D. Farrington,
  • A. García López,
  • T. Gardner,
  • A. P. Hatzes,
  • Th. Henning,
  • E. Herrero,
  • E. Herrero-Cisneros,
  • A. Kaminski,
  • D. Kasper,
  • R. Klement,
  • S. Kraus,
  • A. Labdon,
  • C. Lanthermann,
  • J. -B. Le Bouquin,
  • M. J. López González,
  • R. Luque,
  • A. W. Mann,
  • E. Marfil,
  • J. D. Monnier,
  • D. Montes,
  • J. C. Morales,
  • E. Pallé,
  • S. Pedraz,
  • A. Quirrenbach,
  • S. Reffert,
  • A. Reiners,
  • I. Ribas,
  • C. Rodríguez-López,
  • G. Schaefer,
  • A. Schweitzer,
  • A. Seifahrt,
  • B. R. Setterholm,
  • Y. Shan,
  • D. Shulyak,
  • E. Solano,
  • K. R. Sreenivas,
  • G. Stefánsson,
  • J. Stürmer,
  • H. M. Tabernero,
  • L. Tal-Or,
  • T. ten Brummelaar,
  • S. Vanaverbeke,
  • K. von Braun,
  • A. Youngblood,
  • M. Zechmeister
  • (less)
Astronomy and Astrophysics, 665, p41 (09/2022) doi:10.1051/0004-6361/202243548
abstract + abstract -

Context. The Gl 486 system consists of a very nearby, relatively bright, weakly active M3.5 V star at just 8 pc with a warm transiting rocky planet of about 1.3 R and 3.0 M. It is ideal for both transmission and emission spectroscopy and for testing interior models of telluric planets.
Aims: To prepare for future studies, we aim to thoroughly characterise the planetary system with new accurate and precise data collected with state-of-the-art photometers from space and spectrometers and interferometers from the ground.
Methods: We collected light curves of seven new transits observed with the CHEOPS space mission and new radial velocities obtained with MAROON-X at the 8.1 m Gemini North telescope and CARMENES at the 3.5 m Calar Alto telescope, together with previously published spectroscopic and photometric data from the two spectrographs and TESS. We also performed near-infrared interferometric observations with the CHARA Array and new photometric monitoring with a suite of smaller telescopes (AstroLAB, LCOGT, OSN, TJO). This extraordinary and rich data set was the input for our comprehensive analysis.
Results: From interferometry, we measure a limb-darkened disc angular size of the star Gl 486 at θLDD = 0.390 ± 0.018 mas. Together with a corrected Gaia EDR3 parallax, we obtain a stellar radius R* = 0.339 ± 0.015 R. We also measure a stellar rotation period at Prot = 49.9 ± 5.5 days, an upper limit to its XUV (5-920 A) flux informed by new Hubble/STIS data, and, for the first time, a variety of element abundances (Fe, Mg, Si, V, Sr, Zr, Rb) and C/O ratio. Moreover, we imposed restrictive constraints on the presence of additional components, either stellar or sub-stellar, in the system. With the input stellar parameters and the radial-velocity and transit data, we determine the radius and mass of the planet Gl 486 b at Rp = 1.343−0.062+0.063 R and Mp = 3.00−0.12+0.13 M, with relative uncertainties of the planet radius and mass of 4.7% and 4.2%, respectively. From the planet parameters and the stellar element abundances, we infer the most probable models of planet internal structure and composition, which are consistent with a relatively small metallic core with respect to the Earth, a deep silicate mantle, and a thin volatile upper layer. With all these ingredients, we outline prospects for Gl 486 b atmospheric studies, especially with forthcoming James Webb Space Telescope (Webb) observations.


(969)Improved constraints on cosmic birefringence from the WMAP and Planck cosmic microwave background polarization data
  • Johannes R. Eskilt,
  • Eiichiro Komatsu
Physical Review D, 106 (09/2022) doi:10.1103/PhysRevD.106.063503
abstract + abstract -

The observed pattern of linear polarization of the cosmic microwave background photons is a sensitive probe of physics violating parity symmetry under inversion of spatial coordinates. A new parity-violating interaction might have rotated the plane of linear polarization by an angle β as the cosmic microwave background photons have been traveling for more than 13 billion years. This effect is known as "cosmic birefringence." In this paper, we present new measurements of cosmic birefringence from a joint analysis of polarization data from two space missions, P l a n c k and WMAP. This dataset covers a wide range of frequencies from 23 to 353 GHz. We measure β =0.342 °-0.091° +0.094 ° [68% confidence level (CL)] for nearly full-sky data, which excludes β =0 at 99.987% CL. This corresponds to the statistical significance of 3.6 σ . There is no evidence for frequency dependence of β . We find a similar result, albeit with a larger uncertainty, when removing the Galactic plane from the analysis.


(968)New constraints on the dark matter-neutrino and dark matter-photon scattering cross sections from TXS 0506+056
  • Francesc Ferrer,
  • Gonzalo Herrera,
  • Alejandro Ibarra
arXiv e-prints (09/2022) e-Print:2209.06339
abstract + abstract -

The flux of high energy neutrinos and photons produced in a blazar could get attenuated when they propagate through the dark matter spike around the central black hole and the halo of the host galaxy. Using the observation by IceCube of a few high-energy neutrino events from TXS 0506+056, and their coincident gamma ray events, we obtain new constraints on the dark matter-neutrino and dark matter-photon scattering cross sections. Our constraints are orders of magnitude more stringent than those derived from considering the attenuation through the intergalactic medium and the Milky Way dark matter halo. When the cross-section increases with energy, our constraints are also stronger than those derived from the CMB and large-scale structure.


(967)On the Sensitivity of Halo Shape Measurements
  • Moritz S. Fischer,
  • Lucas M. Valenzuela
(09/2022) e-Print:2209.11244
abstract + abstract -

Shape measurements of galaxies and galaxy clusters are widespread in the analysis of cosmological simulations. But the limitations of those measurements have been poorly investigated. In this paper, we explain why the quality of the shape measurement does not only depend on the numerical resolution, but also on the density gradient. In particular, this can limit the quality of measurements in the central regions of haloes. We propose a criterion to estimate the sensitivity of the measured shapes based on the density gradient of the halo and apply it to cosmological simulations of collisionless and self-interacting dark matter. By this, we demonstrate where reliable measurements of the halo shape are possible and how cored density profiles limit their applicability.


(966)Dark Energy Survey Year 3 results: Magnification modeling and impact on cosmological constraints from galaxy clustering and galaxy-galaxy lensing
  • J. Elvin-Poole,
  • N. MacCrann,
  • S. Everett,
  • J. Prat,
  • E.S. Rykoff
  • +91
  • J. De Vicente,
  • B. Yanny,
  • K. Herner,
  • A. Ferté,
  • E. Di Valentino,
  • A. Choi,
  • D.L. Burke,
  • I. Sevilla-Noarbe,
  • A. Alarcon,
  • O. Alves,
  • A. Amon,
  • F. Andrade-Oliveira,
  • E. Baxter,
  • K. Bechtol,
  • M.R. Becker,
  • G.M. Bernstein,
  • J. Blazek,
  • H. Camacho,
  • A. Campos,
  • A. Carnero Rosell,
  • M. Carrasco Kind,
  • R. Cawthon,
  • C. Chang,
  • R. Chen,
  • J. Cordero,
  • M. Crocce,
  • C. Davis,
  • J. DeRose,
  • H.T. Diehl,
  • S. Dodelson,
  • C. Doux,
  • A. Drlica-Wagner,
  • K. Eckert,
  • T.F. Eifler,
  • F. Elsner,
  • X. Fang,
  • P. Fosalba,
  • O. Friedrich,
  • M. Gatti,
  • G. Giannini,
  • D. Gruen,
  • R.A. Gruendl,
  • I. Harrison,
  • W.G. Hartley,
  • H. Huang,
  • E.M. Huff,
  • D. Huterer,
  • E. Krause,
  • N. Kuropatkin,
  • P.-F. Leget,
  • P. Lemos,
  • A.R. Liddle,
  • J. McCullough,
  • J. Muir,
  • J. Myles,
  • A. Navarro-Alsina,
  • S. Pandey,
  • Y. Park,
  • A. Porredon,
  • M. Raveri,
  • M. Rodriguez-Monroy,
  • R.P. Rollins,
  • A. Roodman,
  • R. Rosenfeld,
  • A.J. Ross,
  • C. Sánchez,
  • J. Sanchez,
  • L.F. Secco,
  • E. Sheldon,
  • T. Shin,
  • M.A. Troxel,
  • I. Tutusaus,
  • T.N. Varga,
  • N. Weaverdyck,
  • R.H. Wechsler,
  • B. Yin,
  • Y. Zhang,
  • J. Zuntz,
  • M. Aguena,
  • S. Avila,
  • D. Bacon,
  • E. Bertin,
  • S. Bocquet,
  • D. Brooks,
  • J. García-Bellido,
  • K. Honscheid,
  • M. Jarvis,
  • T.S. Li,
  • J. Mena-Fernández,
  • C. To,
  • R.D. Wilkinson
  • (less)
(09/2022) e-Print:2209.09782
abstract + abstract -

We study the effect of magnification in the Dark Energy Survey Year 3 analysis of galaxy clustering and galaxy-galaxy lensing, using two different lens samples: a sample of Luminous red galaxies, redMaGiC, and a sample with a redshift-dependent magnitude limit, MagLim. We account for the effect of magnification on both the flux and size selection of galaxies, accounting for systematic effects using the Balrog image simulations. We estimate the impact of magnification on the galaxy clustering and galaxy-galaxy lensing cosmology analysis, finding it to be a significant systematic for the MagLim sample. We show cosmological constraints from the galaxy clustering auto-correlation and galaxy-galaxy lensing signal with different magnifications priors, finding broad consistency in cosmological parameters in $\Lambda$CDM and $w$CDM. However, when magnification bias amplitude is allowed to be free, we find the two-point correlations functions prefer a different amplitude to the fiducial input derived from the image simulations. We validate the magnification analysis by comparing the cross-clustering between lens bins with the prediction from the baseline analysis, which uses only the auto-correlation of the lens bins, indicating systematics other than magnification may be the cause of the discrepancy. We show adding the cross-clustering between lens redshift bins to the fit significantly improves the constraints on lens magnification parameters and allows uninformative priors to be used on magnification coefficients, without any loss of constraining power or prior volume concerns.


(965)Spectra of Puffy Accretion Discs: the kynbb Fit
  • Debora Lančová,
  • Anastasiya Yilmaz,
  • Maciek Wielgus,
  • Michal Dovčiak,
  • Odele Straub
  • +1
(09/2022) e-Print:2209.03713
abstract + abstract -

Puffy disc is a numerical model, expected to capture the properties of the accretion flow in X-ray black hole binaries in the luminous, mildly sub-Eddington state. We fit the kerrbb and kynbb spectral models in XSPEC to synthetic spectra of puffy accretion discs, obtained in general relativistic radiative magnetohydrodynamic simulations, to see if they correctly recover the black hole spin and mass accretion rate assumed in the numerical simulation. We conclude that neither of the two models is capable of correctly interpreting the puffy disc parameters, which highlights a necessity to develop new, more accurate, spectral models for the luminous regime of accretion in X-ray black hole binaries. We propose that such spectral models should be based on the results of numerical simulations of accretion.


(964)Simulating radio synchrotron emission in star-forming galaxies: small-scale magnetic dynamo and the origin of the far-infrared-radio correlation
  • Christoph Pfrommer,
  • Maria Werhahn,
  • Rüdiger Pakmor,
  • Philipp Girichidis,
  • Christine M. Simpson
Monthly Notices of the Royal Astronomical Society, 515, p36 (09/2022) doi:10.1093/mnras/stac1808
abstract + abstract -

In star-forming galaxies, the far-infrared (FIR) and radio-continuum luminosities obey a tight empirical relation over a large range of star-formation rates (SFR). To understand the physics, we examine magnetohydrodynamic galaxy simulations, which follow the genesis of cosmic ray (CR) protons at supernovae and their advective and anisotropic diffusive transport. We show that gravitational collapse of the proto-galaxy generates a corrugated accretion shock, which injects turbulence and drives a small-scale magnetic dynamo. As the shock propagates outwards and the associated turbulence decays, the large velocity shear between the supersonically rotating cool disc with respect to the (partially) pressure-supported hot circumgalactic medium excites Kelvin-Helmholtz surface and body modes. Those interact non-linearly, inject additional turbulence and continuously drive multiple small-scale dynamos, which exponentially amplify weak seed magnetic fields. After saturation at small scales, they grow in scale to reach equipartition with thermal and CR energies in Milky Way-mass galaxies. In small galaxies, the magnetic energy saturates at the turbulent energy while it fails to reach equipartition with thermal and CR energies. We solve for steady-state spectra of CR protons, secondary electrons/positrons from hadronic CR-proton interactions with the interstellar medium, and primary shock-accelerated electrons at supernovae. The radio-synchrotron emission is dominated by primary electrons, irradiates the magnetized disc and bulge of our simulated Milky Way-mass galaxy and weakly traces bubble-shaped magnetically loaded outflows. Our star-forming and star-bursting galaxies with saturated magnetic fields match the global FIR-radio correlation (FRC) across four orders of magnitude. Its intrinsic scatter arises due to (i) different magnetic saturation levels that result from different seed magnetic fields, (ii) different radio synchrotron luminosities for different specific SFRs at fixed SFR, and (iii) a varying radio intensity with galactic inclination. In agreement with observations, several 100-pc-sized regions within star-forming galaxies also obey the FRC, while the centres of starbursts substantially exceed the FRC.


(963)Response approach to the integrated shear 3-point correlation function: the impact of baryonic effects on small scales
  • Anik Halder,
  • Alexandre Barreira
Monthly Notices of the Royal Astronomical Society, 515, p16 (09/2022) doi:10.1093/mnras/stac2046
abstract + abstract -

The integrated shear 3-point correlation function ζ± is a higher-order statistic of the cosmic shear field that describes the modulation of the 2-point correlation function ξ± by long-wavelength features in the field. Here, we introduce a new theoretical model to calculate ζ± that is accurate on small angular scales, and that allows to take baryonic feedback effects into account. Our model builds on the realization that the small-scale ζ± is dominated by the non-linear matter bispectrum in the squeezed limit, which can be evaluated accurately using the non-linear matter power spectrum and its first-order response functions to density and tidal field perturbations. We demonstrate the accuracy of our model by showing that it reproduces the small-scale ζ± measured in simulated cosmic shear maps. The impact of baryonic feedback enters effectively only through the corresponding impact on the non-linear matter power spectrum, thereby permitting to account for these astrophysical effects on ζ± similarly to how they are currently accounted for on ξ±. Using a simple idealized Fisher matrix forecast for a DES-like survey we find that, compared to ξ±, a combined $\xi _{\pm }\ \&\ \zeta _{\pm }$ analysis can lead to improvements of order $20\!-\!40{{\ \rm per\ cent}}$ on the constraints of cosmological parameters such as σ8 or the dark energy equation of state parameter w0. We find similar levels of improvement on the constraints of the baryonic feedback parameters, which strengthens the prospects for cosmic shear data to obtain tight constraints not only on cosmology but also on astrophysical feedback models. These encouraging results motivate future works on the integrated shear 3-point correlation function towards applications to real survey data.


(962)Dust evolution with MUPPI in cosmological volumes
  • Massimiliano Parente,
  • Cinthia Ragone-Figueroa,
  • Gian Luigi Granato,
  • Stefano Borgani,
  • Giuseppe Murante
  • +3
  • Milena Valentini,
  • Alessandro Bressan,
  • Andrea Lapi
  • (less)
Monthly Notices of the Royal Astronomical Society, 515, p19 (09/2022) doi:10.1093/mnras/stac1913
abstract + abstract -

We study the evolution of dust in a cosmological volume using a hydrodynamical simulation in which the dust production is coupled with the MUPPI (MUlti Phase Particle Integrator) sub-resolution model of star formation and feedback. As for the latter, we keep as reference the model setup calibrated previously to match the general properties of Milky Way-like galaxies in zoom-in simulations. However, we suggest that an increase of the star formation efficiency with the local dust-to-gas ratio would better reproduce the observed evolution of the cosmic star formation density. Moreover, the paucity of quenched galaxies at low redshift demands a stronger role of active galactic nucleus feedback. We tune the parameters ruling direct dust production from evolved stars and accretion in the interstellar medium to get scaling relations involving dust, stellar mass and metallicity in good agreement with observations. In low-mass galaxies, the accretion process is inefficient. As a consequence, they remain poorer in silicate and small grains than higher mass ones. We reproduce reasonably well the few available data on the radial distribution of dust outside the galactic region, supporting the assumption that the dust and gas dynamics are well coupled at galactic scales.


(961)Machine Learning Post-Minkowskian Integrals
  • Ryusuke Jinno,
  • Gregor Kälin,
  • Zhengwen Liu,
  • Henrique Rubira
arXiv e-prints (09/2022) e-Print:2209.01091
abstract + abstract -

We study a neural network framework for the numerical evaluation of Feynman loop integrals that are fundamental building blocks for perturbative computations of physical observables in gauge and gravity theories. We show that such a machine learning approach improves the convergence of the Monte Carlo algorithm for high-precision evaluation of multi-dimensional integrals compared to traditional algorithms. In particular, we use a neural network to improve the importance sampling. For a set of representative integrals appearing in the computation of the conservative dynamics for a compact binary system in General Relativity, we perform a quantitative comparison between the Monte Carlo integrators VEGAS and i-flow, an integrator based on neural network sampling.


(960)Anomalous collective dynamics of auto-chemotactic populations
  • Jasper van der Kolk,
  • Florian Rasshofer,
  • Richard Swiderski,
  • Astik Haldar,
  • Abhik Basu
  • +1
arXiv e-prints (09/2022) e-Print:2209.01047
abstract + abstract -

While the role of local interactions in nonequilibrium phase transitions is well studied, a fundamental understanding of the effects of long-range interactions is lacking. We study the critical dynamics of reproducing agents subject to auto-chemotactic interactions and limited resources. A renormalization group analysis reveals distinct scaling regimes for fast (attractive or repulsive) interactions; for slow signal transduction the dynamics is dominated by a diffusive fixed point. Further, we present a novel nonlinear mechanism that stabilizes the continuous transition against the emergence of a characteristic length scale due to a chemotactic collapse.


(959)Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): Scattered light detection of a possible disk wind in RY Tau
  • P. -G. Valegård,
  • C. Ginski,
  • C. Dominik,
  • J. Bae,
  • M. Benisty
  • +12
  • T. Birnstiel,
  • S. Facchini,
  • A. Garufi,
  • M. Hogerheijde,
  • R. G. van Holstein,
  • M. Langlois,
  • C. F. Manara,
  • P. Pinilla,
  • Ch. Rab,
  • Á. Ribas,
  • L. B. F. M. Waters,
  • J. Williams
  • (less)
arXiv e-prints (09/2022) e-Print:2209.01969
abstract + abstract -

Disk winds are an important mechanism for accretion and disk evolution around young stars. The accreting intermediate-mass T-Tauri star RY Tau has an active jet and a previously known disk wind. Archival optical and new near-infrared observations of the RY Tau system show two horn-like components stretching out as a cone from RY Tau. Scattered light from the disk around RY Tau is visible in near-infrared but not seen at optical wavelengths. In the near-infrared, dark wedges that separates the horns from the disk, indicating we may see the scattered light from a disk wind. We use archived ALMA and SPHERE/ZIMPOL I-band observations combined with newly acquired SPEHRE/IRDIS H-band observations and available literature to build a simple geometric model of the RY Tau disk and disk wind. We use Monte Carlo radiative transfer modelling \textit{MCMax3D} to create comparable synthetic observations that test the effect of a dusty wind on the optical effect in the observations. We constrain the grain size and dust mass needed in the disk wind to reproduce the effect from the observations. A model geometrically reminiscent of a dusty disk wind with small micron to sub-micron size grains elevated above the disk can reproduce the optical effect seen in the observations. The mass in the obscuring component of the wind has been constrained to $1\times10^{-9} M_{\odot} \leq M \leq 5\times10^{-8} M_{\odot}$ which corresponds to a lower limit mass loss rate in the wind of about $\sim 1\times10^{-8}M_{\odot}\mathrm{yr}^{-1}$. While an illuminate dust cavity cannot be ruled out without measurements of the gas velocity, we argue that a magnetically launched disk wind is the most likely scenario.


(958)Suppressing variance in 21-cm signal simulations during reionization
  • Sambit K. Giri,
  • Aurel Schneider,
  • Francisco Maion,
  • Raul E. Angulo
arXiv e-prints (09/2022) e-Print:2209.01225
abstract + abstract -

Current best limits on the 21-cm signal during reionization are provided at large scales ($\gtrsim$100 Mpc). To model these scales, enormous simulation volumes are required which are computationally expensive. We find that the primary source of uncertainty at these large scales is sample variance, which decides the minimum size of simulations required to analyse current and upcoming observations. In large-scale structure simulations, the method of `fixing' the initial conditions (ICs) to exactly follow the initial power spectrum and `pairing' two simulations with exactly out-of-phase ICs has been shown to significantly reduce sample variance. Here we apply this `fixing and pairing' (F\&P) approach to reionization simulations whose clustering signal originates from both density fluctuations and reionization bubbles. Using a semi-numerical code, we show that with the traditional method, simulation boxes of $L\simeq 500$ (300) Mpc are required to model the large-scale clustering signal at $k$=0.1 Mpc$^{-1}$ with a precision of 5 (10) per cent. Using F\&P, the simulation boxes can be reduced by a factor of 2 to obtain the same precision level. We conclude that the computing costs can be reduced by at least a factor of 4 when using the F\&P approach.


(957)TDCOSMO XI. Automated Modeling of 9 Strongly Lensed Quasars and Comparison Between Lens Modeling Software
  • S. Ertl,
  • S. Schuldt,
  • S. H. Suyu,
  • T. Schmidt,
  • T. Treu
  • +3
  • S. Birrer,
  • A. J. Shajib,
  • D. Sluse
  • (less)
arXiv e-prints (09/2022) e-Print:2209.03094
abstract + abstract -

To use strong gravitational lenses as an astrophysical or cosmological probe, models of their mass distributions are often needed. We present a new, time-efficient automation code for uniform modeling of strongly lensed quasars with GLEE, a lens modeling software, for high-resolution multi-band data. By using the observed positions of the lensed quasars and the spatially extended surface brightness distribution of the lensed quasar host galaxy, we obtain a model of the mass distribution of the lens galaxy. We apply this uniform modeling pipeline to a sample of nine strongly lensed quasars with HST WFC 3 images. The models show in most cases well reconstructed light components and a good alignment between mass and light centroids. We find that the automated modeling code significantly reduces the user input time during the modeling process. The preparation time of required input files is reduced significantly. This automated modeling pipeline can efficiently produce uniform models of extensive lens system samples which can be used for further cosmological analysis. A blind test through a comparison with the results of an independent automated modeling pipeline based on the modeling software Lenstronomy reveals important lessons. Quantities such as Einstein radius, astrometry, mass flattening and position angle are generally robustly determined. Other quantities depend crucially on the quality of the data and the accuracy of the PSF reconstruction. Better data and/or more detailed analysis will be necessary to elevate our automated models to cosmography grade. Nevertheless, our pipeline enables the quick selection of lenses for follow-up monitoring and further modeling, significantly speeding up the construction of cosmography-grade models. This is an important step forward to take advantage of the orders of magnitude increase in the number of lenses expected in the coming decade.


(956)Improved theory predictions and global analysis of exclusive b → sμ<SUP>+</SUP>μ<SUP>−</SUP> processes
  • Nico Gubernari,
  • Méril Reboud,
  • Danny van Dyk,
  • Javier Virto
Journal of High Energy Physics, 2022 (09/2022) doi:10.1007/JHEP09(2022)133
abstract + abstract -

We provide improved Standard Model theory predictions for the exclusive rare semimuonic processes B → K(*)μ+μ and Bs → ϕμ+μ. Our results are based on a novel parametrization of the non-local form factors, which manifestly respects a recently developed dispersive bound. We critically compare our predictions to those obtained in the framework of QCD factorization. Our predictions provide, for the first time, parametric estimates of the systematic uncertainties due to non-local contributions. Comparing our predictions within the Standard Model to available experimental data, we find a large tension for B → Kμ+μ. A simple model-independent analysis of potential effects beyond the Standard Model yields results compatible with other approaches, albeit with larger uncertainties for the B → K*μ+μ and Bs → ϕμ+μ decays. Our approach yields systematically improvable predictions, and we look forward to its application in further analyses beyond the Standard Model.


(955)A low-threshold diamond cryogenic detector for sub-GeV dark matter searches
  • A. H. Abdelhameed,
  • G. Angloher,
  • A. Bento,
  • E. Bertoldo,
  • A. Bertolini
  • +11
  • L. Canonica,
  • N. Ferreiro Iachellini,
  • D. Fuchs,
  • A. Garai,
  • D. Hauff,
  • A. Nilima,
  • M. Mancuso,
  • F. Petricca,
  • F. Pröbst,
  • F. Pucci,
  • J. Rothe
  • (less)
European Physical Journal C, 82 (09/2022) doi:10.1140/epjc/s10052-022-10829-5
abstract + abstract -

In this work we report the realization of the first low-threshold cryogenic detector that uses diamond as absorber for astroparticle physics applications. We tested two 0.175 g CVD diamond samples, each instrumented with a W-TES. The sensors showed transitions at about 25 mK. We present the performance of the diamond detectors and we highlight the best performing one, where we obtained an energy threshold as low as 16.8 eV. This promising result lays the foundation for the use of diamond for different fields of applications where low threshold and excellent energy resolution are required, as i.e. light dark matter searches and BSM physics with coherent elastic neutrino nucleus scattering.


(954)Characterizing the 3D Kinematics of Young Stars in the Radcliffe Wave
  • Alan J. Tu,
  • Catherine Zucker,
  • Joshua S. Speagle,
  • Angus Beane,
  • Alyssa Goodman
  • +3
  • João Alves,
  • Jacqueline Faherty,
  • Andreas Burkert
  • (less)
The Astrophysical Journal, 936, p17 (09/2022) doi:10.3847/1538-4357/ac82f0
abstract + abstract -

We present an analysis of the kinematics of the Radcliffe Wave, a 2.7 kpc long sinusoidal band of molecular clouds in the solar neighborhood recently detected via 3D dust mapping. With Gaia DR2 astrometry and spectroscopy, we analyze the 3D space velocities of ~1500 young stars along the Radcliffe Wave in action-angle space, using the motion of the wave's newly born stars as a proxy for its gas motion. We find that the vertical angle of young stars-corresponding to their orbital phase perpendicular to the Galactic plane-varies significantly as a function of position along the structure, in a pattern potentially consistent with a wavelike oscillation. This kind of oscillation is not seen in a control sample of older stars from Gaia occupying the same volume, disfavoring formation channels caused by long-lived physical processes. We use a "wavy midplane" model to try to account for the trend in vertical angles seen in young stars, and find that while the best-fit parameters for the wave's spatial period and amplitude are qualitatively consistent with the existing morphology defined by 3D dust, there is no evidence for additional velocity structure. These results support more recent and/or transitory processes in the formation of the Radcliffe Wave, which would primarily affect the motion of the wave's gaseous material. Comparisons of our results with new and upcoming simulations, in conjunction with new stellar radial velocity measurements in Gaia DR3, should allow us to further discriminate between various competing hypotheses.


(953)Standard Model Predictions for Rare K and B Decays without New Physics Infection
  • Andrzej J. Buras
arXiv e-prints (09/2022) e-Print:2209.03968
abstract + abstract -

The Standard Model (SM) does not contain by definition any new physics (NP) contributions to any observable but contains four CKM parameters which are not predicted by this model. We point out that if these four parameters are determined in a global fit that includes processes which are infected by NP, the resulting SM contributions to rare decay branching ratios cannot be considered as true SM contributions to the latter. On the other hand true SM predictions, that are free from the CKM dependence, can be obtained for suitable ratios of the $K$ and $B$ rare decay branching ratios to $\Delta M_s$, $\Delta M_d$ and $|\varepsilon_K|$, all calculated within the SM. These three observables contain by now only small hadronic uncertainties and are already well measured so that rather precise true SM predictions for the ratios in question can be obtained. In this context the rapid test of NP infection in the $\Delta F=2$ sector is provided by a $|V_{cb}|-\gamma$ plot that involves $\Delta M_s$, $\Delta M_d$, $|\varepsilon_K|$, and the mixing induced CP-asymmetry $S_{\psi K_S}$. As with the present hadronic matrix elements this test turns out to be negative, assuming negligible NP infection in the $\Delta F=2$ sector and setting the values of these four observables to the experimental ones, allows to obtain SM predictions for all $K$ and $B$ rare decay branching ratios that are most accurate to date and as a byproduct to obtain the full CKM matrix on the basis of $\Delta F=2$ transitions alone. Using this strategy we obtain SM predictions for 26 branching ratios for rare semileptonic and leptonic $K$ and $B$ decays with the $\mu^+\mu^-$ pair or the $\nu\bar\nu$ pair in the final state. Most interesting turn out to be the anomalies in the low $q^2$ bin in $B^+\to K^+\mu^+\mu^-$ ($5.1\sigma$) and $B_s\to \phi\mu^+\mu^-$ ($4.8\sigma$).


(952)Full-shape BOSS constraints on dark matter interacting with dark radiation and lifting the $S_8$ tension
  • Henrique Rubira,
  • Asmaa Mazoun,
  • Mathias Garny
arXiv e-prints (09/2022) e-Print:2209.03974
abstract + abstract -

In this work we derive constraints on interacting dark matter-dark radiation models from a full-shape analysis of BOSS-DR12 galaxy clustering data, combined with Planck legacy cosmic microwave background (CMB) and baryon acoustic oscillation (BAO) measurements. We consider a set of models parameterized within the effective theory of structure formation (ETHOS), quantifying the lifting of the $S_8$ tension in view of KiDS weak-lensing results. The most favorable scenarios point to a fraction $f\sim 10-100\%$ of interacting dark matter as well as a dark radiation temperature that is smaller by a factor $\xi\sim 0.1-0.15$ compared to the CMB, leading to a reduction of the tension to the $\sim 1\sigma$ level. The temperature dependence of the interaction rate favored by relaxing the $S_8$ tension is realized for a weakly coupled unbroken non-Abelian $SU(N)$ gauge interaction in the dark sector. To map our results onto this $SU(N)$ model, we compute higher-order corrections due to Debye screening. We find a lower bound $\alpha_d\equiv g_d^2/(4\pi)\gtrsim 10^{-8} (10^{-9})$ for dark matter mass $1000 (1)$ GeV for relaxing the $S_8$ tension, consistent with upper bounds from galaxy ellipticities and compatible with self-interactions relevant for small-scale structure formation.


(951)Higgsless simulations of cosmological phase transitions and gravitational waves
  • Ryusuke Jinno,
  • Thomas Konstandin,
  • Henrique Rubira,
  • Isak Stomberg
arXiv e-prints (09/2022) e-Print:2209.04369
abstract + abstract -

First-order cosmological phase transitions in the early Universe source sound waves and, subsequently, a background of stochastic gravitational waves. Currently, predictions of these gravitational waves rely heavily on simulations of a Higgs field coupled to the plasma of the early Universe, the former providing the latent heat of the phase transition. Numerically, this is a rather demanding task since several length scales enter the dynamics. From smallest to largest, these are the thickness of the Higgs interface separating the different phases, the shell thickness of the sound waves, and the average bubble size. In this work, we present an approach to perform Higgsless simulations in three dimensions, producing fully nonlinear results, while at the same time removing the hierarchically smallest scale from the lattice. This significantly reduces the complexity of the problem and contributes to making our approach highly efficient. We provide spectra for the produced gravitational waves for various choices of wall velocity and strength of the phase transition, as well as introduce a fitting function for the spectral shape.


(950)Galaxies in the central regions of simulated galaxy clusters
  • Antonio Ragagnin,
  • Massimo Meneghetti,
  • Luigi Bassini,
  • Cinthia Ragone-Figueroa,
  • Gian Luigi Granato
  • +18
  • Giulia Despali,
  • Carlo Giocoli,
  • Giovanni Granata,
  • Lauro Moscardini,
  • Pietro Bergamini,
  • Elena Rasia,
  • Milena Valentini,
  • Stefano Borgani,
  • Francesco Calura,
  • Klaus Dolag,
  • Claudio Grillo,
  • Amata Mercurio,
  • Giuseppe Murante,
  • Priyamvada Natarajan,
  • Piero Rosati,
  • Giuliano Taffoni,
  • Luca Tornatore,
  • Luca Tortorelli
  • (less)
Astronomy and Astrophysics, 665, p11 (09/2022) doi:10.1051/0004-6361/202243651
abstract + abstract -

Context. Recent observations found that observed cluster member galaxies are more compact than their counterparts in ΛCDM hydrodynamic simulations, as indicated by the difference in their strong gravitational lensing properties, and they reported that measured and simulated galaxy-galaxy strong lensing events on small scales are discrepant by one order of magnitude. Among the possible explanations for this discrepancy, some studies suggest that simulations with better resolution and implementing different schemes for galaxy formation could produce simulations that are in better agreement with the observations.
Aims: In this work, we aim to assess the impact of numerical resolution and of the implementation of energy input from AGN feedback models on the inner structure of cluster sub-haloes in hydrodynamic simulations.
Methods: We compared several zoom-in re-simulations of a sub-sample of cluster-sized haloes obtained by varying mass resolution and softening the length and AGN energy feedback scheme. We studied the impact of these different setups on the sub-halo (SH) abundances, their radial distribution, their density and mass profiles, and the relation between the maximum circular velocity, which is a proxy for SH compactness
Results: Regardless of the adopted numerical resolution and feedback model, SHs with masses of MSH ≲ 1011 h−1 M, the most relevant mass range for galaxy-galaxy strong lensing, have maximum circular velocities ∼30% smaller than those measured from strong lensing observations. We also find that simulations with less effective AGN energy feedback produce massive SHs (MSH ≳ 1011 h−1 M) with higher maximum circular velocity and that their Vmax − MSH relation approaches the observed one. However, the stellar-mass number count of these objects exceeds the one found in observations, and we find that the compactness of these simulated SHs is the result of an extremely over-efficient star formation in their cores, also leading to larger than observed SH stellar mass.
Conclusions: Regardless of the resolution and galaxy formation model adopted, simulations are unable to simultaneously reproduce the observed stellar masses and compactness (or maximum circular velocities) of cluster galaxies. Thus, the discrepancy between theory and observations that emerged previous works. It remains an open question as to whether such a discrepancy reflects limitations of the current implementation of galaxy formation models or the ΛCDM paradigm.


(949)New constraints on the up-quark valence distribution in the proton
  • Ritu Aggarwal,
  • Michiel Botje,
  • Allen Caldwell,
  • Francesca Capel,
  • Oliver Schulz
arXiv e-prints (09/2022) e-Print:2209.06571
abstract + abstract -

The high-$x$ data from the ZEUS Collaboration are used to extract parton density distributions of the proton deep in the perturbative regime of QCD. The data primarily constrain the up-quark valence distribution and new results are presented on its $x$-dependence as well as on the momentum carried by the up-quark. The results were obtained using Bayesian analysis methods which can serve as a model for future parton density extractions.


(948)LYRA III: The smallest Reionization survivors
  • Thales A. Gutcke,
  • Christoph Pfrommer,
  • Greg L. Bryan,
  • Rüdiger Pakmor,
  • Volker Springel
  • +1
arXiv e-prints (09/2022) e-Print:2209.03366
abstract + abstract -

The dividing line between galaxies that are quenched by reionization ("relics") and galaxies that survive reionization (i.e. continue forming stars) is commonly discussed in terms of a halo mass threshold. We probe this threshold in a physically more complete and accurate way than has been possible to date, using five extremely high resolution ($M_\mathrm{target}=4M_\odot$) cosmological zoom-in simulations of dwarf galaxies within the halo mass range $1-4\times10^9M_\odot$. The employed LYRA simulation model features resolved interstellar medium physics and individual, resolved supernova explosions. In our results, we discover an interesting intermediate population of dwarf galaxies close to the threshold mass but which are neither full reionization relics nor full reionization survivors. These galaxies initially quench at the time of reionization but merely remain quiescent for ~500Myr. At $z\approx5$ they recommence star formation in a synchronous way, and remain star-forming until the present day. These results demonstrate that the halo mass at $z=0$ is not a good indicator of survival close to the threshold. While the star formation histories we find are diverse, we show that they are directly related to the ability of a given halo to retain and cool gas. Whereas the latter is most strongly dependent on the mass (or virial temperature) of the host halo at the time of reionization, it also depends on its growth history, the UV background (and its decrease at late times) and the amount of metals retained within the halo.


(947)Assembly bias in the local PNG halo bias and its implication for $f_{\rm NL}$ constraints
  • Titouan Lazeyras,
  • Alexandre Barreira,
  • Fabian Schmidt,
  • Vincent Desjacques
arXiv e-prints (09/2022) e-Print:2209.07251
abstract + abstract -

We use $N$-body simulations to study halo assembly bias (i.e., the dependence of halo clustering on properties beyond total mass) in the density and primordial non-Gaussianity (PNG) linear bias parameters $b_1$ and $b_\phi$, respectively. We consider concentration, spin and sphericity as secondary halo properties, for which we find a clear detection of assembly bias for $b_1$ and $b_\phi$. At fixed total mass, halo spin and sphericity impact $b_1$ and $b_\phi$ in a similar manner, roughly preserving the shape of the linear $b_\phi(b_1)$ relation satisfied by the global halo population. Halo concentration, however, drives $b_1$ and $b_\phi$ in opposite directions. This induces significant changes to the $b_\phi(b_1)$ relation, with higher concentration halos having higher amplitude of $b_\phi(b_1)$. For $z=0.5$ and $b_1 \approx 2$ in particular, the population comprising either all halos, those with the $33\%$ lowest or those with the $33\%$ highest concentrations have a PNG bias of $b_\phi \approx 3$, $b_\phi \approx -1$ and $b_\phi \approx 9$, respectively. Varying the halo concentration can make $b_\phi$ very small and even change its sign. These results have important ramifications for galaxy clustering constraints of the local PNG parameter $f_{\rm NL}$ that assume fixed forms for the $b_\phi(b_1)$ relation. We illustrate the significant impact of halo assembly bias in actual data using the BOSS DR12 galaxy power spectrum: assuming that BOSS galaxies are representative of all halos, the $33\%$ lowest or the $33\%$ highest concentration halos yields $\sigma_{f_{\rm NL}} = 44, 165, 19$, respectively. Our results suggest taking host halo concentration into account in galaxy selection strategies to maximize the signal-to-noise on $f_{\rm NL}$. They also motivate more simulation-based efforts to study the $b_\phi(b_1)$ relation of halos and galaxies.


(946)Operation of an Archaeological Lead PbWO<SUB>4</SUB> Crystal to Search for Neutrinos from Astrophysical Sources with a Transition Edge Sensor
  • N. Ferreiro Iachellini,
  • L. Pattavina,
  • A. H. Abdelhameed,
  • A. Bento,
  • L. Canonica
  • +7
  • F. Danevich,
  • O. M. Dubovik,
  • D. Fuchs,
  • A. Garai,
  • M. Mancuso,
  • F. Petricca,
  • I. A. Tupitsyna
  • (less)
Journal of Low Temperature Physics (09/2022) doi:10.1007/s10909-022-02823-8
abstract + abstract -

The experimental detection of the CEν NS allows the investigation of neutrinos and neutrino sources with all-flavor sensitivity. Given its large content in neutrons and stability, Pb is a very appealing choice as target element. The presence of the radioisotope 210Pb (T1/2∼ 22 yrs) makes natural Pb unsuitable for low-background, low-energy event searches. This limitation can be overcome employing Pb of archaeological origin, where several half-lives of 210Pb have gone by. We present results of a cryogenic measurement of a 15 g PbWO4 crystal, grown with archaeological Pb (older than ∼2000 yrs) that achieved a sub-keV nuclear recoil detection threshold. A ton-scale experiment employing such material, with a detection threshold for nuclear recoils of just 1 keV would probe the entire Milky Way for SuperNovae, with equal sensitivity for all neutrino flavors, allowing the study of the core of such exceptional events.


(945)The Hateful Eight: Connecting Massive Substructures in Galaxy Clusters like Abell 2744 to their Dynamical Assembly State using the Magneticum Simulations
  • Lucas C. Kimmig,
  • Rhea-Silvia Remus,
  • Klaus Dolag,
  • Veronica Biffi
arXiv e-prints (09/2022) e-Print:2209.09916
abstract + abstract -

Substructures are known to be good tracers for the dynamical states and recent accretion histories of the most massive collapsed structures in the Universe, galaxy clusters. Observations find extremely massive substructures in some clusters, especially Abell 2744, which are potentially in tension with the $\Lambda$CDM paradigm since they are not found in simulations directly. However, the methods to measure substructure masses strongly differ between observations and simulations. Using the fully hydrodynamical cosmological simulation suite Magneticum Pathfinder we develop a method to measure substructure masses in projection from simulations, similar to the observational approach. We identify a simulated Abell 2744 counterpart that not only has eight substructures of similar mass fractions but also exhibits similar features in the hot gas component. This cluster formed only recently through a major merger together with at least 6 massive minor merger events since z=1, where prior the most massive component had a mass of less than $1\times10^{14}M_\odot$. We show that the mass fraction of all substructures and of the eighth substructure separately are excellent tracers for the dynamical state and assembly history for all galaxy cluster mass ranges, with high fractions indicating merger events within the last 2Gyr. Finally, we demonstrate that the differences between subhalo masses measured directly from simulations as bound and those measured in projection are due to methodology, with the latter generally 2-3 times larger than the former. We provide a predictor function to estimate projected substructure masses from SubFind masses for future comparison studies between simulations and observations.


(944)Clash of Titans: a MUSE dynamical study of the extreme cluster merger SPT-CL J0307-6225
  • D. Hernández-Lang,
  • A. Zenteno,
  • A. Diaz-Ocampo,
  • H. Cuevas,
  • J. Clancy
  • +21
  • P. H. Prado,
  • F. Aldás,
  • D. Pallero,
  • R. Monteiro-Oliveira,
  • F. A. Gómez,
  • Amelia Ramirez,
  • J. Wynter,
  • E. R. Carrasco,
  • G. K. T. Hau,
  • B. Stalder,
  • M. McDonald,
  • M. Bayliss,
  • B. Floyd,
  • G. Garmire,
  • A. Katzenberger,
  • K. J. Kim,
  • M. Klein,
  • G. Mahler,
  • J. L. Nilo Castellon,
  • A. Saro,
  • T. Somboonpanyakul
  • (less)
Monthly Notices of the Royal Astronomical Society (09/2022) doi:10.1093/mnras/stac2480
abstract + abstract -

We present MUSE spectroscopy, Megacam imaging, and Chandra X-ray emission for SPT-CL J0307-6225, a z=0.58 major merging galaxy cluster with a large BCG-SZ centroid separation and a highly disturbed X-ray morphology. The galaxy density distribution shows two main overdensities with separations of 0.144 and 0.017 arcmin to their respective BCGs. We characterize the central regions of the two colliding structures, namely 0307-6225N and 0307-6225S, finding velocity derived masses of M200, N = 2.44 ± 1.41 × 1014 M and M200, S = 3.16 ± 1.88 × 1014 M, with a line-of-sight velocity difference of |Δv| = 342 km s-1. The total dynamically derived mass is consistent with the SZ derived mass of 7.63 h$_{70}^{-1}$ ± 1.36 × 1014 M. We model the merger using the Monte Carlo Merger Analysis Code, estimating a merging angle of 36$^{+14}_{-12}$ degrees with respect to the plane of the sky. Comparing with simulations of a merging system with a mass ratio of 1:3, we find that the best scenario is that of an ongoing merger that began 0.96$^{+0.31}_{-0.18}$ Gyr ago. We also characterize the galaxy population using Hδ and [OII] λ3727 Å lines. We find that most of the emission-line galaxies belong to 0307-6225S, close to the X-ray peak position, with a third of them corresponding to red-cluster sequence galaxies, and the rest to blue galaxies with velocities consistent with recent periods of accretion. Moreover, we suggest that 0307-6225S suffered a previous merger, evidenced through the two equally bright BCGs at the center with a velocity difference of ~674 km s-1.


(943)The SATIN project I: Turbulent multi-phase ISM in Milky Way simulations with SNe feedback from stellar clusters
  • Rebekka Bieri,
  • Thorsten Naab,
  • Sam Geen,
  • Jonathan P. Coles,
  • Rüdiger Pakmor
  • +1
arXiv e-prints (09/2022) e-Print:2209.06842
abstract + abstract -

We introduce the star formation and Supernova (SN) feedback model of the SATIN (Simulating AGNs Through ISM with Non-Equilibrium Effects) project to simulate the evolution of the star forming multi-phase interstellar medium (ISM) of entire disk galaxies. This galaxy-wide implementation of a successful ISM feedback model naturally covers an order of magnitude in gas surface density, shear and radial motions. It is implemented in the adaptive mesh refinement code RAMSES at a peak resolution of 9 pc. New stars are represented by star cluster (sink) particles with individual SN delay times for massive stars. With SN feedback, cooling and gravity, the galactic ISM develops a realistic three-phase structure. The star formation rates naturally follow observed scaling relations for the local Milky Way gas surface density. SNe drive additional turbulence in the warm (300 K < $T$ < 10$^4$ K) gas and increase the kinetic energy of the cold gas, cooling out of the warm phase. The majority of the gas leaving the galactic ISM is warm and hot with mass loading factors of $3 \le \eta \le 10$. While the hot gas is leaving the system, the warm and cold gas falls back onto the disc in a galactic fountain flow.


(942)On the Sensitivity of Halo Shape Measurements
  • Moritz S. Fischer,
  • Lucas M. Valenzuela
arXiv e-prints (09/2022) e-Print:2209.11244
abstract + abstract -

Shape measurements of galaxies and galaxy clusters are widespread in the analysis of cosmological simulations. But the limitations of those measurements have been poorly investigated. In this paper, we explain why the quality of the shape measurement does not only depend on the numerical resolution, but also on the density gradient. In particular, this can limit the quality of measurements in the central regions of haloes. We propose a criterion to estimate the sensitivity of the measured shapes based on the density gradient of the halo and apply it to cosmological simulations of collisionless and self-interacting dark matter. By this, we demonstrate where reliable measurements of the halo shape are possible and how cored density profiles limit their applicability.


(941)Parameterisations of thermal bomb explosions for core-collapse supernovae and 56Ni production
  • Liliya Imasheva,
  • H. -Thomas Janka,
  • Achim Weiss
arXiv e-prints (09/2022) e-Print:2209.10989
abstract + abstract -

Thermal bombs are a widely used method to artificially trigger explosions of core-collapse supernovae (CCSNe) to determine their nucleosynthesis or ejecta and remnant properties. Recently, their use in spherically symmetric (1D) hydrodynamic simulations led to the result that {56,57}Ni and 44Ti are massively underproduced compared to observational estimates for Supernova 1987A, if the explosions are slow, i.e., if the explosion mechanism of CCSNe releases the explosion energy on long timescales. It was concluded that rapid explosions are required to match observed abundances, i.e., the explosion mechanism must provide the CCSN energy nearly instantaneously on timescales of some ten to order 100 ms. This result, if valid, would disfavor the neutrino-heating mechanism, which releases the CCSN energy on timescales of seconds. Here, we demonstrate by 1D hydrodynamic simulations and nucleosynthetic post-processing that these conclusions are a consequence of disregarding the initial collapse of the stellar core in the thermal-bomb modelling before the bomb releases the explosion energy. We demonstrate that the anti-correlation of 56Ni yield and energy-injection timescale vanishes when the initial collapse is included and that it can even be reversed, i.e., more 56Ni is made by slower explosions, when the collapse proceeds to small radii similar to those where neutrino heating takes place in CCSNe. We also show that the 56Ni production in thermal-bomb explosions is sensitive to the chosen mass cut and that a fixed mass layer or fixed volume for the energy deposition cause only secondary differences. Moreover, we propose a most appropriate setup for thermal bombs.


(940)StaNdaRT: A repository of standardized test models and outputs for supernova radiative transfer
  • Stéphane Blondin,
  • Sergei Blinnikov,
  • Fionntan P. Callan,
  • Christine E. Collins,
  • Luc Dessart
  • +24
  • Wesley Even,
  • Andreas Flörs,
  • Andrew G. Fullard,
  • D. John Hillier,
  • Anders Jerkstrand,
  • Daniel Kasen,
  • Boaz Katz,
  • Wolfgang Kerzendorf,
  • Alexandra Kozyreva,
  • Jack O'Brien,
  • Ezequiel A. Pássaro,
  • Nathaniel Roth,
  • Ken J. Shen,
  • Luke Shingles,
  • Stuart A. Sim,
  • Jaladh Singhal,
  • Isaac G. Smith,
  • Elena Sorokina,
  • Victor P. Utrobin,
  • Christian Vogl,
  • Marc Williamson,
  • Ryan Wollaeger,
  • Stan E. Woosley,
  • Nahliel Wygoda
  • (less)
arXiv e-prints (09/2022) e-Print:2209.11671
abstract + abstract -

We present the first results of a comprehensive supernova (SN) radiative-transfer (RT) code-comparison initiative (StaNdaRT), where the emission from the same set of standardized test models is simulated by currently-used RT codes. A total of ten codes have been run on a set of four benchmark ejecta models of Type Ia supernovae. We consider two sub-Chandrasekhar-mass ($M_\mathrm{tot} = 1.0$ M$_\odot$) toy models with analytic density and composition profiles and two Chandrasekhar-mass delayed-detonation models that are outcomes of hydrodynamical simulations. We adopt spherical symmetry for all four models. The results of the different codes, including the light curves, spectra, and the evolution of several physical properties as a function of radius and time, are provided in electronic form in a standard format via a public repository. We also include the detailed test model profiles and several python scripts for accessing and presenting the input and output files. We also provide the code used to generate the toy models studied here. In this paper, we describe in detail the test models, radiative-transfer codes and output formats and provide access to the repository. We present example results of several key diagnostic features.


(939)Development of the Low Frequency Telescope Focal Plane Detector Modules for LiteBIRD
  • Benjamin Westbrook,
  • Christopher Raum,
  • Shawn Beckman,
  • Adrian T. Lee,
  • Nicole Farias
  • +21
  • Andrew Bogdan,
  • Amber Hornsby,
  • Aritoki Suzuki,
  • Kaja Rotermund,
  • Tucker Elleflot,
  • Jason E. Austermann,
  • James A. Beall,
  • Shannon M. Duff,
  • Johannes Hubmayr,
  • Michael R. Vissers,
  • Michael J. Link,
  • Greg Jaehnig,
  • Nils Halverson,
  • Tomasso Ghigna,
  • Masashi Hazumi,
  • Samantha Stever,
  • Yuto Minami,
  • Keith L. Thompson,
  • Megan Russell,
  • Kam Arnold,
  • Maximiliano Silva-Feaver
  • (less)
arXiv e-prints (09/2022) e-Print:2209.09864
abstract + abstract -

LiteBIRD is a JAXA-led strategic large-class satellite mission designed to measure the polarization of the cosmic microwave background and Galactic foregrounds from 34 to 448 GHz across the entire sky from L2 in the late 2020s. The scientific payload includes three telescopes which are called the low-, mid-, and high-frequency telescopes each with their own receiver that covers a portion of the mission's frequency range. The low frequency telescope will map synchrotron radiation from the Galactic foreground and the cosmic microwave background. We discuss the design, fabrication, and characterization of the low-frequency focal plane modules for low-frequency telescope, which has a total bandwidth ranging from 34 to 161 GHz. There will be a total of 4 different pixel types with 8 overlapping bands to cover the full frequency range. These modules are housed in a single low-frequency focal plane unit which provides thermal isolation, mechanical support, and radiative baffling for the detectors. The module design implements multi-chroic lenslet-coupled sinuous antenna arrays coupled to transition edge sensor bolometers read out with frequency-domain mulitplexing. While this technology has strong heritage in ground-based cosmic microwave background experiments, the broad frequency coverage, low optical loading conditions, and the high cosmic ray background of the space environment require further development of this technology to be suitable for LiteBIRD. In these proceedings, we discuss the optical and bolometeric characterization of a triplexing prototype pixel with bands centered on 78, 100, and 140 GHz.


(938)The impact of dynamic pressure bumps on the observational properties of protoplanetary disks
  • Jochen Stadler,
  • Matías Gárate,
  • Paola Pinilla,
  • Christian Lenz,
  • Cornelis P. Dullemond
  • +2
  • Til Birnstiel,
  • Sebastian M. Stammler
  • (less)
arXiv e-prints (09/2022) e-Print:2209.07931
abstract + abstract -

Over the last years, large (sub-)millimetre surveys of protoplanetary disks have well constrained the demographics of disks, such as their millimetre luminosities, spectral indices, and disk radii. Additionally, several high-resolution observations have revealed an abundance of substructures in the disks dust continuum. The most prominent are ring like structures, likely due to pressure bumps trapping dust particles. The origins and characteristics of these bumps, nevertheless, need to be further investigated. The purpose of this work is to study how dynamic pressure bumps affect observational properties of protoplanetary disks. We further aim to differentiate between the planetary- versus zonal flow-origin of pressure bumps. We perform one-dimensional gas and dust evolution simulations, setting up models with varying pressure bump features. We subsequently run radiative transfer calculations to obtain synthetic images and the different quantities of observations. We find that the outermost pressure bump determines the disks dust size across different millimetre wavelengths. Our modelled dust traps need to form early (< 0.1 Myr), fast (on viscous timescales), and must be long lived (> Myr) to obtain the observed high millimetre luminosities and low spectral indices of disks. While the planetary bump models can reproduce these observables irrespectively of the opacity prescription, the highest opacities are needed for the zonal flow bump model to be in line with observations. Our findings favour the planetary- over the zonal flow-origin of pressure bumps and support the idea that planet formation already occurs in early class 0-1 stages of circumstellar disks. The determination of the disks effective size through its outermost pressure bump also delivers a possible answer to why disks in recent low-resolution surveys appear to have the same sizes across different millimetre wavelengths.


(937)Selection of prebiotic oligonucleotides by cyclic phase separation
  • Giacomo Bartolucci,
  • Adriana Calaça Serrão,
  • Philipp Schwintek,
  • Alexandra Kühnlein,
  • Yash Rana
  • +5
  • Philipp Janto,
  • Dorothea Hofer,
  • Christof B. Mast,
  • Dieter Braun,
  • Christoph A. Weber
  • (less)
arXiv e-prints (09/2022) e-Print:2209.10672
abstract + abstract -

The emergence of functional oligonucleotides on early Earth required a molecular selection mechanism to screen for specific sequences with prebiotic functions. Cyclic processes such as daily temperature oscillations were ubiquitous in this environment and could trigger oligonucleotide phase separation. Here, we propose sequence selection based on phase separation cycles realized through sedimentation in a system subjected to the feeding of oligonucleotides. Using theory and experiments with DNA, we show sequence-specific enrichment in the sedimented dense phase, in particular of short 22-mer DNA sequences. The underlying mechanism selects for complementarity, as it enriches sequences that tightly interact in the condensed phase through base-pairing. Our mechanism also enables initially weakly biased pools to enhance their sequence bias or to replace the most abundant sequences as the cycles progress. Our findings provide an example of a selection mechanism that may have eased screening for the first auto-catalytic self-replicating oligonucleotides.


(936)Instability of bubble expansion at zero temperature
  • Wen-Yuan Ai,
  • Juan S. Cruz,
  • Bjorn Garbrecht,
  • Carlos Tamarit
arXiv e-prints (09/2022) e-Print:2209.00639
abstract + abstract -

In the context of false vacuum decay at zero temperature, it is well known that bubbles expand with uniform acceleration in the rest frame of nucleation. We show that this uniformly accelerating expansion suffers from an instability. This can be observed as a tachyonic mode in the spectrum of fluctuations for the energy functional in the reference frame in which the uniformly accelerating bubble wall appears static. In such a frame, arbitrary small perturbations cause an amplifying departure from the static wall solution. This implies that the nucleated bubble is not a critical point of the energy functional in the rest frame of nucleation but becomes one in the accelerating frame. The aforementioned instability for vacuum bubbles can be related to the well-known instability for the nucleated critical static bubbles during finite-temperature phase transitions in the rest frame of the plasma. It is proposed that zero-temperature vacuum decays as seen from accelerating frames have a dual description in terms of finite-temperature phase transitions.


(935)A giant planet shaping the disk around the very low-mass star CIDA 1
  • P. Curone,
  • A. F. Izquierdo,
  • L. Testi,
  • G. Lodato,
  • S. Facchini
  • +11
  • A. Natta,
  • P. Pinilla,
  • N. T. Kurtovic,
  • C. Toci,
  • M. Benisty,
  • M. Tazzari,
  • F. Borsa,
  • M. Lombardi,
  • C. F. Manara,
  • E. Sanchis,
  • L. Ricci
  • (less)
Astronomy and Astrophysics, 665, p22 (09/2022) doi:10.1051/0004-6361/202142748
abstract + abstract -

Context. Exoplanetary research has provided us with exciting discoveries of planets around very low-mass (VLM) stars (0.08 M ≲ M* ≲ 0.3 M; e.g., TRAPPIST-1 and Proxima Centauri). However, current theoretical models still strive to explain planet formation in these conditions and do not predict the development of giant planets. Recent high-resolution observations from the Atacama Large Millimeter/submillimeter Array (ALMA) of the disk around CIDA 1, a VLM star in Taurus, show substructures that hint at the presence of a massive planet.
Aims: We aim to reproduce the dust ring of CIDA 1, observed in the dust continuum emission in ALMA Band 7 (0.9 mm) and Band 4 (2.1 mm), along with its 12CO (J = 3−2) and 13CO (J = 3−2) channel maps, assuming the structures are shaped by the interaction of the disk with a massive planet. We seek to retrieve the mass and position of the putative planet, through a global simulation that assesses planet-disk interactions to quantitatively reproduce protoplanetary disk observations of both dust and gas emission in a self-consistent way.
Methods: Using a set of hydrodynamical simulations, we model a protoplanetary disk that hosts an embedded planet with a starting mass of between 0.1 and 4.0 MJup and initially located at a distance of between 9 and 11 au from the central star. We compute the dust and gas emission using radiative transfer simulations, and, finally, we obtain the synthetic observations, treating the images as the actual ALMA observations.
Results: Our models indicate that a planet with a minimum mass of ~1.4 MJup orbiting at a distance of ~9−10 au can explain the morphology and location of the observed dust ring in Band 7 and Band 4. We match the flux of the dust emission observation with a dust-to-gas mass ratio in the disk of ~10−2. We are able to reproduce the low spectral index (~2) observed where the dust ring is detected, with a ~40−50% fraction of optically thick emission. Assuming a 12CO abundance of 5 × 10−5 and a 13CO abundance 70 times lower, our synthetic images reproduce the morphology of the 12CO (J = 3−2) and 13CO (J = 3−2) observed channel maps where the cloud absorption allowed a detection. From our simulations, we estimate that a stellar mass M* = 0.2 M and a systemic velocity vsys = 6.25 km s−1 are needed to reproduce the gas rotation as retrieved from molecular line observations. Applying an empirical relation between planet mass and gap width in the dust, we predict a maximum planet mass of ~4−8 MJup.
Conclusions: Our results suggest the presence of a massive planet orbiting CIDA 1, thus challenging our understanding of planet formation around VLM stars.


(934)The static force from generalized Wilson loops using gradient flow
  • Viljami Leino,
  • Nora Brambilla,
  • Julian Mayer-Steudte,
  • Antonio Vairo
European Physical Journal Web of Conferences, 258 (08/2022) doi:10.1051/epjconf/202225804009
abstract + abstract -

We explore a novel approach to compute the force between a static quark-antiquark pair with the gradient flow algorithm on the lattice. The approach is based on inserting a chromoelectric field in a Wilson loop. The renormalization issues, associated with the finite size of the chromoelectric field on the lattice, can be solved with the use of gradient flow. We compare numerical results for the flowed static potential to our previous measurement of the same observable without a gradient flow.


(933)TimeEvolver: A program for time evolution with improved error bound
  • Marco Michel,
  • Sebastian Zell
Computer Physics Communications, 277 (08/2022) doi:10.1016/j.cpc.2022.108374
abstract + abstract -

We present TimeEvolver, a program for computing time evolution in a generic quantum system. It relies on well-known Krylov subspace techniques to tackle the problem of multiplying the exponential of a large sparse matrix iH, where H is the Hamiltonian, with an initial vector v. The fact that H is Hermitian makes it possible to provide an easily computable bound on the accuracy of the Krylov approximation. Apart from effects of numerical roundoff, the resulting a posteriori error bound is rigorous, which represents a crucial novelty as compared to existing software packages such as Expokit[1]. On a standard notebook, TimeEvolver allows to compute time evolution with adjustable precision in Hilbert spaces of dimension greater than 106. Additionally, we provide routines for deriving the matrix H from a more abstract representation of the Hamiltonian operator.


(932)A panchromatic view of star cluster formation in a simulated dwarf galaxy starburst
  • Natalia Lahén,
  • Thorsten Naab,
  • Guinevere Kauffmann
Monthly Notices of the Royal Astronomical Society, 514, p21 (08/2022) doi:10.1093/mnras/stac1594
abstract + abstract -

We present a photometric analysis of star and star cluster (SC) formation in a high-resolution simulation of a dwarf galaxy starburst that allows the formation of individual stars to be followed. Previous work demonstrated that the properties of the SCs formed in the simulation are in good agreement with observations. In this paper, we create mock spectral energy distributions and broad-band photometric images using the radiative transfer code SKIRT 9. We test several observational star formation rate (SFR) tracers and find that 24 $\mu$m, total infrared and Hα trace the underlying SFR during the (post)starburst phase, while UV tracers yield a more accurate picture of star formation during quiescent phases prior to and after the merger. We then place the simulated galaxy at distances of 10 and 50 Mpc and use aperture photometry at Hubble Space Telescope resolution to analyse the simulated SC population. During the starburst phase, a hierarchically forming set of SCs leads inaccurate source separation because of crowding. This results in estimated SC mass function slopes that are up to ~0.3 shallower than the true slope of ~-1.9 to -2 found for the bound clusters identified from the particle data in the simulation. The masses of the largest clusters are overestimated by a factor of up to 2.9 due to unresolved clusters within the apertures. The aperture-based analysis also produces a relation between cluster formation efficiency and SFR surface density that is slightly flatter than that recovered from bound clusters. The differences are strongest in quiescent SF environments.


(931)Low-luminosity type IIP supermnovae: SN 2005cs and SN 2020cxd as very low-energy iron core-collapse explosions
  • Alexandra Kozyreva,
  • Hans-Thomas Janka,
  • Daniel Kresse,
  • Stefan Taubenberger,
  • Petr Baklanov
Monthly Notices of the Royal Astronomical Society, 514, p17 (08/2022) doi:10.1093/mnras/stac1518
abstract + abstract -

SN 2020cxd is a representative of the family of low-energy, underluminous Type IIP supernovae (SNe), whose observations and analysis were recently reported by Yang et al. (2021). Here, we re-evaluate the observational data for the diagnostic SN properties by employing the hydrodynamic explosion model of a 9 M red supergiant progenitor with an iron core and a pre-collapse mass of 8.75 M. The explosion of the star was obtained by the neutrino-driven mechanism in a fully self-consistent simulation in three dimensions (3D). Multiband light curves and photospheric velocities for the plateau phase are computed with the one-dimensional radiation-hydrodynamics code STELLA, applied to the spherically averaged 3D explosion model as well as sphericized radial profiles in different directions of the 3D model. We find that the overall evolution of the bolometric light curve, duration of the plateau phase, and basic properties of the multiband emission can be well reproduced by our SN model with its explosion energy of only 0.7 × 1050 erg and an ejecta mass of 7.4 M. These values are considerably lower than the previously reported numbers, but they are compatible with those needed to explain the fundamental observational properties of the prototype low-luminosity SN 2005cs. Because of the good compatibility of our photospheric velocities with line velocities determined for SN 2005cs, we conclude that the line velocities of SN 2020cxd are probably overestimated by up to a factor of about 3. The evolution of the line velocities of SN 2005cs compared to photospheric velocities in different explosion directions might point to intrinsic asymmetries in the SN ejecta.


(930)Development of the low frequency telescope focal plane detector modules for LiteBIRD
  • B. Westbrook,
  • C. Raum,
  • S. Beckman,
  • A. T. Lee,
  • N. Farias
  • +21
  • A. Bogdan,
  • A. Hornsby,
  • A. Suzuki,
  • K. Rotermund,
  • T. Elleflot,
  • J. E. Austerman,
  • J. A. Beall,
  • S. M. Duff,
  • J. Hubmayr,
  • M. R. Vissers,
  • M. J. Link,
  • G. Jaehnig,
  • N. Halverson,
  • T. Ghigna,
  • M. Hazumi,
  • S. Stever,
  • Y. Minami,
  • K. L. Thompson,
  • M. Russell,
  • K. Arnold,
  • M. Silva-Feaver
  • (less)
Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy XI, 12190, p17 (08/2022) doi:10.1117/12.2630574
abstract + abstract -

LiteBIRD is a JAXA-led strategic large-class satellite mission designed to measure the polarization of the cosmic microwave background and Galactic foregrounds from 34 to 448 GHz across the entire sky from L2 in the late 2020s. The scientific payload includes three telescopes which are called the low-, mid-, and high-frequency telescopes each with their own receiver that covers a portion of the mission's frequency range. The low frequency telescope will map synchrotron radiation from the Galactic foreground and the cosmic microwave background. We discuss the design, fabrication, and characterization of the low-frequency focal plane modules for low-frequency telescope, which has a total bandwidth ranging from 34 to 161 GHz. There will be a total of 4 different pixel types with 8 overlapping bands to cover the full frequency range. These modules are housed in a single low-frequency focal plane unit which provides thermal isolation, mechanical support, and radiative baffling for the detectors. The module design implements multi-chroic lenslet-coupled sinuous antenna arrays coupled to transition edge sensor bolometers read out with frequency-domain mulitplexing. While this technology has strong heritage in ground-based cosmic microwave background experiments, the broad frequency coverage, low optical loading conditions, and the high cosmic ray background of the space environment require further development of this technology to be suitable for LiteBIRD. In these proceedings, we discuss the optical and bolometeric characterization of a triplexing prototype pixel with bands centered on 78, 100, and 140 GHz.


(929)Primordial Dusty Rings and Episodic Outbursts in Protoplanetary Discs
  • Kundan Kadam,
  • Eduard Vorobyov,
  • Shantanu Basu
arXiv e-prints (08/2022) e-Print:2208.12105
abstract + abstract -

We investigate the formation and evolution of "primordial" dusty rings occurring in the inner regions of protoplanetary discs, with the help of long-term, coupled dust-gas, magnetohydrodynamic simulations. The simulations are global and start from the collapse phase of the parent cloud core, while the dead zone is calculated via an adaptive $\alpha$ formulation by taking into account the local ionization balance. The evolution of the dusty component includes its growth and back reaction on to the gas. Previously, using simulations with only a gas component, we showed that dynamical rings form at the inner edge of the dead zone. We find that when dust evolution as well as magnetic field evolution in the flux-freezing limit are included, the dusty rings formed are more numerous and span a larger radial extent in the inner disc, while the dead zone is more robust and persists for a much longer time. We show that these dynamical rings concentrate enough dust mass to become streaming unstable, which should result in rapid planetesimal formation even in the embedded phases of the system. The episodic outbursts caused by the magnetorotational instability have significant impact on the evolution of the rings. The outbursts drain the inner disc of grown dust, however, the period between bursts is sufficiently long for the planetesimal growth via streaming instability.The dust mass contained within the rings is large enough to ultimately produce planetary systems with the core accretion scenario. The low mass systems rarely undergo outbursts and thus, the conditions around such stars can be especially conducive for planet formation.


(928)Lyα Halos around [O III]-selected Galaxies in HETDEX
  • Maja Lujan Niemeyer,
  • William P. Bowman,
  • Robin Ciardullo,
  • Max Gronke,
  • Eiichiro Komatsu
  • +11
  • Maximilian Fabricius,
  • Daniel J. Farrow,
  • Steven L. Finkelstein,
  • Karl Gebhardt,
  • Caryl Gronwall,
  • Gary J. Hill,
  • Chenxu Liu,
  • Erin Mentuch Cooper,
  • Donald P. Schneider,
  • Sarah Tuttle,
  • Gregory R. Zeimann
  • (less)
The Astrophysical Journal, 934, p6 (08/2022) doi:10.3847/2041-8213/ac82e5
abstract + abstract -

We present extended Lyα emission out to 800 kpc of 1034 [O III]-selected galaxies at redshifts 1.9 < z < 2.35 using the Hobby-Eberly Telescope Dark Energy Experiment. The locations and redshifts of the galaxies are taken from the 3D-HST survey. The median-stacked surface brightness profile of the Lyα emission of the [O III]-selected galaxies agrees well with that of 968 bright Lyα-emitting galaxies (LAEs) at r > 40 kpc from the galaxy centers. The surface brightness in the inner parts (r < 10 kpc) around the [O III]-selected galaxies, however, is 10 times fainter than that of the LAEs. Our results are consistent with the notion that photons dominating the outer regions of the Lyα halos are not produced in the central galaxies but originate outside of them.


(927)The Origin of the [C II] Deficit in a Simulated Dwarf Galaxy Merger-driven Starburst
  • Thomas G. Bisbas,
  • Stefanie Walch,
  • Thorsten Naab,
  • Natalia Lahén,
  • Rodrigo Herrera-Camus
  • +4
  • Ulrich P. Steinwandel,
  • Constantina M. Fotopoulou,
  • Chia-Yu Hu,
  • Peter H. Johansson
  • (less)
The Astrophysical Journal, 934, p18 (08/2022) doi:10.3847/1538-4357/ac7960
abstract + abstract -

We present [C II] synthetic observations of smoothed particle hydrodynamics (SPH) simulations of a dwarf galaxy merger. The merging process varies the star formation rate (SFR) by more than three orders of magnitude. Several star clusters are formed, the feedback of which disperses and unbinds the dense gas through expanding H II regions and supernova (SN) explosions. For galaxies with properties similar to the modeled ones, we find that the [C II] emission remains optically thin throughout the merging process. We identify the warm neutral medium ( $3\lt \mathrm{log}{T}_{\mathrm{gas}}\lt 4$ with χ HI > 2χ H2) to be the primary source of [C II] emission (~58% contribution), although at stages when the H II regions are young and dense (during star cluster formation or SNe in the form of ionized bubbles), they can contribute ≳50% to the total [C II] emission. We find that the [C II]/far-IR (FIR) ratio decreases owing to thermal saturation of the [C II] emission caused by strong far-UV radiation fields emitted by the massive star clusters, leading to a [C II] deficit medium. We investigate the [C II]-SFR relation and find an approximately linear correlation that agrees well with observations, particularly those from the Dwarf Galaxy Survey. Our simulation reproduces the observed trends of [C II]/FIR versus ΣSFR and ΣFIR, and it agrees well with the Kennicutt relation of SFR-FIR luminosity. We propose that local peaks of [C II] in resolved observations may provide evidence for ongoing massive cluster formation.


(926)Virgo: Scalable Unsupervised Classification of Cosmological Shock Waves
  • Max Lamparth,
  • Ludwig Böss,
  • Ulrich Steinwandel,
  • Klaus Dolag
arXiv e-prints (08/2022) e-Print:2208.06859
abstract + abstract -

Cosmological shock waves are essential to understanding the formation of cosmological structures. To study them, scientists run computationally expensive high-resolution 3D hydrodynamic simulations. Interpreting the simulation results is challenging because the resulting data sets are enormous, and the shock wave surfaces are hard to separate and classify due to their complex morphologies and multiple shock fronts intersecting. We introduce a novel pipeline, Virgo, combining physical motivation, scalability, and probabilistic robustness to tackle this unsolved unsupervised classification problem. To this end, we employ kernel principal component analysis with low-rank matrix approximations to denoise data sets of shocked particles and create labeled subsets. We perform supervised classification to recover full data resolution with stochastic variational deep kernel learning. We evaluate on three state-of-the-art data sets with varying complexity and achieve good results. The proposed pipeline runs automatically, has only a few hyperparameters, and performs well on all tested data sets. Our results are promising for large-scale applications, and we highlight now enabled future scientific work.


(925)Radiopurity of a kg-scale PbWO<SUB>4</SUB> cryogenic detector produced from archaeological Pb for the RES-NOVA experiment
  • RES-NOVA Group of Interest,
  • J. W. Beeman,
  • G. Benato,
  • C. Bucci,
  • L. Canonica
  • +40
  • P. Carniti,
  • E. Celi,
  • M. Clemenza,
  • A. D'Addabbo,
  • F. A. Danevich,
  • S. Di Domizio,
  • S. DiLorenzo,
  • O. M. Dubovik,
  • N. Ferreiro Iachellini,
  • F. Ferroni,
  • E. Fiorini,
  • S. Fu,
  • A. Garai,
  • S. Ghislandi,
  • L. Gironi,
  • P. Gorla,
  • C. Gotti,
  • P. V. Guillaumon,
  • D. L. Helis,
  • G. P. Kovtun,
  • M. Mancuso,
  • L. Marini,
  • M. Olmi,
  • L. Pagnanini,
  • L. Pattavina,
  • G. Pessina,
  • F. Petricca,
  • S. Pirro,
  • S. Pozzi,
  • A. Puiu,
  • S. Quitadamo,
  • J. Rothe,
  • A. P. Scherban,
  • S. Schönert,
  • D. A. Solopikhin,
  • R. Strauss,
  • E. Tarabini,
  • V. I. Tretyak,
  • I. A. Tupitsyna,
  • V. Wagner
  • (less)
European Physical Journal C, 82 (08/2022) doi:10.1140/epjc/s10052-022-10656-8
abstract + abstract -

RES-NOVA is a newly proposed experiment for detecting neutrinos from astrophysical sources, mainly Supernovae, using an array of cryogenic detectors made of PbWO4 crystals produced from archaeological Pb. This unconventional material, characterized by intrinsic high radiopurity, enables low-background levels in the region of interest for the neutrino detection via Coherent Elastic neutrino-Nucleus Scattering (CEν NS). This signal lies at the detector energy threshold, O(1 keV), and it is expected to be hidden by naturally occurring radioactive contaminants of the crystal absorber. Here, we present the results of a radiopurity assay on a 0.84 kg PbWO4 crystal produced from archaeological Pb operated as a cryogenic detector. The crystal internal radioactive contaminations are: 232Th <40 μ Bq/kg, 238U <30 μ Bq/kg, 226Ra 1.3 mBq/kg and 210Pb 22.5 mBq/kg. We also present a background projection for the final experiment and possible mitigation strategies for further background suppression. The achieved results demonstrate the feasibility of realizing this new class of detectors.


(924)Monitoring accretion rate variability in the Orion Nebula Cluster with the Wendelstein Wide Field Imager
  • S. Flaischlen,
  • T. Preibisch,
  • M. Kluge,
  • C. F. Manara,
  • B. Ercolano
arXiv e-prints (08/2022) e-Print:2208.04823
abstract + abstract -

The understanding of the accretion process has a central role in the understanding of star and planet formation. We aim to test how accretion variability influences previous correlation analyses of the relation between X-ray activity and accretion rates, which is important for understanding the evolution of circumstellar disks and disk photoevaporation. We monitored accreting stars in the Orion Nebula Cluster from November 24, 2014, until February 17, 2019, for 42 epochs with the Wendelstein Wide Field Imager in the Sloan Digital Sky Survey u'g'r' filters on the 2 m Fraunhofer Telescope on Mount Wendelstein. Mass accretion rates were determined from the measured ultraviolet excess. The influence of the mass accretion rate variability on the relation between X-ray luminosities and mass accretion rates was analyzed statistically. We find a typical interquartile range of ~ 0.3 dex for the mass accretion rate variability on timescales from weeks to ~ 2 years. The variability has likely no significant influence on a correlation analysis of the X-ray luminosity and the mass accretion rate observed at different times when the sample size is large enough. The observed anticorrelation between the X-ray luminosity and the mass accretion rate predicted by models of photoevaporation-starved accretion is likely not due to a bias introduced by different observing times.


(923)Elliptic modular graph forms II: Iterated integrals
  • Martijn Hidding,
  • Oliver Schlotterer,
  • Bram Verbeek
arXiv e-prints (08/2022) e-Print:2208.11116
abstract + abstract -

Elliptic modular graph forms (eMGFs) are non-holomorphic modular forms depending on a modular parameter $\tau$ of a torus and marked points $z$ thereon. Traditionally, eMGFs are constructed from nested lattice sums over the discrete momenta on the worldsheet torus in closed-string genus-one amplitudes. In this work, we develop methods to translate the lattice-sum realization of eMGFs into iterated integrals over modular parameters $\tau$ of the torus with particular focus on cases with one marked point. Such iterated-integral representations manifest algebraic and differential relations among eMGFs and their degeneration limit $\tau \rightarrow i\infty$. From a mathematical point of view, our results yield concrete realizations of single-valued elliptic polylogarithms at arbitrary depth in terms of meromorphic iterated integrals over modular forms and their complex conjugates. The basis dimensions of eMGFs at fixed modular and transcendental weights are derived from a simple counting of iterated integrals and a generalization of Tsunogai's derivation algebra.


(922)Analytical evaluation of AdS<SUB>4</SUB> Witten diagrams as flat space multi-loop Feynman integrals
  • Till Heckelbacher,
  • Ivo Sachs,
  • Evgeny Skvortsov,
  • Pierre Vanhove
Journal of High Energy Physics, 2022 (08/2022) doi:10.1007/JHEP08(2022)052
abstract + abstract -

We describe a systematic approach for the evaluation of Witten diagrams for multi-loop scattering amplitudes of a conformally coupled scalar ϕ4-theory in Euclidean AdS4, by recasting the Witten diagrams as flat space Feynman integrals. We derive closed form expressions for the anomalous dimensions for all double-trace operators up to the second order in the coupling constant. We explain the relation between the flat space unitarity methods and the discontinuities of the short distance expansion on the boundary of Witten diagrams.


(921)Scattering Amplitudes and N-Body Post-Minkowskian Hamiltonians in General Relativity and Beyond
  • Callum R. T. Jones,
  • Mikhail Solon
arXiv e-prints (08/2022) e-Print:2208.02281
abstract + abstract -

We present a general framework for calculating post-Minskowskian, classical, conservative Hamiltonians for $N$ non-spinning bodies in general relativity from relativistic scattering amplitudes. Novel features for $N>2$ are described including the subtraction of tree-like iteration contributions and the calculation of non-trivial many-body Fourier transform integrals needed to construct position space potentials. A new approach to calculating these integrals as an expansion in the hierarchical limit is described based on the method of regions. As an explicit example, we present the $\mathcal{O}\left(G^2\right)$ 3-body momentum space potential in general relativity as well as for charged bodies in Einstein-Maxwell. The result is shown to be in perfect agreement with previous post-Newtonian calculations in general relativity up to $\mathcal{O}\left(G^2 v^4\right)$. Furthermore, in appropriate limits the result is shown to agree perfectly with relativistic probe scattering in multi-center extremal black hole backgrounds and with the scattering of slowly-moving extremal black holes in the moduli space approximation.


(920)A new approach to color-coherent parton evolution
  • Florian Herren,
  • Stefan Höche,
  • Frank Krauss,
  • Daniel Reichelt,
  • Marek Schoenherr
arXiv e-prints (08/2022) e-Print:2208.06057
abstract + abstract -

We present a simple parton-shower model that replaces the explicit angular ordering of the coherent branching formalism with a differentially accurate simulation of soft-gluon radiation by means of a non-trivial dependence on azimuthal angles. We introduce a global kinematics mapping and provide an analytic proof that it satisfies the criteria for next-to leading logarithmic accuracy. In the new algorithm, initial and final state evolution are treated on the same footing. We provide an implementation for final-state evolution in the numerical code Alaric and present a first comparison to experimental data.


(919)NLO QCD renormalization group evolution for nonleptonic Δ F =2 transitions in the SMEFT
  • Jason Aebischer,
  • Andrzej J. Buras,
  • Jacky Kumar
Physical Review D, 106 (08/2022) doi:10.1103/PhysRevD.106.035003
abstract + abstract -

We present for the first time Next-to-Leading (NLO) QCD renormalization group (RG) evolution matrices for nonleptonic Δ F =2 transitions in the Standard Model effective field theory (SMEFT). To this end we transform first the known two-loop QCD anomalous dimension matrices (ADMs) of the BSM (Beyond the SM) operators in the so-called Buras Misiak Urban basis into the ones in the common weak effective theory (WET) basis (the so-called Jenkins Manohar Stoffer basis) for which tree-level and one-loop matching to the SMEFT are already known. This subsequently allows us to find the two-loop QCD ADMs for the SMEFT nonleptonic Δ F =2 operators in the Warsaw basis. Having all these ingredients we investigate the impact of these NLO QCD effects on the QCD RG evolution of SMEFT Wilson coefficients for nonleptonic Δ F =2 transitions from the new physics scale Λ down to the electroweak scale μew. The main benefit of these new contributions is that they allow one to remove renormalization scheme dependences present in the one-loop matchings both between the WET and SMEFT and also between SMEFT and a chosen UV completion. But the Next-to-Leading (NLO) QCD effects, calculated here in the Naive dimensional regularisation minimal subtraction scheme, turn out to be small, in the ballpark of a few percent but larger than one-loop Yukawa top effects when only the Δ F =2 operators are considered. The more complicated class of nonleptonic Δ F =1 decays will be presented soon in another publication.


(918)Planes of Satellite Galaxies in the Magneticum Pathfinder Simulations
  • Pascal U. Förster,
  • Rhea-Silvia Remus,
  • Klaus Dolag,
  • Lucas C. Kimmig,
  • Adelheid Teklu
  • +1
arXiv e-prints (08/2022) e-Print:2208.05496
abstract + abstract -

Planes of satellites are observed around many galaxies. However, these observations are still considered a point of tension for the $\Lambda$CDM paradigm. We use the fully hydrodynamical cosmological $\Lambda$CDM state-of-the-art simulation Magneticum Pathfinder to investigate the existence of such planes over a large range of haloes, from Milky Way to galaxy cluster masses. To this end, we develop the Momentum in Thinnest Plane (MTP) method to identify planes and quantify the properties of their constituent satellites, considering both position and momentum. We find that thin planes ($20\%\cdot R_\mathrm{halo}$) containing at least $50\%$ of the total number of satellites can be found in almost all systems. In Milky Way mass-like systems, around 86\% of such planes are even aligned in momentum ($90\%$ of the total satellite momentum), where the fraction is smaller if more satellites are required to be inside the plane. We further find a mass dependency, with more massive systems exhibiting systematically thicker planes. This may point towards the change from continuous accretion of small objects along filaments and sheets for less massive haloes to the accretion of large objects (e.g., major mergers) dominating the growth of more massive haloes. There is no correlation between the existence of a plane and the main galaxy's morphology. Finally, we find a clear preference for the minor axes of the satellite planes and the host galaxy to be aligned, in agreement with recent observations.


(917)A flexible event reconstruction based on machine learning and likelihood principles
  • Philipp Eller,
  • Aaron Fienberg,
  • Jan Weldert,
  • Garrett Wendel,
  • Sebastian Böser
  • +1
arXiv e-prints (08/2022) e-Print:2208.10166
abstract + abstract -

Event reconstruction is a central step in many particle physics experiments, turning detector observables into parameter estimates; for example estimating the energy of an interaction given the sensor readout of a detector. A corresponding likelihood function is often intractable, and approximations need to be constructed. In our work, we first show how the full likelihood for a many-sensor detector can be broken apart into smaller terms, and secondly how we can train neural networks to approximate all terms solely based on forward simulation. Our technique results in a fast, flexible, and close-to-optimal surrogate model proportional to the likelihood and can be used in conjunction with standard inference techniques. We illustrate our technique for parameter inference in neutrino telescopes based on maximum likelihood and Bayesian posterior sampling. Given its great flexibility, we also showcase our method for detector optimization, and apply it to simulation of a ton-scale water-based liquid scintillator detector.


(916)Disintegration of beauty: a precision study
  • Alexander Lenz,
  • Maria Laura Piscopo,
  • Aleksey V. Rusov
arXiv e-prints (08/2022) e-Print:2208.02643
abstract + abstract -

We update the Standard Model (SM) predictions for $B$-meson lifetimes within the heavy quark expansion (HQE). Including for the first time the contribution of the Darwin operator, SU(3)$_F$ breaking corrections to the matrix element of dimension-six four-quark operators and the so-called eye-contractions, we obtain for the total widths $\Gamma (B^+) = (0.58^{+0.11}_{-0.07}) \, \mbox{ps}^{-1}$, $\Gamma (B_d) = (0.63^{+0.11}_{-0.07}) \, \mbox{ps}^{-1}$, $\Gamma (B_s) = (0.63^{+0.11}_{-0.07}) \, \mbox{ps}^{-1}$, and for the lifetime ratios $\tau (B^+) / \tau (B_d) = 1.086 \pm 0.022$, $\tau (B_s) / \tau (B_d) = 1.003 \pm 0.006 \, (1.028 \pm 0.011)$. The two values for the last observable arise from using two different sets of input for the non-perturbative parameters $\mu_\pi^2(B_d)$, $\mu_G^2(B_d)$, and $\rho_D^3(B_d)$ as well as from different estimates of the SU(3)$_F$ breaking in these parameters. Our results are overall in very good agreement with the corresponding experimental data, however, there seems to emerge a tension in $\tau (B_s)/\tau (B_d)$ when considering the second set of input parameters. Specifically, this observable is extremely sensitive to the size of the parameter $\rho_D^3 (B_d)$ and of the SU(3)$_F$ breaking effects in $\mu_\pi^2$, $\mu_G^2$ and $\rho_D^3$; hence, it is of utmost importance to be able to better constrain all these parameters. In this respect, an extraction of $\mu_\pi^2 (B_s), \mu_G^2 (B_s), \rho_D^3 (B_s)$ from future experimental data on inclusive semileptonic $B_s$-meson decays or from direct non-perturbative calculations, as well as more insights about the value of $\rho_D^3 (B)$ extracted from fit, would be very helpful in reducing the corresponding theory uncertainties.


(915)Unusual Gas Structure in an Otherwise Normal Spiral Galaxy Hosting GRB 171205A/SN 2017iuk
  • M. Arabsalmani,
  • S. Roychowdhury,
  • F. Renaud,
  • A. Burkert,
  • E. Emsellem
  • +2
The Astronomical Journal, 164, p6 (08/2022) doi:10.3847/1538-3881/ac77f5
abstract + abstract -

We study the structure of atomic hydrogen (H I) in the host galaxy of GRB 171205A/SN 2017iuk at z = 0.037 through H I 21 cm emission line observations with the Karl G. Jansky Very Large Array. These observations reveal unusual morphology and kinematics of the H I in this otherwise apparently normal galaxy. High column density, cold H I is absent from an extended North-South region passing by the optical center of the galaxy, but instead is extended toward the South, on both sides of the galaxy. Moreover, the H I kinematics do not show a continuous change along the major axis of the galaxy as expected in a classical rotating disk. We explore several scenarios to explain the H I structure and kinematics in the galaxy: feedback from a central starburst and/or an active galactic nucleus, ram-pressure stripping, accretion, and tidal interaction from a companion galaxy. All of these options are ruled out. The most viable remaining explanation is the penetrating passage of a satellite through the disk only a few Myr ago, redistributing the H I in the GRB host without yet affecting its stellar distribution. It can also lead to the rapid formation of peculiar stars due to a violent induced shock. The location of GRB 171205A in the vicinity of the distorted area suggests that its progenitor star(s) originated in extreme conditions that share the same origin as the peculiarities in H I. This could explain the atypical location of GRB 171205A in its host galaxy.


(914)The GIGANTES Data Set: Precision Cosmology from Voids in the Machine-learning Era
  • Christina D. Kreisch,
  • Alice Pisani,
  • Francisco Villaescusa-Navarro,
  • David N. Spergel,
  • Benjamin D. Wandelt
  • +2
The Astrophysical Journal, 935, p19 (08/2022) doi:10.3847/1538-4357/ac7d4b
abstract + abstract -

We present GIGANTES, the most extensive and realistic void catalog suite ever released-containing over 1 billion cosmic voids covering a volume larger than the observable universe, more than 20 TB of data, and created by running the void finder VIDE on QUIJOTE's halo simulations. The GIGANTES suite, spanning thousands of cosmological models, opens up the study of voids, answering compelling questions: Do voids carry unique cosmological information? How is this information correlated with galaxy information? Leveraging the large number of voids in the GIGANTES suite, our Fisher constraints demonstrate voids contain additional information, critically tightening constraints on cosmological parameters. We use traditional void summary statistics (void size function, void density profile) and the void autocorrelation function, which independently yields an error of 0.13 eV on ∑ m ν for a 1 h -3 Gpc3 simulation, without cosmic microwave background priors. Combining halos and voids we forecast an error of 0.09 eV from the same volume, representing a gain of 60% compared to halos alone. Extrapolating to next generation multi-Gpc3 surveys such as the Dark Energy Spectroscopic Instrument, Euclid, the Spectro-Photometer for the History of the Universe and Ices Explorer, and the Roman Space Telescope, we expect voids should yield an independent determination of neutrino mass. Crucially, GIGANTES is the first void catalog suite expressly built for intensive machine-learning exploration. We illustrate this by training a neural network to perform likelihood-free inference on the void size function, giving a ~20% constraint on Ωm. Cosmology problems provide an impetus to develop novel deep-learning techniques. With GIGANTES, machine learning gains an impressive data set, offering unique problems that will stimulate new techniques.


(913)The Young and the Wild: What happens to Protoclusters forming at z = 4?
  • Rhea-Silvia Remus,
  • Klaus Dolag,
  • Helmut Dannerbauer
arXiv e-prints (08/2022) e-Print:2208.01053
abstract + abstract -

Using one of the largest volumes of the hydrodynamical cosmological simulation suit Magneticum, we study the evolution of protoclusters identified at redshift = 4, with properties similar to SPT2349-56. We identify 42 protoclusters in the simulation, as massive and equally rich in substructures as observed, confirming that these structures are already virialized. The dynamics of the internally fast rotating member galaxies within these protoclusters resembles observations, merging rapidly to form the cores of the BCGs of the assembling clusters. Half of the gas reservoir of these structures is in a hot phase, with the metal-enrichment at a very early stage. These systems show a good agreement with the observed amount of cold star-forming gas, largely enriched to solar values. We predict that some of the member galaxies are already quenched at z = 4, rendering them undetectable through measurements of their gas reservoir. Tracing the evolution of protoclusters reveals that none of the typical mass indicators at high redshift are good tracers to predict the present-day mass of the system. We find that none of the simulated protoclusters with properties as SPT2349-56 at z = 4.3, are among the top ten most massive clusters at redshift z = 0, with some barely reaching masses of M = 2 x 10^14Msun. Although the average star-formation and mass-growth rates in the simulated galaxies match observations at high redshift reasonably well, the simulation fails to reproduce the extremely high total star-formation rates within observed protoclusters, indicating that the sub-grid models are lacking the ability to reproduce higher star-formation efficiency (or lower depletion timescales).


(912)Decomposition of galactic X-ray emission with Phox: Contributions from hot gas and XRBs
  • Stephan Vladutescu-Zopp,
  • Veronica Biffi,
  • Klaus Dolag
arXiv e-prints (08/2022) e-Print:2208.04975
abstract + abstract -

We provide a numerical framework with which spatially and spectrally accurate representations of X-ray binary populations can be studied from hydrodynamical cosmological simulations. We construct average spectra accounting for a hot gas component and verify the emergence of observed scaling relations between galaxy wide X-ray luminosity ($L_{X}$) and stellar mass ($M_{\star}$) as well as star-formation rate (SFR). Using simulated galaxy halos extracted from the $(48\,h^{-1} \mathrm{cMpc})^3$ volume of the Magneticum Pathfinder cosmological simulations at $z = 0.07$ we generate mock spectra with the X-ray photon-simulator Phox. We extend the Phox code to account for the stellar component in the simulation and study the resulting contribution in composite galactic spectra. Average X-ray luminosity functions are perfectly reproduced up to the one-photon luminosity limit. Comparing our resulting $L_{X}-\mathrm{SFR}-M_{\star}$ relation for X-ray binaries with recent observations of field galaxies in the Virgo galaxy cluster we find significant overlap. Invoking a metallicity dependent model for high-mass X-ray binaries yields an anti-correlation between mass-weighted stellar metallicity and SFR normalized luminosity. The spatial distribution of high-mass X-ray binaries coincides with star-formation regions of simulated galaxies while low-mass X-ray binaries follow the stellar mass surface density. X-ray binary emission is the dominant contribution in the 2-10 keV band in the absence of an actively accreting central super-massive black hole with 50% contribution in the 0.5-2 keV band rivaling the hot gas component. Our modelling remains consistent with observations despite uncertainties connected to our approach. The predictive power and easily extendable framework hold great value for future investigations of galactic X-ray spectra.


(911)Fragmentation with discontinuous Galerkin schemes: Non-linear fragmentation
  • Maxime Lombart,
  • Mark Hutchison,
  • Yueh-Ning Lee
Monthly Notices of the Royal Astronomical Society (08/2022) doi:10.1093/mnras/stac2232
abstract + abstract -

Small grains play an essential role in astrophysical processes such as chemistry, radiative transfer, gas/dust dynamics. The population of small grains is mainly maintained by the fragmentation process due to colliding grains. An accurate treatment of dust fragmentation is required in numerical modelling. However, current algorithms for solving fragmentation equation suffer from an over-diffusion in the conditions of 3D simulations. To tackle this challenge, we developed a Discontinuous Galerkin scheme to solve efficiently the non-linear fragmentation equation with a limited number of dust bins.


(910)COMET: Clustering Observables Modelled by Emulated perturbation Theory
  • Alexander Eggemeier,
  • Benjamin Camacho-Quevedo,
  • Andrea Pezzotta,
  • Martin Crocce,
  • Román Scoccimarro
  • +1
arXiv e-prints (08/2022) e-Print:2208.01070
abstract + abstract -

In this paper we present COMET, a Gaussian process emulator of the galaxy power spectrum multipoles in redshift-space. The model predictions are based on one-loop perturbation theory and we consider two alternative descriptions of redshift-space distortions: one that performs a full expansion of the real- to redshift-space mapping, as in recent effective field theory models, and another that preserves the non-perturbative impact of small-scale velocities by means of an effective damping function. The outputs of COMET can be obtained at arbitrary redshifts (up to $z \sim 3$), for arbitrary fiducial background cosmologies, and for a large parameter space that covers the shape parameters $\omega_c$, $\omega_b$, and $n_s$, as well as the evolution parameters $h$, $A_s$, $\Omega_K$, $w_0$, and $w_a$. This flexibility does not impair COMET's accuracy, since we exploit an exact degeneracy between the evolution parameters that allows us to train the emulator on a significantly reduced parameter space. While the predictions are sped up by at least two orders of magnitude, validation tests reveal an accuracy of $0.1\,\%$ for the monopole and quadrupole ($0.3\,\%$ for the hexadecapole), or alternatively, better than $0.25\,\sigma$ for all three multipoles in comparison to statistical uncertainties expected for the Euclid survey with a tenfold increase in volume. We show that these differences translate into shifts in mean posterior values that are at most of the same size, meaning that COMET can be used with the same confidence as the exact underlying models. COMET is a publicly available Python package that also provides the tree-level bispectrum multipoles in redshift-space and Gaussian covariance matrices.


(909)Origin of nontopological soliton dark matter: solitosynthesis or phase transition
  • Yang Bai,
  • Sida Lu,
  • Nicholas Orlofsky
arXiv e-prints (08/2022) e-Print:2208.12290
abstract + abstract -

This work demonstrates that nontopological solitons with large global charges and masses, even above the Planck scale, can form in the early universe and dominate the dark matter abundance. In solitosynthesis, solitons prefer to grow as large as possible under equilibrium dynamics when an initial global charge asymmetry is present. Their abundance is set by when soliton formation via particle fusion freezes out, and their charges are set by the time it takes to accumulate free particles. This work improves the estimation of both quantities, and in particular shows that much larger-charged solitons form than previously thought. The results are estimated analytically and validated numerically by solving the coupled Boltzmann equations. Without solitosynthesis, phase transitions can still form solitons from particles left inside false-vacuum pockets and determine their present-day abundance and properties. Even with zero charge asymmetry, solitons formed in this way can have very large charges on account of statistical fluctuations in the numbers of (anti)particles inside each pocket.


(908)KiDS-1000 Cosmology: Constraints from density split statistics
  • Pierre A. Burger,
  • Oliver Friedrich,
  • Joachim Harnois-Déraps,
  • Peter Schneider,
  • Marika Asgari
  • +10
  • Maciej Bilicki,
  • Hendrik Hildebrandt,
  • Angus H. Wright,
  • Tiago Castro,
  • Klaus Dolag,
  • Catherine Heymans,
  • Benjamin Joachimi,
  • Nicolas Martinet,
  • HuanYuan Shan,
  • Tilman Tröster
  • (less)
arXiv e-prints (08/2022) e-Print:2208.02171
abstract + abstract -

Context. Weak lensing and clustering statistics beyond two-point functions can capture non-Gaussian information about the matter density field, thereby improving the constraints on cosmological parameters relative to the mainstream methods based on correlation functions and power spectra. Aims. This paper presents a cosmological analysis of the fourth data release of the Kilo Degree Survey based on the density split statistics, which measures the mean shear profiles around regions classified according to foreground densities. The latter is constructed from a bright galaxy sample, which we further split into red and blue samples, allowing us to probe their respective connection to the underlying dark matter density. Methods. We use the state-of-the-art model of the density splitting statistics and validate its robustness against mock data infused with known systematic effects such as intrinsic galaxy alignment and baryonic feedback. Results. After marginalising over the photometric redshift uncertainty and the residual shear calibration bias, we measure for the full KiDS-bright sample a structure growth parameter of $S_8 = \sigma_8 \sqrt{\Omega_\mathrm{m}/0.3} = 0.74^{+0.03}_{-0.02}$ that is competitive to and consistent with two-point cosmic shear results, a matter density of $\Omega_\mathrm{m} = 0.28 \pm 0.02$, and a constant galaxy bias of $b = 1.32^{+0.12}_{-0.10}$.


(907)SN 2016dsg: A Thermonuclear Explosion Involving a Thick Helium Shell
  • Yize Dong,
  • Stefano Valenti,
  • Abigail Polin,
  • Aoife Boyle,
  • Andreas Flörs
  • +27
  • Christian Vogl,
  • Wolfgang E. Kerzendorf,
  • David J. Sand,
  • Saurabh W. Jha,
  • Łukasz Wyrzykowski,
  • K. Azalee Bostroem,
  • Jeniveve Pearson,
  • Curtis McCully,
  • Jennifer E. Andrews,
  • Stefano Benetti,
  • Stéphane Blondin,
  • L. Galbany,
  • Mariusz Gromadzki,
  • Griffin Hosseinzadeh,
  • D. Andrew Howell,
  • Cosimo Inserra,
  • Jacob E. Jencson,
  • Michael Lundquist,
  • J. D. Lyman,
  • Mark Magee,
  • Kate Maguire,
  • Nicolas Meza,
  • Shubham Srivastav,
  • Stefan Taubenberger,
  • J. H. Terwel,
  • Samuel Wyatt,
  • D. R. Young
  • (less)
The Astrophysical Journal, 934, p13 (08/2022) doi:10.3847/1538-4357/ac75eb
abstract + abstract -

A thermonuclear explosion triggered by a He-shell detonation on a carbon-oxygen white-dwarf core has been predicted to have strong UV line blanketing at early times due to the iron-group elements produced during He-shell burning. We present the photometric and spectroscopic observations of SN 2016dsg, a subluminous peculiar Type I supernova consistent with a thermonuclear explosion involving a thick He shell. With a redshift of 0.04, the i-band peak absolute magnitude is derived to be around -17.5. The object is located far away from its host, an early-type galaxy, suggesting it originated from an old stellar population. The spectra collected after the peak are unusually red, show strong UV line blanketing and weak O I λ7773 absorption lines, and do not evolve significantly over 30 days. An absorption line around 9700-10500 Å is detected in the near-infrared spectrum and is likely from the unburnt He in the ejecta. The spectroscopic evolution is consistent with the thermonuclear explosion models for a sub-Chandrasekhar-mass white dwarf with a thick He shell, while the photometric evolution is not well described by existing models.


(906)Insights on the origin of ORCs from cosmological simulations
  • Klaus Dolag,
  • Ludwig M. Böss,
  • Bärbel S. Koribalski,
  • Ulrich P. Steinwandel,
  • Milena Valentini
arXiv e-prints (08/2022) e-Print:2208.15003
abstract + abstract -

We investigate shock structures driven by merger events in high-resolution simulations that result in a galaxy with a virial mass M ~ 1e12 Msol. We find that the sizes and morphologies of the internal shocks resemble remarkably well those of the newly-detected class of odd radio circles (ORCs). This would highlight a so-far overlooked mechanism to form radio rings, shells and even more complex structures around elliptical galaxies. Mach numbers of M = 2-3 for such internal shocks are in agreement with the spectral indices of the observed ORCs. We estimate that ~5 percent of galaxies could undergo merger events which occasionally lead to such prominent structures within the galactic halo during their lifetime, explaining the low number of observed ORCs. At the time when the shock structures are matching the physical sizes of the observed ORCs, the central galaxies are typically classified as early-type galaxies, with no ongoing star formation, in agreement with observational findings. Although the energy released by such mergers could potentially power the observed radio luminosity already in Milky-Way-like halos, our predicted luminosity from a simple, direct shock acceleration model is much smaller than the observed one. Considering the estimated number of candidates from our cosmological simulations and the higher observed energies, we suggest that the proposed scenario is more likely for halo masses around 1e13 Msol in agreement with the observed stellar masses of the galaxies at the center of ORCs.


(905)Production of loosely-bound hadron molecules from bottomonium decays
  • Davide Marietti,
  • Alessandro Pilloni,
  • Umberto Tamponi
arXiv e-prints (08/2022) e-Print:2208.14185
abstract + abstract -

We present multiple results on the production of loosely-bound molecules in bottomonium annihilations and $e^+e^-$ collisions at $\sqrt{s} = 10.58$ GeV. We perform the first comprehensive test of several models for deuteron production against all the existing data in this energy region. We fit the free parameters of the models to reproduce the observed cross sections, and we predict the deuteron spectrum and production and the cross section for the $e^+e^- \to d\bar{d} + X$ process both at the $\Upsilon(1,2,3S)$ resonances and at $\sqrt{s}=10.58$ GeV. The predicted spectra show differences but are all compatible with the uncertainties of the existing data. These differences could be addressed if larger datasets are collected by the Belle~II experiment. Fixing the source size parameter to reproduce the deuteron data, we then predict the production rates for $H$ dibaryon and hypertriton in this energy region using a simple coalescence model. Our prediction on $H$ dibaryon production rate is below the limits set by the direct search at the Belle experiment, but in the range accessible to the Belle~II experiment. The systematic effect due to the MC modelling of quarks and gluon fragmentation into baryons is reduced deriving a new tuning of the \pythia MonteCarlo generator using the available measurement of single- and double-particle spectra in $\Upsilon$ decays.


(904)Euclid preparation. XXIV. Calibration of the halo mass function in $\Lambda(\nu)$CDM cosmologies
  • Euclid Collaboration,
  • T. Castro,
  • A. Fumagalli,
  • R. E. Angulo,
  • S. Bocquet
  • +174
  • S. Borgani,
  • C. Carbone,
  • J. Dakin,
  • K. Dolag,
  • C. Giocoli,
  • P. Monaco,
  • A. Ragagnin,
  • A. Saro,
  • E. Sefusatti,
  • M. Costanzi,
  • A. Amara,
  • L. Amendola,
  • M. Baldi,
  • R. Bender,
  • C. Bodendorf,
  • E. Branchini,
  • M. Brescia,
  • S. Camera,
  • V. Capobianco,
  • J. Carretero,
  • M. Castellano,
  • S. Cavuoti,
  • A. Cimatti,
  • R. Cledassou,
  • G. Congedo,
  • L. Conversi,
  • Y. Copin,
  • L. Corcione,
  • F. Courbin,
  • A. Da Silva,
  • H. Degaudenzi,
  • M. Douspis,
  • F. Dubath,
  • C. A. J. Duncan,
  • X. Dupac,
  • S. Farrens,
  • S. Ferriol,
  • P. Fosalba,
  • M. Frailis,
  • E. Franceschi,
  • S. Galeotta,
  • B. Garilli,
  • B. Gillis,
  • A. Grazian,
  • F. Gruppi,
  • S. V. H. Haugan,
  • F. Hormuth,
  • A. Hornstrup,
  • P. Hudelot,
  • K. Jahnke,
  • S. Kermiche,
  • T. Kitching,
  • M. Kunz,
  • H. Kurki-Suonio,
  • P. B. Lilje,
  • I. Lloro,
  • O. Mansutti,
  • O. Marggraf,
  • M. Meneghetti,
  • E. Merlin,
  • G. Meylan,
  • M. Moresco,
  • L. Moscardini,
  • E. Munari,
  • S. M. Niemi,
  • C. Padilla,
  • S. Paltani,
  • F. Pasian,
  • K. Pedersen,
  • V. Pettorino,
  • S. Pires,
  • G. Polenta,
  • M. Poncet,
  • L. Popa,
  • L. Pozzetti,
  • F. Raison,
  • R. Rebolo,
  • A. Renzi,
  • J. Rhodes,
  • G. Riccio,
  • E. Romelli,
  • R. Saglia,
  • D. Sapone,
  • B. Sartoris,
  • P. Schneider,
  • G. Seidel,
  • G. Sirri,
  • L. Stanco,
  • P. Tallada Crespí,
  • A. N. Taylor,
  • R. Toledo-Moreo,
  • F. Torradeflot,
  • I. Tutusaus,
  • E. A. Valentijn,
  • L. Valenziano,
  • T. Vassallo,
  • Y. Wang,
  • J. Weller,
  • A. Zacchei,
  • G. Zamorani,
  • S. Andreon,
  • S. Bardelli,
  • E. Bozzo,
  • C. Colodro-Conde,
  • D. Di Ferdinando,
  • M. Farina,
  • J. Graciá-Carpio,
  • V. Lindholm,
  • C. Neissner,
  • V. Scottez,
  • M. Tenti,
  • E. Zucca,
  • C. Baccigalupi,
  • A. Balaguera-Antolínez,
  • M. Ballardini,
  • F. Bernardeau,
  • A. Biviano,
  • A. Blanchard,
  • A. S. Borlaff,
  • C. Burigana,
  • R. Cabanac,
  • A. Cappi,
  • C. S. Carvalho,
  • S. Casas,
  • G. Castignani,
  • A. Cooray,
  • J. Coupon,
  • H. M. Courtois,
  • S. Davini,
  • G. De Lucia,
  • G. Desprez,
  • H. Dole,
  • J. A. Escartin,
  • S. Escoffier,
  • F. Finelli,
  • K. Ganga,
  • J. Garcia-Bellido,
  • K. George,
  • G. Gozaliasl,
  • H. Hildebrandt,
  • I. Hook,
  • S. Ilić,
  • V. Kansal,
  • E. Keihanen,
  • C. C. Kirkpatrick,
  • A. Loureiro,
  • J. Macias-Perez,
  • M. Magliocchetti,
  • R. Maoli,
  • S. Marcin,
  • M. Martinelli,
  • N. Martinet,
  • S. Matthew,
  • M. Maturi,
  • R. B. Metcalf,
  • G. Morgante,
  • S. Nadathur,
  • A. A. Nucita,
  • L. Patrizii,
  • A. Peel,
  • V. Popa,
  • C. Porciani,
  • D. Potter,
  • A. Pourtsidou,
  • M. Pöntinen,
  • A. G. Sánchez,
  • Z. Sakr,
  • M. Schirmer,
  • M. Sereno,
  • A. Spurio Mancini,
  • R. Teyssier,
  • J. Valiviita,
  • A. Veropalumbo,
  • M. Viel
  • (less)
arXiv e-prints (08/2022) e-Print:2208.02174
abstract + abstract -

Euclid's photometric galaxy cluster survey has the potential to be a very competitive cosmological probe. The main cosmological probe with observations of clusters is their number count, within which the halo mass function (HMF) is a key theoretical quantity. We present a new calibration of the analytic HMF, at the level of accuracy and precision required for the uncertainty in this quantity to be subdominant with respect to other sources of uncertainty in recovering cosmological parameters from Euclid cluster counts. Our model is calibrated against a suite of N-body simulations using a Bayesian approach taking into account systematic errors arising from numerical effects in the simulation. First, we test the convergence of HMF predictions from different N-body codes, by using initial conditions generated with different orders of Lagrangian Perturbation theory, and adopting different simulation box sizes and mass resolution. Then, we quantify the effect of using different halo-finder algorithms, and how the resulting differences propagate to the cosmological constraints. In order to trace the violation of universality in the HMF, we also analyse simulations based on initial conditions characterised by scale-free power spectra with different spectral indexes, assuming both Einstein--de Sitter and standard $\Lambda$CDM expansion histories. Based on these results, we construct a fitting function for the HMF that we demonstrate to be sub-percent accurate in reproducing results from 9 different variants of the $\Lambda$CDM model including massive neutrinos cosmologies. The calibration systematic uncertainty is largely sub-dominant with respect to the expected precision of future mass-observation relations; with the only notable exception of the effect due to the halo finder, that could lead to biased cosmological inference.


(903)Cosmological simulations with rare and frequent dark matter self-interactions
  • Moritz S. Fischer,
  • Marcus Brüggen,
  • Kai Schmidt-Hoberg,
  • Klaus Dolag,
  • Felix Kahlhoefer
  • +2
  • Antonio Ragagnin,
  • Andrew Robertson
  • (less)
Monthly Notices of the Royal Astronomical Society (08/2022) doi:10.1093/mnras/stac2207
abstract + abstract -

Dark matter (DM) with self-interactions is a promising solution for the small-scale problems of the standard cosmological model. Here we perform the first cosmological simulation of frequent DM self-interactions, corresponding to small-angle DM scatterings. The focus of our analysis lies in finding and understanding differences to the traditionally assumed rare DM (large-angle) self scatterings. For this purpose, we compute the distribution of DM densities, the matter power spectrum, the two-point correlation function and the halo and subhalo mass functions. Furthermore, we investigate the density profiles of the DM haloes and their shapes. We find that overall large-angle and small-angle scatterings behave fairly similarly with a few exceptions. In particular, the number of satellites is considerably suppressed for frequent compared to rare self-interactions with the same cross-section. Overall we observe that while differences between the two cases may be difficult to establish using a single measure, the degeneracy may be broken through a combination of multiple ones. For instance, the combination of satellite counts with halo density or shape profiles could allow discriminating between rare and frequent self-interactions. As a by-product of our analysis, we provide - for the first time - upper limits on the cross-section for frequent self-interactions.


(902)DustPy: A Python Package for Dust Evolution in Protoplanetary Disks
  • Sebastian M. Stammler,
  • Tilman Birnstiel
The Astrophysical Journal, 935, p16 (08/2022) doi:10.3847/1538-4357/ac7d58
abstract + abstract -

Many processes during the evolution of protoplanetary disks and during planet formation are highly sensitive to the sizes of dust particles that are present in the disk: the efficiency of dust accretion in the disk and volatile transport on dust particles, gravoturbulent instabilities leading to the formation of planetesimals, or the accretion of pebbles onto large planetary embryos to form giant planets are typical examples of processes that depend on the sizes of the dust particles involved. Furthermore, radiative properties like absorption or scattering opacities depend on the particle sizes. To interpret observations of dust in protoplanetary disks, a proper estimate of the dust particle sizes is needed. We present DustPy: a Python package to simulate dust evolution in protoplanetary disks. DustPy solves gas and dust transport including viscous advection and diffusion as well as collisional growth of dust particles. DustPy is written with a modular concept, such that every aspect of the model can be easily modified or extended to allow for a multitude of research opportunities.


(901)TOI-1468: A system of two transiting planets, a super-Earth and a mini-Neptune, on opposite sides of the radius valley
  • P. Chaturvedi,
  • P. Bluhm,
  • E. Nagel,
  • A. P. Hatzes,
  • G. Morello
  • +65
  • M. Brady,
  • J. Korth,
  • K. Molaverdikhani,
  • D. Kossakowski,
  • J. A. Caballero,
  • E. W. Guenther,
  • E. Pallé,
  • N. Espinoza,
  • A. Seifahrt,
  • N. Lodieu,
  • C. Cifuentes,
  • E. Furlan,
  • P. J. Amado,
  • T. Barclay,
  • J. Bean,
  • V. J. S. Béjar,
  • G. Bergond,
  • A. W. Boyle,
  • D. Ciardi,
  • K. A. Collins,
  • K. I. Collins,
  • E. Esparza-Borges,
  • A. Fukui,
  • C. L. Gnilka,
  • R. Goeke,
  • P. Guerra,
  • Th. Henning,
  • E. Herrero,
  • S. B. Howell,
  • S. V. Jeffers,
  • J. M. Jenkins,
  • E. L. N. Jensen,
  • D. Kasper,
  • T. Kodama,
  • D. W. Latham,
  • M. J. López-González,
  • R. Luque,
  • D. Montes,
  • J. C. Morales,
  • M. Mori,
  • F. Murgas,
  • N. Narita,
  • G. Nowak,
  • H. Parviainen,
  • V. M. Passegger,
  • A. Quirrenbach,
  • S. Reffert,
  • A. Reiners,
  • I. Ribas,
  • G. R. Ricker,
  • E. Rodríguez,
  • C. Rodríguez-López,
  • M. Schlecker,
  • R. P. Schwarz,
  • A. Schweitzer,
  • S. Seager,
  • G. Stefánsson,
  • C. Stockdale,
  • L. Tal-Or,
  • J. D. Twicken,
  • S. Vanaverbeke,
  • G. Wang,
  • D. Watanabe,
  • J. N. Winn,
  • M. Zechmeister
  • (less)
arXiv e-prints (08/2022) e-Print:2208.10351
abstract + abstract -

We report the discovery and characterization of two small transiting planets orbiting the bright M3.0V star TOI-1468 (LSPM J0106+1913), whose transit signals were detected in the photometric time series in three sectors of the TESS mission. We confirm the e planetary nature of both of them using precise radial velocity measurements from the CARMENES and MAROON-X spectrographs, and supplement them with ground-based transit photometry. A joint analysis of all these data reveals that the shorter-period planet, TOI-1468 b ($P_{\rm b}$ = 1.88 d), has a planetary mass of $M_{\rm b} = 3.21\pm0.24$ $M_{\oplus}$ and a radius of $R_{\rm b} =1.280^{+0.038}_{-0.039} R_{\oplus}$, resulting in a density of $\rho_{\rm b} = 8.39^{+ 1.05}_{- 0.92}$ g cm$^{-3}$, which is consistent with a mostly rocky composition. For the outer planet, TOI-1468 c ($P_{\rm c} = 15.53$ d), we derive a mass of $M_{\rm c} = 6.64^{+ 0.67}_{- 0.68}$ $M_{\oplus}$, a radius of $R_{\rm c} = 2.06\pm0.04\,R_{\oplus}$, and a bulk density of $\rho_{c} = 2.00^{+ 0.21}_{- 0.19}$ g cm$^{-3}$, which corresponds to a rocky core composition with a H/He gas envelope. These planets are located on opposite sides of the radius valley, making our system an interesting discovery as there are only a handful of other systems with the same properties. This discovery can further help determine a more precise location of the radius valley for small planets around M dwarfs and, therefore, shed more light on planet formation and evolution scenarios.


(900)A Stream Come True -- Connecting tidal tails, shells, streams, and planes with galaxy kinematics and formation history
  • Lucas M. Valenzuela,
  • Rhea-Silvia Remus
arXiv e-prints (08/2022) e-Print:2208.08443
abstract + abstract -

Context. The rapidly improving quality and resolution of both low surface brightness observations and cosmological simulations of galaxies enables an increasingly thorough investigation of the imprints of the formation history in the outer, unrelaxed regions of galaxies, and a direct comparison to another tracer of galaxy formation, the internal kinematics. Aims. Using the state-of-the-art hydrodynamical cosmological simulation Magneticum Pathfinder, we identify tidal tails, shells, streams, and satellite planes, and connect their existence to the amount of rotational support and the formation histories of the host galaxies. Methods. Tidal features are visually classified from a three-dimensional rendering of the simulated galaxies by several scientists independently. Only features that were identified by at least half of the participating individuals are considered as existing features. The results are compared to observations of the MATLAS survey. Results. Shells are preferentially found around kinematically slowly rotating galaxies in both simulations and observations, while streams can be found around all kind of galaxies with a slightly higher probability to be present around less rotationally supported galaxies. Tails and satellite planes, however, appear independently of the internal kinematics of the central galaxy, indicating that they are formed through processes that have not (yet) affected the internal kinematics. Conclusions. As shells are formed through radial merger events while streams are remnants of circular merger infall, this suggests that the orbital angular momentum of the merger event could play a more crucial role in transforming the host galaxy than previously anticipated. The existence of a shell around a given slow rotator can further be used to distinguish the radial merger formation scenario from other formation pathways of slow rotators.


(899)Recent advances in charm mixing and CP violation at LHCb
  • Tommaso Pajero
Modern Physics Letters A, 37 (08/2022) doi:10.1142/S0217732322300129
abstract + abstract -

After playing a pivotal role in the birth of the Standard Model in the 70s, the study of charm physics has undergone a revival during the last decade, triggered by a wealth of precision measurements from the charm and B factories, and from the CDF and especially the LHCb experiments. In this paper, we sum up how the unique phenomenology of charmed hadrons can be used to test the Standard Model and we review the latest measurements performed in this field by the LHCb experiment. These include the historic first observations of CP violation and of a nonzero mass difference between the charmed neutral-meson mass eigenstates, the most precise determination of their decay-width difference to date, and a search for time-dependent CP violation reaching the unprecedented precision of 10−4. These results challenge our comprehension of nonperturbative strong interactions, and their interpretation calls for further studies on both the theoretical and experimental sides. The upcoming upgrades of the LHCb experiment will play a leading role in this quest.


(898)Cosmological simulations predict that AGN preferentially live in gas-rich, star-forming galaxies despite effective feedback
  • S. R. Ward,
  • C. M. Harrison,
  • T. Costa,
  • V. Mainieri
Monthly Notices of the Royal Astronomical Society, 514, p22 (08/2022) doi:10.1093/mnras/stac1219
abstract + abstract -

Negative feedback from active galactic nuclei (AGN) is the leading mechanism for the quenching of massive galaxies in the vast majority of modern galaxy evolution models. However, direct observational evidence that AGN feedback causes quenching on a population scale is lacking. Studies have shown that luminous AGN are preferentially located in gas-rich and star-forming galaxies, an observation that has sometimes been suggested to be in tension with a negative AGN feedback picture. We investigate three of the current cosmological simulations (IllustrisTNG, EAGLE, and SIMBA) along with post-processed models for molecular hydrogen gas masses and perform similar tests to those used by observers. We find that the simulations predict: (i) no strong negative trends between Lbol and $f_{\mathrm{ H}_2}$ or specific star formation rate (sSFR); (ii) both high-luminosity ($L_{\rm {bol}} \ge 10^{44}\rm {\, erg\, s^{-1}}$) and high Eddington ratio (λEdd $\ge 1{{\ \rm per\ cent}}$) AGN are preferentially located in galaxies with high molecular gas fractions and sSFR; and (iii) that the gas-depleted and quenched fractions of AGN host galaxies are lower than a control sample of non-active galaxies. These three findings are in qualitative agreement with observational samples at z = 0 and z = 2 and show that such results are not in tension with the presence of strong AGN feedback, which all simulations we employ require to produce realistic massive galaxies. However, we also find quantifiable differences between predictions from the simulations, which could allow us to observationally test the different subgrid feedback models.


(897)Superresolution trends in the ALMA Taurus survey: structured inner discs and compact discs
  • Jeff Jennings,
  • Marco Tazzari,
  • Cathie J. Clarke,
  • Richard A. Booth,
  • Giovanni P. Rosotti
Monthly Notices of the Royal Astronomical Society, 514, p21 (08/2022) doi:10.1093/mnras/stac1770
abstract + abstract -

The 1.33-mm survey of protoplanetary discs in the Taurus molecular cloud found annular gaps and rings to be common in extended sources (≳ 55AU), when their 1D visibility distributions were fit parametrically. We first demonstrate the advantages and limitations of non-parametric visibility fits for data at the survey's 0.12-arcsec resolution. Then we use the non-parametric model in Frankenstein (frank) to identify new substructure in three compact and seven extended sources. Among the new features, we identify three trends: a higher occurrence rate of substructure in the survey's compact discs than previously seen, underresolved (potentially azimuthally asymmetric) substructure in the innermost disc of extended sources, and a 'shoulder' on the trailing edge of a ring in discs with strong depletion at small radii. Noting the shoulder morphology is present in multiple discs observed at higher resolution, we postulate it is tracing a common physical mechanism. We further demonstrate how a superresolution frank brightness profile is useful in motivating an accurate parametric model, using the highly structured source DL Tau in which frank finds two new rings. Finally, we show that sparse (u, v) plane sampling may be masking the presence of substructure in several additional compact survey sources.


(896)Primordial Lepton Asymmetries in the Precision Cosmology Era: Current Status and Future Sensitivities from BBN and the CMB
  • Miguel Escudero,
  • Alejandro Ibarra,
  • Victor Maura
arXiv e-prints (08/2022) e-Print:2208.03201
abstract + abstract -

Using a new sample of extremely metal poor systems, the EMPRESS survey has recently reported a primordial helium abundance that is $3\sigma$ smaller than the prediction from the Standard BBN scenario. This measurement could be interpreted as a hint for a primordial lepton asymmetry in the electron neutrino flavor. Motivated by the EMPRESS results, we present a comprehensive analysis of the lepton asymmetry using measurements of the abundances of primordial elements, along with CMB data from Planck. Assuming that there is no dark radiation in our Universe, we find an electron neutrino chemical potential $\xi_{\nu_e} = 0.037 \pm 0.013$, which deviates from zero by $2.8\sigma$. If no assumption is made on the abundance of dark radiation in the Universe, the chemical potential is $\xi_{\nu_e} = 0.037 \pm 0.020$, which deviates from zero by $1.9\sigma$. We also find that this result is rather insensitive to the choice of nuclear reaction rates. If the true helium abundance corresponds to the EMPRESS central value, future CMB observations from the Simons Observatory and CMB-S4 will increase the significance for a non-zero lepton asymmetry to $4\sigma$ and $5\sigma$ respectively, assuming no dark radiation, or to $3\sigma$ when no assumption is made on the abundance of dark radiation.


(895)Insights on the origin of ORCs from cosmological simulations
  • Klaus Dolag,
  • Ludwig M. Böss,
  • Bärbel S. Koribalski,
  • Ulrich P. Steinwandel,
  • Milena Valentini
(08/2022) e-Print:2208.15003
abstract + abstract -

We investigate shock structures driven by merger events in high-resolution simulations that result in a galaxy with a virial mass M ~ 1e12 Msol. We find that the sizes and morphologies of the internal shocks resemble remarkably well those of the newly-detected class of odd radio circles (ORCs). This would highlight a so-far overlooked mechanism to form radio rings, shells and even more complex structures around elliptical galaxies. Mach numbers of M = 2-3 for such internal shocks are in agreement with the spectral indices of the observed ORCs. We estimate that ~5 percent of galaxies could undergo merger events which occasionally lead to such prominent structures within the galactic halo during their lifetime, explaining the low number of observed ORCs. At the time when the shock structures are matching the physical sizes of the observed ORCs, the central galaxies are typically classified as early-type galaxies, with no ongoing star formation, in agreement with observational findings. Although the energy released by such mergers could potentially power the observed radio luminosity already in Milky-Way-like halos, our predicted luminosity from a simple, direct shock acceleration model is much smaller than the observed one. Considering the estimated number of candidates from our cosmological simulations and the higher observed energies, we suggest that the proposed scenario is more likely for halo masses around 1e13 Msol in agreement with the observed stellar masses of the galaxies at the center of ORCs.


(894)Extending empirical constraints on the SZ-mass scaling relation to higher redshifts via HST weak lensing measurements of nine clusters from the SPT-SZ survey at $z\gtrsim1$
  • Hannah Zohren,
  • Tim Schrabback,
  • Sebastian Bocquet,
  • Martin Sommer,
  • Fatimah Raihan
  • +15
  • Beatriz Hernández-Martín,
  • Ole Marggraf,
  • Behzad Ansarinejad,
  • Matthew B. Bayliss,
  • Lindsey E. Bleem,
  • Thomas Erben,
  • Henk Hoekstra,
  • Benjamin Floyd,
  • Michael D. Gladders,
  • Florian Kleinebreil,
  • Michael A. McDonald,
  • Mischa Schirmer,
  • Diana Scognamiglio,
  • Keren Sharon,
  • Angus H. Wright
  • (less)
(08/2022) e-Print:2208.10232
abstract + abstract -

We present a Hubble Space Telescope (HST) weak gravitational lensing study of nine distant and massive galaxy clusters with redshifts $1.0 \lesssim z \lesssim 1.7$ ($z_\mathrm{median} = 1.4$) and Sunyaev Zel'dovich (SZ) detection significance $\xi > 6.0$ from the South Pole Telescope Sunyaev Zel'dovich (SPT-SZ) survey. We measured weak lensing galaxy shapes in HST/ACS F606W and F814W images and used additional observations from HST/WFC3 in F110W and VLT/FORS2 in $U_\mathrm{HIGH}$ to preferentially select background galaxies at $z\gtrsim 1.8$, achieving a high purity. We combined recent redshift estimates from the CANDELS/3D-HST and HUDF fields to infer an improved estimate of the source redshift distribution. We measured weak lensing masses by fitting the tangential reduced shear profiles with spherical Navarro-Frenk-White (NFW) models. We obtained the largest lensing mass in our sample for the cluster SPT-CLJ2040$-$4451, thereby confirming earlier results that suggest a high lensing mass of this cluster compared to X-ray and SZ mass measurements. Combining our weak lensing mass constraints with results obtained by previous studies for lower redshift clusters, we extended the calibration of the scaling relation between the unbiased SZ detection significance $\zeta$ and the cluster mass for the SPT-SZ survey out to higher redshifts. We found that the mass scale inferred from our highest redshift bin ($1.2 < z < 1.7$) is consistent with an extrapolation of constraints derived from lower redshifts, albeit with large statistical uncertainties. Thus, our results show a similar tendency as found in previous studies, where the cluster mass scale derived from the weak lensing data is lower than the mass scale expected in a Planck $\nu\Lambda$CDM (i.e. $\nu$$\Lambda$ Cold Dark Matter) cosmology given the SPT-SZ cluster number counts.


(893)The DESI Survey Validation: Results from Visual Inspection of the Quasar Survey Spectra
  • David M. Alexander,
  • Tamara M. Davis,
  • E. Chaussidon,
  • V.A. Fawcett,
  • Alma X. Gonzalez-Morales
  • +67
  • Ting-Wen Lan,
  • Christophe Yeche,
  • S. Ahlen,
  • J.N. Aguilar,
  • E. Armengaud,
  • S. Bailey,
  • D. Brooks,
  • Z. Cai,
  • R. Canning,
  • A. Carr,
  • S. Chabanier,
  • Marie-Claude Cousinou,
  • K. Dawson,
  • A. de la Macorra,
  • A. Dey,
  • Biprateep Dey,
  • G. Dhungana,
  • A.C. Edge,
  • S. Eftekharzadeh,
  • K. Fanning,
  • James Farr,
  • A. Font-Ribera,
  • J. Garcia-Bellido,
  • Lehman Garrison,
  • E. Gaztanaga,
  • Satya Gontcho A. Gontcho,
  • C. Gordon,
  • Stefany Guadalupe Medellin Gonzalez,
  • J. Guy,
  • Hiram K. Herrera-Alcantar,
  • L. Jiang,
  • S. Juneau,
  • Naim Karacayli,
  • R. Kehoe,
  • T. Kisner,
  • A. Kovacs,
  • M. Landriau,
  • Michael E. Levi,
  • C. Magneville,
  • P. Martini,
  • Aaron M. Meisner,
  • M. Mezcua,
  • R. Miquel,
  • P. Montero Camacho,
  • J. Moustakas,
  • Andrea Munoz-Gutierrez,
  • Adam D. Myers,
  • S. Nadathur,
  • L. Napolitano,
  • J.D. Nie,
  • N. Palanque-Delabrouille,
  • Z. Pan,
  • W.J. Percival,
  • I. Perez-Rafols,
  • C. Poppett,
  • F. Prada,
  • Cesar Ramirez-Perez,
  • C. Ravoux,
  • D.J. Rosario,
  • M. Schubnell,
  • Gregory Tarle,
  • M. Walther,
  • B. Weiner,
  • S. Youles,
  • Zhimin Zhou,
  • H. Zou,
  • Siwei Zou
  • (less)
(08/2022) e-Print:2208.08517
abstract + abstract -

A key component of the Dark Energy Spectroscopic Instrument (DESI) survey validation (SV) is a detailed visual inspection (VI) of the optical spectroscopic data to quantify key survey metrics. In this paper we present results from VI of the quasar survey using deep coadded SV spectra. We show that the majority (~70%) of the main-survey targets are spectroscopically confirmed as quasars, with ~16% galaxies, ~6% stars, and ~8% low-quality spectra lacking reliable features. A non-negligible fraction of the quasars are misidentified by the standard DESI spectroscopic pipeline but we show that the majority can be recovered using post-pipeline "afterburner" quasar-identification approaches. We combine these "afterburners" with our standard pipeline to create a modified pipeline to improve the overall quasar completeness. At the depth of the main DESI survey both pipelines achieve a good-redshift purity (reliable redshifts measured within 3000 km/s) of ~99%; however, the modified pipeline recovers ~94% of the visually inspected quasars, as compared to just ~86% from the standard pipeline. We demonstrate that both pipelines achieve an overall redshift precision and accuracy of ~100 km/s and ~70 km/s, respectively. We constructed composite spectra to investigate why some quasars are missed by the standard spectroscopic pipeline and find that they are more host-galaxy dominated and/or dust reddened than the standard-pipeline quasars. We also show example spectra to demonstrate the overall diversity of the DESI quasar sample and provide strong-lensing candidates where two targets contribute to a single DESI spectrum.


(892)Virgo: Scalable Unsupervised Classification of Cosmological Shock Waves
  • Max Lamparth,
  • Ludwig Böss,
  • Ulrich Steinwandel,
  • Klaus Dolag
(08/2022) e-Print:2208.06859
abstract + abstract -

Cosmological shock waves are essential to understanding the formation of cosmological structures. To study them, scientists run computationally expensive high-resolution 3D hydrodynamic simulations. Interpreting the simulation results is challenging because the resulting data sets are enormous, and the shock wave surfaces are hard to separate and classify due to their complex morphologies and multiple shock fronts intersecting. We introduce a novel pipeline, Virgo, combining physical motivation, scalability, and probabilistic robustness to tackle this unsolved unsupervised classification problem. To this end, we employ kernel principal component analysis with low-rank matrix approximations to denoise data sets of shocked particles and create labeled subsets. We perform supervised classification to recover full data resolution with stochastic variational deep kernel learning. We evaluate on three state-of-the-art data sets with varying complexity and achieve good results. The proposed pipeline runs automatically, has only a few hyperparameters, and performs well on all tested data sets. Our results are promising for large-scale applications, and we highlight now enabled future scientific work.


(891)Analytical evaluation of cosmological correlation functions
  • Till Heckelbacher,
  • Ivo Sachs,
  • Evgeny Skvortsov,
  • Pierre Vanhove
Journal of High Energy Physics, 2022 (08/2022) doi:10.1007/JHEP08(2022)139
abstract + abstract -

Using the Schwinger-Keldysh-formalism, reformulated in [1] as an effective field theory in Euclidean anti-de Sitter, we evaluate the one-loop cosmological four-point function of a conformally coupled interacting scalar field in de Sitter. Recasting the Witten cosmological correlator as flat space Feynman integrals, we evaluate the one-loop cosmological four-point functions in de Sitter space in terms of single-valued multiple polylogarithms. From it we derive anomalous dimensions and OPE coefficients of the dual conformal field theory at space-like, future infinity. In particular, we find an interesting degeneracy in the anomalous dimensions relating operators of neighboring spins.


(890)The HD 260655 system: Two rocky worlds transiting a bright M dwarf at 10 pc
  • R. Luque,
  • B. J. Fulton,
  • M. Kunimoto,
  • P. J. Amado,
  • P. Gorrini
  • +62
  • S. Dreizler,
  • C. Hellier,
  • G. W. Henry,
  • K. Molaverdikhani,
  • G. Morello,
  • L. Peña-Moñino,
  • M. Pérez-Torres,
  • F. J. Pozuelos,
  • Y. Shan,
  • G. Anglada-Escudé,
  • V. J. S. Béjar,
  • G. Bergond,
  • A. W. Boyle,
  • J. A. Caballero,
  • D. Charbonneau,
  • D. R. Ciardi,
  • S. Dufoer,
  • N. Espinoza,
  • M. Everett,
  • D. Fischer,
  • A. P. Hatzes,
  • Th. Henning,
  • K. Hesse,
  • A. W. Howard,
  • S. B. Howell,
  • H. Isaacson,
  • S. V. Jeffers,
  • J. M. Jenkins,
  • S. R. Kane,
  • J. Kemmer,
  • S. Khalafinejad,
  • R. C. Kidwell,
  • D. Kossakowski,
  • D. W. Latham,
  • J. Lillo-Box,
  • J. J. Lissauer,
  • D. Montes,
  • J. Orell-Miquel,
  • E. Pallé,
  • D. Pollacco,
  • A. Quirrenbach,
  • S. Reffert,
  • A. Reiners,
  • I. Ribas,
  • G. R. Ricker,
  • L. A. Rogers,
  • J. Sanz-Forcada,
  • M. Schlecker,
  • A. Schweitzer,
  • S. Seager,
  • A. Shporer,
  • K. G. Stassun,
  • S. Stock,
  • L. Tal-Or,
  • E. B. Ting,
  • T. Trifonov,
  • S. Vanaverbeke,
  • R. Vanderspek,
  • J. Villaseñor,
  • J. N. Winn,
  • J. G. Winters,
  • M. R. Zapatero Osorio
  • (less)
Astronomy and Astrophysics, 664, p23 (08/2022) doi:10.1051/0004-6361/202243834
abstract + abstract -

We report the discovery of a multiplanetary system transiting the M0 V dwarf HD 260655 (GJ 239, TOI-4599). The system consists of at least two transiting planets, namely HD 260655 b, with a period of 2.77 d, a radius of Rb = 1.240 ± 0.023 R, a mass of Mb = 2.14 ± 0.34 M, and a bulk density of ρb = 6.2 ± 1.0 g cm−3, and HD 260655 c, with a period of 5.71 d, a radius of {R_c} = 1.533 - 0.046 + 0.051{R_ \oplus }, a mass of Mc = 3.09 ± 0.48 M, and a bulk density of {ρ _c} = 4.7 - 0.8 + 0.9{{g}} g cm−3. The planets have been detected in transit by the Transiting Exoplanet Survey Satellite (TESS) mission and confirmed independently with archival and new precise radial velocities obtained with the HIRES and CARMENES instruments since 1998 and 2016, respectively. At a distance of 10 pc, HD 260655 has become the fourth closest known multitransiting planet system after HD 219134, LTT 1445 A, and AU Mic. Due to the apparent brightness of the host star (J = 6.7 mag), both planets are among the most suitable rocky worlds known today for atmospheric studies with the James Webb Space Telescope, both in transmission and emission.


(889)Asymmetric nuclear matter and neutron star properties in relativistic ab initio theory in the full Dirac space
  • Sibo Wang,
  • Hui Tong,
  • Qiang Zhao,
  • Chencan Wang,
  • Peter Ring
  • +1
Physical Review C, 106 (08/2022) doi:10.1103/PhysRevC.106.L021305
abstract + abstract -

The long-standing controversy about the isospin dependence of the effective Dirac mass in ab initio calculations of asymmetric nuclear matter is clarified by solving the relativistic Brueckner-Hartree-Fock equations in the full Dirac space. The symmetry energy and its slope parameter at the saturation density are Esym0) =33.1 MeV and L =65.2 MeV, in agreement with empirical and experimental values. Further applications predict the neutron star radius R1.4 M ⊙≈12 km and the maximum mass of a neutron star Mmax≤2.4 M .


(888)Bridging scales in a multiscale pattern-forming system
  • Laeschkir Würthner,
  • Fridtjof Brauns,
  • Grzegorz Pawlik,
  • Jacob Halatek,
  • Jacob Kerssemakers
  • +2
Proceedings of the National Academy of Science, 119 (08/2022) doi:10.1073/pnas.2206888119
abstract + abstract -

Biological processes operate in a spatially and temporally ordered manner to reliably fulfill their function. This is achieved by pattern formation, which generally involves many different spatial and temporal scales. The resulting multiscale patterns exhibit complex dynamics for which it is difficult to find a simplified description at large scales while preserving information about the patterns at small scales. Here, we introduce an approach for mass-conserving reaction-diffusion systems that is based on a linear theory and therefore conceptually simple to apply. We investigate multiscale patterns of the Min protein system and show that our approach enables us to explain and predict the intricate dynamics from the large-scale mass redistribution of the total protein densities.


(887)Heavy quarkonium dynamics at next-to-leading order in the binding energy over temperature
  • Nora Brambilla,
  • Miguel Ángel Escobedo,
  • Ajaharul Islam,
  • Michael Strickland,
  • Anurag Tiwari
  • +2
  • Antonio Vairo,
  • Peter Vander Griend
  • (less)
Journal of High Energy Physics, 2022 (08/2022) doi:10.1007/JHEP08(2022)303
abstract + abstract -

Using the potential non-relativistic quantum chromodynamics (pNRQCD) effective field theory, we derive a Lindblad equation for the evolution of the heavy-quarkonium reduced density matrix that is accurate to next-to-leading order (NLO) in the ratio of the binding energy of the state to the temperature of the medium. The resulting NLO Lindblad equation can be used to more reliably describe heavy-quarkonium evolution in the quark-gluon plasma at low temperatures compared to the leading-order truncation. For phenomenological application, we numerically solve the resulting NLO Lindblad equation using the quantum trajectories algorithm. To achieve this, we map the solution of the three-dimensional Lindblad equation to the solution of an ensemble of one-dimensional Schrödinger evolutions with Monte-Carlo sampled quantum jumps. Averaging over the Monte-Carlo sampled quantum jumps, we obtain the solution to the NLO Lindblad equation without truncation in the angular momentum quantum number of the states considered. We also consider the evolution of the system using only the complex effective Hamiltonian without stochastic jumps and find that this provides a reliable approximation for the ground state survival probability at LO and NLO. Finally, we make comparisons with our prior leading-order pNRQCD results and experimental data available from the ATLAS, ALICE, and CMS collaborations.


(886)On the time evolution of the M<SUB>d</SUB>-M<SUB>⋆</SUB> and Ṁ-M<SUB>⋆</SUB> correlations for protoplanetary discs: the viscous time-scale increases with stellar mass
  • Alice Somigliana,
  • Claudia Toci,
  • Giovanni Rosotti,
  • Giuseppe Lodato,
  • Marco Tazzari
  • +3
  • Carlo F. Manara,
  • Leonardo Testi,
  • Federico Lepri
  • (less)
Monthly Notices of the Royal Astronomical Society, 514, p14 (08/2022) doi:10.1093/mnras/stac1587
abstract + abstract -

Large surveys of star-forming regions have unveiled power-law correlations between the stellar mass and the disc parameters, such as the disc mass $M_{\mathrm{d}} \!-\! {M_{\star }}$ and the accretion rate $\dot{M} \!-\! {M_{\star }}$. The observed slopes appear to be increasing with time, but the reason behind the establishment of these correlations and their subsequent evolution is still uncertain. We conduct a theoretical analysis of the impact of viscous evolution on power-law initial conditions for a population of protoplanetary discs. We find that, for evolved populations, viscous evolution enforces the two correlations to have the same slope, λm = λacc, and that this limit is uniquely determined by the initial slopes λm, 0 and λacc, 0. We recover the increasing trend claimed from the observations when the difference in the initial values, δ0 = λm, 0acc, 0, is larger than 1/2; moreover, we find that this increasing trend is a consequence of a positive correlation between the viscous time-scale and the stellar mass. We also present the results of disc population synthesis numerical simulations, that allow us to introduce a spread and analyse the effect of sampling, which show a good agreement with our analytical predictions. Finally, we perform a preliminary comparison of our numerical results with observational data, which allows us to constrain the parameter space of the initial conditions to λm, 0 ∈ [1.2, 2.1], λacc, 0 ∈ [0.7, 1.5].


(885)Accreted or Not Accreted? The Fraction of Accreted Mass in Galaxies from the Magneticum Simulations and Observations
  • Rhea-Silvia Remus,
  • Duncan A. Forbes
The Astrophysical Journal, 935, p23 (08/2022) doi:10.3847/1538-4357/ac7b30
abstract + abstract -

In the two-phase scenario of galaxy formation, a galaxy's stellar mass growth is first dominated by in-situ star formation, and subsequently by accretion. We analyze the radial distribution of the accreted stellar mass in ~500 galaxies from the (48 Mpc/h)3 box volume of the hydrodynamical cosmological simulation Magneticum, in a stellar-mass range of 1010 to 1012 M . We find that higher-mass galaxies have larger accreted fractions, as found in previous works, but predict generally higher accretion fractions for low-mass galaxies. Based on the 3D radial distribution of the accreted and in-situ components, we define six galaxy classes, from completely accretion to completely in-situ dominated, and measure the transition radii between in-situ and accretion-dominated regions for galaxies that reveal a transition. About 70% of our galaxies have one transition radius. However, about 10% of the galaxies are accretion dominated everywhere, and about 13% have two transition radii, with the center and the outskirts both being accretion dominated. We show that these classes are strongly correlated with the galaxy merger histories, especially with the cold gas fraction at the time of merging. We find high total in-situ (low accretion) fractions to be associated with smaller, lower-mass galaxies, lower central dark-matter fractions, and larger transition radii. Finally, we show that the dips in observed surface brightness profiles seen in many early-type galaxies do not correspond to the transition from in-situ to accretion-dominated regions, and that any inferred mass fractions are not indicative of the true accreted mass but contain information about the galaxies' dry-merger history.


(884)Importance of electron-positron pairs on the maximum possible luminosity of the accretion columns in ULXs
  • V. Suleimanov,
  • A. Mushtukov,
  • I. Ognev,
  • V. Doroshenko,
  • K. Werner
arXiv e-prints (08/2022) e-Print:2208.14237
abstract + abstract -

One of the models explaining the high luminosity of pulsing ultra-luminous X-ray sources (pULXs) was suggested by Mushtukov et al. (2015). They showed that the accretion columns on the surfaces of highly magnetized neutron stars can be very luminous due to opacity reduction in the high magnetic field. However, a strong magnetic field leads also to amplification of the electron-positron pairs creation. Therefore, increasing of the electron and positron number densities compensates the cross-section reduction, and the electron scattering opacity does not decrease with the magnetic field magnification. As a result, the maximum possible luminosity of the accretion column does not increase with the magnetic field. It ranges between 10$^{40} - 10^{41}$ erg s$^{-1}$ depending only slightly on the magnetic field strength.


(883)Spectroscopic analysis of VVV CL001 cluster with MUSE
  • J. Olivares Carvajal,
  • M. Zoccali,
  • A. Rojas-Arriagada,
  • R. Contreras Ramos,
  • F. Gran
  • +2
Monthly Notices of the Royal Astronomical Society, 513, p11 (07/2022) doi:10.1093/mnras/stac934
abstract + abstract -

Like most spiral galaxies, the Milky Way contains a population of blue, metal-poor globular clusters and another of red, metal-rich ones. Most of the latter belong to the bulge, and therefore they are poorly studied compared to the blue (halo) ones because they suffer higher extinction and larger contamination from field stars. These intrinsic difficulties, together with a lack of low-mass bulge globular clusters, are reasons to believe that their census is not complete yet. Indeed, a few new clusters have been confirmed in the last few years. One of them is VVV CL001, the subject of the present study. We present a new spectroscopic analysis of the recently confirmed globular cluster VVV CL001, made by means of MUSE@VLT integral field data. Individual spectra were extracted for stars in the VVV CL001 field. Radial velocities were derived by cross-correlation with synthetic templates. Coupled with proper motions from the VVV (VISTA Variables in the Vía Láctea) survey, these data allow us to select 55 potential cluster members, for which we derive metallicities using the public code THE CANNON. The mean radial velocity of the cluster is Vhelio = -324.9 ± 0.8 km s-1, as estimated from 55 cluster members. This high velocity, together with a low metallicity [Fe/H] = -2.04 ± 0.02 dex, suggests that VVV CL001 could be a very old cluster. The estimated distance is d = 8.23 ± 0.46 kpc, placing the cluster in the Galactic bulge. Furthermore, both its current position and the orbital parameters suggest that VVV CL001 is most probably a bulge globular cluster.


(882)Simulating radio synchrotron emission in star-forming galaxies: small-scale magnetic dynamo and the origin of the far-infrared-radio correlation
  • Christoph Pfrommer,
  • Maria Werhahn,
  • Rüdiger Pakmor,
  • Philipp Girichidis,
  • Christine M. Simpson
Monthly Notices of the Royal Astronomical Society (07/2022) doi:10.1093/mnras/stac1808
abstract + abstract -

In star-forming galaxies, the far-infrared (FIR) and radio-continuum luminosities obey a tight empirical relation over a large range of star-formation rates (SFR). To understand the physics, we examine magneto-hydrodynamic galaxy simulations, which follow the genesis of cosmic ray (CR) protons at supernovae and their advective and anisotropic diffusive transport. We show that gravitational collapse of the proto-galaxy generates a corrugated accretion shock, which injects turbulence and drives a small-scale magnetic dynamo. As the shock propagates outwards and the associated turbulence decays, the large velocity shear between the supersonically rotating cool disc with respect to the (partially) pressure-supported hot circumgalactic medium excites Kelvin-Helmholtz surface and body modes. Those interact non-linearly, inject additional turbulence and continuously drive multiple small-scale dynamos, which exponentially amplify weak seed magnetic fields. After saturation at small scales, they grow in scale to reach equipartition with thermal and CR energies in Milky Way-mass galaxies. In small galaxies, the magnetic energy saturates at the turbulent energy while it fails to reach equipartition with thermal and CR energies. We solve for steady-state spectra of CR protons, secondary electrons/positrons from hadronic CR-proton interactions with the interstellar medium, and primary shock-accelerated electrons at supernovae. The radio-synchrotron emission is dominated by primary electrons, irradiates the magnetised disc and bulge of our simulated Milky Way-mass galaxy and weakly traces bubble-shaped magnetically-loaded outflows. Our star-forming and star-bursting galaxies with saturated magnetic fields match the global FIR-radio correlation (FRC) across four orders of magnitude. Its intrinsic scatter arises due to (i) different magnetic saturation levels that result from different seed magnetic fields, (ii) different radio synchrotron luminosities for different specific SFRs at fixed SFR and (iii) a varying radio intensity with galactic inclination. In agreement with observations, several 100-pc-sized regions within star-forming galaxies also obey the FRC, while the centres of starbursts substantially exceed the FRC.


(881)Extensive study of nuclear uncertainties and their impact on the r-process nucleosynthesis in neutron star mergers
  • I. Kullmann,
  • S. Goriely,
  • O. Just,
  • A. Bauswein,
  • H. -T. Janka
arXiv e-prints (07/2022) e-Print:2207.07421
abstract + abstract -

Theoretically predicted yields of elements created by the rapid neutron capture (r-) process carry potentially large uncertainties associated with incomplete knowledge of nuclear properties as well as approximative hydrodynamical modelling of the matter ejection processes. We present an in-depth study of the nuclear uncertainties by systematically varying theoretical nuclear input models that describe the experimentally unknown neutron-rich nuclei. This includes two frameworks for calculating the radiative neutron capture rates and six, four and four models for the nuclear masses, $\beta$-decay rates and fission properties, respectively. Our r-process nuclear network calculations are based on detailed hydrodynamical simulations of dynamically ejected material from NS-NS or NS-BH binary mergers plus the secular ejecta from BH-torus systems. The impact of nuclear uncertainties on the r-process abundance distribution and early radioactive heating rate is found to be modest (within a factor $\sim 20$ for individual $A>90$ nuclei and a factor 2 for the heating rate), however the impact on the late-time heating rate is more significant and depends strongly on the contribution from fission. We witness significantly larger sensitivity to the nuclear physics input if only a single trajectory is used compared to considering ensembles of $\sim$200-300 trajectories, and the quantitative effects of the nuclear uncertainties strongly depend on the adopted conditions for the individual trajectory. We use the predicted Th/U ratio to estimate the cosmochronometric age of six metal-poor stars to set a lower limit of the age of the Galaxy and find the impact of the nuclear uncertainties to be up to 2 Gyr.


(880)Condensed dark matter with a Yukawa interaction
  • Raghuveer Garani,
  • Michel H. G. Tytgat,
  • Jérôme Vandecasteele
arXiv e-prints (07/2022) e-Print:2207.06928
abstract + abstract -

We explore the possible phases of a condensed dark matter (DM) candidate taken to be in the form of a fermion with a Yukawa coupling to a scalar particle, at zero temperature but at finite density. This theory essentially depends on only four parameters, the Yukawa coupling, the fermion mass, the scalar mediator mass, and the DM density. At low fermion densities we delimit the Bardeen-Cooper-Schrieffer (BCS), Bose-Einstein Condensate (BEC) and crossover phases as a function of model parameters using the notion of scattering length. We further study the BCS phase by consistently including emergent effects such as the scalar density condensate and superfluid gaps. Within the mean field approximation, we derive the consistent set of gap equations, retaining their momentum dependence, and valid in both the non-relativistic and relativistic regimes. We present numerical solutions to the set of gap equations, in particular when the mediator mass is smaller and larger than the DM mass. Finally, we discuss the equation of state (EoS) and possible astrophysical implications for asymmetric DM.


(879)Three-loop helicity amplitudes for quark-gluon scattering in QCD
  • Fabrizio Caola,
  • Amlan Chakraborty,
  • Giulio Gambuti,
  • Andreas von Manteuffel,
  • Lorenzo Tancredi
arXiv e-prints (07/2022) e-Print:2207.03503
abstract + abstract -

We compute the three-loop helicity amplitudes for $q\bar{q} \to gg$ and its crossed partonic channels, in massless QCD. Our analytical results provide a non-trivial check of the color quadrupole contribution to the infrared poles for external states in different color representations. At high energies, the $qg \to qg$ amplitude shows the predicted factorized form from Regge theory and confirms previous results for the gluon Regge trajectory extracted from $qq' \to qq'$ and $gg \to gg$ scattering.


(878)A multi-simulation study of relativistic SZ temperature scalings in galaxy clusters and groups
  • Elizabeth Lee,
  • Dhayaa Anbajagane,
  • Priyanka Singh,
  • Jens Chluba,
  • Daisuke Nagai
  • +4
  • Scott T. Kay,
  • Weiguang Cui,
  • Klaus Dolag,
  • Gustavo Yepes
  • (less)
arXiv e-prints (07/2022) e-Print:2207.05834
abstract + abstract -

The Sunyaev-Zeldovich (SZ) effect is a powerful tool in modern cosmology. With future observations promising ever improving SZ measurements, the relativistic corrections to the SZ signals from galaxy groups and clusters are increasingly relevant. As such, it is important to understand the differences between three temperature measures: (a) the average relativistic SZ (rSZ) temperature, (b) the mass-weighted temperature relevant for the thermal SZ (tSZ) effect, and (c) the X-ray spectroscopic temperature. In this work, we compare these cluster temperatures, as predicted by the {\sc Bahamas} \& {\sc Macsis}, {\sc Illustris-TNG}, {\sc Magneticum}, and {\sc The Three Hundred Project} simulations. Despite the wide range of simulation parameters, we find the SZ temperatures are consistent across the simulations. We estimate a $\simeq 10\%$ level correction from rSZ to clusters with $Y\simeq10^{-4}$~Mpc$^{-2}$. Our analysis confirms a systematic offset between the three temperature measures; with the rSZ temperature $\simeq 20\%$ larger than the other measures, and diverging further at higher redshifts. We demonstrate that these measures depart from simple self-similar evolution and explore how they vary with the defined radius of haloes. We investigate how different feedback prescriptions and resolution affect the observed temperatures, and discover the SZ temperatures are rather insensitive to these details. The agreement between simulations indicates an exciting avenue for observational and theoretical exploration, determining the extent of relativistic SZ corrections. We provide multiple simulation-based fits to the scaling relations for use in future SZ modelling.


(877)Testing spin-dependent dark matter interactions with lithium aluminate targets in CRESST-III
  • G. Angloher,
  • S. Banik,
  • G. Benato,
  • A. Bento,
  • A. Bertolini
  • +56
  • R. Breier,
  • C. Bucci,
  • J. Burkhart,
  • L. Canonica,
  • A. D'Addabbo,
  • S. Di Lorenzo,
  • L. Einfalt,
  • A. Erb,
  • F. v. Feilitzsch,
  • N. Ferreiro Iachellini,
  • S. Fichtinger,
  • D. Fuchs,
  • A. Fuss,
  • A. Garai,
  • V. M. Ghete,
  • S. Gerster,
  • P. Gorla,
  • P. V. Guillaumon,
  • S. Gupta,
  • D. Hauff,
  • M. Ješkovský,
  • J. Jochum,
  • M. Kaznacheeva,
  • A. Kinast,
  • H. Kluck,
  • H. Kraus,
  • A. Langenkämper,
  • M. Mancuso,
  • L. Marini,
  • L. Meyer,
  • V. Mokina,
  • A. Nilima,
  • M. Olmi,
  • T. Ortmann,
  • C. Pagliarone,
  • L. Pattavina,
  • F. Petricca,
  • W. Potzel,
  • P. Povinec,
  • F. Pröbst,
  • F. Pucci,
  • F. Reindl,
  • J. Rothe,
  • K. Schäffner,
  • J. Schieck,
  • D. Schmiedmayer,
  • S. Schönert,
  • C. Schwertner,
  • M. Stahlberg,
  • L. Stodolsky,
  • C. Strandhagen,
  • R. Strauss,
  • I. Usherov,
  • F. Wagner,
  • M. Willers,
  • V. Zema
  • (less)
arXiv e-prints (07/2022) e-Print:2207.07640
abstract + abstract -

In the past decades, numerous experiments have emerged to unveil the nature of dark matter, one of the most discussed open questions in modern particle physics. Among them, the CRESST experiment, located at the Laboratori Nazionali del Gran Sasso, operates scintillating crystals as cryogenic phonon detectors. In this work, we present first results from the operation of two detector modules which both have 10.46 g LiAlO$_2$ targets in CRESST-III. The lithium contents in the crystal are $^6$Li, with an odd number of protons and neutrons, and $^7$Li, with an odd number of protons. By considering both isotopes of lithium and $^{27}$Al, we set the currently strongest cross section upper limits on spin-dependent interaction of dark matter with protons and neutrons for the mass region between 0.25 and 1.5 GeV/c$^2$.


(876)CRESCENDO: An on-the-fly Fokker-Planck Solver for Spectral Cosmic Rays in Cosmological Simulations
  • Ludwig M. Böss,
  • Ulrich P. Steinwandel,
  • Klaus Dolag,
  • Harald Lesch
arXiv e-prints (07/2022) e-Print:2207.05087
abstract + abstract -

Non-thermal emission from relativistic Cosmic Ray (CR) electrons gives insight into the strength and morphology of intra-cluster magnetic fields, as well as providing powerful tracers of structure formation shocks. Emission caused by CR protons on the other hand still challenges current observations and is therefore testing models of proton acceleration at intra-cluster shocks. Large-scale simulations including the effects of CRs have been difficult to achieve and have been mainly reduced to simulating an overall energy budget, or tracing CR populations in post-processing of simulation output and has often been done for either protons or electrons. We introduce CRESCENDO: Cosmic Ray Evolution with SpeCtral Electrons aND prOtons, an efficient on-the-fly Fokker-Planck solver to evolve distributions of CR protons and electrons within every resolution element of our simulation. The solver accounts for CR (re-)acceleration at intra-cluster shocks, based on results of recent PIC simulations, adiabatic changes and radiative losses of electrons. We show its performance in test cases as well as idealized galaxy cluster (GC) simulations. We apply the model to an idealized GC merger following best-fit parameters for CIZA J2242.4+5301-1 and study CR injection, radio relic morphology, spectral steepening and synchrotron emission.


(875)Anapole Moment of Majorana Fermions and Implications for Direct Detection of Neutralino Dark Matter
  • Alejandro Ibarra,
  • Merlin Reichard,
  • Ryo Nagai
arXiv e-prints (07/2022) e-Print:2207.01014
abstract + abstract -

For Majorana fermions the anapole moment is the only allowed electromagnetic multipole moment. In this work we calculate the anapole moment induced at one-loop by the Yukawa and gauge interactions of a Majorana fermion, using the pinch technique to ensure the finiteness and gauge-invariance of the result. As archetypical example of a Majorana fermion, we calculate the anapole moment for the lightest neutralino in the Minimal Supersymmetric Standard Model, and specifically in the bino, wino and higgsino limits. Finally, we briefly discuss the implications of the anapole moment for the direct detection of dark matter in the form of Majorana fermions.


(874)Dark Energy Survey Year 3 Results: Constraints on extensions to $\Lambda$CDM with weak lensing and galaxy clustering
  • T.M.C. Abbott,
  • M. Aguena,
  • A. Alarcon,
  • O. Alves,
  • A. Amon
  • +156
  • J. Annis,
  • S. Avila,
  • D. Bacon,
  • E. Baxter,
  • K. Bechtol,
  • M.R. Becker,
  • G.M. Bernstein,
  • S. Birrer,
  • J. Blazek,
  • S. Bocquet,
  • A. Brandao-Souza,
  • S.L. Bridle,
  • D. Brooks,
  • D.L. Burke,
  • H. Camacho,
  • A. Campos,
  • A. Carnero Rosell,
  • M. Carrasco Kind,
  • J. Carretero,
  • F.J. Castander,
  • R. Cawthon,
  • C. Chang,
  • A. Chen,
  • R. Chen,
  • A. Choi,
  • C. Conselice,
  • J. Cordero,
  • M. Costanzi,
  • M. Crocce,
  • L.N. da Costa,
  • M.E.S. Pereira,
  • C. Davis,
  • T.M. Davis,
  • J. DeRose,
  • S. Desai,
  • E. Di Valentino,
  • H.T. Diehl,
  • S. Dodelson,
  • P. Doel,
  • C. Doux,
  • A. Drlica-Wagner,
  • K. Eckert,
  • T.F. Eifler,
  • F. Elsner,
  • J. Elvin-Poole,
  • S. Everett,
  • X. Fang,
  • A. Farahi,
  • I. Ferrero,
  • A. Ferté,
  • B. Flaugher,
  • P. Fosalba,
  • D. Friedel,
  • O. Friedrich,
  • J. Frieman,
  • J. García-Bellido,
  • M. Gatti,
  • L. Giani,
  • T. Giannantonio,
  • G. Giannini,
  • D. Gruen,
  • R.A. Gruendl,
  • J. Gschwend,
  • G. Gutierrez,
  • N. Hamaus,
  • I. Harrison,
  • W.G. Hartley,
  • K. Herner,
  • S.R. Hinton,
  • D.L. Hollowood,
  • K. Honscheid,
  • H. Huang,
  • E.M. Huff,
  • D. Huterer,
  • B. Jain,
  • D.J. James,
  • M. Jarvis,
  • N. Jeffrey,
  • T. Jeltema,
  • A. Kovacs,
  • E. Krause,
  • K. Kuehn,
  • N. Kuropatkin,
  • O. Lahav,
  • S. Lee,
  • P.-F. Leget,
  • P. Lemos,
  • C.D. Leonard,
  • A.R. Liddle,
  • M. Lima,
  • H. Lin,
  • N. MacCrann,
  • J.L. Marshall,
  • J. McCullough,
  • J. Mena-Fernández,
  • F. Menanteau,
  • R. Miquel,
  • V. Miranda,
  • J.J. Mohr,
  • J. Muir,
  • J. Myles,
  • S. Nadathur,
  • A. Navarro-Alsina,
  • R.C. Nichol,
  • R.L.C. Ogando,
  • Y. Omori,
  • A. Palmese,
  • S. Pandey,
  • Y. Park,
  • M. Paterno,
  • F. Paz-Chinchón,
  • W.J. Percival,
  • A. Pieres,
  • A.A. Plazas Malagón,
  • A. Porredon,
  • J. Prat,
  • M. Raveri,
  • M. Rodriguez-Monroy,
  • P. Rogozenski,
  • R.P. Rollins,
  • A.K. Romer,
  • A. Roodman,
  • R. Rosenfeld,
  • A.J. Ross,
  • E.S. Rykoff,
  • S. Samuroff,
  • C. Sánchez,
  • E. Sanchez,
  • J. Sanchez,
  • D. Sanchez Cid,
  • V. Scarpine,
  • D. Scolnic,
  • L.F. Secco,
  • I. Sevilla-Noarbe,
  • E. Sheldon,
  • T. Shin,
  • M. Smith,
  • M. Soares-Santos,
  • E. Suchyta,
  • M. Tabbutt,
  • G. Tarle,
  • D. Thomas,
  • C. To,
  • A. Troja,
  • M.A. Troxel,
  • I. Tutusaus,
  • T.N. Varga,
  • M. Vincenzi,
  • A.R. Walker,
  • N. Weaverdyck,
  • R.H. Wechsler,
  • J. Weller,
  • B. Yanny,
  • B. Yin,
  • Y. Zhang,
  • J. Zuntz
  • (less)
(07/2022) e-Print:2207.05766
abstract + abstract -

We constrain extensions to the $\Lambda$CDM model using measurements from the Dark Energy Survey's first three years of observations and external data. The DES data are the two-point correlation functions of weak gravitational lensing, galaxy clustering, and their cross-correlation. We use simulated data and blind analyses of real data to validate the robustness of our results. In many cases, constraining power is limited by the absence of nonlinear predictions that are reliable at our required precision. The models are: dark energy with a time-dependent equation of state, non-zero spatial curvature, sterile neutrinos, modifications of gravitational physics, and a binned $\sigma_8(z)$ model which serves as a probe of structure growth. For the time-varying dark energy equation of state evaluated at the pivot redshift we find $(w_{\rm p}, w_a)= (-0.99^{+0.28}_{-0.17},-0.9\pm 1.2)$ at 68% confidence with $z_{\rm p}=0.24$ from the DES measurements alone, and $(w_{\rm p}, w_a)= (-1.03^{+0.04}_{-0.03},-0.4^{+0.4}_{-0.3})$ with $z_{\rm p}=0.21$ for the combination of all data considered. Curvature constraints of $\Omega_k=0.0009\pm 0.0017$ and effective relativistic species $N_{\rm eff}=3.10^{+0.15}_{-0.16}$ are dominated by external data. For massive sterile neutrinos, we improve the upper bound on the mass $m_{\rm eff}$ by a factor of three compared to previous analyses, giving 95% limits of $(\Delta N_{\rm eff},m_{\rm eff})\leq (0.28, 0.20\, {\rm eV})$. We also constrain changes to the lensing and Poisson equations controlled by functions $\Sigma(k,z) = \Sigma_0 \Omega_{\Lambda}(z)/\Omega_{\Lambda,0}$ and $\mu(k,z)=\mu_0 \Omega_{\Lambda}(z)/\Omega_{\Lambda,0}$ respectively to $\Sigma_0=0.6^{+0.4}_{-0.5}$ from DES alone and $(\Sigma_0,\mu_0)=(0.04\pm 0.05,0.08^{+0.21}_{-0.19})$ for the combination of all data. Overall, we find no significant evidence for physics beyond $\Lambda$CDM.


(873)Updated neutrino mass constraints from galaxy clustering and CMB lensing-galaxy cross-correlation measurements
  • Isabelle Tanseri,
  • Steffen Hagstotz,
  • Sunny Vagnozzi,
  • Elena Giusarma,
  • Katherine Freese
(07/2022) e-Print:2207.01913
abstract + abstract -

We revisit cosmological constraints on the sum of the neutrino masses $\Sigma m_\nu$ from a combination of full-shape BOSS galaxy clustering [$P(k)$] data and measurements of the cross-correlation between Planck Cosmic Microwave Background (CMB) lensing convergence and BOSS galaxy overdensity maps [$C^{\kappa \text{g}}_{\ell}$], using a simple but theoretically motivated model for the scale-dependent galaxy bias in auto- and cross-correlation measurements. We improve upon earlier related work in several respects, particularly through a more accurate treatment of the correlation and covariance between $P(k)$ and $C^{\kappa \text{g}}_{\ell}$ measurements. When combining these measurements with Planck CMB data, we find a 95% confidence level upper limit of $\Sigma m_\nu<0.14\,{\rm eV}$, while slightly weaker limits are obtained when including small-scale ACTPol CMB data, in agreement with our expectations. We confirm earlier findings that (once combined with CMB data) the full-shape information content is comparable to the geometrical information content in the reconstructed BAO peaks given the precision of current galaxy clustering data, discuss the physical significance of our inferred bias and shot noise parameters, and perform a number of robustness tests on our underlying model. While the inclusion of $C^{\kappa \text{g}}_{\ell}$ measurements does not currently appear to lead to substantial improvements in the resulting $\Sigma m_{\nu}$ constraints, we expect the converse to be true for near-future galaxy clustering measurements, whose shape information content will eventually supersede the geometrical one.


(872)Towards an accurate model of small-scale redshift-space distortions in modified gravity
  • Cheng-Zong Ruan,
  • Carolina Cuesta-Lazaro,
  • Alexander Eggemeier,
  • César Hernández-Aguayo,
  • Carlton M. Baugh
  • +2
Monthly Notices of the Royal Astronomical Society, 514, p20 (07/2022) doi:10.1093/mnras/stac1345
abstract + abstract -

The coming generation of galaxy surveys will provide measurements of galaxy clustering with unprecedented accuracy and data size, which will allow us to test cosmological models at much higher precision than achievable previously. This means that we must have more accurate theoretical predictions to compare with future observational data. As a first step towards more accurate modelling of the redshift space distortions (RSD) of small-scale galaxy clustering in modified gravity (MG) cosmologies, we investigate the validity of the so-called Skew-T (ST) probability distribution function (PDF) of halo pairwise peculiar velocities in these models. We show that, combined with the streaming model of RSD, the ST PDF substantially improves the small-scale predictions by incorporating skewness and kurtosis, for both Λ cold dark matter (ΛCDM) and two leading MG models: f(R) gravity and the DGP braneworld model. The ST model reproduces the velocity PDF and redshift-space halo clustering measured from MG N-body simulations very well down to $\sim 5 \, h^{-1}\, \mathrm{Mpc}$. In particular, we investigate the enhancements of halo pairwise velocity moments with respect to ΛCDM for a larger range of MG variants than previous works, and present simple explanations to the behaviours observed. By performing a simple Fisher analysis, we find a significant increase in constraining power to detect modifications of General Relativity by introducing small-scale information in the RSD analyses.


(871)The importance of X-ray frequency in driving photoevaporative winds
  • Andrew D. Sellek,
  • Cathie J. Clarke,
  • Barbara Ercolano
Monthly Notices of the Royal Astronomical Society, 514, p20 (07/2022) doi:10.1093/mnras/stac1148
abstract + abstract -

Photoevaporative winds are a promising mechanism for dispersing protoplanetary discs, but so far theoretical models have been unable to agree on the relative roles that the X-ray, extreme ultraviolet or far-ultraviolet play in driving the winds. This has been attributed to a variety of methodological differences between studies, including their approach to radiative transfer and thermal balance, the choice of irradiating spectrum employed, and the processes available to cool the gas. We use the MOCASSIN radiative transfer code to simulate wind heating for a variety of spectra on a static density grid taken from simulations of an EUV-driven wind. We explore the impact of choosing a single representative X-ray frequency on their ability to drive a wind by measuring the maximum heated column as a function of photon energy. We demonstrate that for reasonable luminosities and spectra, the most effective energies are at a few 100 eV, firmly in the softer regions of the X-ray spectrum, while X-rays with energies ~1000 eV interact too weakly with disc gas to provide sufficient heating to drive a wind. We develop a simple model to explain these findings. We argue that further increases in the cooling above our models - for example due to molecular rovibrational lines - may further restrict the heating to the softer energies but are unlikely to prevent X-ray heated winds from launching entirely; increasing the X-ray luminosity has the opposite effect. The various results of photoevaporative wind models should therefore be understood in terms of the choice of irradiating spectrum.


(870)THE THREE HUNDRED project: The GIZMO-SIMBA run
  • Weiguang Cui,
  • Romeel Dave,
  • Alexander Knebe,
  • Elena Rasia,
  • Meghan Gray
  • +20
  • Frazer Pearce,
  • Chris Power,
  • Gustavo Yepes,
  • Dhayaa Anbajagane,
  • Daniel Ceverino,
  • Ana Contreras-Santos,
  • Daniel de Andres,
  • Marco De Petris,
  • Stefano Ettori,
  • Roan Haggar,
  • Qingyang Li,
  • Yang Wang,
  • Xiaohu Yang,
  • Stefano Borgani,
  • Klaus Dolag,
  • Ying Zu,
  • Ulrike Kuchner,
  • Rodrigo Cañas,
  • Antonio Ferragamo,
  • Giulia Gianfagna
  • (less)
Monthly Notices of the Royal Astronomical Society, 514, p20 (07/2022) doi:10.1093/mnras/stac1402
abstract + abstract -

We introduce GIZMO-SIMBA, a new suite of galaxy cluster simulations within THE THREE HUNDRED project. THE THREE HUNDRED consists of zoom re-simulations of 324 clusters with $M_{200}\gtrsim 10^{14.8}\, \mathrm{M}_\odot$ drawn from the MultiDark-Planck N-body simulation, run using several hydrodynamic and semi-analytical codes. The GIZMO-SIMBA suite adds a state-of-the-art galaxy formation model based on the highly successful SIMBA simulation, mildly re-calibrated to match $z$ = 0 cluster stellar properties. Comparing to THE THREE HUNDRED zooms run with GADGET-X, we find intrinsic differences in the evolution of the stellar and gas mass fractions, BCG ages, and galaxy colour-magnitude diagrams, with GIZMO-SIMBA generally providing a good match to available data at $z$ ≍ 0. GIZMO-SIMBA's unique black hole growth and feedback model yields agreement with the observed BH scaling relations at the intermediate-mass range and predicts a slightly different slope at high masses where few observations currently lie. GIZMO-SIMBA provides a new and novel platform to elucidate the co-evolution of galaxies, gas, and black holes within the densest cosmic environments.


(869)Transport model comparison studies of intermediate-energy heavy-ion collisions
  • Hermann Wolter,
  • Maria Colonna,
  • Dan Cozma,
  • Pawel Danielewicz,
  • Che Ming Ko
  • +48
  • Rohit Kumar,
  • Akira Ono,
  • ManYee Betty Tsang,
  • Jun Xu,
  • Ying-Xun Zhang,
  • Elena Bratkovskaya,
  • Zhao-Qing Feng,
  • Theodoros Gaitanos,
  • Arnaud Le Fèvre,
  • Natsumi Ikeno,
  • Youngman Kim,
  • Swagata Mallik,
  • Paolo Napolitani,
  • Dmytro Oliinychenko,
  • Tatsuhiko Ogawa,
  • Massimo Papa,
  • Jun Su,
  • Rui Wang,
  • Yong-Jia Wang,
  • Janus Weil,
  • Feng-Shou Zhang,
  • Guo-Qiang Zhang,
  • Zhen Zhang,
  • Joerg Aichelin,
  • Wolfgang Cassing,
  • Lie-Wen Chen,
  • Hui-Gan Cheng,
  • Hannah Elfner,
  • K. Gallmeister,
  • Christoph Hartnack,
  • Shintaro Hashimoto,
  • Sangyong Jeon,
  • Kyungil Kim,
  • Myungkuk Kim,
  • Bao-An Li,
  • Chang-Hwan Lee,
  • Qing-Feng Li,
  • Zhu-Xia Li,
  • Ulrich Mosel,
  • Yasushi Nara,
  • Koji Niita,
  • Akira Ohnishi,
  • Tatsuhiko Sato,
  • Taesoo Song,
  • Agnieszka Sorensen,
  • Ning Wang,
  • Wen-Jie Xie,
  • (TMEP collaboration)
  • (less)
Progress in Particle and Nuclear Physics, 125 (07/2022) doi:10.1016/j.ppnp.2022.103962
abstract + abstract -

Transport models are the main method to obtain physics information on the nuclear equation of state and in-medium properties of particles from low to relativistic-energy heavy-ion collisions. The Transport Model Evaluation Project (TMEP) has been pursued to test the robustness of transport model predictions in reaching consistent conclusions from the same type of physical model. To this end, calculations under controlled conditions of physical input and set-up were performed with various participating codes. These included both calculations of nuclear matter in a box with periodic boundary conditions, which test separately selected ingredients of a transport code, and more realistic calculations of heavy-ion collisions. Over the years, six studies have been performed within this project. In this intermediate review, we summarize and discuss the present status of the project. We also provide condensed descriptions of the 26 participating codes, which contributed to some part of the project. These include the major codes in use today. After a compact description of the underlying transport approaches, we review the main results of the studies completed so far. They show, that in box calculations the differences between the codes can be well understood and a convergence of the results can be reached. These studies also highlight the systematic differences between the two families of transport codes, known under the names of Boltzmann-Uehling-Uhlenbeck (BUU) and Quantum Molecular Dynamics (QMD) type codes. However, when the codes were compared in full heavy-ion collisions using different physical models, as recently for pion production, they still yielded substantially different results. This calls for further comparisons of heavy-ion collisions with controlled models and of box comparisons of important ingredients, like momentum-dependent fields, which are currently underway. Our evaluation studies often indicate improved strategies in performing transport simulations and thus can provide guidance to code developers. Results of transport simulations of heavy-ion collisions from a given code will have more significance if the code can be validated against benchmark calculations such as the ones summarized in this review.


(868)On the superiority of the | V<SUB>cb</SUB>|-γ plots over the unitarity triangle plots in the 2020s