(463)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.

(462)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.

(461)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.

(460)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.

(459)Cosmological implications of the full shape of anisotropic clustering measurements in BOSS and eBOSS
• Agne Semenaite,
• Ariel G. Sánchez,
• Andrea Pezzotta,
• Jiamin Hou,
• Roman Scoccimarro
• +8
• Alexander Eggemeier,
• Martin Crocce,
• Chia-Hsun Chuang,
• Alexander Smith,
• Cheng Zhao,
• Joel R. Brownstein,
• Graziano Rossi,
• Donald P. Schneider
• (less)
Monthly Notices of the Royal Astronomical Society, 512, p14 (06/2022) doi:10.1093/mnras/stac829
abstract + abstract -

We present the analysis of the full shape of anisotropic clustering measurement from the extended Baryon Oscillation Spectroscopic Survey (eBOSS) quasar sample together with the combined galaxy sample from the Baryon Oscillation Spectroscopic Survey (BOSS), re-analysed using an updated recipe for the non-linear matter power spectrum and the non-local bias parameters. We obtain constraints for flat Lambda cold dark matter cosmologies, focusing on the cosmological parameters that are independent of the Hubble parameter h. Our recovered value for the Root Mean Square (RMS) linear perturbation theory variance as measured on the scale of $12\, {\rm Mpc}$ is σ12 = 0.805 ± 0.049, while using the traditional reference scale of $8\, h^{-1}\, {\rm Mpc}$ gives σ8 = 0.815 ± 0.044. We quantify the agreement between our measurements and the latest cosmic microwave background data from Planck using the suspiciousness metric, and find them to be consistent within 0.64 ± 0.03σ. Combining our clustering constraints with the 3 × 2pt data sample from the Dark Energy Survey Year 1 release slightly degrades this agreement to the level of 1.54 ± 0.08σ, while still showing an overall consistency with Planck. We furthermore study the effect of imposing a Planck - like prior on the parameters that define the shape of the linear matter power spectrum, and find significantly tighter constraints on the parameters that control the evolution of density fluctuations. In particular, the combination of low-redshift data sets prefers a value of the physical dark energy density ωDE = 0.335 ± 0.011, which is 1.7σ higher than the one preferred by Planck.

(458)Presolar grain dynamics: Creating nucleosynthetic variations through a combination of drag and viscous evolution
• Mark A. Hutchison,
• Jean-David Bodénan,
• Lucio Mayer,
• Maria Schönbächler
Monthly Notices of the Royal Astronomical Society, 512, p21 (06/2022) doi:10.1093/mnras/stac765
abstract + abstract -

Meteoritic studies of Solar system objects show evidence of nucleosynthetic heterogeneities that are inherited from small presolar grains ($\lt 10\,\, \mu {\mathrm{m}}$) formed in stellar environments external to our own. The initial distribution and subsequent evolution of these grains are currently unconstrained. Using 3D, gas-dust simulations, we find that isotopic variations on the order of those observed in the Solar system can be generated and maintained by drag and viscosity. Small grains are dragged radially outwards without size/density sorting by viscous expansion and backreaction, enriching the outer disc with presolar grains. Meanwhile large aggregates composed primarily of silicates drift radially inwards due to drag, further enriching the relative portion of presolar grains in the outer disc and diluting the inner disc. The late accumulation of enriched aggregates outside Jupiter could explain some of the isotopic variations observed in Solar system bodies, such as the enrichment of supernovae derived material in carbonaceous chondrites. We also see evidence for isotopic variations in the inner disc that may hold implications for enstatite and ordinary chondrites that formed closer to the Sun. Initial heterogeneities in the presolar grain distribution that are not continuously reinforced are dispersed by diffusion, radial surface flows, and/or planetary interactions over the entire lifetime of the disc. For younger, more massive discs we expect turbulent diffusion to be even more homogenizing, suggesting that dust evolution played a more central role in forming the isotopic anomalies in the Solar system than originally thought.

(457)The PEPSI exoplanet transit survey (PETS) I: investigating the presence of a silicate atmosphere on the super-earth 55 Cnc e
• Engin Keles,
• Matthias Mallonn,
• Daniel Kitzmann,
• Katja Poppenhaeger,
• H. Jens Hoeijmakers
• +24
• Ilya Ilyin,
• Xanthippi Alexoudi,
• Thorsten A. Carroll,
• Julian Alvarado-Gomez,
• Laura Ketzer,
• Aldo S. Bonomo,
• Francesco Borsa,
• B. Scott Gaudi,
• Thomas Henning,
• Luca Malavolta,
• Karan Molaverdikhani,
• Valerio Nascimbeni,
• Jennifer Patience,
• Lorenzo Pino,
• Gaetano Scandariato,
• Everett Schlawin,
• Evgenya Shkolnik,
• Daniela Sicilia,
• Alessandro Sozzetti,
• Mary G. Foster,
• Christian Veillet,
• Ji Wang,
• Fei Yan,
• Klaus G. Strassmeier
• (less)
Monthly Notices of the Royal Astronomical Society, 513, p13 (06/2022) doi:10.1093/mnras/stac810
abstract + abstract -

The study of exoplanets and especially their atmospheres can reveal key insights on their evolution by identifying specific atmospheric species. For such atmospheric investigations, high-resolution transmission spectroscopy has shown great success, especially for Jupiter-type planets. Towards the atmospheric characterization of smaller planets, the super-Earth exoplanet 55 Cnc e is one of the most promising terrestrial exoplanets studied to date. Here, we present a high-resolution spectroscopic transit observation of this planet, acquired with the PEPSI instrument at the Large Binocular Telescope. Assuming the presence of Earth-like crust species on the surface of 55 Cnc e, from which a possible silicate-vapor atmosphere could have originated, we search in its transmission spectrum for absorption of various atomic and ionized species such as Fe , Fe +, Ca , Ca +, Mg, and K , among others. Not finding absorption for any of the investigated species, we are able to set absorption limits with a median value of 1.9 × RP. In conclusion, we do not find evidence of a widely extended silicate envelope on this super-Earth reaching several planetary radii.

(456)LYRA - II. Cosmological dwarf galaxy formation with inhomogeneous Population III enrichment
• Thales A. Gutcke,
• Rüdiger Pakmor,
• Thorsten Naab,
• Volker Springel
Monthly Notices of the Royal Astronomical Society, 513, p14 (06/2022) doi:10.1093/mnras/stac867
abstract + abstract -

We present the simulation of a $2\times 10^{9}\, \mathrm{M}_{\odot }$ halo mass cosmological dwarf galaxy run to z = 0 at 4 solar mass gas resolution with resolved supernova feedback. We compare three simple subgrid implementations for the inhomogeneous chemical enrichment from Population III stars and compare them to constraints from Local Group dwarf galaxies. The employed model, LYRA, is a novel high-resolution galaxy formation model built for the moving mesh code AREPO, which is marked by a resolved multiphase interstellar medium, single stars, and individual supernova events. The resulting reionization relic is characterized by a short (<1.5 Gyr) star formation history that is repeatedly brought to a standstill by violent bursts of feedback. Star formation is reignited for a short duration due to a merger at z ≍ 4 and then again at z ≍ 0.2-0 after sustained gas accretion. Our model z = 0 galaxy matches the stellar mass, size, stellar kinematics, and metallicity relations of Local Group dwarf galaxies well. The dark matter profile does not exhibit a core in any version of the model. We show that the host halo masses of Population III stars affect the assembly history of dwarf galaxies. This manifests itself through the initial gaseous collapse in the progenitor haloes, affecting the central density of the stellar component and through the accretion of luminous substructure.

(455)Observations of PAHs in the atmospheres of discs and exoplanets
• Barbara Ercolano,
• Christian Rab,
• Karan Molaverdikhani,
• Billy Edwards,
• Thomas Preibisch
• +3
• Leonardo Testi,
• Inga Kamp,
• Wing-Fai Thi
• (less)
Monthly Notices of the Royal Astronomical Society, 512, p9 (05/2022) doi:10.1093/mnras/stac505
abstract + abstract -

Polycyclic aromatic hydrocarbons (PAHs) play a key role in the chemical and hydrodynamical evolution of the atmospheres of exoplanets and planet-forming discs. If they can survive the planet formation process, PAHs are likely to be involved in pre-biotic chemical reactions eventually leading to more complex molecules such as amino acids and nucleotides, which form the basis for life as we know it. However, the abundance and specific role of PAHs in these environments is largely unknown due to limitations in sensitivity and range of wavelength of current and previous space-borne facilities. Upcoming infrared space spectroscopy missions, such as Twinkle and Ariel, present a unique opportunity to detect PAHs in the atmospheres of exoplanets and planet-forming discs. In this work, we present synthetic observations based on conservative numerical modelling of typical planet-forming discs and a transiting hot Saturnian planet around solar-type star. Our models show that Twinkle and Ariel might both be able to detect the 3.3 $\mu$m PAH feature within reasonable observing time in discs and transiting planets, assuming that PAHs are present with an abundance of at least one-tenth of the interstellar medium value.

(454)Black hole mergers in compact star clusters and massive black hole formation beyond the mass gap
• Francesco Paolo Rizzuto,
• Thorsten Naab,
• Rainer Spurzem,
• Manuel Arca-Sedda,
• Mirek Giersz
• +2
• Jeremiah Paul Ostriker,
• Sambaran Banerjee
• (less)
Monthly Notices of the Royal Astronomical Society, 512, p15 (05/2022) doi:10.1093/mnras/stac231
abstract + abstract -

We present direct N-body simulations, carried out with NBODY6+ + GPU, of young and compact low-metallicity (Z = 0.0002) star clusters with 1.1 × 105 stars, a velocity dispersion of ~15 $\mathrm{km\, s^{-1}}$, a half-mass radius Rh = 0.6 pc, and a binary fraction of $10{{\ \rm per\,cent}}$ including updated evolution models for stellar winds and (pulsation) pair-instability supernovae (PSNe). Within the first tens of megayears, each cluster hosts several black hole (BH) merger events which nearly cover the complete mass range of primary and secondary BH masses for current LIGO-Virgo-KAGRA gravitational wave detections. The importance of gravitational recoil is estimated statistically during post-processing analysis. We present possible formation paths of massive BHs above the assumed lower PSN mass-gap limit ($45\, {\rm M}_\odot$) into the intermediate-mass black hole (IMBH) regime ($\gt 100\, {\rm M}_\odot$) which include collisions of stars, BHs, and the direct collapse of stellar merger remnants with low core masses. The stellar evolution updates result in the early formation of heavier stellar BHs compared to the previous model. The resulting higher collision rates with massive stars support the rapid formation of massive BHs. For models assuming a high accretion efficiency for star-BH mergers, we present a first-generation formation scenario for GW190521-like events: a merger of two BHs which reached the PSN mass-gap merging with massive stars. This event is independent of gravitational recoil and therefore conceivable in dense stellar systems with low escape velocities. One simulated cluster even forms an IMBH binary (153, 173 M) which is expected to merge within a Hubble time.

(453)On the Standard Model Predictions for Rare K and B Decay Branching Ratios: 2022
• Andrzej J. Buras
arXiv e-prints (05/2022)
abstract + abstract -

In this decade one expects a very significant progress in measuring the branching ratios for several rare $K$ and $B$ decays, in particular for the decays $K^+\to\pi^+\nu\bar\nu$, $K_L\to\pi^0\nu\bar\nu$, $B_s\to\mu^+\mu^+$ and $B_d\to\mu^+\mu^+$. On the theory side a very significant progress on calculating these branching ratios has been achieved in the last thirty years culminating recently in rather precise SM predictions for them. It is then unfortunate that some papers still cite the results for $K^+\to\pi^+\nu\bar\nu$ and $K_L\to\pi^0\nu\bar\nu$ presented by us in 2015. They are clearly out of date. Similar comments apply to predictions for $B_{s,d}\to\mu^+\mu^-$. In this note I want to stress again that, in view of the tensions between various determinations of $V_{cb}$ in tree-level decays, presently, the only trustable SM predictions for the branching ratios in question can be obtained by eliminating their dependence on the CKM parameters with the help of $|\varepsilon_K|$, $\Delta M_s$, $\Delta M_d$ and $S_{\psi K_S}$, evaluated in the SM. In this context I am astonished by statements made by some computer code practitioners that setting in this strategy these four $\Delta F=2$ observables to their experimental values is an assumption. The goal of this strategy is not to make an overall SM fit but to predict the SM branching ratios. In the SM there are no new physics (NP) contributions to $\Delta F=2$ transitions and no assumption on the absence of NP is needed. Moreover, presently NP is not required to describe simultaneously the very precise data on $|\varepsilon_K|$, $\Delta M_s$, $\Delta M_d$ and $S_{\psi K_S}$. This strategy for obtaining true SM predictions for rare decay branching ratios is moreover not polluted by hadronic uncertainies and observed anomalies in semi-leptonic decays used often in global analyses.

(452)Probing vainsthein-screening gravity with galaxy clusters using internal kinematics and strong and weak lensing
• Lorenzo Pizzuti,
• Ippocratis D. Saltas,
• Keiichi Umetsu,
• Barbara Sartoris
Monthly Notices of the Royal Astronomical Society, 512, p11 (05/2022) doi:10.1093/mnras/stac746
abstract + abstract -

We use high-precision combined strong/weak lensing and kinematics measurements of the total mass profiles of the observed galaxy clusters MACS J1206.2-0847 and Abell S1063, to constrain the relativistic sector of the general DHOST dark energy theories, which exhibit a partial breaking of the so called Vainsthein screening mechanism, on the linear level of scalar fluctuations around a cosmological background. In particular, by using the MG-MAMMPOSST framework developed in Pizzuti et al., for the kinematics analysis of member galaxies in clusters, along with lensing mass profile reconstructions, we provide new constraints on the coupling Y2 that governs the theory's relativistic contribution to the lensing potential. The new bound from the combination of kinematics and lensing measurements of MACS 1206, $Y_2=-0.12^{+0.66}_{-0.67}$ at 2σ, provides about a two-fold improvement on previous constraints. In the case of Abell S1063, a >2σ tension with the GR expectation arises. We discuss this in some detail, and we investigate the possible sources of systematics that can explain the tension. We further discuss why the combination of kinematics of member galaxies with lensing is capable of providing much tighter bounds compared to kinematics or lensing alone, and we explain how the number density profile of tracers, as well as the choice of the velocity anisotropy profile, affects the final results.

(451)Pulsational pair-instability supernovae: gravitational collapse, black hole formation, and beyond
• N. Rahman,
• H. -T. Janka,
• G. Stockinger,
• S. E. Woosley
Monthly Notices of the Royal Astronomical Society, 512, p38 (05/2022) doi:10.1093/mnras/stac758
abstract + abstract -

We investigate the final collapse of rotating and non-rotating pulsational pair-instability supernova progenitors with zero-age-main-sequence masses of 60, 80, and 115 M and iron cores between 2.37 and 2.72 M by 2D hydrodynamics simulations. Using the general relativistic NADA-FLD code with energy-dependent three-flavour neutrino transport by flux-limited diffusion allows us to follow the evolution beyond the moment when the transiently forming neutron star (NS) collapses to a black hole (BH), which happens within 350-580 ms after bounce in all cases. Because of high neutrino luminosities and mean energies, neutrino heating leads to shock revival within ≲ 250 ms post bounce in all cases except the rapidly rotating 60 M model. In the latter case, centrifugal effects support a 10 per cent higher NS mass but reduce the radiated neutrino luminosities and mean energies by ~20 per cent and ~10 per cent, respectively, and the neutrino-heating rate by roughly a factor of two compared to the non-rotating counterpart. After BH formation, the neutrino luminosities drop steeply but continue on a 1-2 orders of magnitude lower level for several 100 ms because of aspherical accretion of neutrino and shock-heated matter, before the ultimately spherical collapse of the outer progenitor shells suppresses the neutrino emission to negligible values. In all shock-reviving models BH accretion swallows the entire neutrino-heated matter and the explosion energies decrease from maxima around 1.5 × 1051 erg to zero within a few seconds latest. Nevertheless, the shock or a sonic pulse moves outward and may trigger mass-loss, which we estimate by long-time simulations with the PROMETHEUS code. We also provide gravitational-wave signals.

(450)Gravothermal evolution of dark matter halos with differential elastic scattering
• Daneng Yang,
• Hai-Bo Yu
arXiv e-prints (05/2022)
abstract + abstract -

We study gravothermal evolution of dark matter halos in the presence of differential self-scattering that has strong velocity and angular dependencies. We design controlled N-body simulations to model Rutherford and \Moller scatterings in the halo, and follow its evolution in both core-expansion and -collapse phases. The simulations show the commonly-used transfer cross section underestimates the effects of dark matter self-interactions, but the viscosity cross section provides a good approximation for modeling angular-dependent dark matter scattering. We investigate thermodynamic properties of the halo, and find that the three moments of the Boltzmann equation under the fluid approximation are satisfied. We further propose a constant effective cross section, which integrates over the halo's characteristic velocity dispersion with weighting kernels motivated by kinetic theory of heat conduction. The effective cross section provides an approximation to differential self-scattering for most of the halo evolution. However, it can significantly underestimate the growth rate of the central density at late stages of the collapse phase. This indicates that constant and velocity-dependent dark matter self-interactions are fundamentally different, as for the latter the cross section evolves with the halo dynamically, boosting the collapse. This feature may help test different self-interacting dark matter models.

(449)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)
arXiv e-prints (05/2022)
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.

(448)Geometry-induced patterns through mechanochemical coupling
• Laeschkir Würthner,
• Andriy Goychuk,
• Erwin Frey
arXiv e-prints (05/2022)
abstract + abstract -

Intracellular protein patterns regulate a variety of vital cellular processes such as cell division and motility, which often involve dynamic changes of cell shape. These changes in cell shape may in turn affect the dynamics of pattern-forming proteins, hence leading to an intricate feedback loop between cell shape and chemical dynamics. While several computational studies have examined the resulting rich dynamics, the underlying mechanisms are not yet fully understood. To elucidate some of these mechanisms, we explore a conceptual model for cell polarity on a dynamic one-dimensional manifold. Using concepts from differential geometry, we derive the equations governing mass-conserving reaction-diffusion systems on time-evolving manifolds. Analyzing these equations mathematically, we show that dynamic shape changes of the membrane can induce pattern-forming instabilities in parts of the membrane, which we refer to as regional instabilities. Deformations of the local membrane geometry can also (regionally) suppress pattern formation and spatially shift already existing patterns. We explain our findings by applying and generalizing the local equilibria theory of mass-conserving reaction-diffusion systems. This allows us to determine a simple onset criterion for geometry-induced pattern-forming instabilities, which is linked to the phase-space structure of the reaction-diffusion system. The feedback loop between membrane shape deformations and reaction-diffusion dynamics then leads to a surprisingly rich phenomenology of patterns, including oscillations, traveling waves, and standing waves that do not occur in systems with a fixed membrane shape. Our work reveals that the local conformation of the membrane geometry acts as an important dynamical control parameter for pattern formation in mass-conserving reaction-diffusion systems.

(447)Non-linearities in the Lyman-$\alpha$ forest and in its cross-correlation with dark matter halos
• Jahmour J. Givans,
• Andreu Font-Ribera,
• Anže Slosar,
• Louise Seeyave,
• Christian Pedersen
• +4
• Keir K. Rogers,
• Mathias Garny,
• Diego Blas,
• Vid Iršič
• (less)
arXiv e-prints (05/2022)
abstract + abstract -

Three-dimensional correlations of the Lyman-$\alpha$ (Ly$\alpha$) forest and cross correlations between the Ly$\alpha$ forest and quasars have been measured on large scales, allowing a precise measurement of the baryon acoustic oscillation (BAO) feature at redshifts $z>2$. These 3D correlations are often modelled using linear perturbation theory, but full-shape analyses to extract cosmological information beyond BAO will require more realistic models capable of describing non-linearities present at smaller scales. We present a measurement of the Ly$\alpha$ forest flux power spectrum from large hydrodynamic simulations -- the Sherwood simulations -- and compare it to different models describing the small-scale deviations from linear theory. We confirm that the model presented in Arinyo-i-Prats et al. (2015) fits the measured 3D power up to $k=10\, h\rm{Mpc^{-1}}$ with an accuracy better than 5%, and show that the same model can also describe the 1D correlations with similar precision. We also present, for the first time, an equivalent study for the cross-power spectrum of halos with the Ly$\alpha$ forest, and we discuss different challenges we face when modelling the cross-power spectrum beyond linear scales. We make all our measured power spectra public in \url{https://github.com/andreufont/sherwood_p3d}. This study is a step towards joint analyses of 1D and 3D flux correlations, and towards using the quasar-Ly$\alpha$ cross-correlation beyond BAO analyses.

(446)Online triggers for supernova and pre-supernova neutrino detection with cryogenic detectors
• Philipp Eller,
• Nahuel Ferreiro Iachellini,
• Luca Pattavina,
• Lolian Shtembari
arXiv e-prints (05/2022)
abstract + abstract -

Supernovae (SNe) are among the most energetic events in the universe still far from being fully understood. An early and prompt detection of neutrinos is a one-time opportunity for the realization of the first multi-messenger observation of these events. In this work, we present the prospects of detecting neutrinos produced before (pre-SN) and during a SN while running an advanced cryogenic detector. The recent advancements of the cryogenic detector technique and the discovery of coherent elastic neutrino-nucleus scattering offer a wealth of opportunities in neutrino detection. The combination of the excellent energy resolution of this experimental technique, with the high cross section of this detection channel and its equal sensitivity to all neutrino flavors enables the realization of highly sensitive cm-scale neutrino telescopes, as the newly proposed RES-NOVA experiment. We present a detailed study on the detection promptness of pre-SN and SN neutrino signals, with direct comparisons among different classes of test statistics. While the well-established Poisson test offers in general best performance under optimal conditions, the non-parametric Recursive Product of Spacing statistical test (RPS) is more robust and ideal for triggering astrophysical neutrino signals with no specific prior knowledge. Based on our statistical tests the RES-NOVA experiment is able to identify SN neutrino signals at a 15 kpc distance with 95% of success rate, and pre-SN signal as far as 480 pc with a pre-warn time of the order of 10 s. These results demonstrate the potential of RPS for the identification of neutrino signals and the physics reach of the RES-NOVA experiment.

(445)Probing Red Supergiant dynamics through photo-center displacements measured by Gaia
• A. Chiavassa,
• R. Kudritzki,
• B. Davies,
• B. Freytag,
• S. E. de Mink
arXiv e-prints (05/2022)
abstract + abstract -

Red supergiant (RSGs) are cool massive stars in a late phase of their evolution when the stellar envelope becomes fully convective. They are the brightest stars in the universe at infrared light and can be detected in galaxies far beyond the Local Group, allowing for accurate determination of chemical composition of galaxies. The study of their physical properties is extremely important for various phenomena including the final fate of massive stars as type II supernovae and gravitational wave progenitors. We explore the well-studied nearby young stellar cluster chi Per. Using Gaia EDR3 data, we find the distance of the cluster (d = 2.260+-0.020 kpc). We then investigate the variability of the convection-related surface structure as a source for parallax measurement uncertainty. We use state-of-the-art 3D radiative hydrodynamics simulations with CO5BOLD and the post-processing radiative transfer code OPTIM3D to compute intensity maps in the Gaia G photometric system. We calculate the variabiltiy, as a function of time, of the intensity-weighted mean from the synthetic maps. We then select the RSG stars in the cluster and compare their uncertainty on parallaxes to the predictions of photocentre displacements. The synthetic maps of RSG show extremely irregular and temporal variable surfaces due to convection-related dynamics. Consequentially, the position of the photo-center varies during Gaia measurements between 0.033 and 0.130 AU (up to 5% of the corresponding simulation stellar radius). We argue that the variability of the convection-related surface structures accounts for a substantial part of the Gaia EDR3 parallax error of the RSG sample. We suggest that the variation of the uncertainty on Gaia parallax could be exploited quantitatively using appropriate 3D simulations to extract, in a unique way, important information about the stellar dynamics and parameters of RSG stars.

(444)Can we actually constrain $f_{\rm NL}$ using the scale-dependent bias effect? An illustration of the impact of galaxy bias uncertainties using the BOSS DR12 galaxy power spectrum
• Alexandre Barreira
arXiv e-prints (05/2022)
abstract + abstract -

The scale-dependent bias effect on the galaxy power spectrum is a very promising probe of the local primordial non-Gaussianity (PNG) parameter $f_{\rm NL}$, but the amplitude of the effect is proportional to $f_{\rm NL}b_{\phi}$, where $b_{\phi}$ is the linear PNG galaxy bias parameter. Our knowledge of $b_{\phi}$ is currently very limited, yet nearly all existing $f_{\rm NL}$ constraints and forecasts assume precise knowledge for it. Here, we use the BOSS DR12 galaxy power spectrum to illustrate how our uncertain knowledge of $b_{\phi}$ currently prevents us from constraining $f_{\rm NL}$ with a given statistical precision $\sigma_{f_{\rm NL}}$. Assuming different fixed choices for the relation between $b_{\phi}$ and the linear density bias $b_1$, we find that $\sigma_{f_{\rm NL}}$ can vary by as much as an order of magnitude. Our strongest bound is $f_{\rm NL} = 16 \pm 16\ (1\sigma)$, while the loosest is $f_{\rm NL} = 230 \pm 226\ (1\sigma)$ for the same BOSS data. The impact of $b_{\phi}$ can be especially pronounced because it can be close to zero. We also show how marginalizing over $b_{\phi}$ with wide priors is not conservative, and leads in fact to biased constraints through parameter space projection effects. Independently of galaxy bias assumptions, the scale-dependent bias effect can only be used to detect $f_{\rm NL} \neq 0$ by constraining the product $f_{\rm NL}b_{\phi}$, but the error bar $\sigma_{f_{\rm NL}}$ remains undetermined and the results cannot be compared with the CMB; we find $f_{\rm NL}b_{\phi} \neq 0$ with $1.6\sigma$ significance. We also comment on why these issues are important for analyses with the galaxy bispectrum. Our results strongly motivate simulation-based research programs aimed at robust theoretical priors for the $b_{\phi}$ parameter, without which we may never be able to competitively constrain $f_{\rm NL}$ using galaxy data.

(443)Next-to-leading power endpoint factorization and resummation for off-diagonal "gluon" thrust
• M. Beneke,
• M. Garny,
• S. Jaskiewicz,
• J. Strohm,
• R. Szafron
• +2
arXiv e-prints (05/2022)
abstract + abstract -

The lack of convergence of the convolution integrals appearing in next-to-leading-power (NLP) factorization theorems prevents the applications of existing methods to resum power-suppressed large logarithmic corrections in collider physics. We consider thrust distribution in the two-jet region for the flavour-nonsinglet off-diagonal contribution, where a gluon-initiated jet recoils against a quark-antiquark pair, which is power-suppressed. With the help of operatorial endpoint factorization conditions, we obtain a factorization formula, where the individual terms are free from endpoint divergences in convolutions and can be expressed in terms of renormalized hard, soft and collinear functions in four dimensions. This allows us to perform the first resummation of the endpoint-divergent SCET$_{\rm I}$ observables at the leading logarithmic accuracy using exclusively renormalization-group methods. The presented approach relies on universal properties of the soft and collinear limits and may serve as a paradigm for the systematic NLP resummation for other $1\to 2$ and $2\to 1$ collider physics processes.

(442)New constraint on the tensor-to-scalar ratio from the $Planck$ and BICEP/Keck Array data using the profile likelihood
• Paolo Campeti,
• Eiichiro Komatsu
arXiv e-prints (05/2022)
abstract + abstract -

We derive a new upper bound on the tensor-to-scalar ratio parameter $r$ using the frequentist profile likelihood method. We vary all the relevant cosmological parameters of the $\Lambda$CDM model, as well as the nuisance parameters. Unlike the Bayesian analysis using Markov Chain Monte Carlo (MCMC), our analysis is independent of the choice of priors. Using $Planck$ Public Release 4, BICEP/Keck Array 2018, $Planck$ CMB lensing, and BAO data, we find an upper limit of $r<0.037$ at 95% C.L., similar to the Bayesian MCMC result of $r<0.038$ for a flat prior on $r$ and a conditioned $Planck$ lowlEB covariance matrix.

(441)New constraint on the tensor-to-scalar ratio from the $Planck$ and BICEP/Keck Array data using the profile likelihood
• Paolo Campeti,
• Eiichiro Komatsu
(05/2022) e-Print:2205.05617
abstract + abstract -

We derive a new upper bound on the tensor-to-scalar ratio parameter $r$ using the frequentist profile likelihood method. We vary all the relevant cosmological parameters of the $\Lambda$CDM model, as well as the nuisance parameters. Unlike the Bayesian analysis using Markov Chain Monte Carlo (MCMC), our analysis is independent of the choice of priors. Using $Planck$ Public Release 4, BICEP/Keck Array 2018, $Planck$ CMB lensing, and BAO data, we find an upper limit of $r<0.037$ at 95% C.L., similar to the Bayesian MCMC result of $r<0.038$ for a flat prior on $r$ and a conditioned $Planck$ lowlEB covariance matrix.

(440)Online triggers for supernova and pre-supernova neutrino detection with cryogenic detectors
• Philipp Eller,
• Nahuel Iachellini Ferreiro,
• Luca Pattavina,
• Lolian Shtembari
(05/2022) e-Print:2205.03350
abstract + abstract -

Supernovae (SNe) are among the most energetic events in the universe still far from being fully understood. An early and prompt detection of neutrinos is a one-time opportunity for the realization of the first multi-messenger observation of these events. In this work, we present the prospects of detecting neutrinos produced before (pre-SN) and during a SN while running an advanced cryogenic detector. The recent advancements of the cryogenic detector technique and the discovery of coherent elastic neutrino-nucleus scattering offer a wealth of opportunities in neutrino detection. The combination of the excellent energy resolution of this experimental technique, with the high cross section of this detection channel and its equal sensitivity to all neutrino flavors enables the realization of highly sensitive cm-scale neutrino telescopes, as the newly proposed RES-NOVA experiment. We present a detailed study on the detection promptness of pre-SN and SN neutrino signals, with direct comparisons among different classes of test statistics. While the well-established Poisson test offers in general best performance under optimal conditions, the non-parametric Recursive Product of Spacing statistical test (RPS) is more robust and ideal for triggering astrophysical neutrino signals with no specific prior knowledge. Based on our statistical tests the RES-NOVA experiment is able to identify SN neutrino signals at a 15 kpc distance with 95% of success rate, and pre-SN signal as far as 480 pc with a pre-warn time of the order of 10 s. These results demonstrate the potential of RPS for the identification of neutrino signals and the physics reach of the RES-NOVA experiment.

(439)Cosmological Bound on the QCD Axion Mass, Redux
• Francesco D'Eramo,
• Eleonora Di Valentino,
• William Giarè,
• Fazlollah Hajkarim,
• Alessandro Melchiorri
• +3
• Olga Mena,
• Fabrizio Renzi,
• Seokhoon Yun
• (less)
arXiv e-prints (05/2022) e-Print:2205.07849
abstract + abstract -

We revisit the joint constraints in the mixed hot dark matter scenario in which both thermally produced QCD axions and relic neutrinos are present. Upon recomputing the cosmological axion abundance via recent advances in the literature, we improve the state-of-the-art analyses and provide updated bounds on axion and neutrino masses. By avoiding approximate methods, such as the instantaneous decoupling approximation, and limitations due to the limited validity of the perturbative approach in QCD that forced to artificially divide the constraints from the axion-pion and the axion-gluon production channels, we find robust and self-consistent limits. We investigate the two most popular axion frameworks: KSVZ and DFSZ. From Big Bang Nucleosynthesis (BBN) light element abundances data we find for the KSVZ axion $\Delta N_{\rm eff}<0.31$ and an axion mass bound $m_a < 0.53$ eV (i.e., a bound on the axion decay constant $f_a > 1.07 \times 10^7$ GeV) both at $95\%$ CL. These BBN bounds are improved to $\Delta N_{\rm eff}<0.14$ and $m_a< 0.16$ eV ($f_a > 3.56 \times 10^7$ GeV) if a prior on the baryon energy density from Cosmic Microwave Background (CMB) data is assumed. When instead considering cosmological observations from the CMB temperature, polarization and lensing from the Planck satellite combined with large scale structure data we find $\Delta N_{\rm eff}<0.23$, $m_a< 0.28$ eV ($f_a > 2.02 \times 10^7$ GeV) and $\sum m_\nu < 0.16$ eV at $95\%$ CL. This corresponds approximately to a factor of $5$ improvement in the axion mass bound with respect to the existing limits. Very similar results are obtained for the DFSZ axion. We also forecast upcoming observations from future CMB and galaxy surveys, showing that they could reach percent level errors for $m_a\sim 1$ eV.

(438)The origin of the [CII]-deficit in a simulated dwarf galaxies 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)
arXiv e-prints (05/2022) e-Print:2205.08905
abstract + abstract -

We present [CII] synthetic observations of smoothed particle hydrodynamics (SPH) simulations of a dwarf galaxy merger. The merging process varies the star-formation rate by more than three orders of magnitude. Several star clusters are formed, the feedback of which disperses and unbinds the dense gas through expanding HII regions and supernova (SN) explosions. For galaxies with properties similar to the modelled ones, we find that the [CII] emission remains optically thin throughout the merging process. We identify the Warm Neutral Medium ($3<\log T_{\rm gas}4$ with $\chi_{\rm HI}>2\chi_{\rm H2}$) to be the primary source of [CII] emission ($\sim58\%$ contribution), although at stages when the HII regions are young and dense (during star cluster formation or SNe in the form of ionized bubbles) they can contribute $\gtrsim50\%$ to the total [CII] emission. We find that the [CII]/FIR ratio decreases due to thermal saturation of the [CII] emission caused by strong FUV radiation fields emitted by the massive star clusters, leading to a [CII]-deficit medium. We investigate the [CII]-SFR relation and find an approximately linear correlation which agrees well with observations, particularly those from the Dwarf Galaxy Survey. Our simulation reproduces the observed trends of [CII]/FIR versus $\Sigma_{\rm SFR}$ and $\Sigma_{\rm FIR}$, and it agrees well with the Kennicutt relation of SFR-FIR luminosity. We propose that local peaks of [CII] in resolved observations may provide evidence for ongoing massive cluster formation.

(437)Two-loop non-planar hexa-box integrals with one massive leg
• Adam Kardos,
• Costas G. Papadopoulos,
• Alexander V. Smirnov,
• Nikolaos Syrrakos,
• Christopher Wever
Journal of High Energy Physics, 2022 (05/2022) doi:10.1007/JHEP05(2022)033
abstract + abstract -

Based on the Simplified Differential Equations approach, we present results for the two-loop non-planar hexa-box families of master integrals. We introduce a new approach to obtain the boundary terms and establish a one-dimensional integral representation of the master integrals in terms of Generalised Polylogarithms, when the alphabet contains non-factorisable square roots. The results are relevant to the study of NNLO QCD corrections for W, Z and Higgs-boson production in association with two hadronic jets.

(436)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)
arXiv e-prints (05/2022) e-Print:2205.10289
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.

(435)The role of physical and numerical viscosity in hydrodynamical instabilities
• Tirso Marin-Gilabert,
• Milena Valentini,
• Ulrich P. Steinwandel,
• Klaus Dolag
arXiv e-prints (05/2022) e-Print:2205.09135
abstract + abstract -

The evolution of the Kelvin-Helmholtz Instability (KHI) is widely used to assess the performance of numerical methods. We employ this instability to test both the smoothed particle hydrodynamics (SPH) and the meshless finite mass (MFM) implementation in OpenGadget3. We quantify the accuracy of SPH and MFM in reproducing the linear growth of the KHI with different numerical and physical set-ups. Among them, we consider: $i)$ numerical induced viscosity, and $ii)$ physically motivated, Braginskii viscosity, and compare their effect on the growth of the KHI. We find that the changes of the inferred numerical viscosity when varying nuisance parameters such as the set-up or the number of neighbours in our SPH code are comparable to the differences obtained when using different hydrodynamical solvers, i.e. MFM. SPH reproduces the expected reduction of the growth rate in the presence of physical viscosity and recovers well the threshold level of physical viscosity needed to fully suppress the instability. In the case of galaxy clusters with a virial temperature of $3\times10^7$ K, this level corresponds to a suppression factor of $\approx10^{-3}$ of the classical Braginskii value. The intrinsic, numerical viscosity of our SPH implementation in such an environment is inferred to be at least an order of magnitude smaller (i.e. $\approx10^ {-4}$), re-ensuring that modern SPH methods are suitable to study the effect of physical viscosity in galaxy clusters.

(434)B → D<SUB>1</SUB>(2420) and B → D<SUB>1</SUB><SUP>'</SUP>(2430) form factors from QCD light-cone sum rules
• Nico Gubernari,
• Alexander Khodjamirian,
• Rusa Mandal,
• Thomas Mannel
Journal of High Energy Physics, 2022 (05/2022) doi:10.1007/JHEP05(2022)029
abstract + abstract -

We perform the first calculation of form factors in the semileptonic decays B → D1(2420)ℓν and B → D1'(2430)ℓν using QCD light-cone sum rules (LCSRs) with B-meson distribution amplitudes. In this calculation the c-quark mass is finite. Analytical expressions for two-particle contributions up to twist four are obtained. To disentangle the D1 and D1' contributions in the LCSRs, we suggest a novel approach that introduces a combination of two interpolating currents for these charmed mesons. To fix all the parameters in the LCSRs, we use the two-point QCD sum rules for the decay constants of D1 and D1' mesons augmented by a single experimental input, that is the B → D1(2420)ℓν decay width. We provide numerical results for all B → D1 and B → D1' form factors. As a byproduct, we also obtain the D1- and D1'-meson decay constants and predict the lepton-flavour universality ratios R(D1) and R(D1').

(433)Euclid: Cosmological forecasts from the void size function
• S. Contarini,
• G. Verza,
• A. Pisani,
• N. Hamaus,
• M. Sahlén
• +120
• C. Carbone,
• S. Dusini,
• F. Marulli,
• L. Moscardini,
• A. Renzi,
• C. Sirignano,
• L. Stanco,
• M. Bonici,
• G. Castignani,
• H. M. Courtois,
• S. Escoffier,
• D. Guinet,
• A. Kovacs,
• G. Lavaux,
• E. Massara,
• S. Nadathur,
• G. Pollina,
• T. Ronconi,
• F. Ruppin,
• Z. Sakr,
• A. Veropalumbo,
• B. D. Wandelt,
• A. Amara,
• N. Auricchio,
• M. Baldi,
• D. Bonino,
• E. Branchini,
• M. Brescia,
• J. Brinchmann,
• S. Camera,
• V. Capobianco,
• J. Carretero,
• M. Castellano,
• S. Cavuoti,
• R. Cledassou,
• G. Congedo,
• C. J. Conselice,
• L. Conversi,
• Y. Copin,
• L. Corcione,
• F. Courbin,
• M. Cropper,
• A. Da Silva,
• H. Degaudenzi,
• F. Dubath,
• C. A. J. Duncan,
• X. Dupac,
• A. Ealet,
• S. Farrens,
• S. Ferriol,
• P. Fosalba,
• M. Frailis,
• E. Franceschi,
• B. Garilli,
• W. Gillard,
• B. Gillis,
• C. Giocoli,
• A. Grazian,
• F. Grupp,
• L. Guzzo,
• S. Haugan,
• W. Holmes,
• F. Hormuth,
• K. Jahnke,
• M. Kümmel,
• S. Kermiche,
• A. Kiessling,
• M. Kilbinger,
• M. Kunz,
• H. Kurki-Suonio,
• R. Laureijs,
• S. Ligori,
• P. B. Lilje,
• I. Lloro,
• E. Maiorano,
• O. Mansutti,
• O. Marggraf,
• K. Markovic,
• R. Massey,
• M. Melchior,
• M. Meneghetti,
• G. Meylan,
• M. Moresco,
• E. Munari,
• S. M. Niemi,
• C. Padilla,
• S. Paltani,
• F. Pasian,
• K. Pedersen,
• W. J. Percival,
• V. Pettorino,
• S. Pires,
• G. Polenta,
• M. Poncet,
• L. Popa,
• L. Pozzetti,
• F. Raison,
• J. Rhodes,
• E. Rossetti,
• R. Saglia,
• B. Sartoris,
• P. Schneider,
• A. Secroun,
• G. Seidel,
• G. Sirri,
• C. Surace,
• P. Tallada-Crespí,
• A. N. Taylor,
• I. Tereno,
• R. Toledo-Moreo,
• F. Torradeflot,
• E. A. Valentijn,
• L. Valenziano,
• Y. Wang,
• J. Weller,
• G. Zamorani,
• J. Zoubian,
• S. Andreon,
• D. Maino,
• S. Mei
• (less)
arXiv e-prints (05/2022) e-Print:2205.11525
abstract + abstract -

The Euclid mission $-$ with its spectroscopic galaxy survey covering a sky area over $15\,000 \ \mathrm{deg}^2$ in the redshift range $0.9<z<1.8\ -$ will provide a sample of tens of thousands of cosmic voids. This paper explores for the first time the constraining power of the void size function on the properties of dark energy (DE) from a survey mock catalogue, the official Euclid Flagship simulation. We identify voids in the Flagship light-cone, which closely matches the features of the upcoming Euclid spectroscopic data set. We model the void size function considering a state-of-the art methodology: we rely on the volume conserving (Vdn) model, a modification of the popular Sheth & van de Weygaert model for void number counts, extended by means of a linear function of the large-scale galaxy bias. We find an excellent agreement between model predictions and measured mock void number counts. We compute updated forecasts for the Euclid mission on DE from the void size function and provide reliable void number estimates to serve as a basis for further forecasts of cosmological applications using voids. We analyse two different cosmological models for DE: the first described by a constant DE equation of state parameter, $w$, and the second by a dynamic equation of state with coefficients $w_0$ and $w_a$. We forecast $1\sigma$ errors on $w$ lower than the $10\%$, and we estimate an expected figure of merit (FoM) for the dynamical DE scenario $\mathrm{FoM}_{w_0,w_a} = 17$ when considering only the neutrino mass as additional free parameter of the model. The analysis is based on conservative assumptions to ensure full robustness, and is a pathfinder for future enhancements of the technique. Our results showcase the impressive constraining power of the void size function from the Euclid spectroscopic sample, both as a stand-alone probe, and to be combined with other Euclid cosmological probes.

(432)The PEPSI-LBT Exoplanet Transit Survey (PETS). II. A Deep Search for Thermal Inversion Agents in KELT-20 b/MASCARA-2 b with Emission and Transmission Spectroscopy
• Marshall C. Johnson,
• Ji Wang,
• Anusha Pai Asnodkar,
• Aldo S. Bonomo,
• B. Scott Gaudi
• +17
• Thomas Henning,
• Ilya Ilyin,
• Engin Keles,
• Luca Malavolta,
• Matthias Mallonn,
• Karan Molaverdikhani,
• Valerio Nascimbeni,
• Jennifer Patience,
• Katja Poppenhaeger,
• Gaetano Scandariato,
• Everett Schlawin,
• Evgenya Shkolnik,
• Daniela Sicilia,
• Alessandro Sozzetti,
• Klaus G. Strassmeier,
• Christian Veillet,
• Fei Yan
• (less)
arXiv e-prints (05/2022) e-Print:2205.12162
abstract + abstract -

Recent observations have shown that the atmospheres of ultra hot Jupiters (UHJs) commonly possess temperature inversions, where the temperature increases with increasing altitude. Nonetheless, which opacity sources are responsible for the presence of these inversions remains largely observationally unconstrained. We used LBT/PEPSI to observe the atmosphere of the UHJ KELT-20 b in both transmission and emission in order to search for molecular agents which could be responsible for the temperature inversion. We validate our methodology by confirming a previous detection of Fe I in emission at $15.1\sigma$; however, we are unable to reproduce published detections of Fe II, Cr I, or Si I. We attribute the non-detection of Si I to the lack of lines in our bandpass, but the non-detections of Fe II and Cr I are puzzling due to our much higher signal-to-noise ratio than previous works. Our search for the inversion agents TiO, VO, FeH, and CaH results in non-detections. Using injection-recovery testing we set $4\sigma$ upper limits upon the volume mixing ratios for these constituents as low as $\sim1\times10^{-10}$ for TiO. For TiO, VO, and CaH, our limits are much lower than expectations from an equilibrium chemical model, while FeH is lower than the expectations only from a super-Solar metallicity model. We thus rule out TiO, VO, and CaH as the source of the temperature inversion in KELT-20 b, while FeH is disfavored only if KELT-20 b possesses a high-metallicity atmosphere.

(431)The effect of quasar redshift errors on Lyman-$\alpha$ forest correlation functions
• Samantha Youles,
• Julian E. Bautista,
• Andreu Font-Ribera,
• David Bacon,
• James Rich
• +28
• David Brooks,
• Tamara M. Davis,
• Kyle Dawson,
• Govinda Dhungana,
• Peter Doel,
• Kevin Fanning,
• Enrique Gaztañaga,
• Satya Gontcho A. Gontcho,
• Alma X. Gonzalez-Morales,
• Julien Guy,
• Klaus Honscheid,
• Vid Iršič,
• Robert Kehoe,
• David Kirkby,
• Theodore Kisner,
• Martin Landriau,
• Laurent Le Guillou,
• Michael E. Levi,
• Axel de la Macorra,
• Paul Martini,
• Andrea Muñoz-Gutiérrez,
• Nathalie Palanque-Delabrouille,
• Ignasi Pérez-Ràfols,
• Claire Poppett,
• César Ramírez-Pérez,
• Michael Schubnell,
• Gregory Tarlé,
• Michael Walther
• (less)
(05/2022) e-Print:2205.06648
abstract + abstract -

Using synthetic Lyman-$\alpha$ forests from the Dark Energy Spectroscopic Instrument (DESI) survey, we present a study of the impact of errors in the estimation of quasar redshift on the Lyman-$\alpha$ correlation functions. Estimates of quasar redshift have large uncertainties of a few hundred $\text{km s}^{-1}\,$ due to the broadness of the emission lines and the intrinsic shifts from other emission lines. We inject Gaussian random redshift errors into the mock quasar catalogues, and measure the auto-correlation and the Lyman-$\alpha$-quasar cross-correlation functions. We find a smearing of the BAO feature in the radial direction, but changes in the peak position are negligible. However, we see a significant unphysical correlation for small separations transverse to the line of sight which increases with the amplitude of the redshift errors. We interpret this contamination as a result of the broadening of emission lines in the measured mean continuum, caused by quasar redshift errors, combined with the unrealistically strong clustering of the simulated quasars on small scales.

(430)Can we actually constrain $f_{\rm NL}$ using the scale-dependent bias effect? An illustration of the impact of galaxy bias uncertainties using the BOSS DR12 galaxy power spectrum
• Alexandre Barreira
(05/2022) e-Print:2205.05673
abstract + abstract -

The scale-dependent bias effect on the galaxy power spectrum is a very promising probe of the local primordial non-Gaussianity (PNG) parameter $f_{\rm NL}$, but the amplitude of the effect is proportional to $f_{\rm NL}b_{\phi}$, where $b_{\phi}$ is the linear PNG galaxy bias parameter. Our knowledge of $b_{\phi}$ is currently very limited, yet nearly all existing $f_{\rm NL}$ constraints and forecasts assume precise knowledge for it. Here, we use the BOSS DR12 galaxy power spectrum to illustrate how our uncertain knowledge of $b_{\phi}$ currently prevents us from constraining $f_{\rm NL}$ with a given statistical precision $\sigma_{f_{\rm NL}}$. Assuming different fixed choices for the relation between $b_{\phi}$ and the linear density bias $b_1$, we find that $\sigma_{f_{\rm NL}}$ can vary by as much as an order of magnitude. Our strongest bound is $f_{\rm NL} = 16 \pm 16\ (1\sigma)$, while the loosest is $f_{\rm NL} = 230 \pm 226\ (1\sigma)$ for the same BOSS data. The impact of $b_{\phi}$ can be especially pronounced because it can be close to zero. We also show how marginalizing over $b_{\phi}$ with wide priors is not conservative, and leads in fact to biased constraints through parameter space projection effects. Independently of galaxy bias assumptions, the scale-dependent bias effect can only be used to detect $f_{\rm NL} \neq 0$ by constraining the product $f_{\rm NL}b_{\phi}$, but the error bar $\sigma_{f_{\rm NL}}$ remains undetermined and the results cannot be compared with the CMB; we find $f_{\rm NL}b_{\phi} \neq 0$ with $1.6\sigma$ significance. We also comment on why these issues are important for analyses with the galaxy bispectrum. Our results strongly motivate simulation-based research programs aimed at robust theoretical priors for the $b_{\phi}$ parameter, without which we may never be able to competitively constrain $f_{\rm NL}$ using galaxy data.

(429)Spectroscopic analysis of VVV CL001 cluster with MUSE
• Julio Olivares Carvajal,
• Manuela Zoccali,
• Alvaro Rojas-Arriagada,
• Rodrigo Contreras Ramos,
• Felipe Gran
• +2
• Elena Valenti,
• Javier H. Minniti
• (less)
arXiv e-prints (04/2022)
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 PMs from the VVV 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,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.

(428)SHARP - VIII. J 0924+0219 lens mass distribution and time-delay prediction through adaptive-optics imaging
• Geoff C. -F. Chen,
• Christopher D. Fassnacht,
• Sherry H. Suyu,
• Léon V. E. Koopmans,
• David J. Lagattuta
• +4
• John P. McKean,
• Matt W. Auger,
• Simona Vegetti,
• Tommaso Treu
• (less)
Monthly Notices of the Royal Astronomical Society (04/2022) doi:10.1093/mnras/stac1081
abstract + abstract -

Strongly lensed quasars can provide measurements of the Hubble constant (H0) independent of any other methods. One of the key ingredients is exquisite high-resolution imaging data, such as Hubble Space Telescope (HST) imaging and adaptive-optics (AO) imaging from ground-based telescopes, which provide strong constraints on the mass distribution of the lensing galaxy. In this work, we expand on the previous analysis of three time-delay lenses with AO imaging (RXJ 1131-1231, HE 0435-1223, and PG 1115+080), and perform a joint analysis of J 0924+0219 by using AO imaging from the Keck Telescope, obtained as part of the SHARP (Strong lensing at High Angular Resolution Program) AO effort, with HST imaging to constrain the mass distribution of the lensing galaxy. Under the assumption of a flat ΛCDM model with fixed Ωm = 0.3, we show that by marginalizing over two different kinds of mass models (power-law and composite models) and their transformed mass profiles via a mass-sheet transformation, we obtain $\Delta t_{\rm BA}=6.89\substack{+0.8\-0.7}\, h^{-1}\hat{\sigma }_{v}^{2}$ days, $\Delta t_{\rm CA}=10.7\substack{+1.6\-1.2}\, h^{-1}\hat{\sigma }_{v}^{2}$ days, and $\Delta t_{\rm DA}=7.70\substack{+1.0\-0.9}\, h^{-1}\hat{\sigma }_{v}^{2}$ days, where $h=H_{0}/100~\rm km\, s^{-1}\, Mpc^{-1}$ is the dimensionless Hubble constant and $\hat{\sigma }_{v}=\sigma ^{\rm ob}_{v}/(280~\rm km\, s^{-1})$ is the scaled dimensionless velocity dispersion. Future measurements of time delays with 10 per cent uncertainty and velocity dispersion with 5 per cent uncertainty would yield a H0 constraint of ~15 per cent precision.

(427)On the Superiority of the $|V_{cb}|-\gamma$ Plots over the Unitarity Triangle Plots in the 2020s
• Andrzej J. Buras
arXiv e-prints (04/2022)
abstract + abstract -

The UT plots played already for three decades an important role in the tests of the SM and the determination of the CKM parameters. As of 2022, among the four CKM parameters, $V_{us}$ and $\beta$ are already measured with respectable precision, while this is not the case of $|V_{cb}|$ and $\gamma$. In the case of $|V_{cb}|$ the main obstacle are the significant tensions between its inclusive and exclusive determinations from tree-level decays. The present uncertainty in $\gamma$ of $4^\circ$ from tree-level decays will be reduced to $1^\circ$ by the LHCb and Belle II collaborations in the coming years. Unfortunately in the UT plots $|V_{cb}|$ is not seen and the experimental improvements in the determination of $\gamma$ from tree-level decays at the level of a few degrees are difficult to appreciate. In view of these deficiencies of the UT plots with respect to $|V_{cb}|$ and $\gamma$ and the central role these two CKM parameters will play in this decade, the recently proposed plots of $|V_{cb}|$ versus $\gamma$ extracted from various processes appear to be superior to the UT plots in the flavour phenomenology. We illustrate this idea with $\Delta M_s$, $\Delta M_d$, $\epsilon_K$ and with rare decays $B_s\to\mu^+\mu^-$, $B_d\to\mu^+\mu^-$, $K^+\to \pi^+\nu\bar\nu$ and $K_L\to\pi^0\nu\bar\nu$. The power of $\epsilon_K$, $K^+\to\pi^+\nu\bar\nu)$ and $K_{L}\to\pi^0\nu\bar\nu)$ in the determination of $|V_{cb}|$, due to their strong dependence on $|V_{cb}|$, is transparently exhibited in this manner. Combined with future reduced errors on $\gamma$ and $|V_{cb}|$ from tree-level decays such plots can better exhibit possible inconsistenices between various determinations of these two parameters, caused by new physics, than it is possible with the UT plots. This can already be illustrated on the example of the $2.7\sigma$ anomaly in $B_s\to\mu^+\mu^-$.

(426)Gaia EDR3 distances of the young stellar clusters in the extended Carina Nebula complex
• C. Göppl,
• T. Preibisch
Astronomy and Astrophysics, 660, p11 (04/2022) doi:10.1051/0004-6361/202142576
abstract + abstract -

Context. The Carina Nebula complex (CNC) is one of the most massive and active star-forming regions in our Galaxy and it contains several large young star clusters. The distances of the individual clusters and their physical connection were poorly known up to now, with strongly discrepant results reported in the literature.
Aims: We want to determine reliable distances of the young stellar clusters in the central Carina Nebula region (in particular, Tr 14, 15, and 16) and the prominent clusters NGC 3324 and NGC 3293 in the northwestern periphery of the CNC.
Methods: We analyzed the parallaxes in Gaia EDR3 for a comprehensive sample of 237 spectroscopically identified OB stars, as well as for 9562 X-ray-selected young stars throughout the complex. We also performed an astrometric analysis to identify members of the young cluster vdBH 99, which is located in the foreground of the northwestern part of the Carina Nebula.
Results: We find that the distances of the investigated clusters in the CNC are equal within ≤2%, and yield very consistent most likely mean distance values of 2.36−0.05+0.05 kpc for the OB star sample and 2.34−0.06+0.05 kpc for the sample of X-ray-selected young stars.
Conclusions: Our results show that the clusters in the CNC constitute a coherent star-forming region, in particular with regard to NGC 3324 and NGC 3293 at the northwestern periphery, which are (within ≤2%) at the same distance as the central Carina Nebula. For the foreground cluster vdBH 99, we find a mean distance of 441−2+2 pc and an age of ≃60 Myr. We quantified the contamination of X-ray-selected samples of Carina Nebula stars based on members of this foreground cluster.

Table 1 is 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/660/A11

(425)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)
arXiv e-prints (04/2022)
abstract + abstract -

In this paper, we 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. We compare several zoom-in re-simulations of a sub-sample of the cluster-sized haloes studied in Meneghetti et al. (2020), obtained by varying mass resolution, softening length and AGN energy feedback scheme. We study the impact of these different setups on the subhalo abundances, their radial distribution, their density and mass profiles and the relation between the maximum circular velocity, which is a proxy for subhalo compactness. Regardless of the adopted numerical resolution and feedback model, subhaloes with masses Msub < 1e11Msun/h, the most relevant mass-range for galaxy-galaxy strong lensing, have maximum circular velocities ~30% smaller than those measured from strong lensing observations of Bergamini et al. (2019). We also find that simulations with less effective AGN energy feedback produce massive subhaloes (Msub> 1e11 Msun/h ) with higher maximum circular velocity and that their Vmax - Msub 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 subhaloes is the result of an extremely over-efficient star formation in their cores, also leading to larger-than-observed subhalo stellar mass. We conclude that 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 from the analysis of Meneghetti et al. (2020) persists. It remains an open question as to whether such a discrepancy reflects limitations of the current implementation of galaxy formation models or the LCDM paradigm.

(424)Same-hemisphere three-gluon-emission contribution to the zero-jettiness soft function at N3LO QCD
• Daniel Baranowski,
• Maximilian Delto,
• Kirill Melnikov,
• Chen-Yu Wang
arXiv e-prints (04/2022)
abstract + abstract -

We complete the calculation of the three-gluon-emission contribution to the same-hemisphere part of the zero-jettiness soft function at next-to-next-to-next-to-leading order in perturbative QCD.

(423)Signatures of the Many Supermassive Black Hole Mergers in a Cosmologically Forming Massive Early-type Galaxy
• Matias Mannerkoski,
• Peter H. Johansson,
• Antti Rantala,
• Thorsten Naab,
• Shihong Liao
• +1
The Astrophysical Journal, 929, p9 (04/2022) doi:10.3847/1538-4357/ac5f0b
abstract + abstract -

We model here the merger histories of the supermassive black hole (SMBH) population in the late stages of a cosmological simulation of a ~ 2 × 1013 M galaxy group. The gravitational dynamics around the several tens of SMBHs (M > 7.5 × 107 M ) hosted by the galaxies in the group is computed at high accuracy using regularized integration with the KETJU code. The 11 SMBHs that form binaries and a hierarchical triplet eventually merge after hardening through dynamical friction, stellar scattering, and gravitational wave (GW) emission. The binaries form at eccentricities of e ~ 0.3-0.9, with one system evolving to a very high eccentricity of e = 0.998, and merge on timescales of a few tens to several hundred megayears. During the simulation, the merger-induced GW recoil kicks eject one SMBH remnant from the central host galaxy. This temporarily drives the galaxy off the M relation; however, the galaxy returns to the relation due to subsequent galaxy mergers, which bring in new SMBHs. This showcases a possible mechanism contributing to the observed scatter of the M relation. Finally, we show that pulsar timing arrays and LISA would be able to detect parts of the GW signals from the SMBH mergers that occur during the ~4 Gyr time span simulated with KETJU.

(422)Analytical evaluation of cosmological correlation functions
• T. Heckelbacher,
• I. Sachs,
• E. Skvortsov,
• P. Vanhove
arXiv e-prints (04/2022)
abstract + abstract -

Using the Schwinger-Keldysh-formalism, reformulated in arXiv:2108.01695 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.

(421)Lattice Simulations of Axion-U(1) Inflation
• Angelo Caravano,
• Eiichiro Komatsu,
• Kaloian D. Lozanov,
• Jochen Weller
arXiv e-prints (04/2022)
abstract + abstract -

If gauge fields are coupled to an axion field during inflation, they can lead to unique observational signatures. However, this system often shows strong backreaction effects, invalidating the standard perturbation theory approach. In this work, we present the first nonlinear lattice simulation of an axion-U(1) system during inflation. We use it to fully characterize the statistics of the comoving curvature perturbation $\zeta$. We find that non-Gaussianity of $\zeta$ is large in the linear regime, whereas it is suppressed when the dynamics becomes nonlinear. This relaxes bounds from overproduction of primordial black holes, allowing for an observable gravitational waves signal at interferometer scales.

(420)A spectroscopic study of blue supergiant stars in Local Group spiral galaxies: Andromeda and Triangulum
• Cheng Liu,
• Rolf-Peter Kudritzki,
• Gang Zhao,
• Miguel A. Urbaneja,
• Yang Huang
• +2
arXiv e-prints (04/2022)
abstract + abstract -

Low-resolution LAMOST and Keck spectra of blue supergiant stars distributed over the disks of the Local Group spiral galaxies M 31 and M 33 are analyzed to determine stellar effective temperatures, gravities, metallicities, and reddening. Logarithmic metallicities at the center of the galaxies (in solar units) of $0.30\pm0.09$ and $0.11\pm0.04$ and metallicity gradients of $-0.37\pm0.13$ dex/$R_{25}$ and $-0.36\pm0.16$ dex/$R_{25}$ are measured for M 31 and M 33, respectively. For M 33 the 2-dimensional distribution of metallicity indicates a deviation from azimutal symmetry with an off-centre peak. The flux-weighted gravity-luminosity relationship of blue supergiant stars is used to determine a distance modulus of 24.51$\pm$0.13 mag for M 31 and 24.93$\pm$0.07 mag for M 33. For M 31 the flux-weighted gravity--luminosity relationship (FGLR) distance agrees well with other methods. For M 33 the FGLR-based distance is larger than the distances from Cepheids studies but it is in good agreement with work on eclipsing binaries, planetary nebulae , long-period variables, and the tip of the red giant branch.

(419)From B-meson anomalies to Kaon physics with scalar leptoquarks
• David Marzocca,
• Sokratis Trifinopoulos,
• Elena Venturini
European Physical Journal C, 82 (04/2022) doi:10.1140/epjc/s10052-022-10271-7
abstract + abstract -

In this work we study possible connections between B-meson anomalies and Kaon physics observables in the context of combined solutions with the singlet and triplet scalar leptoquarks S1 and S3. By assuming a flavor structure for the leptoquark couplings dictated by a minimally broken U (2) 5 flavor symmetry we can make a sharp connection between these two classes of observables. We find that the bound on B (K+→π+ν ν ) from NA62 puts already some tension in the model, while the present limits on B (KL→μ+μ-) and μ →e conversion in nuclei can be saturated. Relaxing instead the flavor assumption we study what values for B (K+→π+ν ν ) , as well as for B (KL→π0ν ν ) and B (KL ,S→μ+μ-) , are viable compatibly with all other phenomenological constraints.

(418)The bright extragalactic ALMA redshift survey (BEARS) I: redshifts of bright gravitationally lensed galaxies from the Herschel ATLAS
• S. A. Urquhart,
• G. J. Bendo,
• S. Serjeant,
• T. Bakx,
• M. Hagimoto
• +51
• P. Cox,
• R. Neri,
• M. Lehnert,
• C. Sedgwick,
• C. Weiner,
• H. Dannerbauer,
• A. Amvrosiadis,
• P. Andreani,
• A. J. Baker,
• A. Beelen,
• S. Berta,
• E. Borsato,
• V. Buat,
• K. M. Butler,
• A. Cooray,
• G. De Zotti,
• L. Dunne,
• S. Dye,
• S. Eales,
• A. Enia,
• L. Fan,
• R. Gavazzi,
• J. González-Nuevo,
• A. I. Harris,
• C. N. Herrera,
• D. Hughes,
• D. Ismail,
• R. Ivison,
• S. Jin,
• B. Jones,
• K. Kohno,
• M. Krips,
• G. Lagache,
• L. Marchetti,
• M. Massardi,
• H. Messias,
• M. Negrello,
• A. Omont,
• I. Perez-Fournon,
• D. A. Riechers,
• D. Scott,
• M. W. L. Smith,
• F. Stanley,
• Y. Tamura,
• P. Temi,
• C. Vlahakis,
• A. Weiß,
• P. van der Werf,
• A. Verma,
• C. Yang,
• A. J. Young
• (less)
Monthly Notices of the Royal Astronomical Society, 511, p17 (04/2022) doi:10.1093/mnras/stac150
abstract + abstract -

We present spectroscopic measurements for 71 galaxies associated with 62 of the brightest high-redshift submillimetre sources from the Southern fields of the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS), while targeting 85 sources which resolved into 142. We have obtained robust redshift measurements for all sources using the 12-m Array and an efficient tuning of ALMA to optimize its use as a redshift hunter, with 73 per cent of the sources having a robust redshift identification. Nine of these redshift identifications also rely on observations from the Atacama Compact Array. The spectroscopic redshifts span a range 1.41 < z < 4.53 with a mean value of 2.75, and the CO emission line full-width at half-maxima range between $\rm 110\, km\, s^{-1} \lt FWHM \lt 1290\, km\, s^{-1}$ with a mean value of ~500 km s-1, in line with other high-z samples. The derived CO(1-0) luminosity is significantly elevated relative to line-width to CO(1-0) luminosity scaling relation, which is suggestive of lensing magnification across our sources. In fact, the distribution of magnification factors inferred from the CO equivalent widths is consistent with expectations from galaxy-galaxy lensing models, though there is a hint of an excess at large magnifications that may be attributable to the additional lensing optical depth from galaxy groups or clusters.

(417)Effects of boosting on extragalactic components: Methods and statistical studies
• William Coulton,
• Sydney Feldman,
• Karime Maamari,
• Elena Pierpaoli,
• Siavash Yasini
• +1
Monthly Notices of the Royal Astronomical Society (04/2022) doi:10.1093/mnras/stac1017
abstract + abstract -

In this work we examine the impact of our motion with respect to the CMB rest frame on statistics of CMB maps by examining the one-, two-, three- and four- point statistics of simulated maps of the CMB and Sunyaev-Zeldovich (SZ) effects. We validate boosting codes by comparing their outcomes for temperature and polarization power spectra up to ℓ ≃ 6000. We derive and validate a new analytical formula for the computation of the boosted power spectrum of a signal with a generic frequency dependence. As an example we show how this increases the boosting correction to the power spectrum of CMB intensity measurements by $\sim 30{\rm{ per\ cent}}$ at 150 GHz. We examine the effect of boosting on thermal and kinetic SZ power spectra from semianalytical and hydrodynamical simulations; the boosting correction is generally small for both simulations, except when considering frequencies near the tSZ null. For the non-Gaussian statistics, in general we find that boosting has no impact with two exceptions. We find that, whilst the statistics of the CMB convergence field are unaffected, quadratic estimators that are used to measure this field can become biased at the $O(1){\rm{ per\ cent}}$ level by boosting effects. We present a simple modification to the standard estimators that removes this bias. Second, bispectrum estimators can receive a systematic bias from the Doppler induced quadrupole when there is anisotropy in the sky - in practice this anisotropy comes from masking and inhomegenous noise. This effect is unobservable and already removed by existing analysis methods.

(416)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 (04/2022) 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.

(415)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
arXiv e-prints (04/2022)
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 which 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, that 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 $\Delta=200,500,1000$ 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-fit profile, that 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.

(414)Surface Brightness Profile of Lyman-α Halos out to 320 kpc in HETDEX
• Maja Lujan Niemeyer,
• Eiichiro Komatsu,
• Chris Byrohl,
• Dustin Davis,
• Maximilian Fabricius
• +16
• Karl Gebhardt,
• Gary J. Hill,
• Lutz Wisotzki,
• William P. Bowman,
• Robin Ciardullo,
• Daniel J. Farrow,
• Steven L. Finkelstein,
• Eric Gawiser,
• Caryl Gronwall,
• Donghui Jeong,
• Martin Landriau,
• Chenxu Liu,
• Erin Mentuch Cooper,
• Masami Ouchi,
• Donald P. Schneider,
• Gregory R. Zeimann
• (less)
The Astrophysical Journal, 929, p11 (04/2022) doi:10.3847/1538-4357/ac5cb8
abstract + abstract -

We present the median-stacked Lyman-α (Lyα) surface brightness profiles of 968 spectroscopically selected Lyα emitting galaxies (LAEs) at redshifts 1.9 < z < 3.5 in the early data of the Hobby-Eberly Telescope Dark Energy Experiment. The selected LAEs are high-confidence Lyα detections with high signal-to-noise ratios observed with good seeing conditions (point-spread function FWHM <1.″4), excluding active galactic nuclei. The Lyα luminosities of the LAEs are 1042.4-1043 erg s-1. We detect faint emission in the median-stacked radial profiles at the level of <?CDATA $(3.6\pm 1.3)\times {10}^{-20}\,\mathrm{erg}\,{{\rm{s}}}^{-1}\,{\mathrm{cm}}^{-2}\,{\mathrm{arcsec}}^{-2}$?> from the surrounding Lyα halos out to r ≃ 160 kpc (physical). The shape of the median-stacked radial profile is consistent at r < 80 kpc with that of much fainter LAEs at 3 < z < 4 observed with the Multi Unit Spectroscopic Explorer (MUSE), indicating that the median-stacked Lyα profiles have similar shapes at redshifts 2 < z < 4 and across a factor of 10 in Lyα luminosity. While we agree with the results from the MUSE sample at r < 80 kpc, we extend the profile over a factor of two in radius. At r > 80 kpc, our profile is flatter than the MUSE model. The measured profile agrees at most radii with that of galaxies in the Byrohl et al. cosmological radiative transfer simulation at z = 3. This suggests that the surface brightness of a Lyα halo at r ≲ 100 kpc is dominated by resonant scattering of Lyα photons from star-forming regions in the central galaxy, whereas at r > 100 kpc, it is dominated by photons from galaxies in surrounding dark matter halos.

(413)Dust evolution in cosmological simulations
• Massimiliano Parente,
• Cinthia Ragone-Figueroa,
• Gian Luigi Granato,
• Stefano Borgani,
• Giuseppe Murante
• +3
• Milena Valentini,
• Alessandro Bressan,
• Andrea Lapi
• (less)
(04/2022) e-Print:2204.11884
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 AGN feedback. We tune the parameters ruling direct dust production from evolved stars and accretion in the inter stellar 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.

(412)Glueball molecules
• Alexey A. Petrov
(04/2022) e-Print:2204.11269
abstract + abstract -

Experimental searches for pure glueball states have proven challenging and so far yielded no results. This is believed to occur because glueballs mix with the ordinary $q\bar q$ states with the same quantum numbers. We will discuss an alternative mechanism, the formation of the glueball-meson molecular states. We will argue that the wave functions of already observed excited meson states may contain a significant part due to such molecular states. We discuss the phenomenology of glueball molecules and comment on a possible charmless component of the $XYZ$ states.

(411)Multi-Component Imaging of the Fermi Gamma-ray Sky in the Spatio-spectral Domain
• Lukas I. Platz,
• Jakob Knollmüller,
• Philipp Arras,
• Philipp Frank,
• Martin Reinecke
• +2
• Dominik Jüstel,
• Torsten A. Enßlin
• (less)
(04/2022) e-Print:2204.09360
abstract + abstract -

We perform two distinct spatio-spectral reconstructions of the gamma-ray sky in the range of 0.56-316 GeV based on Fermi Large Area Telescope (LAT) data. Both describe the sky brightness to be composed of a diffuse-emission and a point-source component. The first model requires minimal assumptions and provides a template-free reconstruction as a reference. It makes use of spatial and spectral correlations to distinguish between the different components. The second model is physics-informed and further differentiates between diffuse emission of hadronic and leptonic origin. For this, we assume parametric, but spatially varying energy spectra to distinguish between the processes and use thermal Galactic dust observations to indicate the preferred sites of hadronic interactions. To account for instrumental effects we model the point-spread, the energy dispersion, and the exposure of the telescope throughout the observation. The reconstruction problem is formulated as a Bayesian inference task, that is solved by variational inference. We show decompositions of the Gamma-ray flux into diffuse and point-like emissions, and of the diffuse emissions into multiple physically motivated components. The diffuse decomposition provides an unprecedented view of the Galactic leptonic diffuse emission. It shows the Fermi bubbles and their spectral variations in high fidelity and other areas exhibiting strong cosmic ray electron contents, such as a thick disk in the inner Galaxy and outflow regions. Furthermore, we report a hard spectrum gamma ray arc in the northern outer bubble co-spatial with the reported X-ray arc by the eROSITA collaboration. All our spatio-spectral sky reconstructions and their uncertainty quantification are publicly available.

(410)DeepZipper II: Searching for Lensed Supernovae in Dark Energy Survey Data with Deep Learning
• R. Morgan,
• B. Nord,
• K. Bechtol,
• A. Möller,
• W.G. Hartley
• +62
• S. Birrer,
• S.J. González,
• M. Martinez,
• R.A. Gruendl,
• E.J. Buckley-Geer,
• A.J. Shajib,
• A. Carnero Rosell,
• C. Lidman,
• T. Collett,
• T.M.C. Abbott,
• M. Aguena,
• F. Andrade-Oliveira,
• J. Annis,
• D. Bacon,
• S. Bocquet,
• D. Brooks,
• D.L. Burke,
• M. Carrasco Kind,
• J. Carretero,
• F.J. Castander,
• C. Conselice,
• L.N. da Costa,
• M. Costanzi,
• J. De Vicente,
• S. Desai,
• P. Doel,
• S. Everett,
• I. Ferrero,
• B. Flaugher,
• D. Friedel,
• J. Frieman,
• J. García-Bellido,
• E. Gaztanaga,
• D. Gruen,
• G. Gutierrez,
• S.R. Hinton,
• D.L. Hollowood,
• K. Honscheid,
• K. Kuehn,
• N. Kuropatkin,
• O. Lahav,
• M. Lima,
• F. Menanteau,
• R. Miquel,
• A. Palmese,
• F. Paz-Chinchón,
• M.E.S. Pereira,
• A. Pieres,
• A.A. Plazas Malagón,
• J. Prat,
• M. Rodriguez-Monroy,
• A.K. Romer,
• A. Roodman,
• E. Sanchez,
• V. Scarpine,
• I. Sevilla-Noarbe,
• M. Smith,
• E. Suchyta,
• M.E.C. Swanson,
• G. Tarle,
• D. Thomas,
• T.N. Varga
• (less)
(04/2022) e-Print:2204.05924
abstract + abstract -

Gravitationally lensed supernovae (LSNe) are important probes of cosmic expansion, but they remain rare and difficult to find. Current cosmic surveys likely contain and 5-10 LSNe in total while next-generation experiments are expected to contain several hundreds to a few thousands of these systems. We search for these systems in observed Dark Energy Survey (DES) 5-year SN fields -- 10 3-sq. deg. regions of sky imaged in the $griz$ bands approximately every six nights over five years. To perform the search, we utilize the DeepZipper approach: a multi-branch deep learning architecture trained on image-level simulations of LSNe that simultaneously learns spatial and temporal relationships from time series of images. We find that our method obtains a LSN recall of 61.13% and a false positive rate of 0.02% on the DES SN field data. DeepZipper selected 2,245 candidates from a magnitude-limited ($m_i$ $<$ 22.5) catalog of 3,459,186 systems. We employ human visual inspection to review systems selected by the network and find three candidate LSNe in the DES SN fields.

(409)Reevaluation of the cosmic antideuteron flux from cosmic-ray interactions and from exotic sources
• Laura ŠerkšnytÄ--,
• Stephan Königstorfer,
• Philip von Doetinchem,
• Laura Fabbietti,
• Diego Mauricio Gomez-Coral
• +6
• Johannes Herms,
• Alejandro Ibarra,
• Thomas Pöschl,
• Anirvan Shukla,
• Andrew Strong,
• Ivan Vorobyev
• (less)
Physical Review D, 105 (04/2022) doi:10.1103/PhysRevD.105.083021
abstract + abstract -

Cosmic-ray antideuterons could be a key for the discovery of exotic phenomena in our Galaxy, such as dark-matter annihilations or primordial black hole evaporation. Unfortunately the theoretical predictions of the antideuteron flux at Earth are plagued with uncertainties from the mechanism of antideuteron production and propagation in the Galaxy. We present the most up-to-date calculation of the antideuteron fluxes from cosmic-ray collisions with the interstellar medium and from exotic processes. We include for the first time the antideuteron inelastic interaction cross section recently measured by the ALICE collaboration to account for the loss of antideuterons during propagation. In order to bracket the uncertainty in the expected fluxes, we consider several state-of-the-art models of antideuteron production and of cosmic-ray propagation.

(408)The Galactic 3D large-scale dust distribution via Gaussian process regression on spherical coordinates
• R. H. Leike,
• G. Edenhofer,
• J. Knollmüller,
• C. Alig,
• P. Frank
• +1
arXiv e-prints (04/2022) e-Print:2204.11715
abstract + abstract -

Knowing the Galactic 3D dust distribution is relevant for understanding many processes in the interstellar medium and for correcting many astronomical observations for dust absorption and emission. Here, we aim for a 3D reconstruction of the Galactic dust distribution with an increase in the number of meaningful resolution elements by orders of magnitude with respect to previous reconstructions, while taking advantage of the dust's spatial correlations to inform the dust map. We use iterative grid refinement to define a log-normal process in spherical coordinates. This log-normal process assumes a fixed correlation structure, which was inferred in an earlier reconstruction of Galactic dust. Our map is informed through 111 Million data points, combining data of PANSTARRS, 2MASS, Gaia DR2 and ALLWISE. The log-normal process is discretized to 122 Billion degrees of freedom, a factor of 400 more than our previous map. We derive the most probable posterior map and an uncertainty estimate using natural gradient descent and the Fisher-Laplace approximation. The dust reconstruction covers a quarter of the volume of our Galaxy, with a maximum coordinate distance of $16\,\text{kpc}$, and meaningful information can be found up to at distances of $4\,$kpc, still improving upon our earlier map by a factor of 5 in maximal distance, of $900$ in volume, and of about eighteen in angular grid resolution. Unfortunately, the maximum posterior approach chosen to make the reconstruction computational affordable introduces artifacts and reduces the accuracy of our uncertainty estimate. Despite of the apparent limitations of the presented 3D dust map, a good part of the reconstructed structures are confirmed by independent maser observations. Thus, the map is a step towards reliable 3D Galactic cartography and already can serve for a number of tasks, if used with care.

(407)The probability of galaxy-galaxy strong lensing events in hydrodynamical simulations of galaxy clusters
• Massimo Meneghetti,
• Antonio Ragagnin,
• Stefano Borgani,
• Francesco Calura,
• Giulia Despali
• +25
• Carlo Giocoli,
• Gian Luigi Granato,
• Claudio Grillo,
• Lauro Moscardini,
• Elena Rasia,
• Piero Rosati,
• Giuseppe Angora,
• Luigi Bassini,
• Pietro Bergamini,
• Gabriel B. Caminha,
• Giovanni Granata,
• Amata Mercurio,
• Robert Benton Metcalf,
• Priyamvada Natarajan,
• Mario Nonino,
• Giada Venusta Pignataro,
• Cinthia Ragone-Figueroa,
• Eros Vanzella,
• Ana Acebron,
• Klaus Dolag,
• Giuseppe Murante,
• Giuliano Taffoni,
• Luca Tornatore,
• Luca Tortorelli,
• Milena Valentini
• (less)
arXiv e-prints (04/2022) e-Print:2204.09065
abstract + abstract -

Meneghetti et al. (2020) recently reported an excess of galaxy-galaxy strong lensing (GGSL) in galaxy clusters compared to expectations from the LCDM cosmological model. Theoretical estimates of the GGSL probability are based on the analysis of numerical hydrodynamical simulations in the LCDM cosmology. We quantify the impact of the numerical resolution and AGN feedback scheme adopted in cosmological simulations on the predicted GGSL probability and determine if varying these simulation properties can alleviate the gap with observations. We repeat the analysis of Meneghetti et al. (2020) on cluster-size halos simulated with different mass and force resolutions and implementing several independent AGN feedback schemes. We find that improving the mass resolution by a factor of ten and twenty-five, while using the same galaxy formation model that includes AGN feedback, does not affect the GGSL probability. We find similar results regarding the choice of gravitational softening. On the contrary, adopting an AGN feedback scheme that is less efficient at suppressing gas cooling and star formation leads to an increase in the GGSL probability by a factor between three and six. However, we notice that such simulations form overly massive subhalos whose contribution to the lensing cross-section would be significant while their Einstein radii are too large to be consistent with the observations. The primary contributors to the observed GGSL cross-sections are subhalos with smaller masses, that are compact enough to become critical for lensing. The population with these required characteristics appears to be absent in simulations.

(406)Detection of CO emission lines in the dayside atmospheres of WASP-33b and WASP-189b with GIANO
• F. Yan,
• E. Pallé,
• A. Reiners,
• N. Casasayas-Barris,
• D. Cont
• +6
• M. Stangret,
• L. Nortmann,
• P. Mollière,
• Th. Henning,
• G. Chen,
• K. Molaverdikhani
• (less)
arXiv e-prints (04/2022) e-Print:2204.10158
abstract + abstract -

Ultra-hot Jupiters (UHJs) are expected to possess temperature inversion layers in their dayside atmospheres. Recent thermal emission observations have discovered several atomic and molecular species along with temperature inversions in UHJs. We observed the thermal emission spectra of two UHJs (WASP-33b and WASP-189b) with the GIANO-B high-resolution near-infrared spectrograph. Using the cross-correlation technique, we detected carbon monoxide (CO) in the dayside atmospheres of both planets. The detected CO lines are in emission, which agrees with previous discoveries of iron emission lines and temperature inversions in the two planets. This is the first detection of CO lines in emission with high-resolution spectroscopy. Further retrieval work combining the CO lines with other spectral features will enable a comprehensive understanding of the atmospheric properties such as temperature structures and C/O ratios. The detected CO and iron emission lines of WASP-189b have redshifted radial velocities of several km/s, which likely originate from a dayside to nightside wind in its atmosphere. Such a redshifted velocity has not been detected for the emission lines of WASP-33b, suggesting that the atmospheric circulation patterns of the two UHJs may be different.

(405)New Constraint on Early Dark Energy from Planck and BOSS Data Using the Profile Likelihood
• Laura Herold,
• Elisa G. M. Ferreira,
• Eiichiro Komatsu
The Astrophysical Journal, 929, p6 (04/2022) doi:10.3847/2041-8213/ac63a3
abstract + abstract -

A dark energy-like component in the early universe, known as early dark energy (EDE), is a proposed solution to the Hubble tension. Currently, there is no consensus in the literature as to whether EDE can simultaneously solve the Hubble tension and provide an adequate fit to the data from the cosmic microwave background (CMB) and large-scale structure of the universe. In this work, we deconstruct the current constraints from the Planck CMB and the full-shape clustering data of the Baryon Oscillation Spectroscopic Survey to understand the origin of different conclusions in the literature. We use two different analyses, a grid sampling and a profile likelihood, to investigate whether the current constraints suffer from volume effects upon marginalization and are biased toward some values of the EDE fraction, f EDE. We find that the f EDE allowed by the data strongly depends on the particular choice of the other parameters of the model, and that several choices of these parameters prefer larger values of f EDE than in the Markov Chain Monte Carlo analysis. This suggests that volume effects are the reason behind the disagreement in the literature. Motivated by this, we use a profile likelihood to analyze the EDE model and compute a confidence interval for f EDE, finding f EDE = 0.072 ± 0.036 (68% C.L.). Our approach gives a confidence interval that is not subject to volume effects and provides a powerful tool to understand whether EDE is a possible solution to the Hubble tension.

(404)Moment expansion of polarized dust SED: A new path towards capturing the CMB B-modes with LiteBIRD
• L. Vacher,
• J. Aumont,
• L. Montier,
• S. Azzoni,
• F. Boulanger
• +1
Astronomy and Astrophysics, 660, p21 (04/2022) doi:10.1051/0004-6361/202142664
abstract + abstract -

Accurate characterization of the polarized dust emission from our Galaxy will be decisive in the quest for the cosmic microwave background (CMB) primordial B-modes. An incomplete modeling of its potentially complex spectral properties could lead to biases in the CMB polarization analyses and to a spurious measurement of the tensor-to-scalar ratio r. It is particularly crucial for future surveys like the LiteBIRD satellite, the goal of which is to constrain the faint primordial signal leftover by inflation with an accuracy on the tensor-to-scalar ratio r of the order of 10−3. Variations of the dust properties along and between lines of sight lead to unavoidable distortions of the spectral energy distribution (SED) that cannot be easily anticipated by standard component-separation methods. This issue can be tackled using a moment expansion of the dust SED, an innovative parametrization method imposing minimal assumptions on the sky complexity. In the present paper, we apply this formalism to the B-mode cross-angular power spectra computed from simulated LiteBIRD polarization data at frequencies between 100 and 402 GHz that contain CMB, dust, and instrumental noise. The spatial variation of the dust spectral parameters (spectral index β and temperature T) in our simulations lead to significant biases on r (∼21 σr) if not properly taken into account. Performing the moment expansion in β, as in previous studies, reduces the bias but does not lead to sufficiently reliable estimates of r. We introduce, for the first time, the expansion of the cross-angular power spectra SED in both β and T, showing that, at the sensitivity of LiteBIRD, the SED complexity due to temperature variations needs to be taken into account in order to prevent analysis biases on r. Thanks to this expansion, and despite the existing correlations between some of the dust moments and the CMB signal responsible for a rise in the error on r, we can measure an unbiased value of the tensor-to-scalar ratio with a dispersion as low as σr = 8.8 × 10−4.

(403)Dust evolution in cosmological simulations
• Massimiliano Parente,
• Cinthia Ragone-Figueroa,
• Gian Luigi Granato,
• Stefano Borgani,
• Giuseppe Murante
• +3
• Milena Valentini,
• Alessandro Bressan,
• Andrea Lapi
• (less)
arXiv e-prints (04/2022) e-Print:2204.11884
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 AGN feedback. We tune the parameters ruling direct dust production from evolved stars and accretion in the inter stellar 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.

(402)Planar three-loop master integrals for 2 → 2 processes with one external massive particle
• Dhimiter D. Canko,
• Nikolaos Syrrakos
Journal of High Energy Physics, 2022 (04/2022) doi:10.1007/JHEP04(2022)134
abstract + abstract -

We present analytic results for the two tennis-court integral families relevant to 2 → 2 scattering processes involving one massive external particle and massless propagators in terms of Goncharov polylogarithms of up to transcendental weight six. We also present analytic results for physical kinematics for the ladder-box family and the two tennis-court families in terms of real-valued polylogarithmic functions, making our solutions well-suited for phenomenological applications.

(401)Loop counting matters in SMEFT
• G. Buchalla,
• G. Heinrich,
• Ch. Müller-Salditt,
• F. Pandler
arXiv e-prints (04/2022) e-Print:2204.11808
abstract + abstract -

We show that, in addition to the counting of canonical dimensions, a counting of loop orders is necessary to fully specify the power counting of Standard Model Effective Field Theory (SMEFT). Using concrete examples, we demonstrate that considering the canonical dimensions of operators alone may lead to inconsistent results. The counting of both, canonical dimensions and loop orders, establishes a clear hierarchy of the terms in SMEFT. In practice, this serves to identify, and focus on, the potentially dominating effects in any given high-energy process in a meaningful way. Additionally, this will lead to a consistent limitation of free parameters in SMEFT applications.

(400)Stable nickel production in type Ia supernovae: A smoking gun for the progenitor mass?
• S. Blondin,
• E. Bravo,
• F. X. Timmes,
• L. Dessart,
• D. J. Hillier
Astronomy and Astrophysics, 660, p19 (04/2022) doi:10.1051/0004-6361/202142323
abstract + abstract -

Context. At present, there are strong indications that white dwarf (WD) stars with masses well below the Chandrasekhar limit (MCh ≈ 1.4 M) contribute a significant fraction of SN Ia progenitors. The relative fraction of stable iron-group elements synthesized in the explosion has been suggested as a possible discriminant between MCh and sub-MCh events. In particular, it is thought that the higher-density ejecta of MCh WDs, which favours the synthesis of stable isotopes of nickel, results in prominent [Ni II] lines in late-time spectra (≳150 d past explosion).
Aims: We study the explosive nucleosynthesis of stable nickel in SNe Ia resulting from MCh and sub-MCh progenitors. We explore the potential for lines of [Ni II] in the optical an near-infrared (at 7378 Å and 1.94 μm) in late-time spectra to serve as a diagnostic of the exploding WD mass.
Methods: We reviewed stable Ni yields across a large variety of published SN Ia models. Using 1D MCh delayed-detonation and sub-MCh detonation models, we studied the synthesis of stable Ni isotopes (in particular, 58Ni) and investigated the formation of [Ni II] lines using non-local thermodynamic equilibrium radiative-transfer simulations with the CMFGEN code.
Results: We confirm that stable Ni production is generally more efficient in MCh explosions at solar metallicity (typically 0.02-0.08 M for the 58Ni isotope), but we note that the 58Ni yield in sub-MCh events systematically exceeds 0.01 M for WDs that are more massive than one solar mass. We find that the radiative proton-capture reaction 57Co(p, γ)58Ni is the dominant production mode for 58Ni in both MCh and sub-MCh models, while the α-capture reaction on 54Fe has a negligible impact on the final 58Ni yield. More importantly, we demonstrate that the lack of [Ni II] lines in late-time spectra of sub-MCh events is not always due to an under-abundance of stable Ni; rather, it results from the higher ionization of Ni in the inner ejecta. Conversely, the strong [Ni II] lines predicted in our 1D MCh models are completely suppressed when 56Ni is sufficiently mixed with the innermost layers, which are rich in stable iron-group elements.
Conclusions: [Ni II] lines in late-time SN Ia spectra have a complex dependency on the abundance of stable Ni, which limits their use in distinguishing among MCh and sub-MCh progenitors. However, we argue that a low-luminosity SN Ia displaying strong [Ni II] lines would most likely result from a Chandrasekhar-mass progenitor.

(399)Multi-Component Imaging of the Fermi Gamma-ray Sky in the Spatio-spectral Domain
• Lukas I. Platz,
• Jakob Knollmüller,
• Philipp Arras,
• Philipp Frank,
• Martin Reinecke
• +2
• Dominik Jüstel,
• Torsten A. Enßlin
• (less)
arXiv e-prints (04/2022) e-Print:2204.09360
abstract + abstract -

We perform two distinct spatio-spectral reconstructions of the gamma-ray sky in the range of 0.56-316 GeV based on Fermi Large Area Telescope (LAT) data. Both describe the sky brightness to be composed of a diffuse-emission and a point-source component. The first model requires minimal assumptions and provides a template-free reconstruction as a reference. It makes use of spatial and spectral correlations to distinguish between the different components. The second model is physics-informed and further differentiates between diffuse emission of hadronic and leptonic origin. For this, we assume parametric, but spatially varying energy spectra to distinguish between the processes and use thermal Galactic dust observations to indicate the preferred sites of hadronic interactions. To account for instrumental effects we model the point-spread, the energy dispersion, and the exposure of the telescope throughout the observation. The reconstruction problem is formulated as a Bayesian inference task, that is solved by variational inference. We show decompositions of the Gamma-ray flux into diffuse and point-like emissions, and of the diffuse emissions into multiple physically motivated components. The diffuse decomposition provides an unprecedented view of the Galactic leptonic diffuse emission. It shows the Fermi bubbles and their spectral variations in high fidelity and other areas exhibiting strong cosmic ray electron contents, such as a thick disk in the inner Galaxy and outflow regions. Furthermore, we report a hard spectrum gamma ray arc in the northern outer bubble co-spatial with the reported X-ray arc by the eROSITA collaboration. All our spatio-spectral sky reconstructions and their uncertainty quantification are publicly available.

(398)Accurate Relativistic Chiral Nucleon-Nucleon Interaction up to Next-to-Next-to-Leading Order
• Jun-Xu Lu,
• Chun-Xuan Wang,
• Yang Xiao,
• Li-Sheng Geng,
• Jie Meng
• +1
Physical Review Letters, 128 (04/2022) doi:10.1103/PhysRevLett.128.142002
abstract + abstract -

We construct a relativistic chiral nucleon-nucleon interaction up to the next-to-next-to-leading order in covariant baryon chiral perturbation theory. We show that a good description of the n p phase shifts up to Tlab=200 MeV and even higher can be achieved with a χ∼ 2/d .o .f . less than 1. Both the next-to-leading-order results and the next-to-next-to-leading-order results describe the phase shifts equally well up to Tlab=200 MeV , but for higher energies, the latter behaves better, showing satisfactory convergence. The relativistic chiral potential provides the most essential inputs for relativistic ab initio studies of nuclear structure and reactions, which has been in need for almost two decades.

(397)Cosmological simulations predict that AGN preferentially live in gas-rich, star-forming galaxies despite effective feedback
• Samuel Ruthven Ward,
• Chris Harrison,
• Tiago Costa,
• Vincenzo Mainieri
arXiv e-prints (04/2022) e-Print:2204.13712
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 AGN luminosity and molecular gas fraction or sSFR; (ii) both high-luminosity ($L_{bol}>10^{44}$ erg/s) and high-Eddington ratio (>1%) 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.

(396)Fast neutrino conversion in hydrodynamic simulations of neutrino-cooled accretion disks
• Oliver Just,
• Sajad Abbar,
• Meng-Ru Wu,
• Irene Tamborra,
• Hans-Thomas Janka
• +1
Physical Review D, 105 (04/2022) doi:10.1103/PhysRevD.105.083024
abstract + abstract -

The outflows from neutrino-cooled black hole accretion disks formed in neutron-star mergers or cores of collapsing stars are expected to be neutron-rich enough to explain a large fraction of elements created by the rapid neutron-capture process, but their precise chemical composition remains elusive. Here, we investigate the role of fast neutrino flavor conversion, motivated by the findings of our post-processing analysis that shows evidence of electron-neutrino lepton-number crossings deep inside the disk, hence suggesting possibly nontrivial effects due to neutrino flavor mixing. We implement a parametric, dynamically self-consistent treatment of fast conversion in time-dependent simulations and examine the impact on the disk and its outflows. By activating the otherwise inefficient, emission of heavy-lepton neutrinos, fast conversions enhance the disk cooling rates and reduce the absorption rates of electron-type neutrinos, causing a reduction of the electron fraction in the disk by 0.03-0.06 and in the ejected material by 0.01-0.03. The rapid neutron-capture process yields are enhanced by typically no more than a factor of two, rendering the overall impact of fast conversions modest. The kilonova is prolonged as a net result of increased lanthanide opacities and enhanced radioactive heating rates. We observe only mild sensitivity to the disk mass, the condition for the onset of flavor conversion, and to the considered cases of flavor mixing. Remarkably, parametric models of flavor mixing that conserve the lepton numbers per family result in an overall smaller impact than models invoking three-flavor equipartition, often assumed in previous works.

(395)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
• +63
• 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. Howard,
• S. B. Howell,
• H. Isaacson,
• S. V. Jeffers,
• J. M. Jenkins,
• S. R. Kane,
• J. Kemmer,
• S. Khalafinejad,
• R. C.,
• Jr. 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)
arXiv e-prints (04/2022)
abstract + abstract -

We report the discovery of a multi-planetary 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 R$_b$ = 1.240$\pm$0.023 R$_\oplus$, a mass of M$_b$ = 2.14$\pm$0.34 M$_\oplus$, and a bulk density of $\rho_b$ = 6.2$\pm$1.0 g cm$^{-3}$, and HD 260655 c, with a period of 5.71 d, a radius of R$_c$ = 1.533$^{+0.051}_{-0.046}$ R$_\oplus$, a mass of M$_c$ = 3.09$\pm$0.48 M$_\oplus$, and a bulk density of $\rho_c$ = 4.7$^{+0.9}_{-0.8}$ g cm$^{-3}$. The planets were detected in transit by the 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 becomes the fourth closest known multi-transiting 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 JWST, both in transmission and emission.

(394)Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): A Panchromatic View of DO Tau's Complex Kilo-au Environment
• Jane Huang,
• Christian Ginski,
• Myriam Benisty,
• Bin Ren,
• Alexander J. Bohn
• +18
• Élodie Choquet,
• Karin I. Öberg,
• Álvaro Ribas,
• Jaehan Bae,
• Edwin A. Bergin,
• Til Birnstiel,
• Yann Boehler,
• Stefano Facchini,
• Daniel Harsono,
• Michiel Hogerheijde,
• Feng Long,
• Carlo F. Manara,
• François Ménard,
• Paola Pinilla,
• Christophe Pinte,
• Christian Rab,
• Jonathan P. Williams,
• Alice Zurlo
• (less)
arXiv e-prints (04/2022)
abstract + abstract -

While protoplanetary disks are often treated as isolated systems in planet formation models, observations increasingly suggest that vigorous interactions between Class II disks and their environments are not rare. DO Tau is a T Tauri star that has previously been hypothesized to have undergone a close encounter with the HV Tau system. As part of the DESTINYS ESO Large Programme, we present new VLT/SPHERE polarimetric observations of DO Tau and combine them with archival HST scattered light images and ALMA observations of CO isotopologues and CS to map a network of complex structures. The SPHERE and ALMA observations show that the circumstellar disk is connected to arms extending out to several hundred au. HST and ALMA also reveal stream-like structures northeast of DO Tau, some of which are at least several thousand au long. These streams appear not to be gravitationally bound to DO Tau, and comparisons with previous Herschel far-IR observations suggest that the streams are part of a bridge-like structure connecting DO Tau and HV Tau. We also detect a fainter redshifted counterpart to a previously known blueshifted CO outflow. While some of DO Tau's complex structures could be attributed to a recent disk-disk encounter, they might be explained alternatively by interactions with remnant material from the star formation process. These panchromatic observations of DO Tau highlight the need to contextualize the evolution of Class II disks by examining processes occurring over a wide range of size scales.

(393)Radiative transfer in stars by feebly interacting bosons
• Andrea Caputo,
• Georg Raffelt,
• Edoardo Vitagliano
arXiv e-prints (04/2022)
abstract + abstract -

Starting from first principles, we study radiative transfer by new feebly-interacting bosons (FIBs) such as axions, axion-like particles (ALPs), dark photons, and others. Our key simplification is to include only boson emission or absorption (including decay), but not scattering between different modes of the radiation field. Based on a given distribution of temperature and FIB absorption rate in a star, we derive explicit volume-integral expressions for the boson luminosity, reaching from the free-streaming to the strong-trapping limit. The latter is seen explicitly to correspond to quasi-thermal emission from a "FIB sphere" according to the Stefan-Boltzmann law. Our results supersede expressions and approximations found in the recent literature on FIB emission from a supernova core and, for radiatively unstable FIBs, provide explicit expressions for the nonlocal ("ballistic") transfer of energy recently discussed in horizontal-branch stars.

(392)Persistent homology in cosmic shear II: A tomographic analysis of DES-Y1
• Sven Heydenreich,
• Benjamin Brück,
• Pierre Burger,
• Joachim Harnois-Déraps,
• Sandra Unruh
• +3
• Tiago Castro,
• Klaus Dolag,
• Nicolas Martinet
• (less)
arXiv e-prints (04/2022)
abstract + abstract -

We demonstrate how to use persistent homology for cosmological parameter inference in a tomographic cosmic shear survey. We obtain the first cosmological parameter constraints from persistent homology by applying our method to the first-year data of the Dark Energy Survey. To obtain these constraints, we analyse the topological structure of the matter distribution by extracting persistence diagrams from signal-to-noise maps of aperture masses. This presents a natural extension to the widely used peak count statistics. Extracting the persistence diagrams from the cosmo-SLICS, a suite of $N$-body simulations with variable cosmological parameters, we interpolate the signal using Gaussian Processes and marginalise over the most relevant systematic effects, including intrinsic alignments and baryonic effects. We find for the structure growth parameter $S_8=0.747^{+0.025}_{-0.031}$, which is in full agreement with other late-time probes. We also constrain the intrinsic alignment parameter to $A=1.54\pm 0.52$, ruling out the case of no intrinsic alignments at a $3\sigma$-level.

(391)Effective Field Theory of Stückelberg Vector Bosons
• Graham D. Kribs,
• Gabriel Lee,
• Adam Martin
arXiv e-prints (04/2022) e-Print:2204.01755
abstract + abstract -

We explore the effective field theory of a vector field $X^\mu$ that has a Stückelberg mass. The absence of a gauge symmetry for $X^\mu$ implies Lorentz-invariant operators are constructed directly from $X^\mu$. Beyond the kinetic and mass terms, allowed interactions at the renormalizable level include $X_\mu X^\mu H^\dagger H$, $(X_\mu X^\mu)^2$, and $X_\mu j^\mu$, where $j^\mu$ 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 $\sqrt{s}/m_X$, except for the case of $X_\mu j^\mu$ where $j^\mu$ 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 $X_\mu j_{anom}^\mu$, carefully isolating the finite contribution to the fermion triangle diagram. We calculate the longitudinally-enhanced observables $Z \rightarrow X\gamma$ (when $m_X < m_Z$), $f\bar{f} \rightarrow X \gamma$, and $Z\gamma \to Z\gamma$ when $X$ couples to the baryon number current. Introducing a fake gauge-invariance by writing $X^\mu = A^\mu - \partial^\mu \pi/m_X$, the would-be gauge anomaly associated with $A_\mu j_{anom}^\mu$ is canceled by $j_{anom}^\mu \partial_\mu \pi/m_X$; this is the four-dimensional Green-Schwarz anomaly-cancellation mechanism at work. Our analysis suggests there is no free lunch by appealing to Stückelberg for the mass of a vector field: the price paid for avoiding a dark Higgs sector is replaced by the non-generic set of interactions that the Stückelberg vector field must have to avoid amplitudes that grow with energy.

(390)Cosmological simulations predict that AGN preferentially live in gas-rich, star-forming galaxies despite effective feedback
• Samuel Ruthven Ward,
• Chris Harrison,
• Tiago Costa,
• Vincenzo Mainieri
(04/2022) e-Print:2204.13712
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 AGN luminosity and molecular gas fraction or sSFR; (ii) both high-luminosity ($L_{bol}>10^{44}$ erg/s) and high-Eddington ratio (>1%) 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.

(389)The importance of X-ray frequency in driving photoevaporative winds
• Andrew D. Sellek,
• Cathie J. Clarke,
• Barbara Ercolano
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 \textsc{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 $100~\mathrm{eV}$, firmly in the softer regions of the X-ray spectrum, while X-rays with energies $\sim1000~\mathrm{eV}$ 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.

(388)Substructure of Multiquark Hadrons (Snowmass 2021 White Paper)
• Nora Brambilla,
• Hua-Xing Chen,
• Angelo Esposito,
• Jacopo Ferretti,
• Anthony Francis
• +25
• Feng-Kun Guo,
• Christoph Hanhart,
• Atsushi Hosaka,
• Robert L. Jaffe,
• Marek Karliner,
• Richard Lebed,
• Randy Lewis,
• Luciano Maiani,
• Nilmani Mathur,
• Ulf-G. Meißner,
• Alessandro Pilloni,
• Antonio Davide Polosa,
• Sasa Prelovsek,
• Jean-Marc Richard,
• Veronica Riquer,
• Mitja Rosina,
• Jonathan L. Rosner,
• Elena Santopinto,
• Eric S. Swanson,
• Adam P. Szczepaniak,
• Sachiko Takeuchi,
• Makoto Takizawa,
• Frank Wilczek,
• Yasuhiro Yamaguchi,
• Bing-Song Zou
• (less)
(03/2022) e-Print:2203.16583
abstract + abstract -

In recent years there has been a rapidly growing body of experimental evidence for existence of exotic, multiquark hadrons, i.e. mesons which contain additional quarks, beyond the usual quark-antiquark pair and baryons which consist of more than three quarks. In all cases with robust evidence they contain at least one heavy quark Q=c or b, the majority including two heavy quarks. Two key theoretical questions have been triggered by these discoveries: (a) how are quarks organized inside these multiquark states -- as compact objects with all quarks within one confinement volume, interacting via color forces, perhaps with an important role played by diquarks, or as deuteron-like hadronic molecules, bound by light-meson exchange? (b) what other multiquark states should we expect? The two questions are tightly intertwined. Each of the interpretations provides a natural explanation of parts of the data, but neither explains all of the data. It is quite possible that both kinds of structures appear in Nature. It may also be the case that certain states are superpositions of the compact and molecular configurations. This Whitepaper brings together contributions from many leading practitioners in the field, representing a wide spectrum of theoretical interpretations. We discuss the importance of future experimental and phenomenological work, which will lead to better understandingof multiquark phenomena in QCD.

(387)The DECam Local Volume Exploration Survey Data Release 2
• A. Drlica-Wagner,
• P.S. Ferguson,
• M. Adamów,
• M. Aguena,
• F. Andrade-Oliveira
• +119
• D. Bacon,
• K. Bechtol,
• E.F. Bell,
• E. Bertin,
• P. Bilaji,
• S. Bocquet,
• C.R. Bom,
• D. Brooks,
• D.L. Burke,
• J.A. Carballo-Bello,
• J.L. Carlin,
• A. Carnero Rosell,
• M. Carrasco Kind,
• J. Carretero,
• F.J. Castander,
• W. Cerny,
• C. Chang,
• Y. Choi,
• C. Conselice,
• M. Costanzi,
• D. Crnojević,
• L.N. da Costa,
• J. De Vicente,
• S. Desai,
• J. Esteves,
• S. Everett,
• I. Ferrero,
• M. Fitzpatrick,
• B. Flaugher,
• D. Friedel,
• J. Frieman,
• J. García-Bellido,
• M. Gatti,
• E. Gaztanaga,
• D.W. Gerdes,
• D. Gruen,
• R.A. Gruendl,
• J. Gschwend,
• W.G. Hartley,
• D. Hernandez-Lang,
• S.R. Hinton,
• D.L. Hollowood,
• K. Honscheid,
• A.K. Hughes,
• A. Jacques,
• D.J. James,
• M.D. Johnson,
• K. Kuehn,
• N. Kuropatkin,
• O. Lahav,
• T.S. Li,
• C. Lidman,
• H. Lin,
• M. March,
• J.L. Marshall,
• D. Martínez-Delgado,
• C.E. Martínez-Vázquez,
• P. Massana,
• S. Mau,
• M. McNanna,
• P. Melchior,
• F. Menanteau,
• A.E. Miller,
• R. Miquel,
• J.J. Mohr,
• R. Morgan,
• B. Mutlu-Pakdil,
• R.R. Muñoz,
• E.H. Neilsen,
• D.L. Nidever,
• R. Nikutta,
• J.L. Nilo Castellon,
• N.E.D. Noël,
• R.L.C. Ogando,
• K.A.G. Olsen,
• A.B. Pace,
• A. Palmese,
• F. Paz-Chinchón,
• M.E.S. Pereira,
• A. Pieres,
• A.A. Plazas Malagón,
• J. Prat,
• A.H. Riley,
• M. Rodriguez-Monroy,
• A.K. Romer,
• A. Roodman,
• M. Sako,
• J.D. Sakowska,
• E. Sanchez,
• F.J. Sánchez,
• D.J. Sand,
• L. Santana-Silva,
• B. Santiago,
• M. Schubnell,
• S. Serrano,
• I. Sevilla-Noarbe,
• J.D. Simon,
• M. Smith,
• M. Soares-Santos,
• G.S. Stringfellow,
• E. Suchyta,
• D.J. Suson,
• C.Y. Tan,
• G. Tarle,
• K. Tavangar,
• D. Thomas,
• C. To,
• E.J. Tollerud,
• M.A. Troxel,
• D.L. Tucker,
• T.N. Varga,
• A.K. Vivas,
• A.R. Walker,
• J. Weller,
• R.D. Wilkinson,
• J.F. Wu,
• B. Yanny,
• E. Zaborowski,
• A. Zenteno
• (less)
(03/2022) e-Print:2203.16565
abstract + abstract -

We present the second public data release (DR2) from the DECam Local Volume Exploration survey (DELVE). DELVE DR2 combines new DECam observations with archival DECam data from the Dark Energy Survey, the DECam Legacy Survey, and other DECam community programs. DELVE DR2 consists of ~160,000 exposures that cover >21,000 deg^2 of the high Galactic latitude (|b| > 10 deg) sky in four broadband optical/near-infrared filters (g, r, i, z). DELVE DR2 provides point-source and automatic aperture photometry for ~2.5 billion astronomical sources with a median 5σ point-source depth of g=24.3, r=23.9, i=23.5, and z=22.8 mag. A region of ~17,000 deg^2 has been imaged in all four filters, providing four-band photometric measurements for ~618 million astronomical sources. DELVE DR2 covers more than four times the area of the previous DELVE data release and contains roughly five times as many astronomical objects. DELVE DR2 is publicly available via the NOIRLab Astro Data Lab science platform.

(386)Systematic Parametrization of the Leading $B$-meson Light-Cone Distribution Amplitude
• Thorsten Feldmann,
• Philip Lüghausen,
• Danny van Dyk
(03/2022) e-Print:2203.15679
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 ${}_1F_1$ 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 production expansion. We showcase the versatility of the parametrization in a series of phenomenological pseudo-fits.

(385)Dark Energy Survey Year 3 results: imprints of cosmic voids and superclusters in the Planck CMB lensing map
• A. Kovács,
• P. Vielzeuf,
• I. Ferrero,
• P. Fosalba,
• U. Demirbozan
• +80
• R. Miquel,
• C. Chang,
• N. Hamaus,
• G. Pollina,
• K. Bechtol,
• M. Becker,
• A. Carnero Rosell,
• M. Carrasco Kind,
• R. Cawthon,
• M. Crocce,
• A. Drlica-Wagner,
• J. Elvin-Poole,
• M. Gatti,
• G. Giannini,
• R.A. Gruendl,
• A. Porredon,
• A.J. Ross,
• E.S. Rykoff,
• I. Sevilla-Noarbe,
• E. Sheldon,
• B. Yanny,
• T. Abbott,
• M. Aguena,
• S. Allam,
• J. Annis,
• D. Bacon,
• G. Bernstein,
• E. Bertin,
• S. Bocquet,
• D. Brooks,
• D. Burke,
• J. Carretero,
• F.J. Castander,
• M. Costanzi,
• L.N. da Costa,
• M.E.S. Pereira,
• J. De Vicente,
• S. Desai,
• H.T. Diehl,
• J. Dietrich,
• A. Ferté,
• B. Flaugher,
• J. Frieman,
• J. García-Bellido,
• E. Gaztañaga,
• D. Gerdes,
• T. Giannantonio,
• D. Gruen,
• J. Gschwend,
• G. Gutierrez,
• S. Hinton,
• D.L. Hollowood,
• K. Honscheid,
• D. Huterer,
• K. Kuehn,
• O. Lahav,
• M. Lima,
• M. March,
• J. Marshall,
• P. Melchior,
• F. Menanteau,
• R. Morgan,
• J. Muir,
• R. Ogando,
• A. Palmese,
• F. Paz-Chinchon,
• A. Pieres,
• A. Plazas Malagón,
• M. Rodriguez Monroy,
• A. Roodman,
• E. Sanchez,
• M. Schubnell,
• S. Serrano,
• M. Smith,
• E. Suchyta,
• G. Tarle,
• D. Thomas,
• C.-H. To,
• T.N. Varga,
• J. Weller
• (less)
(03/2022) e-Print:2203.11306
abstract + abstract -

The CMB lensing signal from cosmic voids and superclusters probes the growth of structure in the low-redshift cosmic web. In this analysis, we cross-correlated the Planck CMB lensing map with voids detected in the Dark Energy Survey Year 3 (Y3) data set ($\sim$5,000 deg$^{2}$), extending previous measurements using Y1 catalogues ($\sim$1,300 deg$^{2}$). Given the increased statistical power compared to Y1 data, we report a $6.6\sigma$ detection of negative CMB convergence ($\kappa$) imprints using approximately 3,600 voids detected from a redMaGiC luminous red galaxy sample. However, the measured signal is lower than expected from the MICE N-body simulation that is based on the $\Lambda$CDM model (parameters $\Omega_{\rm m} = 0.25$, $\sigma_8 = 0.8$). The discrepancy is associated mostly with the void centre region. Considering the full void lensing profile, we fit an amplitude $A_{\kappa}=\kappa_{\rm DES}/\kappa_{\rm MICE}$ to a simulation-based template with fixed shape and found a moderate $2\sigma$ deviation in the signal with $A_{\kappa}\approx0.79\pm0.12$. We also examined the WebSky simulation that is based on a Planck 2018 $\Lambda$CDM cosmology, but the results were even less consistent given the slightly higher matter density fluctuations than in MICE. We then identified superclusters in the DES and the MICE catalogues, and detected their imprints at the $8.4\sigma$ level; again with a lower-than-expected $A_{\kappa}=0.84\pm0.10$ amplitude. The combination of voids and superclusters yields a $10.3\sigma$ detection with an $A_{\kappa}=0.82\pm0.08$ constraint on the CMB lensing amplitude, thus the overall signal is $2.3\sigma$ weaker than expected from MICE.

(384)Production and Polarization of $S$-Wave Quarkonia in Potential Nonrelativistic QCD
• Nora Brambilla,
• Hee Sok Chung,
• Antonio Vairo,
• Xiang-Peng Wang
(03/2022) e-Print:2203.07778
abstract + abstract -

Based on the potential nonrelativistic QCD formalism, we compute the nonrelativistic QCD long-distance matrix elements (LDMEs) for inclusive production of $S$-wave heavy quarkonia. This greatly reduces the number of nonperturbative unknowns and brings in a substantial enhancement in the predictive power of the NRQCD factorization formalism. We obtain improved determinations of the LDMEs and find cross sections and polarizations of $J/\psi$, $\psi(2S)$, and excited $\Upsilon$ states that agree well with LHC data. Our results may have important implications in pinning down the heavy quarkonium production mechanism.

(383)Snowmass white paper: Need for amplitude analysis in the discovery of new hadrons
• Miguel Albaladejo,
• Marco Battaglieri,
• Lukasz Bibrzycki,
• Andrea Celentano,
• Igor V. Danilkin
• +20
• Sebastian M. Dawid,
• Michael Doring,
• Cristiano Fanelli,
• Cesar Fernandez-Ramirez,
• Sergi Gonzalez-Solis,
• Astrid N. Hiller Blin,
• Andrew W. Jackura,
• Vincent Mathieu,
• Mikhail Mikhasenko,
• Victor I. Mokeev,
• Emilie Passemar,
• Robert J. Perry,
• Alessandro Pilloni,
• Arkaitz Rodas,
• Matthew R. Shepherd,
• Nathaniel Sherrill,
• Jorge A. Silva-Castro,
• Tomasz Skwarnicki,
• Adam P. Szczepaniak,
• Daniel Winney
• (less)
(03/2022) e-Print:2203.08208
abstract + abstract -

We highlight the need for the development of comprehensive amplitude analysis methods to further our understanding of hadron spectroscopy. Reaction amplitudes constrained by first principles of $S$-matrix theory and by QCD phenomenology are needed to extract robust interpretations of the data from experiments and from lattice calculations.

(382)Snowmass2021 Cosmic Frontier White Paper: Prospects for obtaining Dark Matter Constraints with DESI
• Monica Valluri,
• Solene Chabanier,
• Vid Irsic,
• Eric Armengaud,
• Michael Walther
• +27
• Connie Rockosi,
• Miguel A. Sanchez-Conde,
• Leandro Beraldo e Silva,
• Andrew P. Cooper,
• Elise Darragh-Ford,
• Kyle Dawson,
• Alis J. Deason,
• Simone Ferraro,
• Jaime E. Forero-Romero,
• Antonella Garzilli,
• Ting Li,
• Zarija Lukic,
• Christopher J. Manser,
• Nathalie Palanque-Delabrouille,
• Corentin Ravoux,
• Ting Tan,
• Wenting Wang,
• Risa Weschler,
• Andreia Carrillo,
• Arjun Dey,
• Sergey E. Koposov,
• Yao-Yuan Mao,
• Paulo Montero-Camacho,
• Ekta Patel,
• Graziano Rossi,
• L. Arturo Urena-Lopez,
• Octavio Valenzuela
• (less)
(03/2022) e-Print:2203.07491
abstract + abstract -

Despite efforts over several decades, direct-detection experiments have not yet led to the discovery of the dark matter (DM) particle. This has led to increasing interest in alternatives to the Lambda CDM (LCDM) paradigm and alternative DM scenarios (including fuzzy DM, warm DM, self-interacting DM, etc.). In many of these scenarios, DM particles cannot be detected directly and constraints on their properties can ONLY be arrived at using astrophysical observations. The Dark Energy Spectroscopic Instrument (DESI) is currently one of the most powerful instruments for wide-field surveys. The synergy of DESI with ESA's Gaia satellite and future observing facilities will yield datasets of unprecedented size and coverage that will enable constraints on DM over a wide range of physical and mass scales and across redshifts. DESI will obtain spectra of the Lyman-alpha forest out to z~5 by detecting about 1 million QSO spectra that will put constraints on clustering of the low-density intergalactic gas and DM halos at high redshift. DESI will obtain radial velocities of 10 million stars in the Milky Way (MW) and Local Group satellites enabling us to constrain their global DM distributions, as well as the DM distribution on smaller scales. The paradigm of cosmological structure formation has been extensively tested with simulations. However, the majority of simulations to date have focused on collisionless CDM. Simulations with alternatives to CDM have recently been gaining ground but are still in their infancy. While there are numerous publicly available large-box and zoom-in simulations in the LCDM framework, there are no comparable publicly available WDM, SIDM, FDM simulations. DOE support for a public simulation suite will enable a more cohesive community effort to compare observations from DESI (and other surveys) with numerical predictions and will greatly impact DM science.

(381)Radiopurity of a kg-scale PbWO$_4$ cryogenic detector produced from archaeological Pb for the RES-NOVA experiment
• J.W. Beeman,
• G. Benato,
• C. Bucci,
• L. Canonica,
• P. Carniti
• +39
• E. Celi,
• M. Clemenza,
• A. D'Addabbo,
• F.A. Danevich,
• S. Di Domizio,
• S. Di Lorenzo,
• 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. Schoenert,
• D.A. Solopikhin,
• R. Strauss,
• E. Tarabini,
• V.I. Tretyak,
• I.A. Tupitsyna,
• V. Wagner
• (less)
(03/2022) e-Print:2203.07441
abstract + abstract -

RES-NOVA is a newly proposed experiment for the detection of neutrinos from astrophysical sources, mainly Supernovae, using an array of cryogenic detectors made of PbWO$_4$ crystals produced from archaeological Pb. This unconventional material, characterized by intrinsic high radiopurity, enables to achieve low-background levels in the region of interest for the neutrino detection via Coherent Elastic neutrino-Nucleus Scattering (CE$\nu$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 PbWO$_4$ crystal produced from archaeological Pb operated as a cryogenic detector. The crystal internal radioactive contaminations are: $^{232}$Th $<$40 $\mu$Bq/kg, $^{238}$U $<$30 $\mu$Bq/kg, $^{226}$Ra 1.3 mBq/kg and $^{210}$Pb 22.5 mBq/kg. We present also 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.

(380)Snowmass 2021 White Paper Instrumentation Frontier 05 - White Paper 1: MPGDs: Recent advances and current R&D
• K. Dehmelt,
• M. Della Pietra,
• H. Muller,
• S.E. Tzamarias,
• A. White
• +65
• S. White,
• Z. Zhang,
• M. Alviggi,
• I. Angelis,
• S. Aune,
• J. Bortfeldt,
• M. Bregant,
• F. Brunbauer,
• M.T. Camerlingo,
• V. Canale,
• V. D'Amico,
• D. Desforge,
• C. Di Donato,
• R. Di Nardo,
• G. Fanourakis,
• K.J. Floethner,
• M. Gallinaro,
• F. Garcia,
• I. Giomataris,
• K. Gnanvo,
• T. Gustavsson,
• R. Hall-Wilton,
• P. Iengo,
• F.J. Iguaz,
• M. Iodice,
• D. Janssens,
• A. Kallitsopoulou,
• M. Kebbiri,
• K. Kordas,
• C. Lampoudis,
• P. Legou,
• M. Lisowska,
• J. Liu,
• M. Lupberger,
• S. Malace,
• I. Maniatis,
• I. Manthos,
• Y. Meng,
• H. Natal da Luz,
• E. Oliveri,
• G. Orlandini,
• T. Papaevangelou,
• K. Paraschou,
• F. Petrucci,
• D. Pfeiffer,
• M. Pomorski,
• S. Popescu,
• F. Resnati,
• L. Ropelewski,
• A. Rusu,
• D. Sampsonidis,
• L. Scharenberg,
• T. Schneider,
• G. Sekhniaidze,
• M. Sessa,
• M. Shao,
• L. Sohl,
• J. Toledo-Alarcon,
• A. Tsiamis,
• Y. Tsipolitis,
• A. Utrobicic,
• M. van Stenis,
• R. Veenhof,
• X. Wang,
• Y. Zhou
• (less)
(03/2022) e-Print:2203.06562
abstract + abstract -

This paper will review the origins, development, and examples of new versions of Micro-Pattern Gas Detectors. The goal for MPGD development was the creation of detectors that could cost-effectively cover large areas while offering excellent position and timing resolution, and the ability to operate at high incident particle rates. The early MPGD developments culminated in the formation of the RD51 collaboration which has become the critical organization for the promotion of MPGDs and all aspects of their production, characterization, simulation, and uses in an expanding array of experimental configurations. For the Snowmass 2021 study, a number of Letters of Interest were received that illustrate ongoing developments and expansion of the use of MPGDs. In this paper, we highlight high precision timing, high rate application, trigger capability expansion of the SRS readout system, and a structure designed for low ion backflow.

(379)Studying $\Delta L=2$ Lepton Flavor Violation with Muons
• Alexey A. Petrov,
• Renae Conlin,
• Cody Grant
Universe, 8, p169 (03/2022) e-Print:2203.04161 doi:10.3390/universe8030169
abstract + abstract -

Flavor violating processes in the lepton sector have highly suppressed branching ratios in the standard model. Thus, observation of lepton flavor violation (LFV) constitutes a clear indication of physics beyond the standard model (BSM). We review new physics searches in the processes that violate the conservation of lepton (muon) flavor by two units with muonia and muonium–antimuonium oscillations.

(378)Dark Energy and the Spinning Superparticle
• Daniel Bockisch,
• Ivo Sachs
arXiv e-prints (03/2022) e-Print:2203.06014
abstract + abstract -

We revisit the theory of background fields constructed on the BRST-algebra of a spinning particle with $\mathcal{N}=4$ worldline supersymmetry, whose spectrum contains the graviton but no other fields. On a generic background, the closure of the BRST algebra implies the vacuum Einstein equations with a cosmological constant that is undetermined. On the other hand, in the "vacuum" background with no metric, the cohomology is given by a collection of free scalar- and vector fields. Only certain combinations of linear excitations, necessarily involving a vector field, can be extended beyond the linear level with the vector field inducing an Einstein metric.

(377)RG of GR from on-shell amplitudes
• Pietro Baratella,
• Dominik Haslehner,
• Maximilian Ruhdorfer,
• Javi Serra,
• Andreas Weiler
Journal of High Energy Physics, 2022 (03/2022) doi:10.1007/JHEP03(2022)156
abstract + abstract -

We study the renormalization group of generic effective field theories that include gravity. We follow the on-shell amplitude approach, which provides a simple and efficient method to extract anomalous dimensions avoiding complications from gauge redundancies. As an invaluable tool we introduce a modified helicity h ∼ under which gravitons carry one unit instead of two. With this modified helicity we easily explain old and uncover new non-renormalization theorems for theories including gravitons. We provide complete results for the one-loop gravitational renormalization of a generic minimally coupled gauge theory with scalars and fermions and all orders in MPl, as well as for the renormalization of dimension-six operators including at least one graviton, all up to four external particles.

(376)Unequal-mass mergers of dark matter haloes with rare and frequent self-interactions
• Moritz S. Fischer,
• Marcus Brüggen,
• Kai Schmidt-Hoberg,
• Klaus Dolag,
• Antonio Ragagnin
• +1
Monthly Notices of the Royal Astronomical Society, 510, p20 (03/2022) doi:10.1093/mnras/stab3544
abstract + abstract -

Dark matter (DM) self-interactions have been proposed to solve problems on small length scales within the standard cold DM cosmology. Here, we investigate the effects of DM self-interactions in merging systems of galaxies and galaxy clusters with equal and unequal mass ratios. We perform N-body DM-only simulations of idealized setups to study the effects of DM self-interactions that are elastic and velocity-independent. We go beyond the commonly adopted assumption of large-angle (rare) DM scatterings, paying attention to the impact of small-angle (frequent) scatterings on astrophysical observables and related quantities. Specifically, we focus on DM-galaxy offsets, galaxy-galaxy distances, halo shapes, morphology, and the phase-space distribution. Moreover, we compare two methods to identify peaks: one based on the gravitational potential and one based on isodensity contours. We find that the results are sensitive to the peak finding method, which poses a challenge for the analysis of merging systems in simulations and observations, especially for minor mergers. Large DM-galaxy offsets can occur in minor mergers, especially with frequent self-interactions. The subhalo tends to dissolve quickly for these cases. While clusters in late merger phases lead to potentially large differences between rare and frequent scatterings, we believe that these differences are non-trivial to extract from observations. We therefore study the galaxy/star populations which remain distinct even after the DM haloes have coalesced. We find that these collisionless tracers behave differently for rare and frequent scatterings, potentially giving a handle to learn about the micro-physics of DM.

(375)Gravitational soft theorem from emergent soft gauge symmetries
• Martin Beneke,
• Patrick Hager,
• Robert Szafron
Journal of High Energy Physics, 2022 (03/2022) doi:10.1007/JHEP03(2022)199
abstract + abstract -

We consider and derive the gravitational soft theorem up to the sub-subleading power from the perspective of effective Lagrangians. The emergent soft gauge symmetries of the effective Lagrangian provide a transparent explanation of why soft graviton emission is universal to sub-subleading power, but gauge boson emission is not. They also suggest a physical interpretation of the form of the soft factors in terms of the charges related to the soft transformations and the kinematics of the multipole expansion. The derivation is done directly at Lagrangian level, resulting in an operatorial form of the soft theorems. In order to highlight the differences and similarities of the gauge-theory and gravitational soft theorems, we include an extensive discussion of soft gauge-boson emission from scalar, fermionic and vector matter at subleading power.

(374)zELDA: fitting Lyman alpha line profiles using deep learning
• Siddhartha Gurung-López,
• Max Gronke,
• Shun Saito,
• Silvia Bonoli,
• Álvaro A. Orsi
Monthly Notices of the Royal Astronomical Society, 510, p31 (03/2022) doi:10.1093/mnras/stab3554
abstract + abstract -

We present zELDA (redshift Estimator for Line profiles of Distant Lyman Alpha emitters), an open source code to fit Lyman α (Ly α) line profiles. The main motivation is to provide the community with an easy to use and fast tool to analyse Ly α line profiles uniformly to improve the understating of Ly α emitting galaxies. zELDA is based on line profiles of the commonly used 'shell-model' pre-computed with the full Monte Carlo radiative transfer code LyaRT. Via interpolation between these spectra and the addition of noise, we assemble a suite of realistic Ly α spectra which we use to train a deep neural network.We show that the neural network can predict the model parameters to high accuracy (e.g. ≲ 0.34 dex H I column density for R ~ 12 000) and thus allows for a significant speedup over existing fitting methods. As a proof of concept, we demonstrate the potential of zELDA by fitting 97 observed Ly α line profiles from the LASD data base. Comparing the fitted value with the measured systemic redshift of these sources, we find that Ly α determines their rest frame Ly α wavelength with a remarkable good accuracy of ~0.3 Å ($\sim 75\,\, {\rm km\, s}^{-1}$). Comparing the predicted outflow properties and the observed Ly α luminosity and equivalent width, we find several possible trends. For example, we find an anticorrelation between the Ly α luminosity and the outflow neutral hydrogen column density, which might be explained by the radiative transfer process within galaxies.

(373)Moderately misaligned orbit of the warm sub-Saturn HD 332231 b
• E. Sedaghati,
• A. Sánchez-López,
• S. Czesla,
• M. López-Puertas,
• P. J. Amado
• +7
• E. Palle,
• K. Molaverdikhani,
• J. A. Caballero,
• L. Nortmann,
• A. Quirrenbach,
• A. Reiners,
• I. Ribas
• (less)
Astronomy and Astrophysics, 659, p14 (03/2022) doi:10.1051/0004-6361/202142471
abstract + abstract -

Measurements of exoplanetary orbital obliquity angles for different classes of planets are an essential tool in testing various planet formation theories. Measurements for those transiting planets on relatively large orbital periods (P > 10 d) present a rather difficult observational challenge. Here we present the obliquity measurement for the warm sub-Saturn planet HD 332231 b, which was discovered through Transiting Exoplanet Survey Satellite photometry of sectors 14 and 15, on a relatively large orbital period (18.7 d). Through a joint analysis of previously obtained spectroscopic data and our newly obtained CARMENES transit observations, we estimated the spin-orbit misalignment angle, λ, to be −42.0−10.6+11.3 deg, which challenges Laplacian ideals of planet formation. Through the addition of these new radial velocity data points obtained with CARMENES, we also derived marginal improvements on other orbital and bulk parameters for the planet, as compared to previously published values. We showed the robustness of the obliquity measurement through model comparison with an aligned orbit. Finally, we demonstrated the inability of the obtained data to probe any possible extended atmosphere of the planet, due to a lack of precision, and place the atmosphere in the context of a parameter detection space.

(372)Low-luminosity supernovae: SN 2005cs and SN 2020cxd as very low-energy iron core-collapse explosions
• Alexandra Kozyreva,
• Hans-Thomas Janka,
• Daniel Kresse,
• Stefan Taubenberger
arXiv e-prints (03/2022) e-Print:2203.00473
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 MSun red supergiant progenitor with an iron core and a pre-collapse mass of 8.75 Msun. The explosion of the star was obtained by the neutrino-driven mechanism in a fully self-consistent simulation in three dimensions (3D). Multi-band 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 spherisized 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 multi-band emission can be well reproduced by our SN model with its explosion energy of only 0.7x10^50 erg and an ejecta mass of 7.4 Msun. 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.

(371)Functions Beyond Multiple Polylogarithms for Precision Collider Physics
• Jacob L. Bourjaily,
• Johannes Broedel,
• Ekta Chaubey,
• Claude Duhr,
• Hjalte Frellesvig
• +12
• Martijn Hidding,
• Robin Marzucca,
• Andrew J. McLeod,
• Marcus Spradlin,
• Lorenzo Tancredi,
• Cristian Vergu,
• Matthias Volk,
• Anastasia Volovich,
• Matt von Hippel,
• Stefan Weinzierl,
• Matthias Wilhelm,
• Chi Zhang
• (less)
arXiv e-prints (03/2022) e-Print:2203.07088
abstract + abstract -

Feynman diagrams constitute one of the essential ingredients for making precision predictions for collider experiments. Yet, while the simplest Feynman diagrams can be evaluated in terms of multiple polylogarithms -- whose properties as special functions are well understood -- more complex diagrams often involve integrals over complicated algebraic manifolds. Such diagrams already contribute at NNLO to the self-energy of the electron, $t \bar{t}$ production, $\gamma \gamma$ production, and Higgs decay, and appear at two loops in the planar limit of maximally supersymmetric Yang-Mills theory. This makes the study of these more complicated types of integrals of phenomenological as well as conceptual importance. In this white paper contribution to the Snowmass community planning exercise, we provide an overview of the state of research on Feynman diagrams that involve special functions beyond multiple polylogarithms, and highlight a number of research directions that constitute essential avenues for future investigation.

(370)Hadronic vacuum polarization contribution to the muon $g-2$ in holographic QCD
• Josef Leutgeb,
• Anton Rebhan,
• Michael Stadlbauer
arXiv e-prints (03/2022) e-Print:2203.16508
abstract + abstract -

We evaluate the leading-order hadronic vacuum polarization contribution to the anomalous magnetic moment of the muon with two light flavors in minimal hard-wall and soft-wall holographic QCD models, as well as in simple generalizations thereof, and compare with the rather precise results available from dispersive and lattice approaches. While holographic QCD cannot be expected to shed light on the existing small discrepancies between the latter, this comparison in turn provides useful information on the holographic models, which have been used to evaluate hadronic light-by-light contributions where errors in data-driven and lattice approaches are more sizable. In particular, in the hard-wall model that has recently been used to implement the Melnikov-Vainshtein short-distance constraint on hadronic light-by-light contributions, a matching of the hadronic vacuum polarization to the data-driven approach points to the same correction of parameters that has been proposed recently in order to account for next-to-leading order effects.

(369)NLO QCD Renormalization Group Evolution for Non-Leptonic $\Delta F=2$ Transitions in the SMEFT
• Jason Aebischer,
• Andrzej J. Buras,
• Jacky Kumar
arXiv e-prints (03/2022) e-Print:2203.11224
abstract + abstract -

We present for the first time NLO QCD Renormalization Group (RG) evolution matrices for non-leptonic $\Delta F=2$ 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 operators in the so-called BMU basis into the ones in the common Weak Effective Theory (WET) basis (the so-called JMS basis) for which tree-level and one-loop matching to the SMEFT are already known. This allows us subsequently to find the two-loop QCD ADMs for the SMEFT non-leptonic $\Delta F=2$ 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 non-leptonic $\Delta F=2$ transitions from the new physics scale $\Lambda$ down to the electroweak scale $\mu_\text{ew}$. The main benefit of these new contributions is that they allow to remove renormalization scheme dependences present both in the one-loop matchings between the WET and SMEFT and also between SMEFT and a chosen UV completion. But the NLO QCD effects, calculated here in the NDR scheme, turn out to be small, in the ballpark of a few percent but larger than one-loop Yukawa top effects when only the $\Delta F=2$ operators are considered. The technology developed in our paper allows to obtain the ADMs in the SMEFT from the ones of the BMU basis also for non-leptonic $\Delta F=1$ decays and the results of this more involved analysis will be presented soon in another publication.

(368)α -event characterization and rejection in point-contact HPGe detectors
• I. J. Arnquist,
• F. T. Avignone,
• A. S. Barabash,
• C. J. Barton,
• F. E. Bertrand
• +60
• E. Blalock,
• B. Bos,
• M. Busch,
• M. Buuck,
• T. S. Caldwell,
• Y. -D. Chan,
• C. D. Christofferson,
• P. -H. Chu,
• M. L. Clark,
• C. Cuesta,
• J. A. Detwiler,
• A. Drobizhev,
• T. R. Edwards,
• D. W. Edwins,
• F. Edzards,
• Y. Efremenko,
• S. R. Elliott,
• T. Gilliss,
• G. K. Giovanetti,
• M. P. Green,
• J. Gruszko,
• I. S. Guinn,
• V. E. Guiseppe,
• C. R. Haufe,
• R. J. Hegedus,
• R. Henning,
• D. Hervas Aguilar,
• E. W. Hoppe,
• A. Hostiuc,
• I. Kim,
• R. T. Kouzes,
• A. M. Lopez,
• J. M. López-Castaño,
• E. L. Martin,
• R. D. Martin,
• R. Massarczyk,
• S. J. Meijer,
• S. Mertens,
• J. Myslik,
• T. K. Oli,
• G. Othman,
• W. Pettus,
• A. W. P. Poon,
• D. C. Radford,
• J. Rager,
• A. L. Reine,
• K. Rielage,
• N. W. Ruof,
• B. Saykı,
• S. Schönert,
• M. J. Stortini,
• D. Tedeschi,
• R. L. Varner,
• S. Vasilyev,
• J. F. Wilkerson,
• M. Willers,
• C. Wiseman,
• W. Xu,
• C. -H. Yu,
• B. X. Zhu
• (less)
European Physical Journal C, 82 (03/2022) doi:10.1140/epjc/s10052-022-10161-y
abstract + abstract -

P-type point contact (PPC) HPGe detectors are a leading technology for rare event searches due to their excellent energy resolution, low thresholds, and multi-site event rejection capabilities. We have characterized a PPC detector's response to α particles incident on the sensitive passivated and p+ surfaces, a previously poorly-understood source of background. The detector studied is identical to those in the MAJORANADEMONSTRATOR experiment, a search for neutrinoless double-beta decay (0 ν β β ) in 76Ge. α decays on most of the passivated surface exhibit significant energy loss due to charge trapping, with waveforms exhibiting a delayed charge recovery (DCR) signature caused by the slow collection of a fraction of the trapped charge. The DCR is found to be complementary to existing methods of α identification, reliably identifying α background events on the passivated surface of the detector. We demonstrate effective rejection of all surface α events (to within statistical uncertainty) with a loss of only 0.2% of bulk events by combining the DCR discriminator with previously-used methods. The DCR discriminator has been used to reduce the background rate in the 0 ν β β region of interest window by an order of magnitude in the MAJORANADEMONSTRATOR and will be used in the upcoming LEGEND-200 experiment.

(367)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
arXiv e-prints (03/2022) e-Print:2203.05397
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 $E_{\text{sym}}(\rho_0)=33.1$ MeV and $L=65.2$ MeV, in agreement with empirical and experimental values. Further applications predict the neutron star radius $R_{1.4M_\odot}\approx 12$ km and the maximum mass of a neutron star $M_{\text{max}}\leq 2.4M_\odot$.

(366)The relativistic Schrödinger equation through FFTW 3: An extension of quantumfdtd
• Rafael L. Delgado,
• Sebastian Steinbeißer,
• Michael Strickland,
• Johannes Heinrich Weber
Computer Physics Communications, 272 (03/2022) doi:10.1016/j.cpc.2021.108250
abstract + abstract -

In order to solve the time-independent three-dimensional Schrödinger equation, one can transform the time-dependent Schrödinger equation to imaginary time and use a parallelized iterative method to obtain the full three-dimensional eigen-states and eigen-values on very large lattices. In the case of the non-relativistic Schrödinger equation, there exists a publicly available code called quantumfdtd which implements this algorithm. In this paper, we (a) extend the quantumfdtd code to include the case of the relativistic Schrödinger equation and (b) add two optimized Fast Fourier Transform (FFT) based kinetic energy terms for non-relativistic cases. The new kinetic energy terms (two non-relativistic and one relativistic) are computed using the parallelized FFT-algorithm provided by the FFTW 3 library. The resulting quantumfdtd v3 code, which is publicly released with this paper, is backwards compatible with version 2, supporting explicit finite-differences schemes in addition to the new FFT-based schemes. Finally, we (c) extend the original code so that it supports arbitrary external file-based potentials and the option to project out distinct parity eigen-states from the solutions. Herein, we provide details of the quantumfdtd v3 implementation, comparisons and tests of the three new kinetic energy terms, and code documentation.

(365)Boundary Heisenberg algebras and their deformations
• Martín Enríquez Rojo,
• H. R. Safari
Journal of High Energy Physics, 2022 (03/2022) doi:10.1007/JHEP03(2022)089
abstract + abstract -

We investigate the deformations and rigidity of boundary Heisenberg-like algebras. In particular, we focus on the Heisenberg and Heisenberg ⊕ witt algebras which arise as symmetry algebras in three-dimensional gravity theories. As a result of the deformation procedure we find a large class of algebras. While some of these algebras are new, some of them have already been obtained as asymptotic and boundary symmetry algebras, supporting the idea that symmetry algebras associated to diverse boundary conditions and spacetime loci are algebraically interconnected through deformation of algebras. The deformation/contraction relationships between the new algebras are investigated. In addition, it is also shown that the deformation procedure reaches new algebras inaccessible to the Sugawara construction. As a byproduct of our analysis, we obtain that Heisenberg ⊕ witt and the asymptotic symmetry algebra Weyl-bms3 are not connected via single deformation but in a more subtle way.

(364)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)
arXiv e-prints (03/2022) e-Print:2203.11999
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.

(363)Production and Polarization of $S$-Wave Quarkonia in Potential Nonrelativistic QCD
• Nora Brambilla,
• Hee Sok Chung,
• Antonio Vairo,
• Xiang-Peng Wang
arXiv e-prints (03/2022) e-Print:2203.07778
abstract + abstract -

Based on the potential nonrelativistic QCD formalism, we compute the nonrelativistic QCD long-distance matrix elements (LDMEs) for inclusive production of $S$-wave heavy quarkonia. This greatly reduces the number of nonperturbative unknowns and brings in a substantial enhancement in the predictive power of the NRQCD factorization formalism. We obtain improved determinations of the LDMEs and find cross sections and polarizations of $J/\psi$, $\psi(2S)$, and excited $\Upsilon$ states that agree well with LHC data. Our results may have important implications in pinning down the heavy quarkonium production mechanism.

(362)The Diffuse Gamma-Ray Flux from Clusters of Galaxies
• Saqib Hussain,
• Rafael Alves Batista,
• Elisabete M. de Gouveia Dal Pino,
• Klaus Dolag
arXiv e-prints (03/2022) e-Print:2203.01260
abstract + abstract -

The origin of the diffuse gamma-ray background (DGRB) detected by EGRET and Fermi-LAT, the one that remains after subtracting all individual sources from the observed gamma-ray sky, is unknown. The DGRB possibly encompasses contributions from different source populations such as star-forming galaxies, starburst galaxies, active galactic nuclei, gamma-ray bursts, or galaxy clusters. Here, we combine cosmological magnetohydrodynamical simulations of clusters of galaxies with the propagation of CRs using Monte Carlo simulations, in the redshift range $z\leq 5.0$, and find that the integrated gamma-ray flux from clusters can contribute up to $100\%$ of the DGRB flux observed by Fermi-LAT above $100$~GeV, for CR spectral indices $\alpha = 1.5 - 2.5$ and energy cutoffs $E_{\text{max}} = 10^{16} - 10^{17}$~eV. The flux is dominated by clusters with masses $10^{13}< M/M_{\odot} < 10^{15}$ and redshift $z \leq 0.3$. Our results also predict the potential observation of high-energy gamma rays from clusters by experiments like HAWC, LHAASO, and even the upcoming CTA.

(361)Coarsening and wavelength selection far from equilibrium: a unifying framework based on singular perturbation theory
• Henrik Weyer,
• Fridtjof Brauns,
• Erwin Frey
arXiv e-prints (03/2022) e-Print:2203.03892
abstract + abstract -

Intracellular protein patterns are described by (nearly) mass-conserving reaction-diffusion systems. While these patterns initially form out of a homogeneous steady state due to the well-understood Turing instability, no general theory exists for the dynamics of fully nonlinear patterns. We develop a unifying theory for wavelength-selection dynamics in (nearly) mass-conserving two-component reaction-diffusion systems independent of the specific mathematical model chosen. This encompasses both the dynamics of the mesa- and peak-shaped patterns found in these systems. Our analysis uncovers a diffusion- and a reaction-limited regime of the dynamics, which provides a systematic link between the dynamics of mass-conserving reaction-diffusion systems and the Cahn-Hilliard as well as conserved Allen-Cahn equations, respectively. A stability threshold in the family of stationary patterns with different wavelengths predicts the wavelength selected for the final stationary pattern. At short wavelengths, self-amplifying mass transport between single pattern domains drives coarsening while at large wavelengths weak source terms that break strict mass conservation lead to an arrest of the coarsening process. The rate of mass competition between pattern domains is calculated analytically using singular perturbation theory, and rationalized in terms of the underlying physical processes. The resulting closed-form analytical expressions enable us to quantitatively predict the coarsening dynamics and the final pattern wavelength. We find excellent agreement of these expressions with numerical results. The systematic understanding of the length-scale dynamics of fully nonlinear patterns in two-component systems provided here builds the basis to reveal the mechanisms underlying wavelength selection in multi-component systems with potentially several conservation laws.

(360)NOEMA confirmation of an optically dark ALMA-AzTEC submillimetre galaxy at z = 5.24. A late-stage starburst prior to quenching
• S. Ikarashi,
• R. J. Ivison,
• W. I. Cowley,
• K. Kohno
Astronomy and Astrophysics, 659, p9 (03/2022) doi:10.1051/0004-6361/202141196
abstract + abstract -

We have obtained deep 1 and 3 mm spectral-line scans towards a candidate z ≳ 5 ALMA-identified AzTEC submillimetre galaxy (SMG) in the Subaru/XMM-Newton Deep Field (or UKIDSS UDS), ASXDF1100.053.1, using the NOrthern Extended Millimeter Array (NOEMA), aiming to obtain its spectroscopic redshift. ASXDF1100.053.1 is an unlensed optically dark millimetre-bright SMG with S1100 μm = 3.5 mJy and KAB > 25.7 (2σ), which was expected to lie at z = 5-7 based on its radio-submillimetre photometric redshift. Our NOEMA spectral scan detected line emission due to 12CO(J = 5-4) and (J = 6-5), providing a robust spectroscopic redshift, zCO = 5.2383 ± 0.0005. Energy-coupled spectral energy distribution modelling from optical to radio wavelengths indicates an infrared luminosity LIR = 8.3−1.4+1.5 × 1012 L, a star formation rate SFR = 630−380+260 M yr−1, a dust mass Md = 4.4−0.3+0.4 × 108 M, a stellar mass Mstellar = 3.5−1.4+3.6 × 1011 M, and a dust temperature Td = 37.4−1.8+2.3 K. The CO luminosity allows us to estimate a gas mass Mgas = 3.1 ± 0.3 × 1010 M, suggesting a gas-to-dust mass ratio of around 70, fairly typical for z ∼ 2 SMGs. ASXDF1100.053.1 has ALMA continuum size Re = 1.0−0.1+0.2 kpc, so its surface infrared luminosity density ΣIR is 1.2−0.2+0.1 × 1012 L kpc−2. These physical properties indicate that ASXDF1100.053.1 is a massive dusty star-forming galaxy with an unusually compact starburst. It lies close to the star-forming main sequence at z ∼ 5, with low Mgas/Mstellar = 0.09, SFR/SFRMS(RSB) = 0.6, and a gas-depletion time τdep of ≈50 Myr, modulo assumptions about the stellar initial mass function in such objects. ASXDF1100.053.1 has extreme values of Mgas/Mstellar, RSB, and τdep compared to SMGs at z ∼ 2-4, and those of ASXDF1100.053.1 are the smallest among SMGs at z > 5. ASXDF1100.053.1 is likely a late-stage dusty starburst prior to passivisation. The number of z = 5.1-5.3 unlensed SMGs now suggests a number density dN/dz = 30.4 ± 19.0 deg−2, barely consistent with the latest cosmological simulations.

(359)A tentative detection of He I in the atmosphere of GJ 1214 b
• J. Orell-Miquel,
• F. Murgas,
• E. Pallé,
• M. Lampón,
• M. López-Puertas
• +25
• J. Sanz-Forcada,
• E. Nagel,
• A. Kaminski,
• N. Casasayas-Barris,
• L. Nortmann,
• R. Luque,
• K. Molaverdikhani,
• E. Sedaghati,
• J. A. Caballero,
• P. J. Amado,
• G. Bergond,
• S. Czesla,
• A. P. Hatzes,
• Th. Henning,
• S. Khalafinejad,
• D. Montes,
• G. Morello,
• A. Quirrenbach,
• A. Reiners,
• I. Ribas,
• A. Sánchez-López,
• A. Schweitzer,
• M. Stangret,
• F. Yan,
• M. R. Zapatero Osorio
• (less)
Astronomy and Astrophysics, 659, p12 (03/2022) doi:10.1051/0004-6361/202142455
abstract + abstract -

The He I λ10833 Å triplet is a powerful tool for characterising the upper atmosphere of exoplanets and tracing possible mass loss. Here, we analysed one transit of GJ 1214 b observed with the CARMENES high-resolution spectrograph to study its atmosphere via transmission spectroscopy around the He I triplet. Although previous studies using lower resolution instruments have reported non-detections of He I in the atmosphere of GJ 1214 b, we report here the first potential detection. We reconcile the conflicting results arguing that previous transit observations did not present good opportunities for the detection of He I, due to telluric H2O absorption and OH emission contamination. We simulated those earlier observations, and show evidence that the planetary signal was contaminated. From our single non-telluric-contaminated transit, we determined an excess absorption of 2.10−0.50+0.45% (4.6 σ) with a full width at half maximum (FWHM) of 1.30−0.25+0.30 Å. The detection of He I is statistically significant at the 4.6 σ level, but repeatability of the detection could not be confirmed due to the availability of only one transit. By applying a hydrodynamical model and assuming an H/He composition of 98/2, we found that GJ 1214 b would undergo hydrodynamic escape in the photon-limited regime, losing its primary atmosphere with a mass-loss rate of (1.5-18) × 1010 g s−1 and an outflow temperature in the range of 2900-4400 K. Further high-resolution follow-up observations of GJ 1214 b are needed to confirm and fully characterise the detection of an extended atmosphere surrounding GJ 1214 b. If confirmed, this would be strong evidence that this planet has a primordial atmosphere accreted from the original planetary nebula. Despite previous intensive observations from space- and ground-based observatories, our He I excess absorption is the first tentative detection of a chemical species in the atmosphere of this benchmark sub-Neptune planet.

(358)Soft-collinear gravity beyond the leading power
• Martin Beneke,
• Patrick Hager,
• Robert Szafron
Journal of High Energy Physics, 2022 (03/2022) doi:10.1007/JHEP03(2022)080
abstract + abstract -

We construct "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. Despite the absence of collinear divergences in gravity at leading power, the construction exhibits remarkable similarities with soft-collinear effective theory of QCD (gauge fields). It reveals an emergent soft background gauge symmetry, which allows for a manifestly gauge-invariant representation of the interactions in terms of a soft covariant derivative, the soft Riemann tensor, and a covariant generalisation of the collinear light-cone gauge metric field. The gauge symmetries control both the unsuppressed collinear field components and the inherent inhomogeneity in λ of the invariant objects to all orders, resulting in a consistent expansion.

(357)Effective-range expansion of the $T_{cc}^+$ state at the complex $D^{*+}D^0$ threshold
• Mikhail Mikhasenko
arXiv e-prints (03/2022) e-Print:2203.04622
abstract + abstract -

Evaluation of the effective-range parameters for the $T_{cc}^+$ state in the LHCb model is examined. The finite width of $D^*$ leads to a shift of the expansion point into the complex plane to match analytical properties of the expanded amplitude. We perform an analytic continuation of the three-body scattering amplitude to the complex plane in a vicinity of the branch point and develop a robust procedure for computation of the expansion coefficients. The results yield a nearly-real scattering length, and two contributions to the the effective range which have not been accounted before.

(356)neos: End-to-End-Optimised Summary Statistics for High Energy Physics
• Nathan Simpson,
• Lukas Heinrich
arXiv e-prints (03/2022) e-Print:2203.05570
abstract + abstract -

The advent of deep learning has yielded powerful tools to automatically compute gradients of computations. This is because training a neural network equates to iteratively updating its parameters using gradient descent to find the minimum of a loss function. Deep learning is then a subset of a broader paradigm; a workflow with free parameters that is end-to-end optimisable, provided one can keep track of the gradients all the way through. This work introduces neos: an example implementation following this paradigm of a fully differentiable high-energy physics workflow, capable of optimising a learnable summary statistic with respect to the expected sensitivity of an analysis. Doing this results in an optimisation process that is aware of the modelling and treatment of systematic uncertainties.

(355)Two-loop mixed QCD-EW corrections to $q \overline{q} \to H g$, $qg \to Hq$, and $\overline{q}g \to H\overline{q}$
• Marco Bonetti,
• Erik Panzer,
• Lorenzo Tancredi
arXiv e-prints (03/2022) e-Print:2203.17202
abstract + abstract -

We compute the two-loop mixed QCD-Electroweak corrections to $q \overline{q} \to H g$ and its crossed channels $q g \to H q$, $\overline{q} g \to H \overline{q}$, limiting ourselves to the contribution of light virtual quarks. We compute the independent helicity amplitudes as well as the form factors for this process, expressing them in terms of hyperlogarithms with algebraic arguments. The Feynman integrals are computed by direct integration over Feynman parameters and the results are expressed in terms of a basis of rational prefactors.

(354)Pseudo-Kähler-Einstein geometries
• Carlos G. Boiza,
• Jose A. R. Cembranos
Physical Review D, 105 (03/2022) doi:10.1103/PhysRevD.105.065006
abstract + abstract -

Solutions to vacuum Einstein field equations with cosmological constants, such as the de Sitter space and the anti-de Sitter space, are basic in different cosmological and theoretical developments. It is also well known that complex structures admit metrics of this type. The most famous example is the complex projective space endowed with the Fubini-Study metric. In this work, we perform a systematic study of Einstein complex geometries derived from a logarithmic Kähler potential. Depending on the different contribution to the argument of such logarithmic term, we shall distinguish among direct, inverted and hybrid coordinates. They are directly related to the signature of the metric and determine the maximum domain of the complex space where the geometry can be defined.

(353)Mineral Snowflakes on Exoplanets and Brown Dwarfs: Coagulation and Fragmentation of Cloud Particles with {\sc HyLandS}
• Dominic Samra,
• Christiane Helling,
• Tilman Birnstiel
arXiv e-prints (03/2022) e-Print:2203.07461
abstract + abstract -

Brown dwarfs and exoplanets provide unique atmospheric regimes that hold information about their formation routes and evolutionary states. Modelling mineral cloud particle formation is key to prepare for missions and instruments like CRIRES+, JWST and ARIEL as well as possible polarimetry missions like {\sc PolStar}. The aim is to support more detailed observations that demand greater understanding of microphysical cloud processes. We extend our kinetic cloud formation model that treats nucleation, condensation, evaporation and settling of mixed material cloud particles to consistently model cloud particle-particle collisions. The new hybrid code, {\sc HyLandS}, is applied to a grid of {\sc Drift-Phoenix} (T, p)-profiles. Effective medium theory and Mie theory are used to investigate the optical properties. Turbulence is the main driving process of collisions, with collisions becoming the dominant process at the cloud base ($p>10^{-4}\,{\rm bar}$). Collisions produce one of three outcomes: fragmenting atmospheres ($\log_{10}(g)=3$), coagulating atmospheres ($\log_{10}(g)=5$, $T_{\rm eff} \leq 1800\, {\rm K}$) and condensational growth dominated atmospheres ($\log_{10}(g\,)=5$, $T_{\rm eff} > 1800\, {\rm K}$). Cloud particle opacity slope at optical wavelengths (HST) is increased with fragmentation, as are the silicate features at mid-infrared wavelengths. The hybrid moment-bin method {\sc HyLandS} demonstrates the feasibility of combining a moment and a bin method whilst assuring element conservation. It provides a powerful and fast tool for capturing general trends of particle collisions, consistently with other microphysical processes. Collisions are important in exoplanet and brown dwarf atmospheres but cannot be assumed to be hit-and-stick only. The spectral effects of collisions complicates inferences of cloud particle size and material composition from observational data.

(352)Rare radiative decays of charm baryons
• Nico Adolph,
• Gudrun Hiller
arXiv e-prints (03/2022) e-Print:2203.14982
abstract + abstract -

We study weak radiative $|\Delta c|=|\Delta u|=1$ decays of the charmed anti-triplett ($\Lambda_c$, $\Xi_c^{+}$, $\Xi_c^{0}$) and sextet ($\Sigma_c^{++}$, $\Sigma_c^+$, $\Sigma_c^0$, $\Xi_c^{\prime +}$, $\Xi_c^{\prime 0}$, $\Omega_c$) baryons in the standard model (SM) and beyond. We work out $SU(2)$ and $SU(3)_F$-symmetry relations. We propose to study self-analyzing decay chains such as $\Xi_c^+ \to \Sigma^+ (\to p \pi^0) \gamma$ and $\Xi_c^0 \to \Lambda (\to p \pi^-) \gamma$, which enable new physics sensitive polarization studies. SM contributions can be controlled by corresponding analysis of the Cabibbo-favored decays $\Lambda_c^+ \to \Sigma^+ (\to p \pi^0) \gamma$ and $\Xi_c^0 \to \Xi^0 (\to \Lambda \pi^0) \gamma$. Further tests of the SM are available with initially polarized baryons including $\Lambda_c \to p \gamma$ together with $\Lambda_c \to \Sigma^+ \gamma$ decays, or $\Omega_c \to \Xi^0 \gamma$ together with $\Omega_c \to (\Lambda,\Sigma^0) \gamma$. In addition, CP-violating new physics contributions to dipole operators can enhance CP-asymmetries up to few percent.

(351)Data and Analysis Preservation, Recasting, and Reinterpretation
• Stephen Bailey,
• Christian Bierlich,
• Andy Buckley,
• Jon Butterworth,
• Kyle Cranmer
• +13
• Matthew Feickert,
• Lukas Heinrich,
• Axel Huebl,
• Sabine Kraml,
• Anders Kvellestad,
• Clemens Lange,
• Andre Lessa,
• Kati Lassila-Perini,
• Christine Nattrass,
• Mark S. Neubauer,
• Sezen Sekmen,
• Giordon Stark,
• Graeme Watt
• (less)
arXiv e-prints (03/2022) e-Print:2203.10057
abstract + abstract -

We make the case for the systematic, reliable preservation of event-wise data, derived data products, and executable analysis code. This preservation enables the analyses' long-term future reuse, in order to maximise the scientific impact of publicly funded particle-physics experiments. We cover the needs of both the experimental and theoretical particle physics communities, and outline the goals and benefits that are uniquely enabled by analysis recasting and reinterpretation. We also discuss technical challenges and infrastructure needs, as well as sociological challenges and changes, and give summary recommendations to the particle-physics community.

(350)Systematic Parametrization of the Leading $B$-meson Light-Cone Distribution Amplitude
• Thorsten Feldmann,
• Philip Lüghausen,
• Danny van Dyk
arXiv e-prints (03/2022) e-Print:2203.15679
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 ${}_1F_1$ 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 production expansion. We showcase the versatility of the parametrization in a series of phenomenological pseudo-fits.

(349)Complementarity of experiments in probing the non-relativistic effective theory of dark matter-nucleon interactions
• Anja Brenner,
• Gonzalo Herrera,
• Alejandro Ibarra,
• Sunghyun Kang,
• Stefano Scopel
• +1
arXiv e-prints (03/2022) e-Print:2203.04210
abstract + abstract -

The non-relativistic effective theory of dark matter-nucleon interactions depends on 28 coupling strengths for dark matter spin up to 1/2. Due to the vast parameter space of the effective theory, most experiments searching for dark matter interpret the results assuming that only one of the coupling strengths is non-zero. On the other hand, dark matter models generically lead in the non-relativistic limit to several interactions which interfere with one another, therefore the published limits cannot be straightforwardly applied to model predictions. We present a method to determine a rigorous upper limit on the dark matter-nucleon interaction strength including all possible interferences among operators. We illustrate the method to derive model independent upper limits on the interaction strengths from the null search results from XENON1T, PICO-60 and IceCube. For some interactions, the limits on the coupling strengths are relaxed by more than one order of magnitude. We also present a method that allows to combine the results from different experiments, thus exploiting the synergy between different targets in exploring the parameter space of dark matter-nucleon interactions.

(348)A new tool to search for physics beyond the Standard Model in ${\bar B}\to D^{*+}\ell^- {\bar\nu}$
• Bhubanjyoti Bhattacharya,
• Thomas Browder,
• Quinn Campagna,
• Alakabha Datta,
• Shawn Dubey
• +2
• Lopamudra Mukherjee,
• Alexei Sibidanov
• (less)
arXiv e-prints (03/2022) e-Print:2203.07189
abstract + abstract -

Recent experimental results in $B$ physics from Belle, BaBar and LHCb suggest new physics (NP) in the weak $b\to c$ charged-current and the $b\to s$ neutral-current processes. Here we focus on the charged-current case and specifically on the decay modes $B\to D^{*+}\ell^- \bar{\nu}$ with $\ell = e, \mu,$ and $\tau$. The world averages of the ratios $R_D$ and $R_D^{*}$ currently differ from the Standard Model (SM) by $3.4\sigma$ while $\Delta A_{FB} = A_{FB}(B\to D^{*} \mu\nu) - A_{FB} (B\to D^{*} e \nu)$ is found to be $4.1\sigma$ away from the SM prediction in an analysis of 2019 Belle data. These intriguing results suggest an urgent need for improved simulation and analysis techniques in $B\to D^{*+}\ell^- \bar{\nu}$ decays. Here we describe a Monte Carlo Event-generator tool based on EVTGEN developed to allow simulation of the NP signatures in $B\to D^*\ell^- \nu$, which arise due to the interference between the SM and NP amplitudes. As a demonstration of the proposed approach, we exhibit some examples of NP couplings that are consistent with current data and could explain the $\Delta A_{FB}$ anomaly in $B\to D^*\ell^- \nu$ while remaining consistent with other constraints. We show that the $\Delta$-type observables such as $\Delta A_{FB}$ and $\Delta S_5$ eliminate most QCD uncertainties from form factors and allow for clean measurements of NP. We introduce correlated observables that improve the sensitivity to NP. We discuss prospects for improved observables sensitive to NP couplings with the expected 50 ab$^{-1}$ of Belle II data, which seems to be ideally suited for this class of measurements.

(347)On the Importance of Rare Kaon Decays: A Snowmass 2021 White Paper
• Jason Aebischer,
• Andrzej J. Buras,
• Jacky Kumar
arXiv e-prints (03/2022) e-Print:2203.09524
abstract + abstract -

We stress the importance of precise measurements of rare decays $K^+\rightarrow\pi^+\nu\bar\nu$, $K_L\rightarrow\pi^0\nu\bar\nu$, $K_{L,S}\to\mu^+\mu^-$ and $K_{L,S}\to\pi^0\ell^+\ell^-$ for the search of new physics (NP). This includes both branching ratios and the distributions in $q^2$, the invariant mass-squared of the neutrino system in the case of $K^+\rightarrow\pi^+\nu\bar\nu$ and $K_L\rightarrow\pi^0\nu\bar\nu$ and of the $\ell^+\ell^-$ system in the case of the remaining decays. In particular the correlations between these observables and their correlations with the ratio $\varepsilon'/\varepsilon$ in $K_L\to\pi\pi$ decays, the CP-violating parameter $\varepsilon_K$ and the $K^0-\bar K^0$ mass difference $\Delta M_K$, should help to disentangle the nature of possible NP. We stress the strong sensitivity of all observables with the exception of $\Delta M_K$ to the CKM parameter $|V_{cb}|$ and list a number of $|V_{cb}|$-independent ratios within the SM which exhibit rather different dependences on the angles $\beta$ and $\gamma$ of the unitarity triangle. The particular role of these decays in probing very short distance scales far beyond the ones explored at the LHC is emphasized. In this context the role of the Standard Model Effective Field Theory (SMEFT) is very important. We also address briefly the issue of the footprints of Majorana neutrinos in $K^+\rightarrow\pi^+\nu\bar\nu$ and $K_L\rightarrow\pi^0\nu\bar\nu$.

(346)Cosmic Birefringence from the Planck Data Release 4
• P. Diego-Palazuelos,
• J. R. Eskilt,
• Y. Minami,
• M. Tristram,
• R. M. Sullivan
• +10
• A. J. Banday,
• R. B. Barreiro,
• H. K. Eriksen,
• K. M. Górski,
• R. Keskitalo,
• E. Komatsu,
• E. Martínez-González,
• D. Scott,
• P. Vielva,
• I. K. Wehus
• (less)
Physical Review Letters, 128 (03/2022) doi:10.1103/PhysRevLett.128.091302
abstract + abstract -

We search for the signature of parity-violating physics in the cosmic microwave background, called cosmic birefringence, using the Planck data release 4. We initially find a birefringence angle of β =0.30 °±0.11 ° (68% C.L.) for nearly full-sky data. The values of β decrease as we enlarge the Galactic mask, which can be interpreted as the effect of polarized foreground emission. Two independent ways to model this effect are used to mitigate the systematic impact on β for different sky fractions. We choose not to assign cosmological significance to the measured value of β until we improve our knowledge of the foreground polarization.

(345)Filament collapse: A two phase process
• Elena Hoemann,
• Stefan Heigl,
• Andreas Burkert
arXiv e-prints (03/2022) e-Print:2203.07002
abstract + abstract -

Using numerical simulations, we investigate the gravitational evolution of filamentary molecular cloud structures and their condensation into dense protostellar cores. One possible process is the so called 'edge effect', the pile-up of matter at the end of the filament due to self-gravity. This effect is predicted by theory but only rarely observed. To get a better understanding of the underlying processes we used a simple analytic approach to describe the collapse and the corresponding collapse time. We identify a model of two distinct phases: The first phase is free fall dominated, due to the self-gravity of the filament. In the second phase, after the turning point, the collapse is balanced by the ram pressure, produced by the inside material of the filament, which leads to a constant collapse velocity. This approach reproduces the established collapse time of uniform density filaments and agrees well with our hydrodynamic simulations. In addition, we investigate the influence of different radial density profiles on the collapse. We find that the deviations compared to the uniform filament are less than 10%. Therefore, the analytic collapse model of the uniform density filament is an excellent general approach.

(344)Radiopurity of a kg-scale PbWO$_4$ cryogenic detector produced from archaeological Pb for the RES-NOVA experiment
• J. W. Beeman,
• G. Benato,
• C. Bucci,
• L. Canonica,
• P. Carniti
• +39
• E. Celi,
• M. Clemenza,
• A. D'Addabbo,
• F. A. Danevich,
• S. Di Domizio,
• S. Di Lorenzo,
• 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. Schoenert,
• D. A. Solopikhin,
• R. Strauss,
• E. Tarabini,
• V. I. Tretyak,
• I. A. Tupitsyna,
• V. Wagner
• (less)
arXiv e-prints (03/2022) e-Print:2203.07441
abstract + abstract -

RES-NOVA is a newly proposed experiment for the detection of neutrinos from astrophysical sources, mainly Supernovae, using an array of cryogenic detectors made of PbWO$_4$ crystals produced from archaeological Pb. This unconventional material, characterized by intrinsic high radiopurity, enables to achieve low-background levels in the region of interest for the neutrino detection via Coherent Elastic neutrino-Nucleus Scattering (CE$\nu$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 PbWO$_4$ crystal produced from archaeological Pb operated as a cryogenic detector. The crystal internal radioactive contaminations are: $^{232}$Th $<$40 $\mu$Bq/kg, $^{238}$U $<$30 $\mu$Bq/kg, $^{226}$Ra 1.3 mBq/kg and $^{210}$Pb 22.5 mBq/kg. We present also 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.

(343)Joint analysis of DES Year 3 data and CMB lensing from SPT and Planck II: Cross-correlation measurements and cosmological constraints
• C. Chang,
• Y. Omori,
• E. J. Baxter,
• C. Doux,
• A. Choi
• +161
• S. Pandey,
• A. Alarcon,
• O. Alves,
• A. Amon,
• F. Andrade-Oliveira,
• K. Bechtol,
• M. R. Becker,
• G. M. Bernstein,
• F. Bianchini,
• J. Blazek,
• L. E. Bleem,
• H. Camacho,
• A. Campos,
• A. Carnero Rosell,
• M. Carrasco Kind,
• R. Cawthon,
• R. Chen,
• J. Cordero,
• T. M. Crawford,
• M. Crocce,
• C. Davis,
• J. DeRose,
• S. Dodelson,
• A. Drlica-Wagner,
• K. Eckert,
• T. F. Eifler,
• F. Elsner,
• J. Elvin-Poole,
• S. Everett,
• X. Fang,
• A. Ferté,
• P. Fosalba,
• O. Friedrich,
• M. Gatti,
• G. Giannini,
• D. Gruen,
• R. A. Gruendl,
• I. Harrison,
• K. Herner,
• H. Huang,
• E. M. Huff,
• D. Huterer,
• M. Jarvis,
• A. Kovacs,
• E. Krause,
• N. Kuropatkin,
• P. -F. Leget,
• P. Lemos,
• A. R. Liddle,
• N. MacCrann,
• J. McCullough,
• J. Muir,
• J. Myles,
• A. Navarro-Alsina,
• Y. Park,
• A. Porredon,
• J. Prat,
• M. Raveri,
• R. P. Rollins,
• A. Roodman,
• R. Rosenfeld,
• A. J. Ross,
• E. S. Rykoff,
• C. Sánchez,
• J. Sanchez,
• L. F. Secco,
• I. Sevilla-Noarbe,
• E. Sheldon,
• T. Shin,
• M. A. Troxel,
• I. Tutusaus,
• T. N. Varga,
• N. Weaverdyck,
• R. H. Wechsler,
• W. L. K. Wu,
• B. Yanny,
• B. Yin,
• Y. Zhang,
• J. Zuntz,
• T. M. C. Abbott,
• M. Aguena,
• S. Allam,
• J. Annis,
• D. Bacon,
• B. A. Benson,
• E. Bertin,
• S. Bocquet,
• D. Brooks,
• D. L. Burke,
• J. E. Carlstrom,
• J. Carretero,
• C. L. Chang,
• R. Chown,
• M. Costanzi,
• L. N. da Costa,
• A. T. Crites,
• M. E. S. Pereira,
• T. de Haan,
• J. De Vicente,
• S. Desai,
• H. T. Diehl,
• M. A. Dobbs,
• P. Doel,
• W. Everett,
• I. Ferrero,
• B. Flaugher,
• D. Friedel,
• J. Frieman,
• J. García-Bellido,
• E. Gaztanaga,
• E. M. George,
• T. Giannantonio,
• 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,
• O. Lahav,
• A. T. Lee,
• M. Lima,
• D. Luong-Van,
• M. March,
• J. J. McMahon,
• P. Melchior,
• F. Menanteau,
• S. S. Meyer,
• R. Miquel,
• L. Mocanu,
• J. J. Mohr,
• R. Morgan,
• T. Natoli,
• S. Padin,
• A. Palmese,
• F. Paz-Chinchón,
• A. Pieres,
• A. A. Plazas Malagón,
• C. Pryke,
• C. L. Reichardt,
• M. Rodríguez-Monroy,
• A. K. Romer,
• J. E. Ruhl,
• E. Sanchez,
• K. K. Schaffer,
• M. Schubnell,
• S. Serrano,
• E. Shirokoff,
• M. Smith,
• Z. Staniszewski,
• A. A. Stark,
• E. Suchyta,
• G. Tarle,
• D. Thomas,
• C. To,
• J. D. Vieira,
• J. Weller,
• R. Williamson
• (less)
arXiv e-prints (03/2022) e-Print:2203.12440
abstract + abstract -

Cross-correlations of galaxy positions and galaxy shears with maps of gravitational lensing of the cosmic microwave background (CMB) are sensitive to the distribution of large-scale structure in the Universe. Such cross-correlations are also expected to be immune to some of the systematic effects that complicate correlation measurements internal to galaxy surveys. We present measurements and modeling of the cross-correlations between galaxy positions and galaxy lensing measured in the first three years of data from the Dark Energy Survey with CMB lensing maps derived from a combination of data from the 2500 deg$^2$ SPT-SZ survey conducted with the South Pole Telescope and full-sky data from the Planck satellite. The CMB lensing maps used in this analysis have been constructed in a way that minimizes biases from the thermal Sunyaev Zel'dovich effect, making them well suited for cross-correlation studies. The total signal-to-noise of the cross-correlation measurements is 23.9 (25.7) when using a choice of angular scales optimized for a linear (nonlinear) galaxy bias model. We use the cross-correlation measurements to obtain constraints on cosmological parameters. For our fiducial galaxy sample, which consist of four bins of magnitude-selected galaxies, we find constraints of $\Omega_{m} = 0.272^{+0.032}_{-0.052}$ and $S_{8} \equiv \sigma_8 \sqrt{\Omega_{m}/0.3}= 0.736^{+0.032}_{-0.028}$ ($\Omega_{m} = 0.245^{+0.026}_{-0.044}$ and $S_{8} = 0.734^{+0.035}_{-0.028}$) when assuming linear (nonlinear) galaxy bias in our modeling. Considering only the cross-correlation of galaxy shear with CMB lensing, we find $\Omega_{m} = 0.270^{+0.043}_{-0.061}$ and $S_{8} = 0.740^{+0.034}_{-0.029}$. Our constraints on $S_8$ are consistent with recent cosmic shear measurements, but lower than the values preferred by primary CMB measurements from Planck.

(342)Hydro-, Magnetohydro-, and Dust-Gas Dynamics of Protoplanetary Disks
• G. Lesur,
• B. Ercolano,
• M. Flock,
• M. -K. Lin,
• C. -C. Yang
• +14
• J. A. Barranco,
• P. Benitez-Llambay,
• J. Goodman,
• A. Johansen,
• H. Klahr,
• G. Laibe,
• W. Lyra,
• P. Marcus,
• R. P. Nelson,
• J. Squire,
• J. B. Simon,
• N. Turner,
• O. M. Umurhan,
• A. N. Youdin
• (less)
arXiv e-prints (03/2022) e-Print:2203.09821
abstract + abstract -

The building of planetary systems is controlled by the gas and dust dynamics of protoplanetary disks. While the gas is simultaneously accreted onto the central star and dissipated away by winds, dust grains aggregate and collapse to form planetesimals and eventually planets. This dust and gas dynamics involves instabilities, turbulence and complex non-linear interactions which ultimately control the observational appearance and the secular evolution of these disks. This chapter is dedicated to the most recent developments in our understanding of the dynamics of gaseous and dusty disks, covering hydrodynamic and magnetohydrodynamic turbulence, gas-dust instabilities, dust clumping and disk winds. We show how these physical processes have been tested from observations and highlight standing questions that should be addressed in the future.

(341)Learning Optimal Test Statistics in the Presence of Nuisance Parameters
• Lukas Heinrich
arXiv e-prints (03/2022) e-Print:2203.13079
abstract + abstract -

The design of optimal test statistics is a key task in frequentist statistics and for a number of scenarios optimal test statistics such as the profile-likelihood ratio are known. By turning this argument around we can find the profile likelihood ratio even in likelihood-free cases, where only samples from a simulator are available, by optimizing a test statistic within those scenarios. We propose a likelihood-free training algorithm that produces test statistics that are equivalent to the profile likelihood ratios in cases where the latter is known to be optimal.

(340)The Exclusive Vision of Rare $K$ and $B$ Decays and of the Quark Mixing in the Standard Model
• Andrzej J. Buras,
• Elena Venturini
arXiv e-prints (03/2022) e-Print:2203.11960
abstract + abstract -

The most common predictions for rare $K$ and $B$ decay branching ratios in the Standard Model are based on the CKM elements $|V_{cb}|$ and $|V_{ub}|$ resulting from global fits, that are in the ballpark of their inclusive and exclusive determinations, respectively. In the present paper we follow another route. We assume that the future true values of $|V_{cb}|$ and $|V_{ub}|$ will be both from exclusive determinations and set them equal to the most recent ones from FLAG. An unusual pattern of SM predictions results from this study with some existing tensions being dwarfed and new tensions being born. In particular using the HPQCD $B^0_{s,d}-\bar B^0_{s,d}$ hadronic matrix elements a $3.1\sigma$ tension in $\Delta M_s$ independently of $\gamma$ is found. For $60^\circ\le\gamma\le 75^\circ$ the tension in $\Delta M_d$ between $4.0\sigma$ and $1.1\sigma$ is found and in the case of $\epsilon_K$ between $5.2\sigma$ and $2.1\sigma$. Moreover, the room for new physics in $K^+\to\pi^+\nu\bar\nu$, $K_L\to\pi^0\nu\bar\nu$ and $B\to K(K^*)\nu\bar\nu$ decays is significantly increased. We compare the results in this EXCLUSIVE scenario with the HYBRID one in which $|V_{cb}|$ in the former scenario is replaced by the most recent inclusive $|V_{cb}|$ and present the dependence of all observables considered by us in both scenarios as functions of $\gamma$. We also compare the determination of $|V_{cb}|$ from $\Delta M_s$, $\Delta M_d$, $\epsilon_K$ and $S_{\psi K_S}$ using $B^0_{s,d}-\bar B^0_{s,d}$ hadronic matrix elements from LQCD with $2+1+1$ flavours, $2+1$ flavours and their average. Only for the $2+1+1$ case values for $\beta$ and $\gamma$ exist for which the same value of $|V_{cb}|$ is found: $|V_{cb}|=42.6(7)\times 10^{-3}$. This in turn implies a $2.7\sigma$ anomaly in $B_s\to\mu^+\mu^-$.

(339)Snowmass white paper: Need for amplitude analysis in the discovery of new hadrons
• Miguel Albaladejo,
• Marco Battaglieri,
• Lukasz Bibrzycki,
• Andrea Celentano,
• Igor V. Danilkin
• +20
• Sebastian M. Dawid,
• Michael Doring,
• Cristiano Fanelli,
• Cesar Fernandez-Ramirez,
• Sergi Gonzalez-Solis,
• Astrid N. Hiller Blin,
• Andrew W. Jackura,
• Vincent Mathieu,
• Mikhail Mikhasenko,
• Victor I. Mokeev,
• Emilie Passemar,
• Robert J. Perry,
• Alessandro Pilloni,
• Arkaitz Rodas,
• Matthew R. Shepherd,
• Nathaniel Sherrill,
• Jorge A. Silva-Castro,
• Tomasz Skwarnicki,
• Adam P. Szczepaniak,
• Daniel Winney
• (less)
arXiv e-prints (03/2022) e-Print:2203.08208
abstract + abstract -

We highlight the need for the development of comprehensive amplitude analysis methods to further our understanding of hadron spectroscopy. Reaction amplitudes constrained by first principles of $S$-matrix theory and by QCD phenomenology are needed to extract robust interpretations of the data from experiments and from lattice calculations.

(338)Is cosmic birefringence due to dark energy or dark matter? A tomographic approach
• Hiromasa Nakatsuka,
• Toshiya Namikawa,
• Eiichiro Komatsu
arXiv e-prints (03/2022) e-Print:2203.08560
abstract + abstract -

A pseudoscalar "axionlike" field, $\phi$, may explain the $3\sigma$ hint of cosmic birefringence observed in the $EB$ power spectrum of the cosmic microwave background (CMB) polarization data. Is $\phi$ dark energy or dark matter? A tomographic approach can answer this question. The effective mass of dark energy field responsible for the accelerated expansion of the Universe today must be smaller than $m_\phi\simeq 10^{-33}$ eV. If $m_\phi \gtrsim 10^{-32}$ eV, $\phi$ starts evolving before the epoch of reionization and we should observe different amounts of birefringence from the $EB$ power spectrum at low ($l\lesssim 10$) and high multipoles. Such an observation, which requires a full-sky satellite mission, would rule out $\phi$ being dark energy. If $m_\phi \gtrsim 10^{-28}$ eV, $\phi$ starts oscillating during the epoch of recombination, leaving a distinct signature in the $EB$ power spectrum at high multipoles, which can be measured precisely by ground-based CMB observations. Our tomographic approach relies on the shape of the $EB$ power spectrum and is less sensitive to miscalibration of polarization angles.

(337)Standard Model Predictions for Rare $K$ and $B$ Decays without $|V_{cb}|$ and $|V_{ub}|$ Uncertainties
• Andrzej J. Buras,
• Elena Venturini
arXiv e-prints (03/2022) e-Print:2203.10099
abstract + abstract -

The persistent tensions between inclusive and exclusive determinations of $|V_{cb}|$ and $|V_{ub}|$ weaken the power of theoretically clean rare $K$ and $B$ decays in the search for new physics (NP). We demonstrate how this uncertainty can be practically removed by considering within the SM suitable ratios of various branching ratios. This includes the branching ratios for $K^+\to\pi^+\nu\bar\nu$, $K_{L}\to\pi^0\nu\bar\nu$, $K_S\to\mu^+\mu^-$, $B_{s,d}\to\mu^+\mu^-$ and $B\to K(K^*)\nu\bar\nu$. Also $\epsilon_K$, $\Delta M_d$, $\Delta M_s$ and the mixing induced CP-asymmetry $S_{\psi K_S}$, all measured already very precisely, play an important role in this analysis. The highlights of our analysis are 16 $|V_{cb}|$ and $|V_{ub}|$ independent ratios that often are independent of the CKM arameters or depend only on the angles $\beta$ and $\gamma$ in the Unitarity Triangle with $\beta$ already precisely known and $\gamma$ to be measured precisely in the coming years by the LHCb and Belle II collaborations. Once $\gamma$ Once $\gamma$ is measured precisely these 16 ratios taken together are expected to be a powerful tool in the search for new physics. Assuming no NP in $|\epsilon_K|$ and $S_{\psi K_S}$ we determine independently of $|V_{cb}|$: $\mathcal{B}(K^+\to\pi^+\nu\bar\nu)_\text{SM}= (8.60\pm0.42)\times 10^{-11}$ and $\mathcal{B}(K_L\to\pi^0\nu\bar\nu)_\text{SM}=(2.94\pm 0.15)\times 10^{-11}$. This are the most precise determinations to date. Assuming no NP in $\Delta M_{s,d}$ allows to obtain analogous results for all $B$ decay branching ratios considered in our paper without any CKM uncertainties.

(336)Dust entrainment in photoevaporative winds: Synthetic observations of transition disks
• R. Franz,
• G. Picogna,
• B. Ercolano,
• S. Casassus,
• T. Birnstiel
• +2
Astronomy and Astrophysics, 659, p29 (03/2022) doi:10.1051/0004-6361/202142785
abstract + abstract -

Context. X-ray- and extreme-ultraviolet- (XEUV-) driven photoevaporative winds acting on protoplanetary disks around young T Tauri stars may strongly impact disk evolution, affecting both gas and dust distributions. Small dust grains in the disk are entrained in the outflow and may produce a detectable signal. In this work, we investigate the possibility of detecting dusty outflows from transition disks with an inner cavity.
Aims: We compute dust densities for the wind regions of XEUV-irradiated transition disks and determine whether they can be observed at wavelengths 0.7 ≲ λobs [μm] ≲ 1.8 with current instrumentation.
Methods: We simulated dust trajectories on top of 2D hydrodynamical gas models of two transition disks with inner holes of 20 and 30 AU, irradiated by both X-ray and EUV spectra from a central T Tauri star. The trajectories and two different settling prescriptions for the dust distribution in the underlying disk were used to calculate wind density maps for individual grain sizes. Finally, the resulting dust densities were converted to synthetic observations in scattered and polarised light.
Results: For an XEUV-driven outflow around a M* = 0.7 M T Tauri star with LX = 2 × 1030 erg s-1, we find dust mass-loss rates Ṁdust ≲ 2.0 × 10−3gas, and if we invoke vertical settling, the outflow is quite collimated. The synthesised images exhibit a distinct chimney-like structure. The relative intensity of the chimneys is low, but their detection may still be feasible with current instrumentation under optimal conditions.
Conclusions: Our results motivate observational campaigns aimed at the detection of dusty photoevaporative winds in transition disks using JWST NIRCam and SPHERE IRDIS.

(335)New constraints on axion-gauge field dynamics during inflation from Planck and BICEP/Keck data sets
• Paolo Campeti,
• Ogan Özsoy,
• Ippei Obata,
• Maresuke Shiraishi
arXiv e-prints (03/2022) e-Print:2203.03401
abstract + abstract -

We present new constraints on spectator axion-${\rm U}(1)$ gauge field interactions during inflation using the latest Planck ($PR4$) and BICEP/Keck 2018 data releases. This model can source tensor perturbations from amplified gauge field fluctuations, driven by an axion rolling for a few e-folds during inflation. The gravitational waves sourced in this way have a strongly scale-dependent (and chiral) spectrum, with potentially visible contributions to large/intermediate scale $B$-modes of the CMB. We first derive theoretical bounds on the model imposing validity of the perturbative regime and negligible backreaction of the gauge field on the background dynamics. Then, we determine bounds from current CMB observations, adopting a frequentist profile likelihood approach. We study the behaviour of constraints for typical choices of the model's parameters, analyzing the impact of different dataset combinations. We find that observational bounds are competitive with theoretical ones and together they exclude a significant portion of the model's parameter space. We argue that the parameter space still remains large and interesting for future CMB experiments targeting large/intermediate scales $B$-modes.

(334)Discovery and mass measurement of the hot, transiting, Earth-sized planet, GJ 3929 b
• J. Kemmer,
• S. Dreizler,
• D. Kossakowski,
• S. Stock,
• A. Quirrenbach
• +62
• J. A. Caballero,
• P. J. Amado,
• K. A. Collins,
• N. Espinoza,
• E. Herrero,
• J. M. Jenkins,
• D. W. Latham,
• J. Lillo-Box,
• N. Narita,
• E. Pallé,
• A. Reiners,
• I. Ribas,
• G. Ricker,
• E. Rodríguez,
• S. Seager,
• R. Vanderspek,
• R. Wells,
• J. Winn,
• F. J. Aceituno,
• V. J. S. Béjar,
• T. Barclay,
• P. Bluhm,
• P. Chaturvedi,
• C. Cifuentes,
• K. I. Collins,
• M. Cortés-Contreras,
• B. -O. Demory,
• M. M. Fausnaugh,
• A. Fukui,
• Y. Gómez Maqueo Chew,
• D. Galadí-Enríquez,
• T. Gan,
• M. Gillon,
• A. Golovin,
• A. P. Hatzes,
• Th. Henning,
• C. Huang,
• S. V. Jeffers,
• A. Kaminski,
• M. Kunimoto,
• M. Kürster,
• M. J. López-González,
• M. Lafarga,
• R. Luque,
• J. McCormac,
• K. Molaverdikhani,
• D. Montes,
• J. C. Morales,
• V. M. Passegger,
• S. Reffert,
• L. Sabin,
• P. Schöfer,
• N. Schanche,
• M. Schlecker,
• U. Schroffenegger,
• R. P. Schwarz,
• A. Schweitzer,
• A. Sota,
• P. Tenenbaum,
• T. Trifonov,
• S. Vanaverbeke,
• M. Zechmeister
• (less)
Astronomy and Astrophysics, 659, p23 (03/2022) doi:10.1051/0004-6361/202142653
abstract + abstract -

We report the discovery of GJ 3929 b, a hot Earth-sized planet orbiting the nearby M3.5 V dwarf star, GJ 3929 (G 180-18, TOI-2013). Joint modelling of photometric observations from TESS sectors 24 and 25 together with 73 spectroscopic observations from CARMENES and follow-up transit observations from SAINT-EX, LCOGT, and OSN yields a planet radius of Rb = 1.150 ± 0.040 R, a mass of Mb = 1.21 ± 0.42 M, and an orbital period of Pb = 2.6162745 ± 0.0000030 d. The resulting density of ρb = 4.4 ± 1.6 g cm−3 is compatible with the Earth's mean density of about 5.5 g cm−3. Due to the apparent brightness of the host star (J = 8.7 mag) and its small size, GJ 3929 b is a promising target for atmospheric characterisation with the JWST. Additionally, the radial velocity data show evidence for another planet candidate with P[c] = 14.303 ± 0.035 d, which is likely unrelated to the stellar rotation period, Prot = 122 ± 13 d, which we determined from archival HATNet and ASAS-SN photometry combined with newly obtained TJO data.

RV data and stellar activity indices 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/659/A17

(333)Toward the End-to-End Optimization of Particle Physics Instruments with Differentiable Programming: a White Paper
• Tommaso Dorigo,
• Andrea Giammanco,
• Pietro Vischia,
• Max Aehle,
• Mateusz Bawaj
• +31
• Alexey Boldyrev,
• Pablo de Castro Manzano,
• Denis Derkach,
• Julien Donini,
• Auralee Edelen,
• Federica Fanzago,
• Nicolas R. Gauger,
• Christian Glaser,
• Atılım G. Baydin,
• Lukas Heinrich,
• Ralf Keidel,
• Jan Kieseler,
• Claudius Krause,
• Maxime Lagrange,
• Max Lamparth,
• Lukas Layer,
• Gernot Maier,
• Federico Nardi,
• Helge E. S. Pettersen,
• Alberto Ramos,
• Fedor Ratnikov,
• Dieter Röhrich,
• Roberto Ruiz de Austri,
• Pablo Martínez Ruiz del Árbol,
• Oleg Savchenko,
• Nathan Simpson,
• Giles C. Strong,
• Angela Taliercio,
• Mia Tosi,
• Andrey Ustyuzhanin,
• Haitham Zaraket
• (less)
arXiv e-prints (03/2022) e-Print:2203.13818
abstract + abstract -

The full optimization of the design and operation of instruments whose functioning relies on the interaction of radiation with matter is a super-human task, given the large dimensionality of the space of possible choices for geometry, detection technology, materials, data-acquisition, and information-extraction techniques, and the interdependence of the related parameters. On the other hand, massive potential gains in performance over standard, "experience-driven" layouts are in principle within our reach if an objective function fully aligned with the final goals of the instrument is maximized by means of a systematic search of the configuration space. The stochastic nature of the involved quantum processes make the modeling of these systems an intractable problem from a classical statistics point of view, yet the construction of a fully differentiable pipeline and the use of deep learning techniques may allow the simultaneous optimization of all design parameters. In this document we lay down our plans for the design of a modular and versatile modeling tool for the end-to-end optimization of complex instruments for particle physics experiments as well as industrial and medical applications that share the detection of radiation as their basic ingredient. We consider a selected set of use cases to highlight the specific needs of different applications.

(332)Joint analysis of DES Year 3 data and CMB lensing from SPT and Planck I: Construction of CMB Lensing Maps and Modeling Choices
• Y. Omori,
• E. J. Baxter,
• C. Chang,
• O. Friedrich,
• A. Alarcon
• +158
• O. Alves,
• A. Amon,
• F. Andrade-Oliveira,
• K. Bechtol,
• M. R. Becker,
• G. M. Bernstein,
• J. Blazek,
• L. E. Bleem,
• H. Camacho,
• A. Campos,
• A. Carnero Rosell,
• M. Carrasco Kind,
• R. Cawthon,
• R. Chen,
• A. Choi,
• J. Cordero,
• T. M. Crawford,
• M. Crocce,
• C. Davis,
• J. DeRose,
• S. Dodelson,
• C. Doux,
• A. Drlica-Wagner,
• K. Eckert,
• T. F. Eifler,
• F. Elsner,
• J. Elvin-Poole,
• S. Everett,
• X. Fang,
• A. Ferté,
• P. Fosalba,
• M. Gatti,
• G. Giannini,
• D. Gruen,
• R. A. Gruendl,
• I. Harrison,
• K. Herner,
• H. Huang,
• E. M. Huff,
• D. Huterer,
• M. Jarvis,
• E. Krause,
• N. Kuropatkin,
• P. -F. Leget,
• P. Lemos,
• A. R. Liddle,
• N. MacCrann,
• J. McCullough,
• J. Muir,
• J. Myles,
• A. Navarro-Alsina,
• S. Pandey,
• Y. Park,
• A. Porredon,
• J. Prat,
• M. Raveri,
• R. P. Rollins,
• A. Roodman,
• R. Rosenfeld,
• A. J. Ross,
• E. S. Rykoff,
• C. Sánchez,
• J. Sanchez,
• L. F. Secco,
• I. Sevilla-Noarbe,
• E. Sheldon,
• T. Shin,
• M. A. Troxel,
• I. Tutusaus,
• T. N. Varga,
• N. Weaverdyck,
• R. H. Wechsler,
• W. L. K. Wu,
• B. Yanny,
• B. Yin,
• Y. Zhang,
• J. Zuntz,
• T. M. C. Abbott,
• M. Aguena,
• S. Allam,
• J. Annis,
• D. Bacon,
• B. A. Benson,
• E. Bertin,
• S. Bocquet,
• D. Brooks,
• D. L. Burke,
• J. E. Carlstrom,
• J. Carretero,
• C. L. Chang,
• R. Chown,
• M. Costanzi,
• L. N. da Costa,
• A. T. Crites,
• M. E. S. Pereira,
• T. de Haan,
• J. De Vicente,
• S. Desai,
• H. T. Diehl,
• M. A. Dobbs,
• P. Doel,
• W. Everett,
• I. Ferrero,
• B. Flaugher,
• D. Friedel,
• J. Frieman,
• J. García-Bellido,
• E. Gaztanaga,
• E. M. George,
• T. Giannantonio,
• 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,
• O. Lahav,
• A. T. Lee,
• M. Lima,
• D. Luong-Van,
• M. March,
• J. J. McMahon,
• P. Melchior,
• F. Menanteau,
• S. S. Meyer,
• R. Miquel,
• L. Mocanu,
• J. J. Mohr,
• R. Morgan,
• T. Natoli,
• S. Padin,
• A. Palmese,
• F. Paz-Chinchón,
• A. Pieres,
• A. A. Plazas Malagón,
• C. Pryke,
• C. L. Reichardt,
• A. K. Romer,
• J. E. Ruhl,
• E. Sanchez,
• K. K. Schaffer,
• M. Schubnell,
• S. Serrano,
• E. Shirokoff,
• M. Smith,
• Z. Staniszewski,
• A. A. Stark,
• E. Suchyta,
• G. Tarle,
• D. Thomas,
• C. To,
• J. D. Vieira,
• J. Weller,
• R. Williamson
• (less)
arXiv e-prints (03/2022) e-Print:2203.12439
abstract + abstract -

Joint analyses of cross-correlations between measurements of galaxy positions, galaxy lensing, and lensing of the cosmic microwave background (CMB) offer powerful constraints on the large-scale structure of the Universe. In a forthcoming analysis, we will present cosmological constraints from the analysis of such cross-correlations measured using Year 3 data from the Dark Energy Survey (DES), and CMB data from the South Pole Telescope (SPT) and Planck. Here we present two key ingredients of this analysis: (1) an improved CMB lensing map in the SPT-SZ survey footprint, and (2) the analysis methodology that will be used to extract cosmological information from the cross-correlation measurements. Relative to previous lensing maps made from the same CMB observations, we have implemented techniques to remove contamination from the thermal Sunyaev Zel'dovich effect, enabling the extraction of cosmological information from smaller angular scales of the cross-correlation measurements than in previous analyses with DES Year 1 data. We describe our model for the cross-correlations between these maps and DES data, and validate our modeling choices to demonstrate the robustness of our analysis. We then forecast the expected cosmological constraints from the galaxy survey-CMB lensing auto and cross-correlations. We find that the galaxy-CMB lensing and galaxy shear-CMB lensing correlations will on their own provide a constraint on $S_8=\sigma_8 \sqrt{\Omega_{\rm m}/0.3}$ at the few percent level, providing a powerful consistency check for the DES-only constraints. We explore scenarios where external priors on shear calibration are removed, finding that the joint analysis of CMB lensing cross-correlations can provide constraints on the shear calibration amplitude at the 5 to 10% level.

(331)Constraining the multi-scale dark-matter distribution in CASSOWARY 31 with strong gravitational lensing and stellar dynamics
• H. Wang,
• R. Cañameras,
• G. B. Caminha,
• S. H. Suyu,
• A. Yıldırım
• +4
• G. Chirivì,
• L. Christensen,
• C. Grillo,
• S. Schuldt
• (less)
arXiv e-prints (03/2022) e-Print:2203.13759
abstract + abstract -

We study the inner structure of the group-scale lens CASSOWARY 31 (CSWA 31) by adopting both strong lensing and dynamical modeling. CSWA 31 is a peculiar lens system. The brightest group galaxy (BGG) is an ultra-massive elliptical galaxy at z = 0.683 with a weighted mean velocity dispersion of $\sigma = 432 \pm 31$ km s$^{-1}$. It is surrounded by group members and several lensed arcs probing up to ~150 kpc in projection. Our results significantly improve previous analyses of CSWA 31 thanks to the new HST imaging and MUSE integral-field spectroscopy. From the secure identification of five sets of multiple images and measurements of the spatially-resolved stellar kinematics of the BGG, we conduct a detailed analysis of the multi-scale mass distribution using various modeling approaches, both in the single and multiple lens-plane scenarios. Our best-fit mass models reproduce the positions of multiple images and provide robust reconstructions for two background galaxies at z = 1.4869 and z = 2.763. The relative contributions from the BGG and group-scale halo are remarkably consistent in our three reference models, demonstrating the self-consistency between strong lensing analyses based on image position and extended image modeling. We find that the ultra-massive BGG dominates the projected total mass profiles within 20 kpc, while the group-scale halo dominates at larger radii. The total projected mass enclosed within $R_{eff}$ = 27.2 kpc is $1.10_{-0.04}^{+0.02} \times 10^{13}$ M$_\odot$. We find that CSWA 31 is a peculiar fossil group, strongly dark-matter dominated towards the central region, and with a projected total mass profile similar to higher-mass cluster-scale halos. The total mass-density slope within the effective radius is shallower than isothermal, consistent with previous analyses of early-type galaxies in overdense environments.

(330)Snowmass White Paper: Probing New Physics with $\mu^+ \mu^- \to bs$ at a Muon Collider
• Wolfgang Altmannshofer,
• Sri Aditya Gadam,
• Stefano Profumo
arXiv e-prints (03/2022) e-Print:2203.07495
abstract + abstract -

In this white paper for the Snowmass process, we discuss the prospects of probing new physics explanations of the persistent rare $B$ decay anomalies with a muon collider. If the anomalies are indirect signs of heavy new physics, non-standard rates for $\mu^+ \mu^- \to b s$ production should be observed with high significance at a muon collider with center of mass energy of $\sqrt{s} = 10$ TeV. The forward-backward asymmetry of the $b$-jet provides diagnostics of the chirality structure of the new physics couplings. In the absence of a signal, $\mu^+ \mu^- \to b s$ can indirectly probe new physics scales as large as $86$ TeV. Beam polarization would have an important impact on the new physics sensitivity.

(329)Machine Learning and LHC Event Generation
• Anja Butter,
• Tilman Plehn,
• Steffen Schumann,
• Simon Badger,
• Sascha Caron
• +46
• Kyle Cranmer,
• Francesco Armando Di Bello,
• Etienne Dreyer,
• Stefano Forte,
• Sanmay Ganguly,
• Dorival Gonçalves,
• Eilam Gross,
• Theo Heimel,
• Gudrun Heinrich,
• Lukas Heinrich,
• Alexander Held,
• Stefan Höche,
• Jessica N. Howard,
• Philip Ilten,
• Joshua Isaacson,
• Timo Janßen,
• Stephen Jones,
• Marumi Kado,
• Michael Kagan,
• Gregor Kasieczka,
• Felix Kling,
• Sabine Kraml,
• Claudius Krause,
• Frank Krauss,
• Kevin Kröninger,
• Rahool Kumar Barman,
• Michel Luchmann,
• Vitaly Magerya,
• Daniel Maitre,
• Bogdan Malaescu,
• Fabio Maltoni,
• Till Martini,
• Olivier Mattelaer,
• Benjamin Nachman,
• Sebastian Pitz,
• Juan Rojo,
• Matthew Schwartz,
• David Shih,
• Frank Siegert,
• Roy Stegeman,
• Bob Stienen,
• Jesse Thaler,
• Rob Verheyen,
• Daniel Whiteson,
• Ramon Winterhalder,
• Jure Zupan
• (less)
arXiv e-prints (03/2022) e-Print:2203.07460
abstract + abstract -

First-principle simulations are at the heart of the high-energy physics research program. They link the vast data output of multi-purpose detectors with fundamental theory predictions and interpretation. This review illustrates a wide range of applications of modern machine learning to event generation and simulation-based inference, including conceptional developments driven by the specific requirements of particle physics. New ideas and tools developed at the interface of particle physics and machine learning will improve the speed and precision of forward simulations, handle the complexity of collision data, and enhance inference as an inverse simulation problem.

(328)Impact of the Coulomb field on charged-pion spectra in few-GeV heavy-ion collisions
• J. Adamczewski-Musch,
• O. Arnold,
• C. Behnke,
• A. Belounnas,
• A. Belyaev
• +122
• J.C. Berger-Chen,
• A. Blanco,
• C. Blume,
• M. Böhmer,
• P. Bordalo,
• S. Chernenko,
• L. Chlad,
• I. Ciepał,
• C. Deveaux,
• J. Dreyer,
• E. Epple,
• L. Fabbietti,
• O. Fateev,
• P. Filip,
• P. Fonte,
• C. Franco,
• J. Friese,
• I. Fröhlich,
• T. Galatyuk,
• J.A. Garzon,
• R. Gernhäuser,
• S. Gläßel,
• R. Greifenhagen,
• F. Guber,
• M. Gumberidze,
• S. Harabasz,
• T. Heinz,
• T. Hennino,
• S. Hlavac,
• C. Höhne,
• R. Holzmann,
• A. Ierusalimov,
• A. Ivashkin,
• B. Kämpfer,
• T. Karavicheva,
• B. Kardan,
• I. Koenig,
• W. Koenig,
• M. Kohls,
• B.W. Kolb,
• G. Korcyl,
• G. Kornakov,
• F. Kornas,
• R. Kotte,
• A. Kugler,
• T. Kunz,
• A. Kurepin,
• A. Kurilkin,
• P. Kurilkin,
• V. Ladygin,
• R. Lalik,
• K. Lapidus,
• A. Lebedev,
• S. Linev,
• L. Lopes,
• M. Lorenz,
• T. Mahmoud,
• L. Maier,
• A. Malige,
• A. Mangiarotti,
• J. Markert,
• T. Matulewicz,
• S. Maurus,
• V. Metag,
• J. Michel,
• D.M. Mihaylov,
• S. Morozov,
• C. Müntz,
• R. Münzer,
• M. Nabroth,
• L. Naumann,
• K. Nowakowski,
• Y. Parpottas,
• M. Parschau,
• V. Pechenov,
• O. Pechenova,
• O. Petukhov,
• K. Piasecki,
• J. Pietraszko,
• W. Przygoda,
• K. Pysz,
• S. Ramos,
• B. Ramstein,
• N. Rathod,
• A. Reshetin,
• P. Rodriguez-Ramos,
• P. Rosier,
• A. Rost,
• A. Rustamov,
• A. Sadovsky,
• P. Salabura,
• T. Scheib,
• H. Schuldes,
• N. Schild,
• E. Schwab,
• F. Scozzi,
• F. Seck,
• P. Sellheim,
• I. Selyuzhenkov,
• J. Siebenson,
• L. Silva,
• U. Singh,
• J. Smyrski,
• Yu.G. Sobolev,
• S. Spataro,
• S. Spies,
• H. Ströbele,
• J. Stroth,
• C. Sturm,
• K. Sumara,
• O. Svoboda,
• M. Szala,
• P. Tlusty,
• M. Traxler,
• H. Tsertos,
• E. Usenko,
• V. Wagner,
• C. Wendisch,
• M.G. Wiebusch,
• J. Wirth,
• Y. Zanevsky,
• P. Zumbruch
• (less)
(02/2022) e-Print:2202.12750
abstract + abstract -

In nuclear collisions the incident protons generate a Coulomb field which acts on produced charged particles. The impact of these interactions on charged pion transverse-mass and rapidity spectra, as well as on pion-pion momentum correlations is investigated in Au+Au collisions at $\sqrt{s_{NN}}$ = 2.4 GeV. We show that the low-mt part of the data ($m_t < 0.2$ GeV/c$^2$) can be well described with a Coulomb-modified Boltzmann distribution that also takes changes of the Coulomb field during the expansion of the fireball into account. The observed centrality dependence of the fitted mean Coulomb potential deviates strongly from a $A_{part}^{2/3}$ scaling, indicating that, next to the fireball, the non-interacting charged spectators have to be taken into account. For the most central collisions, the Coulomb modifications of the HBT source radii are found to be consistent with the potential extracted from the single-pion transverse-mass distributions. This finding suggests that the region of homogeneity obtained from two-pion correlations coincides with the region in which the pions freeze-out. Using the inferred mean-square radius of the charge distribution at freeze-out, we have deduced a baryon density, in fair agreement with values obtained from statistical hadronization model fits to the particle yields.

(327)Measuring Cosmological Parameters with Type Ia Supernovae in redMaGiC galaxies
• R. Chen,
• D. Scolnic,
• E. Rozo,
• E.S. Rykoff,
• B. Popovic
• +80
• R. Kessler,
• M. Vincenzi,
• T.M. Davis,
• P. Armstrong,
• D. Brout,
• L. Galbany,
• L. Kelsey,
• C. Lidman,
• A. Möller,
• B. Rose,
• M. Sako,
• M. Sullivan,
• G. Taylor,
• P. Wiseman,
• J. Asorey,
• A. Carr,
• C. Conselice,
• K. Kuehn,
• G.F. Lewis,
• E. Macaulay,
• M. Rodriguez-Monroy,
• B.E. Tucker,
• T.M.C. Abbott,
• M. Aguena,
• S. Allam,
• F. Andrade-Oliveira,
• J. Annis,
• D. Bacon,
• E. Bertin,
• S. Bocquet,
• D. Brooks,
• D.L. Burke,
• A. Carnero Rosell,
• M. Carrasco Kind,
• J. Carretero,
• R. Cawthon,
• M. Costanzi,
• L.N. da Costa,
• M.E.S. Pereira,
• S. Desai,
• H.T. Diehl,
• P. Doel,
• S. Everett,
• I. Ferrero,
• B. Flaugher,
• D. Friedel,
• J. Frieman,
• J. García-Bellido,
• M. Gatti,
• E. Gaztanaga,
• D. Gruen,
• S.R. Hinton,
• D.L. Hollowood,
• K. Honscheid,
• D.J. James,
• O. Lahav,
• M. Lima,
• M. March,
• F. Menanteau,
• R. Miquel,
• R. Morgan,
• A. Palmese,
• F. Paz-Chinchón,
• A. Pieres,
• A.A. Plazas Malagón,
• J. Prat,
• A.K. Romer,
• A. Roodman,
• E. Sanchez,
• M. Schubnell,
• S. Serrano,
• I. Sevilla-Noarbe,
• M. Smith,
• M. Soares-Santos,
• E. Suchyta,
• G. Tarle,
• D. Thomas,
• C. To,
• D.L. Tucker,
• T.N. Varga
• (less)
(02/2022) e-Print:2202.10480
abstract + abstract -

Current and future cosmological analyses with Type Ia Supernovae (SNe Ia) face three critical challenges: i) measuring redshifts from the supernova or its host galaxy; ii) classifying SNe without spectra; and iii) accounting for correlations between the properties of SNe Ia and their host galaxies. We present here a novel approach that addresses each challenge. In the context of the Dark Energy Survey (DES), we analyze a SNIa sample with host galaxies in the redMaGiC galaxy catalog, a selection of Luminous Red Galaxies. Photo-$z$ estimates for these galaxies are expected to be accurate to $\sigma_{\Delta z/(1+z)}\sim0.02$. The DES-5YR photometrically classified SNIa sample contains approximately 1600 SNe and 125 of these SNe are in redMaGiC galaxies. We demonstrate that redMaGiC galaxies almost exclusively host SNe Ia, reducing concerns with classification uncertainties. With this subsample, we find similar Hubble scatter (to within $\sim0.01$ mag) using photometric redshifts in place of spectroscopic redshifts. With detailed simulations, we show the bias due to using photo-$z$s from redMaGiC host galaxies on the measurement of the dark energy equation-of-state $w$ is up to $\Delta w \sim 0.01-0.02$. With real data, we measure a difference in $w$ when using redMaGiC photometric redshifts versus spectroscopic redshifts of $\Delta w = 0.005$. Finally, we discuss how SNe in redMaGiC galaxies appear to be a more standardizable population due to a weaker relation between color and luminosity ($\beta$) compared to the DES-3YR population by $\sim5\sigma$; this finding is consistent with predictions that redMaGiC galaxies exhibit lower reddening ratios ($\textrm{R}_\textrm{V}$) than the general population of SN host galaxies. These results establish the feasibility of performing redMaGiC SN cosmology with photometric survey data in the absence of spectroscopic data.

(326)Observation of the doubly charmed baryon decay ${\varXi}_{cc}^{++}\to {\varXi}_c^{\prime +}{\pi}^{+}$
• Roel Aaij,
• Ahmed Sameh Wagih Abdelmotteleb,
• Carlos Abellán Beteta,
• Fernando Jesus Abudinén,
• Thomas Ackernley
• +1006
• Bernardo Adeva,
• Marco Adinolfi,
• Hossein Afsharnia,
• Christina Agapopoulou,
• Christine Angela Aidala,
• Salvatore Aiola,
• Ziad Ajaltouni,
• Simon Akar,
• Johannes Albrecht,
• Federico Alessio,
• Michael Alexander,
• Alejandro Alfonso Albero,
• Zakariya Aliouche,
• Georgy Alkhazov,
• Paula Alvarez Cartelle,
• Sandra Amato,
• Jake Lewis Amey,
• Yasmine Amhis,
• Liupan An,
• Lucio Anderlini,
• Martin Andersson,
• Aleksei Andreianov,
• Mirco Andreotti,
• Dong Ao,
• Flavio Archilli,
• Alexander Artamonov,
• Marina Artuso,
• Kenenbek Arzymatov,
• Elie Aslanides,
• Michele Atzeni,
• Benjamin Audurier,
• Sebastian Bachmann,
• Marie Bachmayer,
• John Back,
• Pablo Baladron Rodriguez,
• Vladislav Balagura,
• Wander Baldini,
• Juan Baptista de Souza Leite,
• Matteo Barbetti,
• Roger Barlow,
• Sergey Barsuk,
• William Barter,
• Matteo Bartolini,
• Fedor Baryshnikov,
• Jan-Marc Basels,
• Giovanni Bassi,
• Baasansuren Batsukh,
• Alexander Battig,
• Aurelio Bay,
• Anja Beck,
• Maik Becker,
• Franco Bedeschi,
• Ignacio Bediaga,
• Andrew Beiter,
• Vladislav Belavin,
• Samuel Belin,
• Violaine Bellee,
• Konstantin Belous,
• Ilia Belov,
• Ivan Belyaev,
• Giovanni Bencivenni,
• Eli Ben-Haim,
• Alexander Berezhnoy,
• Roland Bernet,
• Daniel Berninghoff,
• Harris Conan Bernstein,
• Claudia Bertella,
• Alessandro Bertolin,
• Christopher Betancourt,
• Federico Betti,
• Ia. Bezshyiko,
• Iaroslava Bezshyiko,
• Srishti Bhasin,
• Jihyun Bhom,
• Lingzhu Bian,
• Martin Stefan Bieker,
• Nicolo Vladi Biesuz,
• Simone Bifani,
• Pierre Billoir,
• Alice Biolchini,
• Matthew Birch,
• Fionn Caitlin Ros Bishop,
• Alexander Bitadze,
• Andrea Bizzeti,
• Mikkel Bjørn,
• Michele Piero Blago,
• Thomas Blake,
• Frederic Blanc,
• Steven Blusk,
• Dana Bobulska,
• Julian Alexander Boelhauve,
• Oscar Boente Garcia,
• Thomas Boettcher,
• Alexey Boldyrev,
• Alexander Bondar,
• Nikolay Bondar,
• Silvia Borghi,
• Maxim Borisyak,
• Martino Borsato,
• Jozef Tomasz Borsuk,
• Sonia Amina Bouchiba,
• Themistocles Bowcock,
• Alexandre Boyer,
• Concezio Bozzi,
• Matthew John Bradley,
• Svende Braun,
• Alexandre Brea Rodriguez,
• Jolanta Brodzicka,
• Arnau Brossa Gonzalo,
• Davide Brundu,
• Annarita Buonaura,
• Laura Buonincontri,
• Aodhan Tomas Burke,
• Christopher Burr,
• Albert Bursche,
• Anatoly Butkevich,
• Jordy Sebastiaan Butter,
• Jan Buytaert,
• Wiktor Byczynski,
• Sandro Cadeddu,
• Hao Cai,
• Roberto Calabrese,
• Lukas Calefice,
• Stefano Cali,
• Ryan Calladine,
• Marta Calvi,
• Miriam Calvo Gomez,
• Patricia Camargo Magalhaes,
• Pierluigi Campana,
• Angel Fernando Campoverde Quezada,
• Simone Capelli,
• Lorenzo Capriotti,
• Angelo Carbone,
• Giovanni Carboni,
• Roberta Cardinale,
• Alessandro Cardini,
• Ina Carli,
• Paolo Carniti,
• Leon David Carus,
• Kazuyoshi Carvalho Akiba,
• Adrian Casais Vidal,
• Rowina Caspary,
• Gianluigi Casse,
• Marco Cattaneo,
• Giovanni Cavallero,
• Sara Celani,
• Jacopo Cerasoli,
• Daniel Cervenkov,
• Abbie Jane Chadwick,
• Matthew George Chapman,
• Matthew Charles,
• Philippe Charpentier,
• Ph. Charpentier,
• Carlos Alberto Chavez Barajas,
• Maximilien Chefdeville,
• Chen Chen,
• Shanzhen Chen,
• Aleksei Chernov,
• Veronika Chobanova,
• Serhii Cholak,
• Marcin Chrzaszcz,
• Alexsei Chubykin,
• Vladimir Chulikov,
• Paolo Ciambrone,
• Maria Flavia Cicala,
• Xabier Cid Vidal,
• Gregory Ciezarek,
• P.E. L. Clarke,
• Marco Clemencic,
• Harry Cliff,
• Joel Closier,
• John Leslie Cobbledick,
• Victor Coco,
• Joao A B Coelho,
• Julien Cogan,
• Eric Cogneras,
• Lucian Cojocariu,
• Paula Collins,
• Tommaso Colombo,
• Liliana Congedo,
• Andrea Contu,
• Naomi Cooke,
• George Coombs,
• Imanol Corredoira,
• Gloria Corti,
• Cayo Mar Costa Sobral,
• Benjamin Couturier,
• Daniel Charles Craik,
• Jana Crkovská,
• Melissa Maria Cruz Torres,
• Robert Currie,
• Cesar Luiz Da Silva,
• Shakhzod Dadabaev,
• Lingyun Dai,
• Elena Dall'Occo,
• Jeremy Dalseno,
• Carmelo D'Ambrosio,
• Anna Danilina,
• Philippe d'Argent,
• Aigerim Dashkina,
• Jonathan Edward Davies,
• Adam Davis,
• Oscar De Aguiar Francisco,
• Kristof De Bruyn,
• Stefano De Capua,
• Michel De Cian,
• Ulisses De Freitas Carneiro Da Graca,
• Erika De Lucia,
• Jussara De Miranda,
• Leandro De Paula,
• Marilisa De Serio,
• Dario De Simone,
• Patrizia De Simone,
• Fabio De Vellis,
• Jacco de Vries,
• Cameron Thomas Dean,
• Francesco Debernardis,
• Daniel Decamp,
• Vlad-George Dedu,
• Luigi Del Buono,
• Blaise Delaney,
• Hans Peter Dembinski,
• Vadym Denysenko,
• Denis Derkach,
• Olivier Deschamps,
• Francesco Dettori,
• Biplab Dey,
• Alessandro Di Cicco,
• Pasquale Di Nezza,
• Sergey Didenko,
• Lorena Dieste Maronas,
• Shuchong Ding,
• Vasyl Dobishuk,
• Chenzhi Dong,
• Amanda May Donohoe,
• Francesca Dordei,
• Alberto dos Reis,
• Lauren Douglas,
• Anatoliy Dovbnya,
• Anthony Gavin Downes,
• Maciej Wojciech Dudek,
• Laurent Dufour,
• Viacheslav Duk,
• Paolo Durante,
• John Matthew Durham,
• Deepanwita Dutta,
• Agnieszka Dziurda,
• Alexey Dzyuba,
• Sajan Easo,
• Ulrik Egede,
• Victor Egorychev,
• Semen Eidelman,
• Stephan Eisenhardt,
• Surapat Ek-In,
• Lars Eklund,
• Scott Ely,
• Alexandru Ene,
• Eliane Epple,
• Stephan Escher,
• Jonas Nathanael Eschle,
• Sevda Esen,
• Timothy Evans,
• Lucas Falcao,
• Yanting Fan,
• Bo Fang,
• Stephen Farry,
• Davide Fazzini,
• Mauricio Féo,
• Antonio Fernandez Prieto,
• Alex Daniel Fernez,
• Fabio Ferrari,
• Lino Ferreira Lopes,
• Fernando Ferreira Rodrigues,
• Silvia Ferreres Sole,
• Martina Ferrillo,
• Massimiliano Ferro-Luzzi,
• Sergey Filippov,
• Rosa Anna Fini,
• Massimiliano Fiorini,
• Miroslaw Firlej,
• Kamil Leszek Fischer,
• K.M. Fischer,
• Dillon Scott Fitzgerald,
• Conor Fitzpatrick,
• Tomasz Fiutowski,
• Aristeidis Fkiaras,
• Frederic Fleuret,
• Marianna Fontana,
• Flavio Fontanelli,
• Roger Forty,
• Daniel Foulds-Holt,
• Vinicius Franco Lima,
• Manuel Franco Sevilla,
• Markus Frank,
• Edoardo Franzoso,
• Giulia Frau,
• Christoph Frei,
• David Anthony Friday,
• Jinlin Fu,
• Quentin Fuehring,
• Emmy Gabriel,
• Giuliana Galati,
• Abraham Gallas Torreira,
• Domenico Galli,
• Silvia Gambetta,
• Yuyue Gan,
• Miriam Gandelman,
• Paolo Gandini,
• Yuanning Gao,
• Michela Garau,
• Luis Miguel Garcia Martin,
• Paula Garcia Moreno,
• Julián García Pardiñas,
• Beatriz Garcia Plana,
• Felipe Andres Garcia Rosales,
• Lluis Garrido,
• Clara Gaspar,
• Robbert Erik Geertsema,
• David Gerick,
• Louis Lenard Gerken,
• Evelina Gersabeck,
• Marco Gersabeck,
• Timothy Gershon,
• Luca Giambastiani,
• Valerie Gibson,
• Henryk Karol Giemza,
• Alexander Leon Gilman,
• Matteo Giovannetti,
• Alessandra Gioventù,
• Pere Gironella Gironell,
• Carmen Giugliano,
• Konstantin Gizdov,
• Evangelos Leonidas Gkougkousis,
• Vladimir Gligorov,
• Carla Göbel,
• Elisabet Golobardes,
• Dmitry Golubkov,
• Andrey Golutvin,
• Alvaro Gomes,
• Sergio Gomez Fernandez,
• Fernanda Goncalves Abrantes,
• Mateusz Goncerz,
• Guanghua Gong,
• Petr Gorbounov,
• Igor Vladimirovich Gorelov,
• Claudio Gotti,
• Jascha Peter Grabowski,
• Thomas Grammatico,
• Luis Alberto Granado Cardoso,
• Eugeni Graugés,
• Elena Graverini,
• Giacomo Graziani,
• Alexandru Grecu,
• Lex Marinus Greeven,
• Nathan Allen Grieser,
• Lucia Grillo,
• Sergey Gromov,
• Barak Raimond Gruberg Cazon,
• Chenxi Gu,
• Marco Guarise,
• Manuel Guittiere,
• Paul Andre Günther,
• Evgeny Gushchin,
• Andreas Guth,
• Yury Guz,
• Thierry Gys,
• Thomas Hadavizadeh,
• Guido Haefeli,
• Christophe Haen,
• Jakob Haimberger,
• Susan Haines,
• Tabitha Halewood-leagas,
• Phoebe Meredith Hamilton,
• Jan Patrick Hammerich,
• Qundong Han,
• Xiaoxue Han,
• Eva Brottmann Hansen,
• Stephanie Hansmann-Menzemer,
• Neville Harnew,
• Thomas Harrison,
• Christoph Hasse,
• Mark Hatch,
• Jibo He,
• Kevin Heijhoff,
• Kevin Heinicke,
• Riley Dylan Leslie Henderson,
• Arthur Marius Hennequin,
• Karol Hennessy,
• Louis Henry,
• Johannes Heuel,
• Adlène Hicheur,
• Donal Hill,
• Martha Hilton,
• Sophie Elizabeth Hollitt,
• Ruiwe Hou,
• Yingrui Hou,
• Jiangqiao Hu,
• Jifeng Hu,
• Wenhua Hu,
• Xiaofan Hu,
• Wenqian Huang,
• Xiaotao Huang,
• Wouter Hulsbergen,
• Ross John Hunter,
• Mikhail Hushchyn,
• David Hutchcroft,
• Daniel Hynds,
• Philipp Ibis,
• Marek Idzik,
• Dmitrii Ilin,
• Philip Ilten,
• Alexander Inglessi,
• Aleksandr Iniukhin,
• Artur Ishteev,
• Kuzma Ivshin,
• Richard Jacobsson,
• Hendrik Jage,
• Sune Jakobsen,
• Eddy Jans,
• Brij Kishor Jashal,
• Abolhassan Jawahery,
• Vukan Jevtic,
• Xiaojie Jiang,
• Malcolm John,
• Daniel Johnson,
• Christopher Jones,
• Thomas Peter Jones,
• Beat Jost,
• Nathan Jurik,
• Sergii Kandybei,
• Youen Kang,
• Matthias Karacson,
• Dmitrii Karpenkov,
• Maksim Karpov,
• Jacob William Kautz,
• Floris Keizer,
• Dustin Michael Keller,
• Matthew Kenzie,
• Tjeerd Ketel,
• Basem Khanji,
• Anastasiia Kharisova,
• Sergei Kholodenko,
• Thomas Kirn,
• Veronica Soelund Kirsebom,
• Ouail Kitouni,
• Suzanne Klaver,
• Nico Kleijne,
• Konrad Klimaszewski,
• Mateusz Rafal Kmiec,
• Serhii Koliiev,
• Almagul Kondybayeva,
• Anatoly Konoplyannikov,
• Pawel Kopciewicz,
• Renata Kopecna,
• Patrick Koppenburg,
• Mikhail Korolev,
• Igor Kostiuk,
• Oleksander Kot,
• Sofia Kotriakhova,
• Anastasiia Kozachuk,
• Polina Kravchenko,
• Leonid Kravchuk,
• Rafal Dominik Krawczyk,
• Michal Kreps,
• Sophie Katharina Kretzschmar,
• Pavel Krokovny,
• Wojciech Krupa,
• Wojciech Krzemien,
• Jakub Kubat,
• Marcin Kucharczyk,
• Vasily Kudryavtsev,
• Hilbrand Steffen Kuindersma,
• Gerd Joachim Kunde,
• Tengiz Kvaratskheliya,
• Daniel Lacarrere,
• George Lafferty,
• Adriano Lai,
• Andrea Lampis,
• Davide Lancierini,
• John Jake Lane,
• Richard Lane,
• Gaia Lanfranchi,
• Christoph Langenbruch,
• Jan Langer,
• Oliver Lantwin,
• Thomas Latham,
• Federico Lazzari,
• Renaud Le Gac,
• Sook Hyun Lee,
• Regis Lefèvre,
• Alexander Leflat,
• Sergey Legotin,
• Olivier Leroy,
• Tadeusz Lesiak,
• Blake Leverington,
• Hengne Li,
• Peilian Li,
• Shiyang Li,
• Yiming Li,
• Zhuoming Li,
• Xixin Liang,
• Tai-hua Lin,
• Rolf Lindner,
• Vitalii Lisovskyi,
• Roman Litvinov,
• Guoming Liu,
• Huanhuan Liu,
• Qian Liu,
• Shuaiyi Liu,
• Aniol Lobo Salvia,
• Angelo Loi,
• Riccardo Lollini,
• Julian Lomba Castro,
• Iain Longstaff,
• Jose Lopes,
• Saúl López Soliño,
• George Holger Lovell,
• Yu Lu,
• Chiara Lucarelli,
• Donatella Lucchesi,
• Stanislav Luchuk,
• Miriam Lucio Martinez,
• Valeriia Lukashenko,
• Yiheng Luo,
• Anna Lupato,
• Eleonora Luppi,
• Oliver Lupton,
• Alberto Lusiani,
• Xiao-Rui Lyu,
• Lishuang Ma,
• Ruiting Ma,
• Serena Maccolini,
• Frederic Machefert,
• Florin Maciuc,
• Vladimir Macko,
• Patrick Mackowiak,
• Samuel Maddrell-Mander,
• Lakshan Ram Madhan Mohan,
• Oleg Maev,
• Artem Maevskiy,
• Dmitrii Maisuzenko,
• Maciej Witold Majewski,
• Jakub Jacek Malczewski,
• Sneha Malde,
• Bartosz Malecki,
• Alexander Malinin,
• Timofei Maltsev,
• Hanna Malygina,
• Giulia Manca,
• Giampiero Mancinelli,
• Daniele Manuzzi,
• Claudio Andrea Manzari,
• Daniele Marangotto,
• Jan Maratas,
• Jean François Marchand,
• Umberto Marconi,
• Saverio Mariani,
• Carla Marin Benito,
• Matthieu Marinangeli,
• Jörg Marks,
• Alexander Mclean Marshall,
• Phillip John Marshall,
• Gabriele Martelli,
• Giuseppe Martellotti,
• Loris Martinazzoli,
• Maurizio Martinelli,
• Diego Martinez Santos,
• Fernando Martinez Vidal,
• André Massafferri,
• Marcel Materok,
• Rosen Matev,
• Abhijit Mathad,
• Viacheslav Matiunin,
• Clara Matteuzzi,
• Kara Renee Mattioli,
• Andrea Mauri,
• Emilie Maurice,
• Juan Mauricio,
• Michal Kazimierz Mazurek,
• Michael McCann,
• Lucas Mcconnell,
• Tamaki Holly Mcgrath,
• Niall Thomas Mchugh,
• Andrew McNab,
• Ronan McNulty,
• James Vincent Mead,
• Brian Meadows,
• Gerwin Meier,
• Dmytro Melnychuk,
• Simone Meloni,
• Marcel Merk,
• Andrea Merli,
• Lucas Meyer Garcia,
• Mikhail Mikhasenko,
• Diego Alejandro Milanes,
• Edward James Millard,
• Marko Milovanovic,
• Marie-Noelle Minard,
• Alessandro Minotti,
• Sara Elizabeth Mitchell,
• Biljana Mitreska,
• Dominik Stefan Mitzel,
• Antje Mödden,
• Rizwaan Adeeb Mohammed,
• Razvan Daniel Moise,
• Sergei Mokhnenko,
• Titus Mombächer,
• Igancio Alberto Monroy,
• Stephane Monteil,
• Mauro Morandin,
• Gianfranco Morello,
• Michael Joseph Morello,
• Jakub Moron,
• Adam Benjamin Morris,
• Andrew George Morris,
• Raymond Mountain,
• Hongjie Mu,
• Franz Muheim,
• Mick Mulder,
• Katharina Müller,
• Colm Harold Murphy,
• Donal Murray,
• Rebecca Murta,
• Piera Muzzetto,
• Paras Naik,
• Tatsuya Nakada,
• Raja Nandakumar,
• Tara Nanut,
• Irina Nasteva,
• Matthew Needham,
• Nicola Neri,
• Sebastian Neubert,
• Niko Neufeld,
• Ryan Newcombe,
• Elisabeth Maria Niel,
• Simon Nieswand,
• Nikolay Nikitin,
• Niklas Stefan Nolte,
• Camille Normand,
• Cynthia Nunez,
• Agnieszka Oblakowska-Mucha,
• Vladimir Obraztsov,
• Thomas Oeser,
• Daniel Patrick O'Hanlon,
• Shinichi Okamura,
• Rudolf Oldeman,
• Federica Oliva,
• Mario Edgardo Olivares,
• C.J. G. Onderwater,
• Ryunosuke Hugo O'Neil,
• Juan Martin Otalora Goicochea,
• Tatiana Ovsiannikova,
• Patrick Owen,
• Maria Aranzazu Oyanguren,
• Ozlem Ozcelik,
• Klaas Ole Padeken,
• Bhagyashree Pagare,
• Preema Rennee Pais,
• Tommaso Pajero,
• Antimo Palano,
• Matteo Palutan,
• Yue Pan,
• Gennady Panshin,
• Antonios Papanestis,
• Marco Pappagallo,
• Luciano Pappalardo,
• Cheryl Pappenheimer,
• William Parker,
• Christopher Parkes,
• Barbara Passalacqua,
• Giovanni Passaleva,
• Alessandra Pastore,
• Mitesh Patel,
• Claudia Patrignani,
• Christopher James Pawley,
• Alex Pearce,
• Antonio Pellegrino,
• Monica Pepe Altarelli,
• Stefano Perazzini,
• Dmitrii Pereima,
• Asier Pereiro Castro,
• Pascal Perret,
• Marko Petric,
• Konstantinos Petridis,
• Alessandro Petrolini,
• Aleksandr Petrov,
• Stefano Petrucci,
• Marco Petruzzo,
• Thi Thuy Hang Pham,
• Anton Philippov,
• Roberto Piandani,
• Lorenzo Pica,
• Mauro Piccini,
• Boleslaw Pietrzyk,
• Guillaume Pietrzyk,
• Martina Pili,
• Davide Pinci,
• Flavio Pisani,
• Marco Pizzichemi,
• P.K. Resmi,
• Vlad-Mihai Placinta,
• Jonathan Plews,
• Maximo Plo Casasus,
• Francesco Polci,
• Marco Poli Lener,
• Mariia Poliakova,
• Anton Poluektov,
• Natalia Polukhina,
• Ivan Polyakov,
• Erica Polycarpo,
• Sebastien Ponce,
• Dmitry Popov,
• Sergei Popov,
• Stanislav Poslavskii,
• Kodassery Prasanth,
• Laura Promberger,
• Claire Prouve,
• Valery Pugatch,
• Veronique Puill,
• Giovanni Punzi,
• Hongrong Qi,
• Wenbin Qian,
• Ning Qin,
• Renato Quagliani,
• Naomi Veronika Raab,
• Raul Iraq Rabadan Trejo,
• Bartlomiej Rachwal,
• Jonas Rademacker,
• Rohan Rajagopalan,
• Matteo Rama,
• Miguel Ramos Pernas,
• Murilo Rangel,
• Fedor Ratnikov,
• Gerhard Raven,
• Meril Reboud,
• Federico Redi,
• Florian Reiss,
• Clara Remon Alepuz,
• Zan Ren,
• Victor Renaudin,
• Roberto Ribatti,
• Alessandro Maria Ricci,
• Stefania Ricciardi,
• Kurt Rinnert,
• Patrick Robbe,
• Gary Robertson,
• Ana Barbara Rodrigues,
• Eduardo Rodrigues,
• Jairo Alexis Rodriguez Lopez,
• E.R. R. Rodriguez Rodriguez,
• Alexandra Paige Rollings,
• Philipp Roloff,
• Vladimir Romanovskiy,
• Marcos Romero Lamas,
• Antonio Romero Vidal,
• Jordan Daniel Roth,
• Marcello Rotondo,
• Matthew Scott Rudolph,
• Thomas Ruf,
• Ramon Angel Ruiz Fernandez,
• Joan Ruiz Vidal,
• Artem Ryzhikov,
• Jakub Ryzka,
• Juan Jose Saborido Silva,
• Naylya Sagidova,
• Niladribihari Sahoo,
• Biagio Saitta,
• Matteo Salomoni,
• Cristina Sanchez Gras,
• Izaac Sanderswood,
• Roberta Santacesaria,
• Cibran Santamarina Rios,
• Marco Santimaria,
• Emanuele Santovetti,
• Danila Saranin,
• Gediminas Sarpis,
• Mindaugas Sarpis,
• Alessio Sarti,
• Celestina Satriano,
• Alessia Satta,
• Miroslav Saur,
• Darya Savrina,
• Halime Sazak,
• Luke George Scantlebury Smead,
• Alessandro Scarabotto,
• Stefan Schael,
• Sigrid Scherl,
• Manuel Schiller,
• Heinrich Schindler,
• Michael Schmelling,
• Burkhard Schmidt,
• Sebastian Schmitt,
• Olivier Schneider,
• Andreas Schopper,
• Maxime Schubiger,
• Sebastian Schulte,
• Marie Helene Schune,
• Rainer Schwemmer,
• Barbara Sciascia,
• Sara Sellam,
• Alexander Semennikov,
• Mara Senghi Soares,
• Antonino Sergi,
• Nicola Serra,
• Lorenzo Sestini,
• Alex Seuthe,
• Yiduo Shang,
• Desmond Mzamo Shangase,
• Mikhail Shapkin,
• Ivan Shchemerov,
• Lesya Shchutska,
• Tara Shears,
• Lev Shekhtman,
• Zhihong Shen,
• Shuqi Sheng,
• Vladimir Shevchenko,
• Edward Brendan Shields,
• Yuya Shimizu,
• Evgenii Shmanin,
• Joseph David Shupperd,
• Benedetto Gianluca Siddi,
• Rafael Silva Coutinho,
• Gabriele Simi,
• Saverio Simone,
• Minni Singla,
• Nicola Skidmore,
• Raphael Skuza,
• Tomasz Skwarnicki,
• Mark Slater,
• Igor Slazyk,
• Jennifer Clare Smallwood,
• John Gordon Smeaton,
• Eluned Smith,
• Mark Smith,
• Aleksandra Snoch,
• Lais Soares Lavra,
• Michael Sokoloff,
• F.J. P. Soler,
• Aleksandr Solovev,
• Ivan Solovyev,
• Felipe Luan Souza De Almeida,
• Bruno Souza De Paula,
• Bernhard Spaan,
• Elisabetta Spadaro Norella,
• Patrick Spradlin,
• Federico Stagni,
• Marian Stahl,
• Sascha Stahl,
• Seophine Stanislaus,
• Olaf Steinkamp,
• Oleg Stenyakin,
• Holger Stevens,
• Sheldon Stone,
• Daria Strekalina,
• Fidan Suljik,
• Jiayin Sun,
• Liang Sun,
• Yipeng Sun,
• Peter Svihra,
• Paul Nathaniel Swallow,
• Krzysztof Swientek,
• Adam Szabelski,
• Tomasz Szumlak,
• Maciej Pawel Szymanski,
• Shantam Taneja,
• Alastair Roger Tanner,
• Martin Duy Tat,
• Aleksandr Terentev,
• Frederic Teubert,
• Eric Thomas,
• Daniel James David Thompson,
• Kayleigh Anne Thomson,
• Hanae Tilquin,
• Vincent Tisserand,
• Stephane T'Jampens,
• Mark Tobin,
• Luca Tomassetti,
• Xingyu Tong,
• Diego Torres Machado,
• Da Yu Tou,
• Ekaterina Trifonova,
• Stoyan Miroslavov Trilov,
• Carina Trippl,
• Giulia Tuci,
• Alison Tully,
• Niels Tuning,
• Artur Ukleja,
• Daniel Joachim Unverzagt,
• Eduard Ursov,
• Andrii Usachov,
• Andrey Ustyuzhanin,
• Ulrich Uwer,
• Alexander Vagner,
• Vincenzo Vagnoni,
• Andrea Valassi,
• Giovanni Valenti,
• Nuria Valls Canudas,
• Martinus van Beuzekom,
• Maarten Van Dijk,
• Hubert Van Hecke,
• Eric van Herwijnen,
• Maarten van Veghel,
• Ricardo Vazquez Gomez,
• Pablo Vazquez Regueiro,
• Carlos Vázquez Sierra,
• Stefania Vecchi,
• Jaap Velthuis,
• Michele Veltri,
• Aravindhan Venkateswaran,
• Michele Veronesi,
• Mika Vesterinen,
• Daniel Vieira,
• Maria Vieites Diaz,
• Harald Viemann,
• Xavier Vilasis-Cardona,
• Eva Vilella Figueras,
• Andrea Villa,
• Pascal Vincent,
• Felicia Carolin Volle,
• Dorothea Vom Bruch,
• Alexey Vorobyev,
• Vitaly Vorobyev,
• Nikolai Voropaev,
• Kimberley Vos,
• Roland Waldi,
• John Walsh,
• Chishuai Wang,
• Jialu Wang,
• Jianchun Wang,
• Jianqiao Wang,
• Jike Wang,
• Mengzhen Wang,
• Rui Wang,
• Yilong Wang,
• Zhenzi Wang,
• Zirui Wang,
• Ziyi Wang,
• Jake Alexander Ward,
• Nigel Watson,
• David Websdale,
• Constantin Weisser,
• Benedict Donald C Westhenry,
• Dylan Jaide White,
• Mark Whitehead,
• Aidan Richard Wiederhold,
• Dirk Wiedner,
• Guy Wilkinson,
• Michael Kent Wilkinson,
• Ifan Williams,
• Mike Williams,
• Mark Richard James Williams,
• Fergus Wilson,
• Wojciech Wislicki,
• Mariusz Witek,
• Lukas Witola,
• Guy Wormser,
• Stephen Wotton,
• Hangyi Wu,
• Kenneth Wyllie,
• Zhiyu Xiang,
• Dong Xiao,
• Yuehong Xie,
• Ao Xu,
• Jingyi Xu,
• Li Xu,
• Menglin Xu,
• Qingnian Xu,
• Zehua Xu,
• Zhihao Xu,
• Di Yang,
• Shuangli Yang,
• Youhua Yang,
• Zhenwei Yang,
• Zishuo Yang,
• Yuezhe Yao,
• Lauren Emma Yeomans,
• Hang Yin,
• Jiesheng Yu,
• Xuhao Yuan,
• Oleg Yushchenko,
• Ettore Zaffaroni,
• Mikhail Zavertyaev,
• Milosz Zdybal,
• Oleksandr Zenaiev,
• Ming Zeng,
• Dongliang Zhang,
• Liming Zhang,
• Shulei Zhang,
• Shunan Zhang,
• Yanxi Zhang,
• Yu Zhang,
• Alina Zharkova,
• Alexey Zhelezov,
• Yangheng Zheng,
• Tianwen Zhou,
• Xiaokang Zhou,
• Yixiong Zhou,
• Valeriia Zhovkovska,
• Xianglei Zhu,
• Xiaoyu Zhu,
• Zhanwen Zhu,
• Valery Zhukov,
• Quan Zou,
• Stefano Zucchelli,
• Davide Zuliani,
• Gianluca Zunica
• (less)
abstract + abstract -

The ${\varXi}_{cc}^{++}\to {\varXi}_c^{\prime +}{\pi}^{+}$ decay is observed using proton-proton collisions collected by the LHCb experiment at a centre-of-mass energy of 13 TeV, corresponding to an integrated luminosity of 5.4 fb−1. The ${\varXi}_{cc}^{++}\to {\varXi}_c^{\prime +}{\pi}^{+}$ decay is reconstructed partially, where the photon from the ${\varXi}_c^{\prime +}\to {\varXi}_c^{+}\gamma$ decay is not reconstructed and the pK$^{−}$π$^{+}$ final state of the ${\varXi}_c^{+}$ baryon is employed. The ${\varXi}_{cc}^{++}\to {\varXi}_c^{\prime +}{\pi}^{+}$branching fraction relative to that of the ${\varXi}_{cc}^{++}\to {\varXi}_c^{+}{\pi}^{+}$ decay is measured to be 1.41 ± 0.17 ± 0.10, where the first uncertainty is statistical and the second systematic.[graphic not available: see fulltext]

(325)EXCESS workshop: Descriptions of rising low-energy spectra
• A. Fuss,
• M. Kaznacheeva,
• F. Reindl,
• F. Wagner,
• P. Adari
• +305
• A. Aguilar-Arevalo,
• D. Amidei,
• G. Angloher,
• E. Armengaud,
• C. Augier,
• L. Balogh,
• S. Banik,
• D. Baxter,
• C. Beaufort,
• G. Beaulieu,
• V. Belov,
• Y. Ben Gal,
• G. Benato,
• A. Benoît,
• A. Bento,
• L. Bergé,
• A. Bertolini,
• R. Bhattacharyya,
• J. Billard,
• I.M. Bloch,
• A. Botti,
• R. Breier,
• G. Bres,
• J-.L. Bret,
• A. Broniatowski,
• A. Brossard,
• C. Bucci,
• R. Bunker,
• M. Cababie,
• M. Calvo,
• P. Camus,
• G. Cancelo,
• L. Canonica,
• F. Cappella,
• L. Cardani,
• J.-F. Caron,
• N. Casali,
• G. del Castello,
• A. Cazes,
• R. Cerulli,
• B.A. Cervantes Vergara,
• D. Chaize,
• M. Chapellier,
• L. Chaplinsky,
• F. Charlieux,
• M. Chaudhuri,
• A.E. Chavarria,
• G. Chemin,
• R. Chen,
• H. Chen,
• F. Chierchie,
• I. Colantoni,
• J. Colas,
• J. Cooley,
• J.-M. Coquillat,
• E.C. Corcoran,
• S. Crawford,
• M. Crisler,
• A. Cruciani,
• P. Cushman,
• A. D'Addabbo,
• J.C. D'Olivo,
• A. Dastgheibi-Fard,
• M. De Jésus,
• Y. Deng,
• J.B. Dent,
• E.L. Depaoli,
• K. Dering,
• S. Dharani,
• S. Di Lorenzo,
• A. Drlica-Wagner,
• L. Dumoulin,
• D. Durnford,
• B. Dutta,
• L. Einfalt,
• A. Erb,
• A. Erhart,
• R. Essig,
• J. Estrada,
• E. Etzion,
• O. Exshaw,
• F. Favela-Perez,
• F.v. Feilitzsch,
• G. Fernandez Moroni,
• N. Ferreiro Iachellini,
• S. Ferriol,
• S. Fichtinger,
• E. Figueroa-Feliciano,
• J.-B. Filippini,
• D. Filosofov,
• J.A. Formaggio,
• M. Friedl,
• S. Fuard,
• D. Fuchs,
• A. Fuss,
• R. Gaïor,
• A. Garai,
• C. Garrah,
• J. Gascon,
• G. Gerbier,
• M. Ghaith,
• V.M. Ghete,
• D. Gift,
• I. Giomataris,
• G. Giroux,
• A. Giuliani,
• P. Gorel,
• P. Gorla,
• C. Goupy,
• J. Goupy,
• C. Goy,
• M. Gros,
• P. Gros,
• Y. Guardincerri,
• C. Guerin,
• V. Guidi,
• O. Guillaudin,
• S. Gupta,
• E. Guy,
• P. Harrington,
• D. Hauff,
• S.T. Heine,
• S.A. Hertel,
• S.E. Holland,
• Z. Hong,
• E.W. Hoppe,
• T.W. Hossbach,
• J.-C. Ianigro,
• V. Iyer,
• A. Jastram,
• M. Ješkovský,
• Y. Jin,
• J. Jochum,
• J.P. Johnston,
• A. Juillard,
• D. Karaivanov,
• V. Kashyap,
• I. Katsioulas,
• S. Kazarcev,
• M. Kaznacheeva,
• F. Kelly,
• B. Kilminster,
• A. Kinast,
• L. Klinkenberg,
• H. Kluck,
• P. Knights,
• Y. Korn,
• H. Kraus,
• B. von Krosigk,
• A. Kubik,
• N.A. Kurinsky,
• J. Lamblin,
• A. Langenkämper,
• S. Langrock,
• T. Lasserre,
• H. Lattaud,
• P. Lautridou,
• I. Lawson,
• S.J. Lee,
• M. Lee,
• A. Letessier-Selvon,
• D. Lhuillier,
• M. Li,
• Y.-T. Lin,
• A. Lubashevskiy,
• R. Mahapatra,
• S. Maludze,
• M. Mancuso,
• I. Manthos,
• L. Marini,
• S. Marnieros,
• R.D. Martin,
• A. Matalon,
• J. Matthews,
• B. Mauri,
• D.W. Mayer,
• A. Mazzolari,
• E. Mazzucato,
• H. Meyer zu Theenhausen,
• E. Michielin,
• J. Minet,
• N. Mirabolfathi,
• K.v. Mirbach,
• D. Misiak,
• P. Mitra,
• J-.L. Mocellin,
• B. Mohanty,
• V. Mokina,
• J.-P. Mols,
• A. Monfardini,
• F. Mounier,
• S. Munagavalasa,
• J.-F. Muraz,
• X.-F. Navick,
• T. Neep,
• H. Neog,
• H. Neyrial,
• K. Nikolopoulos,
• A. Nilima,
• C. Nones,
• V. Novati,
• P. O'Brien,
• L. Oberauer,
• E. Olivieri,
• M. Olmi,
• A. Onillon,
• C. Oriol,
• A. Orly,
• J.L. Orrell,
• T. Ortmann,
• C.T. Overman,
• C. Pagliarone,
• V. Palušová,
• P. Pari,
• P.K. Patel,
• L. Pattavina,
• F. Petricca,
• A. Piers,
• H.D. Pinckney,
• M.-C. Piro,
• M. Platt,
• D. Poda,
• D. Ponomarev,
• W. Potzel,
• P. Povinec,
• F. Pröbst,
• P. Privitera,
• F. Pucci,
• K. Ramanathan,
• J.-S. Real,
• T. Redon,
• F. Reindl,
• R. Ren,
• A. Robert,
• J. Da Rocha,
• D. Rodrigues,
• R. Rogly,
• J. Rothe,
• N. Rowe,
• S. Rozov,
• I. Rozova,
• T. Saab,
• N. Saffold,
• T. Salagnac,
• J. Sander,
• V. Sanglard,
• D. Santos,
• Y. Sarkis,
• V. Savu,
• G. Savvidis,
• I. Savvidis,
• S. Schönert,
• K. Schäffner,
• N. Schermer,
• J. Schieck,
• B. Schmidt,
• D. Schmiedmayer,
• C. Schwertner,
• L. Scola,
• M. Settimo,
• Ye. Shevchik,
• V. Sibille,
• I. Sidelnik,
• A. Singal,
• R. Smida,
• M. Sofo Haro,
• T. Soldner,
• J. Stachurska,
• M. Stahlberg,
• L. Stefanazzi,
• L. Stodolsky,
• C. Strandhagen,
• R. Strauss,
• A. Stutz,
• R. Thomas,
• A. Thompson,
• J. Tiffenberg,
• C. Tomei,
• M. Traina,
• S. Uemura,
• I. Usherov,
• L. Vagneron,
• W. Van De Pontseele,
• F.A. Vazquez de Sola Fernandez,
• M. Vidal,
• M. Vignati,
• A.L. Virto,
• M. Vivier,
• T. Volansky,
• V. Wagner,
• F. Wagner,
• J. Walker,
• R. Ward,
• S.L. Watkins,
• A. Wex,
• M. Willers,
• M.J. Wilson,
• L. Winslow,
• E. Yakushev,
• T.-T. Yu,
• M. Zampaolo,
• A. Zaytsev,
• V. Zema,
• D. Zinatulina,
• A. Zolotarova
• (less)
(02/2022) e-Print:2202.05097
abstract + abstract -

Many low-threshold experiments observe sharply rising event rates of yet unknown origins below a few hundred eV, and larger than expected from known backgrounds. Due to the significant impact of this excess on the dark matter or neutrino sensitivity of these experiments, a collective effort has been started to share the knowledge about the individual observations. For this, the EXCESS Workshop was initiated. In its first iteration in June 2021, ten rare event search collaborations contributed to this initiative via talks and discussions. The contributing collaborations were CONNIE, CRESST, DAMIC, EDELWEISS, MINER, NEWS-G, NUCLEUS, RICOCHET, SENSEI and SuperCDMS. They presented data about their observed energy spectra and known backgrounds together with details about the respective measurements. In this paper, we summarize the presented information and give a comprehensive overview of the similarities and differences between the distinct measurements. The provided data is furthermore publicly available on the workshop's data repository together with a plotting tool for visualization.

(324)TDCOSMO. IX. Systematic comparison between lens modelling software programs: time delay prediction for WGD 2038$-$4008
• A. J. Shajib,
• K. C. Wong,
• S. Birrer,
• S. H. Suyu,
• T. Treu
• +13
• E. Buckley-Geer,
• H. Lin,
• C. E. Rusu,
• J. Poh,
• A. Palmese,
• A. Agnello,
• M. W. Auger,
• A. Galan,
• S. Schuldt,
• D. Sluse,
• F. Courbin,
• J. Frieman,
• M. Millon
• (less)
arXiv e-prints (02/2022) e-Print:2202.11101
abstract + abstract -

The importance of alternative methods to measure the Hubble constant such as time-delay cosmography is highlighted by the recent Hubble tension. It is paramount to thoroughly investigate and rule out systematic biases in all measurement methods before we can accept new physics as the source of this tension. In this study, we perform a check for systematic biases in the lens modelling procedure of time-delay cosmography by comparing independent and blind time-delay predictions of the system WGD 2038$-$4008 from two teams using two different software programs: Glee and lenstronomy. The predicted time delays from both teams incorporate the stellar kinematics of the deflector and the external convergence from line-of-sight structures. The unblinded time-delay predictions from the two teams agree within $1.2\sigma$ implying that once the time delay is measured the inferred Hubble constant will also be mutually consistent. However, there is a $\sim$4$\sigma$ discrepancy between the power-law model slope and external shear, which is a significant discrepancy at the level of lens models before incorporating the stellar kinematics and the external convergence. We identify the difference in the reconstructed point spread function (PSF) to be the source of this discrepancy. If the same reconstructed PSF is used by both teams, then we achieve excellent agreement within $\sim$0.6$\sigma$, indicating that potential systematics stemming from source reconstruction algorithms and investigator choices are well under control. We recommend future studies to supersample the PSF as needed and marginalize over multiple algorithms/realizations for the PSF reconstruction to mitigate the systematic associated with the PSF. A future study will measure the time delays of the system WGD 2038$-$4008 and infer the Hubble constant based on our mass models.

(323)Irreversibility in linear systems with colored noise
• Grzegorz Gradziuk,
• Gabriel Torregrosa,
• Chase P. Broedersz
Physical Review E, 105 (02/2022) doi:10.1103/PhysRevE.105.024118
abstract + abstract -

Time irreversibility is a distinctive feature of nonequilibrium dynamics and several measures of irreversibility have been introduced to assess the distance from thermal equilibrium of a stochastically driven system. While the dynamical noise is often approximated as white, in many real applications the time correlations of the random forces can actually be significantly long-lived compared to the relaxation times of the driven system. We analyze the effects of temporal correlations in the noise on commonly used measures of irreversibility and demonstrate how the theoretical framework for white-noise-driven systems naturally generalizes to the case of colored noise. Specifically, we express the autocorrelation function, the area enclosing rates, and mean phase space velocity in terms of solutions of a Lyapunov equation and in terms of their white-noise limit values.

(322)Periodic temporal environmental variations induce coexistence in resource competition models
• Tom Burkart,
• Erwin Frey
arXiv e-prints (02/2022) e-Print:2202.11635
abstract + abstract -

Natural ecosystems, in particular on the microbial scale, are inhabited by a large number of species. The population size of each species is affected by interactions of individuals with each other and by spatial and temporal changes in environmental conditions, such as resource abundance. Here, we use a generic population dynamics model to study how, and under what conditions, a periodic temporal environmental variation can alter an ecosystem's composition and biodiversity. We demonstrate that using time scale separation allows one to qualitatively predict the long-term population dynamics of interacting species in varying environments. We show that the notion of competitive exclusion, a well-known principle that applies for constant environments, can be extended to temporally varying environments if the time scale of environmental changes (e.g., the circadian cycle of a host) is much faster than the time scale of population growth (doubling time in bacteria). When these time scales are similar, our analysis shows that a varying environment deters the system from reaching a steady state, and coexistence between multiple species becomes possible. Our results posit that biodiversity can in parts be attributed to natural environmental variations.

(321)On phase-space integrals with Heaviside functions
• Daniel Baranowski,
• Maximilian Delto,
• Kirill Melnikov,
• Chen-Yu Wang
Journal of High Energy Physics, 2022 (02/2022) doi:10.1007/JHEP02(2022)081
abstract + abstract -

We discuss peculiarities that arise in the computation of real-emission contributions to observables that contain Heaviside functions. A prominent example of such a case is the zero-jettiness soft function in SCET, whose calculation at next-to-next-to-next-to-leading order in perturbative QCD is an interesting problem. Since the zero-jettiness soft function distinguishes between emissions into different hemispheres, its definition involves θ-functions of light-cone components of emitted soft partons. This prevents a direct use of multi-loop methods, based on reverse unitarity, for computing the zero-jettiness soft function in high orders of perturbation theory. We propose a way to bypass this problem and illustrate its effectiveness by computing various non-trivial contributions to the zero-jettiness soft function at NNLO and N3LO in perturbative QCD.

(320)Three-loop helicity amplitudes for diphoton production in gluon fusion
• Piotr Bargieła,
• Fabrizio Caola,
• Andreas von Manteuffel,
• Lorenzo Tancredi
Journal of High Energy Physics, 2022 (02/2022) doi:10.1007/JHEP02(2022)153
abstract + abstract -

We present a calculation of the helicity amplitudes for the process gg → γγ in three-loop massless QCD. We employ a recently proposed method to calculate scattering amplitudes in the 't Hooft-Veltman scheme that reduces the amount of spurious non-physical information needed at intermediate stages of the computation. Our analytic results for the three-loop helicity amplitudes are remarkably compact, and can be efficiently evaluated numerically. This calculation provides the last missing building block for the computation of NNLO QCD corrections to diphoton production in gluon fusion.

(319)The iron and oxygen content of LMC Classical Cepheids and its implications for the extragalactic distance scale and Hubble constant. Equivalent width analysis with Kurucz stellar atmosphere models
• Martino Romaniello,
• Adam Riess,
• Sara Mancino,
• Richard I. Anderson,
• Wolfram Freudling
• +4
• Rolf-Peter Kudritzki,
• Lucas Macrì,
• Alessio Mucciarelli,
• Wenlong Yuan
• (less)
Astronomy and Astrophysics, 658, p13 (02/2022) doi:10.1051/0004-6361/202142441
abstract + abstract -

Context. Classical Cepheids are primary distance indicators and a crucial stepping stone in determining the present-day value of the Hubble constant H0 to the precision and accuracy required to constrain apparent deviations from the ΛCDM Concordance Cosmological Model.
Aims: We measured the iron and oxygen abundances of a statistically significant sample of 89 Cepheids in the Large Magellanic Cloud (LMC), one of the anchors of the local distance scale, quadrupling the prior sample and including 68 of the 70 Cepheids used to constrain H0 by the SH0ES program. The goal is to constrain the extent to which the luminosity of Cepheids is influenced by their chemical composition, which is an important contributor to the uncertainty on the determination of the Hubble constant itself and a critical factor in the internal consistency of the distance ladder.
Methods: We derived stellar parameters and chemical abundances from a self-consistent spectroscopic analysis based on equivalent width of absorption lines.
Results: The iron distribution of Cepheids in the LMC can be very accurately described by a single Gaussian with a mean [Fe/H] = −0.409 ± 0.003 dex and σ = 0.076 ± 0.003 dex. We estimate a systematic uncertainty on the absolute mean values of 0.1 dex. The width of the distribution is fully compatible with the measurement error and supports the low dispersion of 0.069 mag seen in the near-infrared Hubble Space Telescope LMC period-luminosity relation. The uniformity of the abundance has the important consequence that the LMC Cepheids alone cannot provide any meaningful constraint on the dependence of the Cepheid period-luminosity relation on chemical composition at any wavelength. This revises a prior claim based on a small sample of 22 LMC Cepheids that there was little dependence (or uncertainty) between composition and near-infrared luminosity, a conclusion which would produce an apparent conflict between anchors of the distance ladder with different mean abundance. The chemical homogeneity of the LMC Cepheid population makes it an ideal environment in which to calibrate the metallicity dependence between the more metal-poor Small Magellanic Cloud and metal-rich Milky Way and NGC 4258.

Full Tables 1-8 and Appendix B 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/658/A29

Based on observations collected at the European Southern Observatory under ESO programmes 66.D-0571 and 106.21ML.003.

(318)Double copy for Lagrangians at trilinear order
• M. Beneke,
• P. Hager,
• A. F. Sanfilippo
Journal of High Energy Physics, 2022 (02/2022) doi:10.1007/JHEP02(2022)083
abstract + abstract -

We present a novel double-copy prescription for gauge fields at the Lagrangian level and apply it to the original double copy, couplings to matter and the soft theorem. The Yang-Mills Lagrangian in light-cone gauge is mapped directly to the N = 0 supergravity Lagrangian in light-cone gauge to trilinear order, and we show that the obtained result is manifestly equivalent to Einstein gravity at tree level up to this order. The application of the double-copy prescription to couplings to matter is exemplified by scalar and fermionic QCD and finally the soft-collinear effective QCD Lagrangian. The mapping of the latter yields an effective description of an energetic Dirac fermion coupled to the graviton, Kalb-Ramond, and dilaton fields, from which the fermionic gravitational soft and next-to-soft theorems follow.

(317)Dynamical ejecta of neutron star mergers with nucleonic weak processes I: nucleosynthesis
• I. Kullmann,
• S. Goriely,
• O. Just,
• R. Ardevol-Pulpillo,
• A. Bauswein
• +1
Monthly Notices of the Royal Astronomical Society, 510, p16 (02/2022) doi:10.1093/mnras/stab3393
abstract + abstract -

We present a coherent study of the impact of neutrino interactions on the r-process element nucleosynthesis and the heating rate produced by the radioactive elements synthesized in the dynamical ejecta of neutron star-neutron star (NS-NS) mergers. We have studied the material ejected from four NS-NS merger systems based on hydrodynamical simulations which handle neutrino effects in an elaborate way by including neutrino equilibration with matter in optically thick regions and re-absorption in optically thin regions. We find that the neutron richness of the dynamical ejecta is significantly affected by the neutrinos emitted by the post-merger remnant, in particular when compared to a case neglecting all neutrino interactions. Our nucleosynthesis results show that a solar-like distribution of r-process elements with mass numbers $A \gtrsim 90$ is produced, including a significant enrichment in Sr and a reduced production of actinides compared to simulations without inclusion of the nucleonic weak processes. The composition of the dynamically ejected matter as well as the corresponding rate of radioactive decay heating are found to be rather independent of the system mass asymmetry and the adopted equation of state. This approximate degeneracy in abundance pattern and heating rates can be favourable for extracting the ejecta properties from kilonova observations, at least if the dynamical component dominates the overall ejecta. Part II of this work will study the light curve produced by the dynamical ejecta of our four NS merger models.

(316)Cassiopeia A reveals past interaction with circumstellar shell
• 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)
arXiv e-prints (02/2022) e-Print:2202.01643
abstract + abstract -

Observations of the SNR Cassiopeia A (Cas A) show asymmetries in the reverse shock that cannot be explained by models describing a remnant expanding through a spherically symmetric wind of the progenitor star. We investigate whether a past interaction of Cas A with a massive asymmetric shell of the circumstellar medium can account for the observed asymmetries. We performed 3D MHD simulations that describe the remnant evolution from the SN to its interaction with a circumstellar shell. The initial conditions are provided by a 3D neutrino-driven SN model whose morphology resembles Cas A. We explored the parameter space of the shell, searching for a set of parameters able to produce reverse shock asymmetries at the age of 350 years analogous to those observed in Cas A. The interaction of the remnant with the shell can match the observed reverse shock asymmetries if the shell was asymmetric with the densest portion in the nearside to the northwest (NW). According to our models, the shell was thin with radius 1.5 pc. 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 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; 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) than in other regions (below 2000 km/s). Our findings suggest the interaction of Cas A with an asymmetric circumstellar shell between 180 and 240 years after the SN event. We suggest that the shell was, most likely, the result of a massive eruption from the progenitor star that occurred about 10^5 years prior to core-collapse. We estimate a total mass of the shell of approximately 2.6 Msun.

(315)Synthetic galaxy clusters and observations based on Dark Energy Survey Year 3 Data
• T. N. Varga,
• D. Gruen,
• S. Seitz,
• N. MacCrann,
• E. Sheldon
• +75
• W. G. Hartley,
• A. Amon,
• A. Choi,
• A. Palmese,
• Y. Zhang,
• M. R. Becker,
• J. McCullough,
• E. Rozo,
• E. S. Rykoff,
• C. To,
• S. Grandis,
• G. M. Bernstein,
• S. Dodelson,
• K. Eckert,
• S. Everett,
• R. A. Gruendl,
• I. Harrison,
• K. Herner,
• R. P. Rollins,
• I. Sevilla-Noarbe,
• M. A. Troxel,
• B. Yanny,
• J. Zuntz,
• H. T. Diehl,
• M. Jarvis,
• M. Aguena,
• S. Allam,
• J. Annis,
• E. Bertin,
• S. Bhargava,
• D. Brooks,
• A. Carnero Rosell,
• M. Carrasco Kind,
• J. Carretero,
• M. Costanzi,
• L. N. da Costa,
• M. E. S. Pereira,
• J. De Vicente,
• S. Desai,
• J. P. Dietrich,
• I. Ferrero,
• B. Flaugher,
• J. García-Bellido,
• E. Gaztanaga,
• D. W. Gerdes,
• J. Gschwend,
• G. Gutierrez,
• S. R. Hinton,
• K. Honscheid,
• T. Jeltema,
• K. Kuehn,
• N. Kuropatkin,
• M. A. G. Maia,
• M. March,
• P. Melchior,
• F. Menanteau,
• R. Miquel,
• R. Morgan,
• J. Myles,
• F. Paz-Chinchón,
• A. A. Plazas,
• A. K. Romer,
• E. Sanchez,
• V. Scarpine,
• M. Schubnell,
• S. Serrano,
• M. Smith,
• M. Soares-Santos,
• E. Suchyta,
• M. E. C. Swanson,
• G. Tarle,
• D. Thomas,
• J. Weller,
• J. Weller,
• DES Collaboration
• (less)
Monthly Notices of the Royal Astronomical Society, 509, p21 (02/2022) doi:10.1093/mnras/stab3269
abstract + abstract -

We develop a novel data-driven method for generating synthetic optical observations of galaxy clusters. In cluster weak lensing, the interplay between analysis choices and systematic effects related to source galaxy selection, shape measurement, and photometric redshift estimation can be best characterized in end-to-end tests going from mock observations to recovered cluster masses. To create such test scenarios, we measure and model the photometric properties of galaxy clusters and their sky environments from the Dark Energy Survey Year 3 (DES Y3) data in two bins of cluster richness $\lambda \in [30; 45)$, $\lambda \in [45; 60)$ and three bins in cluster redshift ($z\in [0.3; 0.35)$, $z\in [0.45; 0.5)$ and $z\in [0.6; 0.65)$. Using deep-field imaging data, we extrapolate galaxy populations beyond the limiting magnitude of DES Y3 and calculate the properties of cluster member galaxies via statistical background subtraction. We construct mock galaxy clusters as random draws from a distribution function, and render mock clusters and line-of-sight catalogues into synthetic images in the same format as actual survey observations. Synthetic galaxy clusters are generated from real observational data, and thus are independent from the assumptions inherent to cosmological simulations. The recipe can be straightforwardly modified to incorporate extra information, and correct for survey incompleteness. New realizations of synthetic clusters can be created at minimal cost, which will allow future analyses to generate the large number of images needed to characterize systematic uncertainties in cluster mass measurements.

(314)CMB/kSZ and Compton-y Maps from 2500 deg<SUP>2</SUP> of SPT-SZ and Planck Survey Data
• L. E. Bleem,
• T. M. Crawford,
• B. Ansarinejad,
• B. A. Benson,
• S. Bocquet
• +35
• J. E. Carlstrom,
• C. L. Chang,
• R. Chown,
• A. T. Crites,
• T. de Haan,
• M. A. Dobbs,
• W. B. Everett,
• E. M. George,
• R. Gualtieri,
• N. W. Halverson,
• G. P. Holder,
• W. L. Holzapfel,
• J. D. Hrubes,
• L. Knox,
• A. T. Lee,
• D. Luong-Van,
• D. P. Marrone,
• J. J. McMahon,
• S. S. Meyer,
• M. Millea,
• L. M. Mocanu,
• J. J. Mohr,
• T. Natoli,
• Y. Omori,
• S. Padin,
• C. Pryke,
• S. Raghunathan,
• C. L. Reichardt,
• J. E. Ruhl,
• K. K. Schaffer,
• E. Shirokoff,
• Z. Staniszewski,
• A. A. Stark,
• J. D. Vieira,
• R. Williamson
• (less)
The Astrophysical Journal Supplement Series, 258, p19 (02/2022) doi:10.3847/1538-4365/ac35e9
abstract + abstract -

We present component-separated maps of the primary cosmic microwave background/kinematic Sunyaev-Zel'dovich (SZ) amplitude and the thermal SZ Compton-y parameter, created using data from the South Pole Telescope (SPT) and the Planck satellite. These maps, which cover the ~2500 deg2

of the southern sky imaged by the SPT-SZ survey, represent a significant improvement over previous such products available in this region by virtue of their higher angular resolution ( $1\buildrel{\,\prime}\over{.} 25$ for our highest-resolution Compton-y maps) and lower noise at small angular scales. In this work we detail the construction of these maps using linear combination techniques, including our method for limiting the correlation of our lowest-noise Compton-y map products with the cosmic infrared background. We perform a range of validation tests on these data products to test our sky modeling and combination algorithms, and we find good performance in all of these tests. Recognizing the potential utility of these data products for a wide range of astrophysical and cosmological analyses, including studies of the gas properties of galaxies, groups, and clusters, we make these products publicly available at pole.uchicago.edu/public/data/sptsz_ymap and on the NASA/LAMBDA website.

(313)Dynamical ejecta of neutron star mergers with nucleonic weak processes - II: kilonova emission
• O. Just,
• I. Kullmann,
• S. Goriely,
• A. Bauswein,
• H. -T. Janka
• +1
Monthly Notices of the Royal Astronomical Society, 510, p21 (02/2022) doi:10.1093/mnras/stab3327
abstract + abstract -

The majority of existing results for the kilonova (or macronova) emission from material ejected during a neutron-star (NS) merger is based on (quasi-) one-zone models or manually constructed toy-model ejecta configurations. In this study, we present a kilonova analysis of the material ejected during the first $\sim 10\,$ ms of a NS merger, called dynamical ejecta, using directly the outflow trajectories from general relativistic smoothed-particle hydrodynamics simulations, including a sophisticated neutrino treatment and the corresponding nucleosynthesis results, which have been presented in Part I of this study. We employ a multidimensional two-moment radiation transport scheme with approximate M1 closure to evolve the photon field and use a heuristic prescription for the opacities found by calibration with atomic-physics-based reference results. We find that the photosphere is generically ellipsoidal but augmented with small-scale structure and produces emission that is about 1.5-3 times stronger towards the pole than the equator. The kilonova typically peaks after $0.7\!-\!1.5\,$ d in the near-infrared frequency regime with luminosities between $3\!-\!7\times 10^{40}\,$ erg s-1 and at photospheric temperatures of $2.2\!-\!2.8\times 10^3\,$ K. A softer equation of state or higher binary-mass asymmetry leads to a longer and brighter signal. Significant variations of the light curve are also obtained for models with artificially modified electron fractions, emphasizing the importance of a reliable neutrino-transport modelling. None of the models investigated here, which only consider dynamical ejecta, produces a transient as bright as AT2017gfo. The near-infrared peak of our models is incompatible with the early blue component of AT2017gfo.

(312)Differentiable Matrix Elements with MadJax
• Lukas Heinrich,
• Michael Kagan
arXiv e-prints (02/2022) e-Print:2203.00057
abstract + abstract -

MadJax is a tool for generating and evaluating differentiable matrix elements of high energy scattering processes. As such, it is a step towards a differentiable programming paradigm in high energy physics that facilitates the incorporation of high energy physics domain knowledge, encoded in simulation software, into gradient based learning and optimization pipelines. MadJax comprises two components: (a) a plugin to the general purpose matrix element generator MadGraph that integrates matrix element and phase space sampling code with the JAX differentiable programming framework, and (b) a standalone wrapping API for accessing the matrix element code and its gradients, which are computed with automatic differentiation. The MadJax implementation and example applications of simulation based inference and normalizing flow based matrix element modeling, with capabilities enabled uniquely with differentiable matrix elements, are presented.

(311)Smearing scale in Laguerre reconstructions of the correlation function
• Farnik Nikakhtar,
• Ravi K. Sheth,
• Idit Zehavi
Physical Review D, 105 (02/2022) doi:10.1103/PhysRevD.105.043536
abstract + abstract -

To a good approximation, on large scales, the evolved two-point correlation function of biased tracers is related to the initial one by a convolution with a smearing kernel. For Gaussian initial conditions, the smearing kernel is Gaussian, so if the initial correlation function is parametrized using simple polynomials, then the evolved correlation function is a sum of generalized Laguerre functions of half-integer order. This motivates an analytic "Laguerre reconstruction" algorithm which previous work has shown is fast and accurate. This reconstruction requires as input the width of the smearing kernel. We show that the method can be extended to estimate the width of the smearing kernel from the same dataset. This estimate, and associated uncertainties, can then be used to marginalize over the distribution of reconstructed shapes and hence provide error estimates on the value of the distance scale. This procedure is not tied to a particular cosmological model. We also show that if, instead, we parametrize the evolved correlation function using simple polynomials, then the initial one is a sum of Hermite polynomials, again enabling fast and accurate deconvolution. If one is willing to use constraints on the smearing scale from other datasets, then marginalizing over its value is simpler for this latter, "Hermite" reconstruction, potentially providing further speed-ups in cosmological analyses.

(310)Euclid: Forecasts from redshift-space distortions and the Alcock-Paczynski test with cosmic voids
• N. Hamaus,
• M. Aubert,
• A. Pisani,
• S. Contarini,
• G. Verza
• +125
• M. -C. Cousinou,
• S. Escoffier,
• A. Hawken,
• G. Lavaux,
• G. Pollina,
• B. D. Wandelt,
• J. Weller,
• M. Bonici,
• C. Carbone,
• L. Guzzo,
• A. Kovacs,
• F. Marulli,
• E. Massara,
• L. Moscardini,
• P. Ntelis,
• W. J. Percival,
• S. Radinović,
• M. Sahlén,
• Z. Sakr,
• A. G. Sánchez,
• H. A. Winther,
• N. Auricchio,
• S. Awan,
• R. Bender,
• C. Bodendorf,
• D. Bonino,
• E. Branchini,
• M. Brescia,
• J. Brinchmann,
• V. Capobianco,
• J. Carretero,
• F. J. Castander,
• M. Castellano,
• S. Cavuoti,
• A. Cimatti,
• R. Cledassou,
• G. Congedo,
• L. Conversi,
• Y. Copin,
• L. Corcione,
• M. Cropper,
• A. Da Silva,
• H. Degaudenzi,
• M. Douspis,
• F. Dubath,
• C. A. J. Duncan,
• X. Dupac,
• S. Dusini,
• A. Ealet,
• S. Ferriol,
• P. Fosalba,
• M. Frailis,
• E. Franceschi,
• P. Franzetti,
• M. Fumana,
• B. Garilli,
• B. Gillis,
• C. Giocoli,
• A. Grazian,
• F. Grupp,
• S. V. H. Haugan,
• W. Holmes,
• F. Hormuth,
• K. Jahnke,
• S. Kermiche,
• A. Kiessling,
• M. Kilbinger,
• T. Kitching,
• M. Kümmel,
• M. Kunz,
• H. Kurki-Suonio,
• S. Ligori,
• P. B. Lilje,
• I. Lloro,
• E. Maiorano,
• O. Marggraf,
• K. Markovic,
• R. Massey,
• S. Maurogordato,
• M. Melchior,
• M. Meneghetti,
• G. Meylan,
• M. Moresco,
• E. Munari,
• S. M. Niemi,
• C. Padilla,
• S. Paltani,
• F. Pasian,
• K. Pedersen,
• V. Pettorino,
• S. Pires,
• M. Poncet,
• L. Popa,
• L. Pozzetti,
• R. Rebolo,
• J. Rhodes,
• H. Rix,
• M. Roncarelli,
• E. Rossetti,
• R. Saglia,
• P. Schneider,
• A. Secroun,
• G. Seidel,
• S. Serrano,
• C. Sirignano,
• G. Sirri,
• J. -L. Starck,
• P. Tallada-Crespí,
• D. Tavagnacco,
• A. N. Taylor,
• I. Tereno,
• R. Toledo-Moreo,
• F. Torradeflot,
• E. A. Valentijn,
• L. Valenziano,
• Y. Wang,
• N. Welikala,
• G. Zamorani,
• J. Zoubian,
• S. Andreon,
• M. Baldi,
• S. Camera,
• S. Mei,
• C. Neissner,
• E. Romelli
• (less)
Astronomy and Astrophysics, 658, p14 (02/2022) doi:10.1051/0004-6361/202142073
abstract + abstract -

Euclid is poised to survey galaxies across a cosmological volume of unprecedented size, providing observations of more than a billion objects distributed over a third of the full sky. Approximately 20 million of these galaxies will have their spectroscopy available, allowing us to map the three-dimensional large-scale structure of the Universe in great detail. This paper investigates prospects for the detection of cosmic voids therein and the unique benefit they provide for cosmological studies. In particular, we study the imprints of dynamic (redshift-space) and geometric (Alcock-Paczynski) distortions of average void shapes and their constraining power on the growth of structure and cosmological distance ratios. To this end, we made use of the Flagship mock catalog, a state-of-the-art simulation of the data expected to be observed with Euclid. We arranged the data into four adjacent redshift bins, each of which contains about 11 000 voids and we estimated the stacked void-galaxy cross-correlation function in every bin. Fitting a linear-theory model to the data, we obtained constraints on f/b and DMH, where f is the linear growth rate of density fluctuations, b the galaxy bias, DM the comoving angular diameter distance, and H the Hubble rate. In addition, we marginalized over two nuisance parameters included in our model to account for unknown systematic effects in the analysis. With this approach, Euclid will be able to reach a relative precision of about 4% on measurements of f/b and 0.5% on DMH in each redshift bin. Better modeling or calibration of the nuisance parameters may further increase this precision to 1% and 0.4%, respectively. Our results show that the exploitation of cosmic voids in Euclid will provide competitive constraints on cosmology even as a stand-alone probe. For example, the equation-of-state parameter, w, for dark energy will be measured with a precision of about 10%, consistent with previous more approximate forecasts.

This paper is published on behalf of the Euclid Consortium.

(309)Galaxy velocity bias in cosmological simulations: towards per cent-level calibration
• Dhayaa Anbajagane,
• Han Aung,
• August E. Evrard,
• Arya Farahi,
• Daisuke Nagai
• +6
• David J. Barnes,
• Weiguang Cui,
• Klaus Dolag,
• Ian G. McCarthy,
• Elena Rasia,
• Gustavo Yepes
• (less)
Monthly Notices of the Royal Astronomical Society, 510, p18 (02/2022) doi:10.1093/mnras/stab3587
abstract + abstract -

Galaxy cluster masses, rich with cosmological information, can be estimated from internal dark matter (DM) velocity dispersions, which in turn can be observationally inferred from satellite galaxy velocities. However, galaxies are biased tracers of the DM, and the bias can vary over host halo and galaxy properties as well as time. We precisely calibrate the velocity bias, bv - defined as the ratio of galaxy and DM velocity dispersions - as a function of redshift, host halo mass, and galaxy stellar mass threshold ($M_{\rm \star , sat}$), for massive haloes ($M_{\rm 200c}\gt 10^{13.5} \, {\rm M}_\odot$) from five cosmological simulations: IllustrisTNG, Magneticum, Bahamas + Macsis, The Three Hundred Project, and MultiDark Planck-2. We first compare scaling relations for galaxy and DM velocity dispersion across simulations; the former is estimated using a new ensemble velocity likelihood method that is unbiased for low galaxy counts per halo, while the latter uses a local linear regression. The simulations show consistent trends of bv increasing with M200c and decreasing with redshift and $M_{\rm \star , sat}$. The ensemble-estimated theoretical uncertainty in bv is 2-3 per cent, but becomes percent-level when considering only the three highest resolution simulations. We update the mass-richness normalization for an SDSS redMaPPer cluster sample, and find our improved bv estimates reduce the normalization uncertainty from 22 to 8 per cent, demonstrating that dynamical mass estimation is competitive with weak lensing mass estimation. We discuss necessary steps for further improving this precision. Our estimates for $b_v(M_{\rm 200c}, M_{\rm \star , sat}, z)$ are made publicly available.

(308)Muonic boson limits: Supernova redux
• Andrea Caputo,
• Georg Raffelt,
• Edoardo Vitagliano
Physical Review D, 105 (02/2022) doi:10.1103/PhysRevD.105.035022
abstract + abstract -

We derive supernova (SN) bounds on muon-philic bosons, taking advantage of the recent emergence of muonic SN models. Our main innovations are to consider scalars ϕ in addition to pseudoscalars a and to include systematically the generic two-photon coupling Gγ γ implied by a muon triangle loop. This interaction allows for Primakoff scattering and radiative boson decays. The globular-cluster bound Gγ γ<0.67 ×10-10 GeV-1 carries over to the muonic Yukawa couplings as ga<3.1 ×10-9 and gϕ<4.6 ×10-9 for ma ,ϕ≲100 keV , so SN arguments become interesting mainly for larger masses. If bosons escape freely from the SN core the main constraints originate from SN 1987A γ rays and the diffuse cosmic γ -ray background. The latter allows at most 10-4 of a typical total SN energy of ESN≃3 ×1053 erg to show up as γ rays, for ma ,ϕ≳100 keV implying ga≲0.9 ×10-10 and gϕ≲0.4 ×10-10. In the trapping regime the bosons emerge as quasi-thermal radiation from a region near the neutrino sphere and match Lν for ga ,ϕ≃10-4. However, the 2 γ decay is so fast that all the energy is dumped into the surrounding progenitor-star matter, whereas at most 10-2ESN may show up in the explosion. To suppress boson emission below this level we need yet larger couplings, ga≳2 ×10-3 and gϕ≳4 ×10-3. Muonic scalars can explain the muon magnetic-moment anomaly for gϕ≃0.4 ×10-3, a value hard to reconcile with SN physics despite the uncertainty of the explosion-energy bound. For generic axionlike particles, this argument covers the "cosmological triangle" in the Ga γ γ- ma parameter space.

(307)On the tidal formation of dark matter-deficient galaxies
• Go Ogiya,
• Frank C. van den Bosch,
• Andreas Burkert
Monthly Notices of the Royal Astronomical Society, 510, p16 (02/2022) doi:10.1093/mnras/stab3658
abstract + abstract -

Previous studies have shown that dark matter-deficient galaxies (DMDG) such as NGC 1052-DF2 (hereafter DF2) can result from tidal stripping. An important question, though, is whether such a stripping scenario can explain DF2's large specific frequency of globular clusters (GCs). After all, tidal stripping and shocking preferentially remove matter from the outskirts. We examine this using idealized, high-resolution simulations of a regular dark matter-dominated galaxy that is accreted on to a massive halo. As long as the initial (pre-infall) dark matter halo of the satellite is cored, which is consistent with predictions of cosmological, hydrodynamical simulations, the tidal remnant can be made to resemble DF2 in all its properties, including its GC population. The required orbit has a pericentre at the 8.3 percentile of the distribution for subhaloes at infall, and thus is not particularly extreme. On this orbit the satellite loses 98.5 (30) per cent of its original dark matter (stellar) mass, and thus evolves into a DMDG. The fraction of GCs that is stripped off depends on the initial radial distribution. If, at infall, the median projected radius of the GC population is roughly two times that of the stars, consistent with observations of isolated galaxies, only ~20 per cent of the GCs are stripped off. This is less than for the stars, which is due to dynamical friction counteracting the tidal stirring. We predict that, if indeed DF2 was crafted by strong tides, its stellar outskirts should have a very shallow metallicity gradient.

(306)A novel black hole mass scaling relation based on coronal gas, and its dependence with the accretion disc
• Almudena Prieto,
• Alberto Rodríguez-Ardila,
• Swayamtrupta Panda,
• Murilo Marinello
Monthly Notices of the Royal Astronomical Society, 510, p21 (02/2022) doi:10.1093/mnras/stab3414
abstract + abstract -

Using bona-fide black hole (BH) mass estimates from reverberation mapping and the line ratio [Si VI] 1.963$\rm{\mu m}$/Brγbroad as tracer of the AGN ionizing continuum, a novel BH-mass scaling relation of the form log(MBH) = (6.40 ± 0.17) - (1.99 ± 0.37) × log ([Si VI]/Brγbroad), dispersion 0.47 dex, over the BH mass interval, 106-108 M is found. Following on the geometrically thin accretion disc approximation and after surveying a basic parameter space for coronal lines production, we believe one of main drivers of the relation is the effective temperature of the disc, which is effectively sampled by the [Si VI] 1.963$\rm{\mu m}$ coronal line for the range of BH masses considered. By means of CLOUDY photoionization models, the observed anticorrelation appears to be formally in line with the thin disc prediction Tdisc ∝ MBH-1/4.

(305)Simple Rules for Evanescent Operators in One-Loop Basis Transformations
• Jason Aebischer,
• Andrzej J. Buras,
• Jacky Kumar
arXiv e-prints (02/2022) e-Print:2202.01225
abstract + abstract -

Basis transformations often involve Fierz and other relations which are only valid in $D=4$ dimensions. In general $D$ space-time dimensions however, evanescent operators have to be introduced, in order to preserve such identities. Such evanescent operators contribute to one-loop basis transformations as well as to two-loop renormalization group running. We present a simple procedure on how to systematically change basis at the one-loop level by obtaining shifts due to evanescent operators. As an example we apply this method to derive the one-loop basis transformation from the BMU basis useful for NLO QCD calculations, to the JMS basis used in the matching to the SMEFT.

(304)Subdiffusive Activity Spreading in the Diffusive Epidemic Process
• Borislav Polovnikov,
• Patrick Wilke,
• Erwin Frey
Physical Review Letters, 128 (02/2022) doi:10.1103/PhysRevLett.128.078302
abstract + abstract -

The diffusive epidemic process is a paradigmatic example of an absorbing state phase transition in which healthy and infected individuals spread with different diffusion constants. Using stochastic activity spreading simulations in combination with finite-size scaling analyses we reveal two qualitatively different processes that characterize the critical dynamics: subdiffusive propagation of infection clusters and diffusive fluctuations in the healthy population. This suggests the presence of a strong-coupling regime and sheds new light on a long-standing debate about the theoretical classification of the system.

(303)The challenge of simulating the star cluster population of dwarf galaxies with resolved interstellar medium
• Jessica M. Hislop,
• Thorsten Naab,
• Ulrich P. Steinwandel,
• Natalia Lahén,
• Dimitrios Irodotou
• +2
• Peter H. Johansson,
• Stefanie Walch
• (less)
Monthly Notices of the Royal Astronomical Society, 509, p17 (02/2022) doi:10.1093/mnras/stab3347
abstract + abstract -

We present results on the star cluster properties from a series of high resolution smoothed particles hydrodynamics (SPH) simulations of isolated dwarf galaxies as part of the GRIFFIN project. The simulations at sub-parsec spatial resolution and a minimum particle mass of 4 M incorporate non-equilibrium heating, cooling, and chemistry processes, and realize individual massive stars. The simulations follow feedback channels of massive stars that include the interstellar-radiation field variable in space and time, the radiation input by photo-ionization and supernova explosions. Varying the star formation efficiency per free-fall time in the range ϵff = 0.2-50${{\ \rm per\ cent}}$ neither changes the star formation rates nor the outflow rates. While the environmental densities at star formation change significantly with ϵff, the ambient densities of supernovae are independent of ϵff indicating a decoupling of the two processes. At low ϵff, gas is allowed to collapse more before star formation, resulting in more massive, and increasingly more bound star clusters are formed, which are typically not destroyed. With increasing ϵff, there is a trend for shallower cluster mass functions and the cluster formation efficiency Γ for young bound clusters decreases from $50 {{\ \rm per\ cent}}$ to $\sim 1 {{\ \rm per\ cent}}$ showing evidence for cluster disruption. However, none of our simulations form low mass (<103 M) clusters with structural properties in perfect agreement with observations. Traditional star formation models used in galaxy formation simulations based on local free-fall times might therefore be unable to capture star cluster properties without significant fine tuning.

(302)Probing Cosmic Inflation with the LiteBIRD Cosmic Microwave Background Polarization Survey
• LiteBIRD Collaboration,
• E. Allys,
• K. Arnold,
• J. Aumont,
• R. Aurlien
• +182
• S. Azzoni,
• C. Baccigalupi,
• A. J. Banday,
• R. Banerji,
• R. B. Barreiro,
• N. Bartolo,
• L. Bautista,
• D. Beck,
• S. Beckman,
• M. Bersanelli,
• F. Boulanger,
• M. Brilenkov,
• M. Bucher,
• E. Calabrese,
• P. Campeti,
• A. Carones,
• F. J. Casas,
• A. Catalano,
• V. Chan,
• K. Cheung,
• Y. Chinone,
• S. E. Clark,
• F. Columbro,
• G. D'Alessandro,
• P. de Bernardis,
• T. de Haan,
• E. de la Hoz,
• M. De Petris,
• S. Della Torre,
• P. Diego-Palazuelos,
• T. Dotani,
• J. M. Duval,
• T. Elleflot,
• H. K. Eriksen,
• J. Errard,
• T. Essinger-Hileman,
• F. Finelli,
• R. Flauger,
• C. Franceschet,
• U. Fuskeland,
• M. Galloway,
• K. Ganga,
• M. Gerbino,
• M. Gervasi,
• R. T. Génova-Santos,
• T. Ghigna,
• S. Giardiello,
• E. Gjerløw,
• J. Grain,
• F. Grupp,
• A. Gruppuso,
• J. E. Gudmundsson,
• N. W. Halverson,
• P. Hargrave,
• T. Hasebe,
• M. Hasegawa,
• M. Hazumi,
• S. Henrot-Versillé,
• B. Hensley,
• L. T. Hergt,
• D. Herman,
• E. Hivon,
• R. A. Hlozek,
• A. L. Hornsby,
• Y. Hoshino,
• J. Hubmayr,
• K. Ichiki,
• T. Iida,
• H. Imada,
• H. Ishino,
• G. Jaehnig,
• N. Katayama,
• A. Kato,
• R. Keskitalo,
• T. Kisner,
• Y. Kobayashi,
• A. Kogut,
• K. Kohri,
• E. Komatsu,
• K. Komatsu,
• K. Konishi,
• N. Krachmalnicoff,
• C. L. Kuo,
• L. Lamagna,
• M. Lattanzi,
• A. T. Lee,
• C. Leloup,
• F. Levrier,
• E. Linder,
• G. Luzzi,
• J. Macias-Perez,
• B. Maffei,
• D. Maino,
• S. Mandelli,
• E. Martínez-González,
• S. Masi,
• M. Massa,
• S. Matarrese,
• F. T. Matsuda,
• T. Matsumura,
• L. Mele,
• M. Migliaccio,
• Y. Minami,
• A. Moggi,
• J. Montgomery,
• L. Montier,
• G. Morgante,
• B. Mot,
• Y. Nagano,
• T. Nagasaki,
• R. Nagata,
• R. Nakano,
• T. Namikawa,
• F. Nati,
• P. Natoli,
• S. Nerval,
• F. Noviello,
• K. Odagiri,
• S. Oguri,
• H. Ohsaki,
• L. Pagano,
• A. Paiella,
• D. Paoletti,
• A. Passerini,
• G. Patanchon,
• F. Piacentini,
• M. Piat,
• G. Polenta,
• D. Poletti,
• T. Prouvé,
• G. Puglisi,
• D. Rambaud,
• C. Raum,
• S. Realini,
• M. Reinecke,
• M. Remazeilles,
• A. Ritacco,
• G. Roudil,
• J. A. Rubino-Martin,
• M. Russell,
• H. Sakurai,
• Y. Sakurai,
• M. Sasaki,
• D. Scott,
• Y. Sekimoto,
• K. Shinozaki,
• M. Shiraishi,
• P. Shirron,
• G. Signorelli,
• F. Spinella,
• S. Stever,
• R. Stompor,
• S. Sugiyama,
• R. M. Sullivan,
• A. Suzuki,
• T. L. Svalheim,
• E. Switzer,
• R. Takaku,
• H. Takakura,
• Y. Takase,
• A. Tartari,
• Y. Terao,
• J. Thermeau,
• H. Thommesen,
• K. L. Thompson,
• M. Tomasi,
• M. Tominaga,
• M. Tristram,
• M. Tsuji,
• M. Tsujimoto,
• L. Vacher,
• P. Vielva,
• N. Vittorio,
• W. Wang,
• K. Watanuki,
• I. K. Wehus,
• J. Weller,
• B. Westbrook,
• J. Wilms,
• E. J. Wollack,
• J. Yumoto,
• M. Zannoni
• (less)
arXiv e-prints (02/2022) e-Print:2202.02773
abstract + abstract -

LiteBIRD, the Lite (Light) satellite for the study of B-mode polarization and Inflation from cosmic background Radiation Detection, is a space mission for primordial cosmology and fundamental physics. The Japan Aerospace Exploration Agency (JAXA) selected LiteBIRD in May 2019 as a strategic large-class (L-class) mission, with an expected launch in the late 2020s using JAXA's H3 rocket. LiteBIRD is planned to orbit the Sun-Earth Lagrangian point L2, where it will map the cosmic microwave background (CMB) polarization over the entire sky for three years, with three telescopes in 15 frequency bands between 34 and 448 GHz, to achieve an unprecedented total sensitivity of 2.2$\mu$K-arcmin, with a typical angular resolution of 0.5$^\circ$ at 100 GHz. The primary scientific objective of LiteBIRD is to search for the signal from cosmic inflation, either making a discovery or ruling out well-motivated inflationary models. The measurements of LiteBIRD will also provide us with insight into the quantum nature of gravity and other new physics beyond the standard models of particle physics and cosmology. We provide an overview of the LiteBIRD project, including scientific objectives, mission and system requirements, operation concept, spacecraft and payload module design, expected scientific outcomes, potential design extensions and synergies with other projects.

(301)HOLISMOKES. VII. Time-delay measurement of strongly lensed Type Ia supernovae using machine learning
• S. Huber,
• S. H. Suyu,
• D. Ghoshdastidar,
• S. Taubenberger,
• V. Bonvin
• +5
• J. H. H. Chan,
• M. Kromer,
• U. M. Noebauer,
• S. A. Sim,
• L. Leal-Taixé
• (less)
Astronomy and Astrophysics, 658, p25 (02/2022) doi:10.1051/0004-6361/202141956
abstract + abstract -

The Hubble constant (H0) is one of the fundamental parameters in cosmology, but there is a heated debate around the > 4σ tension between the local Cepheid distance ladder and the early Universe measurements. Strongly lensed Type Ia supernovae (LSNe Ia) are an independent and direct way to measure H0, where a time-delay measurement between the multiple supernova (SN) images is required. In this work, we present two machine learning approaches for measuring time delays in LSNe Ia, namely, a fully connected neural network (FCNN) and a random forest (RF). For the training of the FCNN and the RF, we simulate mock LSNe Ia from theoretical SN Ia models that include observational noise and microlensing. We test the generalizability of the machine learning models by using a final test set based on empirical LSN Ia light curves not used in the training process, and we find that only the RF provides a low enough bias to achieve precision cosmology; as such, RF is therefore preferred over our FCNN approach for applications to real systems. For the RF with single-band photometry in the i band, we obtain an accuracy better than 1% in all investigated cases for time delays longer than 15 days, assuming follow-up observations with a 5σ point-source depth of 24.7, a two day cadence with a few random gaps, and a detection of the LSNe Ia 8 to 10 days before peak in the observer frame. In terms of precision, we can achieve an approximately 1.5-day uncertainty for a typical source redshift of ∼0.8 on the i band under the same assumptions. To improve the measurement, we find that using three bands, where we train a RF for each band separately and combine them afterward, helps to reduce the uncertainty to ∼1.0 day. The dominant source of uncertainty is the observational noise, and therefore the depth is an especially important factor when follow-up observations are triggered. We have publicly released the microlensed spectra and light curves used in this work.

https://github.com/shsuyu/HOLISMOKES-public/tree/main/HOLISMOKES_VII

(300)Exploring the relation between turbulent velocity and density fluctuations in the stratified intracluster medium
• M. Simonte,
• F. Vazza,
• F. Brighenti,
• M. Brüggen,
• T. W. Jones
• +1
Astronomy and Astrophysics, 658, p14 (02/2022) doi:10.1051/0004-6361/202141703
abstract + abstract -

Context. The dynamics of the intracluster medium (ICM) is affected by turbulence driven by several processes, such as mergers, accretion and feedback from active galactic nuclei.
Aims: X-ray surface brightness fluctuations have been used to constrain turbulence in galaxy clusters. Here, we use simulations to further investigate the relation between gas density and turbulent velocity fluctuations, with a focus on the effect of the stratification of the ICM.
Methods: In this work, we studied the turbulence driven by hierarchical accretion by analysing a sample of galaxy clusters simulated with the cosmological code ENZO. We used a fixed scale filtering approach to disentangle laminar from turbulent flows.
Results: In dynamically perturbed galaxy clusters, we found a relation between the root mean square of density and velocity fluctuations, albeit with a different slope than previously reported. The Richardson number is a parameter that represents the ratio between turbulence and buoyancy, and we found that this variable has a strong dependence on the filtering scale. However, we could not detect any strong relation between the Richardson number and the logarithmic density fluctuations, in contrast to results by recent and more idealised simulations. In particular, we find a strong effect from radial accretion, which appears to be the main driver for the gas fluctuations. The ubiquitous radial bias in the dynamics of the ICM suggests that homogeneity and isotropy are not always valid assumptions, even if the turbulent spectra follow Kolmogorov's scaling. Finally, we find that the slope of the velocity and density spectra are independent of cluster-centric radii.

(299)Hidden in the haystack: low-luminosity globular clusters towards the Milky Way bulge
• F. Gran,
• M. Zoccali,
• I. Saviane,
• E. Valenti,
• A. Rojas-Arriagada
• +6
• R. Contreras Ramos,
• J. Hartke,
• J. A. Carballo-Bello,
• C. Navarrete,
• M. Rejkuba,
• J. Olivares Carvajal
• (less)
Monthly Notices of the Royal Astronomical Society, 509, p20 (02/2022) doi:10.1093/mnras/stab2463
abstract + abstract -

Recent wide-area surveys have enabled us to study the Milky Way with unprecedented detail. Its inner regions, hidden behind dust and gas, have been partially unveiled with the arrival of near-infrared (IR) photometric and spectroscopic data sets. Among recent discoveries, there is a population of low-mass globular clusters, known to be missing, especially towards the Galactic bulge. In this work, five new low-luminosity globular clusters located towards the bulge area are presented. They were discovered by searching for groups in the multidimensional space of coordinates, colours, and proper motions from the Gaia EDR3 catalogue and later confirmed with deeper VVV survey near-IR photometry. The clusters show well-defined red giant branches and, in some cases, horizontal branches with their members forming a dynamically coherent structure in proper motion space. Four of them were confirmed by spectroscopic follow-up with the MUSE instrument on the ESO VLT. Photometric parameters were derived, and when available, metallicities, radial velocities, and orbits were determined. The new clusters Gran 1 and 5 are bulge globular clusters, while Gran 2, 3 and 4 present halo-like properties. Preliminary orbits indicate that Gran 1 might be related to the Main Progenitor, or the so-called 'low-energy' group, while Gran 2, 3 and 5 appears to follow the Gaia-Enceladus/Sausage structure. This study demonstrates that the Gaia proper motions, combined with the spectroscopic follow-up and colour-magnitude diagrams, are required to confirm the nature of cluster candidates towards the inner Galaxy. High stellar crowding and differential extinction may hide other low-luminosity clusters.

(298)New physics from the polarised light of the cosmic microwave background
• Eiichiro Komatsu
arXiv e-prints (02/2022) e-Print:2202.13919
abstract + abstract -

Cosmology requires new physics beyond the Standard Model of elementary particles and fields. What is the fundamental physics behind dark matter and dark energy? What generated the initial fluctuations in the early Universe? Polarised light of the cosmic microwave background (CMB) may hold the key to answers. In this article, we discuss two new developments in this research area. First, if the physics behind dark matter and dark energy violates parity symmetry, their coupling to photons rotates the plane of linear polarisation as the CMB photons travel more than 13 billion years. This effect is known as cosmic birefringence': space filled with dark matter and dark energy behaves as if it were a birefringent material, like a crystal. A tantalising hint for such a signal has been found with the statistical significance of $3\sigma$. Next, the period of accelerated expansion in the very early Universe, called cosmic inflation', produced a stochastic background of primordial gravitational waves (GW). What generated GW? The leading idea is vacuum fluctuations in spacetime, but matter fields could also produce a significant amplitude of primordial GW. Finding its origin using CMB polarisation opens a new window into the physics behind inflation. These new scientific targets may influence how data from future CMB experiments are collected, calibrated, and analysed.

(297)The Three Hundred project: The Gizmo-Simba runs
• 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 Ferragam,
• Giulia Gianfagna
• (less)
arXiv e-prints (02/2022) e-Print:2202.14038
abstract + abstract -

We introduce \textsc{Gizmo-Simba}, a new suite of galaxy cluster simulations within \textsc{The Three Hundred} project. \textsc{The Three Hundred} consists of zoom re-simulations of 324 clusters with $M_{200}\gtrsim 10^{14.8}M_\odot$ drawn from the MultiDark-Planck $N$-body simulation, run using several hydrodynamic and semi-analytic codes. The \textsc{Gizmo-Simba} suite adds a state-of-the-art galaxy formation model based on the highly successful {\sc Simba} simulation, mildly re-calibrated to match $z=0$ cluster stellar properties. Comparing to \textsc{The Three Hundred} zooms run with \textsc{Gadget-X}, we find intrinsic differences in the evolution of the stellar and gas mass fractions, BCG ages, and galaxy colour-magnitude diagrams, with \textsc{Gizmo-Simba} generally providing a good match to available data at $z \approx 0$. \textsc{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. \textsc{Gizmo-Simba} provides a new and novel platform to elucidate the co-evolution of galaxies, gas, and black holes within the densest cosmic environments.

(296)Milky Way Satellite Census. IV. Constraints on Decaying Dark Matter from Observations of Milky Way Satellite Galaxies
• S. Mau,
• E.O. Nadler,
• R.H. Wechsler,
• A. Drlica-Wagner,
• K. Bechtol
• +64
• G. Green,
• D. Huterer,
• T.S. Li,
• Y.-Y. Mao,
• C.E. Martínez-Vázquez,
• M. McNanna,
• B. Mutlu-Pakdil,
• A.B. Pace,
• A. Peter,
• A.H. Riley,
• L. Strigari,
• M.-Y. Wang,
• M. Aguena,
• S. Allam,
• J. Annis,
• D. Bacon,
• E. Bertin,
• S. Bocquet,
• D. Brooks,
• D.L. Burke,
• A. Carnero Rosell,
• M. Carrasco Kind,
• J. Carretero,
• M. Costanzi,
• M. Crocce,
• M.E.S. Pereira,
• T.M. Davis,
• J. De Vicente,
• S. Desai,
• P. Doel,
• I. Ferrero,
• B. Flaugher,
• J. Frieman,
• J. García-Bellido,
• M. Gatti,
• G. Giannini,
• D. Gruen,
• R.A. Gruendl,
• J. Gschwend,
• G. Gutierrez,
• S.R. Hinton,
• D.L. Hollowood,
• K. Honscheid,
• D.J. James,
• K. Kuehn,
• O. Lahav,
• M.A.G. Maia,
• J.L. Marshall,
• R. Miquel,
• J.J. Mohr,
• R. Morgan,
• R.L.C. Ogando,
• F. Paz-Chinchón,
• A. Pieres,
• M. Rodriguez-Monroy,
• E. Sanchez,
• V. Scarpine,
• S. Serrano,
• I. Sevilla-Noarbe,
• E. Suchyta,
• G. Tarle,
• C. To,
• D.L. Tucker,
• J. Weller
• (less)
(01/2022) e-Print:2201.11740
abstract + abstract -

We use a recent census of the Milky Way (MW) satellite galaxy population to constrain the lifetime of particle dark matter (DM). We consider two-body decaying dark matter (DDM) in which a heavy DM particle decays with lifetime $\tau$ comparable to the age of the Universe to a lighter DM particle (with mass splitting $\epsilon$) and to a dark radiation species. These decays impart a characteristic "kick velocity," $V_{\mathrm{kick}}=\epsilon c$, on the DM daughter particles, significantly depleting the DM content of low-mass subhalos and making them more susceptible to tidal disruption. We fit the suppression of the present-day DDM subhalo mass function (SHMF) as a function of $\tau$ and $V_{\mathrm{kick}}$ using a suite of high-resolution zoom-in simulations of MW-mass halos, and we validate this model on new DDM simulations of systems specifically chosen to resemble the MW. We implement our DDM SHMF predictions in a forward model that incorporates inhomogeneities in the spatial distribution and detectability of MW satellites and uncertainties in the mapping between galaxies and DM halos, the properties of the MW system, and the disruption of subhalos by the MW disk using an empirical model for the galaxy--halo connection. By comparing to the observed MW satellite population, we conservatively exclude DDM models with $\tau < 18\ \mathrm{Gyr}$ ($29\ \mathrm{Gyr}$) for $V_{\mathrm{kick}}=20\ \mathrm{km}\, \mathrm{s}^{-1}$ ($40\ \mathrm{km}\, \mathrm{s}^{-1}$) at $95\%$ confidence. These constraints are among the most stringent and robust small-scale structure limits on the DM particle lifetime and strongly disfavor DDM models that have been proposed to alleviate the Hubble and $S_8$ tensions.

(295)Assessing coincident neutrino detections using population models
• F. Capel,
• J.M. Burgess,
• D.J. Mortlock,
• P. Padovani
(01/2022) e-Print:2201.05633
abstract + abstract -

Several marginally significant associations between high-energy neutrinos and potential astrophysical sources have been recently reported, but a conclusive identification of these sources remains challenging. We explore the use of Monte Carlo simulations to gain deeper insight into the implications of, in particular, the IC170922A-TXS 0506+056 observation. Assuming a null model, we find a 7.6% chance to mistakenly identify coincidences between flaring blazars and neutrino alerts in 10-year surveys. We confirm that a blazar-neutrino connection based on the ${\gamma}$-ray flux is required to find a low chance coincidence probability and, therefore, a significant IC170922A-TXS 0506+056 association. We then assume this blazar-neutrino connection for the whole population and find that the ratio of neutrino to ${\gamma}$-ray fluxes must be $\lesssim 10^{-2}$ in order not to overproduce the total number of neutrino alerts seen by IceCube. For the IC170922A-TXS 0506+056 association to make sense, we must either accept this low flux ratio or suppose that only some rare sub-population of blazars is capable of high-energy neutrino production. For example, if we consider neutrino production only in blazar flares, we expect the flux ratio of between $10^{-3}$ and $10^{-1}$ to be consistent with a single coincident observation of a neutrino alert and flaring blazar. These conclusions are robust with respect to the uncertainties in our modelling assumptions.

(294)Fast and precise model calculation for KATRIN using a neural network
• Christian Karl,
• Philipp Eller,
• Susanne Mertens
Eur.Phys.J.C, 82, p439 (01/2022) e-Print:2201.04523 doi:10.1140/epjc/s10052-022-10384-z
abstract + abstract -

We present a fast and precise method to approximate the physics model of the Karlsruhe Tritium Neutrino (KATRIN) experiment using a neural network. KATRIN is designed to measure the effective electron anti-neutrino mass $m_\nu$ using the kinematics of $\upbeta$-decay with a sensitivity of 200 meV at 90% confidence level. To achieve this goal, a highly accurate model prediction with relative errors below the $10^{-4}$-level is required. Using the regular numerical model for the analysis of the final KATRIN dataset is computationally extremely costly or requires approximations to decrease the computation time. Our solution to reduce the computational requirements is to train a neural network to learn the predicted $\upbeta$-spectrum and its dependence on all relevant input parameters. This results in a speed-up of the calculation by about three orders of magnitude, while meeting the stringent accuracy requirements of KATRIN.

(293)Probing spin-dependent dark matter interactions with $^6$Li: CRESST Collaboration
• G. Angloher,
• G. Benato,
• A. Bento,
• E. Bertoldo,
• A. Bertolini
• +53
• R. Breier,
• C. Bucci,
• 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,
• P. Gorla,
• S. Gupta,
• D. Hauff,
• M. Ješkovský,
• J. Jochum,
• M. Kaznacheeva,
• A. Kinast,
• H. Kluck,
• H. Kraus,
• A. Langenkämper,
• M. Mancuso,
• L. Marini,
• V. Mokina,
• A. Nilima,
• M. Olmi,
• T. Ortmann,
• C. Pagliarone,
• V. Palušová,
• 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)
Eur.Phys.J.C, 82, p207 (01/2022) e-Print:2201.03863 doi:10.1140/epjc/s10052-022-10140-3
abstract + abstract -

CRESST is one of the most prominent direct detection experiments for dark matter particles with sub-GeV/c$^2$ mass. One of the advantages of the CRESST experiment is the possibility to include a large variety of nuclides in the target material used to probe dark matter interactions. In this work, we discuss in particular the interactions of dark matter particles with protons and neutrons of $^{6}$Li. This is now possible thanks to new calculations on nuclear matrix elements of this specific isotope of Li. To show the potential of using this particular nuclide for probing dark matter interactions, we used the data collected previously by a CRESST prototype based on LiAlO$_2$ and operated in an above ground test-facility at Max-Planck-Institut für Physik in Munich, Germany. In particular, the inclusion of $^{6}$Li in the limit calculation drastically improves the result obtained for spin-dependent interactions with neutrons in the whole mass range. The improvement is significant, greater than two order of magnitude for dark matter masses below 1 GeV/c$^2$, compared to the limit previously published with the same data.

(292)Analytical evaluation of AdS${}_4$ Witten diagrams as flat space multi-loop Feynman integrals
• Till Heckelbacher,
• Ivo Sachs,
• Evgeny Skvortsov,
• Pierre Vanhove
arXiv e-prints (01/2022) e-Print:2201.09626
abstract + abstract -

We describe a systematic approach for the evaluation of Witten diagrams for multi-loop scattering amplitudes of a conformally coupled scalar $\phi^4$-theory in Euclidean AdS$_4$, 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.

(291)Redshift-space effects in voids and their impact on cosmological tests - II. The void-galaxy cross-correlation function
• Carlos M. Correa,
• Dante J. Paz,
• Nelson D. Padilla,
• Ariel G. Sánchez,
• Andrés N. Ruiz
• +1
Monthly Notices of the Royal Astronomical Society, 509, p14 (01/2022) doi:10.1093/mnras/stab3070
abstract + abstract -

This is the second part of a thorough investigation of the redshift-space effects that affect void properties and the impact they have on cosmological tests. Here, we focus on the void-galaxy cross-correlation function, specifically, on the projected versions that we developed in a previous work. The pillar of the analysis is the one-to-one relationship between real and redshift-space voids above the shot-noise level identified with a spherical void finder. Under this mapping, void properties are affected by three effects: (i) a systematic expansion as a consequence of the distortions induced by galaxy dynamics, (ii) the Alcock-Paczynski volume effect, which manifests as an overall expansion or contraction depending on the fiducial cosmology, and (iii) a systematic off-centring along the line of sight as a consequence of the distortions induced by void dynamics. We found that correlations are also affected by an additional source of distortions: the ellipticity of voids. This is the first time that distortions due to the off-centring and ellipticity effects are detected and quantified. With a simplified test, we verified that the Gaussian streaming model is still robust provided all these effects are taken into account, laying the foundations for improvements in current models in order to obtain unbiased cosmological constraints from spectroscopic surveys. Besides this practical importance, this analysis also encodes key information about the structure and dynamics of the Universe at the largest scales. Furthermore, some of the effects constitute cosmological probes by themselves, as is the case of the void ellipticity.

(290)Dust entrainment in photoevaporative winds: Densities and imaging
• R. Franz,
• B. Ercolano,
• S. Casassus,
• G. Picogna,
• T. Birnstiel
• +3
Astronomy and Astrophysics, 657, p14 (01/2022) doi:10.1051/0004-6361/202140812
abstract + abstract -

Context. X-ray- and extreme-ultraviolet- (together: XEUV-) driven photoevaporative winds acting on protoplanetary disks around young T-Tauri stars may crucially impact disk evolution, affecting both gas and dust distributions.
Aims: We constrain the dust densities in a typical XEUV-driven outflow, and determine whether these winds can be observed at μm-wavelengths.
Methods: We used dust trajectories modelled atop a 2D hydrodynamical gas model of a protoplanetary disk irradiated by a central T-Tauri star. With these and two different prescriptions for the dust distribution in the underlying disk, we constructed wind density maps for individual grain sizes. We used the dust density distributions obtained to synthesise observations in scattered and polarised light.
Results: For an XEUV-driven outflow around a M* = 0.7 M T-Tauri star with LX = 2 × 1030 erg s−1, we find a dust mass-loss rate Ṁdust ≲ 4.1 × 10−11 M yr−1 for an optimistic estimate of dust densities in the wind (compared to Ṁgas ≈ 3.7 × 10−8 M yr−1). The synthesised scattered-light images suggest a distinct chimney structure emerging at intensities I∕Imax < 10−4.5 (10−3.5) at λobs = 1.6 (0.4) μm, while the features in the polarised-light images are even fainter. Observations synthesised from our model do not exhibit clear features for SPHERE IRDIS, but show a faint wind signature for JWST NIRCam under optimal conditions.
Conclusions: Unambiguous detections of photoevaporative XEUV winds launched from primordial disks are at least challenging with current instrumentation; this provides a possible explanation as to why disk winds are not routinely detected in scattered or polarised light. Our calculations show that disk scale heights retrieved from scattered-light observations should be only marginally affected by the presence of an XEUV wind.

(289)Precision tests of fundamental physics with η and η<SUP>′</SUP> mesons
• Liping Gan,
• Bastian Kubis,
• Emilie Passemar,
• Sean Tulin
Physics Reports, 945, p105 (01/2022) doi:10.1016/j.physrep.2021.11.001
abstract + abstract -

Decays of the neutral and long-lived η and η mesons provide a unique, flavor-conserving laboratory to test low-energy Quantum Chromodynamics and search for new physics beyond the Standard Model. They have drawn world-wide attention in recent years and have inspired broad experimental programs in different high-intensity-frontier centers. New experimental data will offer critical inputs to precisely determine the light quark mass ratios, η-η mixing parameters, and hadronic contributions to the anomalous magnetic moment of the muon. At the same time, it will provide a sensitive probe to test potential new physics. This includes searches for hidden photons, light Higgs scalars, and axion-like particles that are complementary to worldwide efforts to detect new light particles below the GeV mass scale, as well as tests of discrete symmetry violation. In this review, we give an update on theoretical developments, discuss the experimental opportunities, and identify future research needed in this field.

(288)Driving Galactic Outflows with Magnetic Fields at Low and High Redshift
• Ulrich P. Steinwandel,
• Klaus Dolag,
• Harald Lesch,
• Andreas Burkert
The Astrophysical Journal, 924, p17 (01/2022) doi:10.3847/1538-4357/ac2ffd
abstract + abstract -

Although galactic outflows play a key role in our understanding of the evolution of galaxies, the exact mechanism by which galactic outflows are driven is still far from being understood and, therefore, our understanding of associated feedback mechanisms that control the evolution of galaxies is still plagued by many enigmas. In this work, we present a simple toy model that can provide insight on how non-axisymmetric instabilities in galaxies (bars, spiral arms, warps) can lead to local exponential magnetic field growth by radial flows beyond the equipartition value by at least two orders of magnitude on a timescale of a few 100 Myr. Our predictions show that the process can lead to galactic outflows in barred spiral galaxies with a mass-loading factor η ≍ 0.1, in agreement with our numerical simulations. Moreover, our outflow mechanism could contribute to an understanding of the large fraction of barred spiral galaxies that show signs of galactic outflows in the CHANG-ES survey. Extending our model shows the importance of such processes in high-redshift galaxies by assuming equipartition between magnetic energy and turbulent energy. Simple estimates for the star formation rate in our model together with cross correlated masses from the star-forming main sequence at redshifts z ~ 2 allow us to estimate the outflow rate and mass-loading factors by non-axisymmetric instabilities and a subsequent radial inflow dynamo, giving mass-loading factors of η ≍ 0.1 for galaxies in the range of M = 109-1012 M , in good agreement with recent results of SINFONI and KMOS 3D.

(287)Assessing coincident neutrino detections using population models
• F. Capel,
• J. M. Burgess,
• D. J. Mortlock,
• P. Padovani
arXiv e-prints (01/2022) e-Print:2201.05633
abstract + abstract -

Several marginally significant associations between high-energy neutrinos and potential astrophysical sources have been recently reported, but a conclusive identification of these sources remains challenging. We explore the use of Monte Carlo simulations to gain deeper insight into the implications of, in particular, the IC170922A-TXS 0506+056 observation. Assuming a null model, we find a 7.6% chance to mistakenly identify coincidences between flaring blazars and neutrino alerts in 10-year surveys. We confirm that a blazar-neutrino connection based on the ${\gamma}$-ray flux is required to find a low chance coincidence probability and, therefore, a significant IC170922A-TXS 0506+056 association. We then assume this blazar-neutrino connection for the whole population and find that the ratio of neutrino to ${\gamma}$-ray fluxes must be $\lesssim 10^{-2}$ in order not to overproduce the total number of neutrino alerts seen by IceCube. For the IC170922A-TXS 0506+056 association to make sense, we must either accept this low flux ratio or suppose that only some rare sub-population of blazars is capable of high-energy neutrino production. For example, if we consider neutrino production only in blazar flares, we expect the flux ratio of between $10^{-3}$ and $10^{-1}$ to be consistent with a single coincident observation of a neutrino alert and flaring blazar. These conclusions are robust with respect to the uncertainties in our modelling assumptions.

(286)Asymptotic dynamics and charges for FLRW spacetimes
• Martin Enriquez-Rojo,
• Till Heckelbacher,
• Roberto Oliveri
arXiv e-prints (01/2022) e-Print:2201.07600
abstract + abstract -

We investigate the asymptotia of decelerating and spatially flat FLRW spacetimes at future null infinity. We find that the asymptotic algebra of diffeomorphisms can be enlarged to a one-parameter deformation of the recently discovered Weyl-BMS algebra for asymptotically flat spacetimes by relaxing the boundary conditions. The deformation parameter is related to the equation of state of the fluid. We then study the equations of motion for asymptotically FLRW spacetimes with finite fluxes and show that the dynamics is fully constrained by the stress-tensor of the source. Finally, we propose an expression for the charges which are associated with the cosmological supertranslations and whose evolution equation features a novel contribution arising from the Hubble flow.

(285)Truncated affine Rozansky--Witten models as extended TQFTs
• Ilka Brunner,
• Nils Carqueville,
• Daniel Roggenkamp
arXiv e-prints (01/2022) e-Print:2201.03284
abstract + abstract -

We construct extended TQFTs associated to Rozansky--Witten models with target manifolds $T^*\mathbb{C}^n$. The starting point of the construction is the 3-category whose objects are such Rozansky--Witten models, and whose morphisms are defects of all codimensions. By truncation, we obtain a (non-semisimple) 2-category $\mathcal{C}$ of bulk theories, surface defects, and isomorphism classes of line defects. Through a systematic application of the cobordism hypothesis we construct a unique extended oriented 2-dimensional TQFT valued in $\mathcal{C}$ for every affine Rozansky--Witten model. By evaluating this TQFT on closed surfaces we obtain the infinite-dimensional state spaces (graded by flavour and R-charges) of the initial 3-dimensional theory. Furthermore, we explicitly compute the commutative Frobenius algebras that classify the restrictions of the extended theories to circles and bordisms between them.

(284)HOLISMOKES. VIII. High-redshift Strong Lens Candidates from the Hyper Suprime-Cam Subaru Strategic Program
• Yiping Shu,
• Raoul Cañameras,
• Stefan Schuldt,
• Sherry H. Suyu,
• Stefan Taubenberger
• +2
• Kaiki Taro Inoue,
• Anton T. Jaelani
• (less)
arXiv e-prints (01/2022) e-Print:2201.11135
abstract + abstract -

We carry out a dedicated search for strong-lens systems with high-redshift lens galaxies with the goal of extending strong lensing-assisted galaxy evolutionary studies to earlier cosmic time. Two strong-lens classifiers are constructed from a deep residual network and trained with datasets of different lens redshift and brightness distributions. We classify a sample of 5,356,628 pre-selected objects from the Wide layer fields in the second public data release of the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) by applying the two classifiers to their HSC $gri$-filter cutouts. Cutting off at thresholds that correspond to a false-positive rate of $10^{-3}$ on our test set, the two classifiers identify 5,468 and 6,119 strong-lens candidates. Visually inspecting the cutouts of those candidates results in 735 grade-A/B strong-lens candidates in total, of which 277 candidates are discovered for the first time. This is the single largest set of galaxy-scale strong-lens candidates discovered with HSC data to date, and nearly half of it (331/735) contains lens galaxies with photometric redshifts above 0.6. Our discoveries will serve as a valuable target list for ongoing and scheduled spectroscopic surveys such as the Dark Energy Spectroscopic Instrument, the Subaru Prime Focus Spectrograph project, and the Maunakea Spectroscopic Explorer.

(283)Fast and precise model calculation for KATRIN using a neural network
• Christian Karl,
• Philipp Eller,
• Susanne Mertens
arXiv e-prints (01/2022) e-Print:2201.04523
abstract + abstract -

We present a fast and precise method to approximate the physics model of the Karlsruhe Tritium Neutrino (KATRIN) experiment using a neural network. KATRIN is designed to measure the effective electron anti-neutrino mass using the kinematics of beta-decay with a sensitivity of 200 meV at 90% confidence level. To achieve this goal, a highly accurate model prediction with relative errors below the 1e-4-level is required. Using the regular numerical model for the analysis of the final KATRIN dataset is computationally extremely costly or requires approximations to decrease the computation time. Our solution to reduce the computational requirements is to train a neural network to learn the predicted beta-spectrum and its dependence on all relevant input parameters. This results in a speed-up of the calculation by about three orders of magnitude, while meeting the stringent accuracy requirements of KATRIN.

(282)Silicon in the dayside atmospheres of two ultra-hot Jupiters
• D. Cont,
• F. Yan,
• A. Reiners,
• L. Nortmann,
• K. Molaverdikhani
• +20
• E. Pallé,
• M. Stangret,
• Th. Henning,
• I. Ribas,
• A. Quirrenbach,
• J. A. Caballero,
• M. R. Zapatero Osorio,
• P. J. Amado,
• J. Aceituno,
• N. Casasayas-Barris,
• S. Czesla,
• A. Kaminski,
• M. López-Puertas,
• D. Montes,
• J. C. Morales,
• G. Morello,
• E. Nagel,
• A. Sánchez-López,
• E. Sedaghati,
• M. Zechmeister
• (less)
Astronomy and Astrophysics, 657, p12 (01/2022) doi:10.1051/0004-6361/202142776
abstract + abstract -

Atmospheres of highly irradiated gas giant planets host a large variety of atomic and ionic species. Here we observe the thermal emission spectra of the two ultra-hot Jupiters WASP-33b and KELT-20b/MASCARA-2b in the near-infrared wavelength range with CARMENES. Via high-resolution Doppler spectroscopy, we searched for neutral silicon (Si) in their dayside atmospheres. We detect the Si spectral signature of both planets via cross-correlation with model spectra. Detection levels of 4.8σ and 5.4σ, respectively, are observed when assuming a solar atmospheric composition. This is the first detection of Si in exoplanet atmospheres. The presence of Si is an important finding due to its fundamental role in cloud formation and, hence, for the planetary energy balance. Since the spectral lines are detected in emission, our results also confirm the presence of an inverted temperature profile in the dayside atmospheres of both planets.

(281)Final Report for SAG 21: The Effect of Stellar Contamination on Space-based Transmission Spectroscopy
• Benjamin V. Rackham,
• Néstor Espinoza,
• Svetlana V. Berdyugina,
• Heidi Korhonen,
• Ryan J. MacDonald
• +56
• Benjamin T. Montet,
• Brett M. Morris,
• Mahmoudreza Oshagh,
• Alexander I. Shapiro,
• Yvonne C. Unruh,
• Elisa V. Quintana,
• Robert T. Zellem,
• Dániel Apai,
• Thomas Barclay,
• Joanna K. Barstow,
• Giovanni Bruno,
• Ludmila Carone,
• Sarah L. Casewell,
• Heather M. Cegla,
• Serena Criscuoli,
• Catherine Fischer,
• Damien Fournier,
• Mark S. Giampapa,
• Helen Giles,
• Aishwarya Iyer,
• Greg Kopp,
• Nadiia M. Kostogryz,
• Natalie Krivova,
• Matthias Mallonn,
• Chima McGruder,
• Karan Molaverdikhani,
• Elisabeth R. Newton,
• Mayukh Panja,
• Sarah Peacock,
• Kevin Reardon,
• Rachael M. Roettenbacher,
• Gaetano Scandariato,
• Sami Solanki,
• Keivan G. Stassun,
• Oskar Steiner,
• Kevin B. Stevenson,
• Jeremy Tregloan-Reed,
• Adriana Valio,
• Sven Wedemeyer,
• Luis Welbanks,
• Jie Yu,
• Munazza K. Alam,
• James R. A. Davenport,
• Drake Deming,
• Chuanfei Dong,
• Elsa Ducrot,
• Chloe Fisher,
• Emily Gilbert,
• Veselin Kostov,
• Mercedes López-Morales,
• Mike Line,
• Teo Močnik,
• Susan Mullally,
• Rishi R. Paudel,
• Ignasi Ribas,
• Jeff A. Valenti
• (less)
arXiv e-prints (01/2022) e-Print:2201.09905
abstract + abstract -

Study Analysis Group 21 (SAG21) of the Exoplanet Exploration Program Analysis Group (ExoPAG) was organized to study the effect of stellar contamination on space-based transmission spectroscopy, a method for studying exoplanetary atmospheres by measuring the wavelength-dependent radius of a planet as it transits its star. Transmission spectroscopy relies on a precise understanding of the spectrum of the star being occulted. However, stars are not homogeneous, constant light sources but have temporally evolving photospheres and chromospheres with inhomogeneities like spots, faculae, and plages. This SAG has brought together an interdisciplinary team of more than 100 scientists, with observers and theorists from the heliophysics, stellar astrophysics, planetary science, and exoplanetary atmosphere research communities, to study the current needs that can be addressed in this context to make the most of transit studies from current NASA facilities like HST and JWST. The analysis produced 14 findings, which fall into three Science Themes encompassing (1) how the Sun is used as our best laboratory to calibrate our understanding of stellar heterogeneities ("The Sun as the Stellar Benchmark"), (2) how stars other than the Sun extend our knowledge of heterogeneities ("Surface Heterogeneities of Other Stars") and (3) how to incorporate information gathered for the Sun and other stars into transit studies ("Mapping Stellar Knowledge to Transit Studies").

(280)Neutrino absorption and other physics dependencies in neutrino-cooled black hole accretion discs
• O. Just,
• S. Goriely,
• H. -Th Janka,
• S. Nagataki,
• A. Bauswein
Monthly Notices of the Royal Astronomical Society, 509, p36 (01/2022) doi:10.1093/mnras/stab2861
abstract + abstract -

Black hole (BH) accretion discs formed in compact-object mergers or collapsars may be major sites of the rapid-neutron-capture (r-)process, but the conditions determining the electron fraction (Ye) remain uncertain given the complexity of neutrino transfer and angular-momentum transport. After discussing relevant weak-interaction regimes, we study the role of neutrino absorption for shaping Ye using an extensive set of simulations performed with two-moment neutrino transport and again without neutrino absorption. We vary the torus mass, BH mass and spin, and examine the impact of rest-mass and weak-magnetism corrections in the neutrino rates. We also test the dependence on the angular-momentum transport treatment by comparing axisymmetric models using the standard α-viscosity with viscous models assuming constant viscous length-scales (lt) and 3D magnetohydrodynamic (MHD) simulations. Finally, we discuss the nucleosynthesis yields and basic kilonova properties. We find that absorption pushes Ye towards ~0.5 outside the torus, while inside increasing the equilibrium value $Y_\mathrm{ e}^{\mathrm{eq}}$ by ~0.05-0.2. Correspondingly, a substantial ejecta fraction is pushed above Ye = 0.25, leading to a reduced lanthanide fraction and a brighter, earlier, and bluer kilonova than without absorption. More compact tori with higher neutrino optical depth, τ, tend to have lower $Y_\mathrm{ e}^{\mathrm{eq}}$ up to τ ~ 1-10, above which absorption becomes strong enough to reverse this trend. Disc ejecta are less (more) neutron rich when employing an lt = const. viscosity (MHD treatment). The solar-like abundance pattern found for our MHD model marginally supports collapsar discs as major r-process sites, although a strong r-process may be limited to phases of high mass-infall rates, $\dot{M}\, \, \raise0.14em\rm{\gt }\lower0.28em\rm{\sim }\, \, 2\times 10^{-2}$ M s-1.

(279)Massive quiescent galaxies at $z\sim3$: a comparison of selection, stellar population and structural properties with simulation predictions
• Peter Lustig,
• Veronica Strazzullo,
• Rhea-Silvia Remus,
• Chiara D'Eugenio,
• Emanuele Daddi
• +11
• Andreas Burkert,
• Gabriella De Lucia,
• Ivan Delvecchio,
• Klaus Dolag,
• Fabio Fontanot,
• Raphael Gobat,
• Joseph J. Mohr,
• Masato Onodera,
• Maurilio Pannella,
• Annalisa Pillepich,
• Alvio Renzini
• (less)
arXiv e-prints (01/2022) e-Print:2201.09068
abstract + abstract -

We study stellar population and structural properties of massive $\log(M_{\star} / M_{\odot}) > 11$ galaxies at $z\sim2.7$ in the Magneticum (box 3) and IllustrisTNG (TNG100, TNG300) hydrodynamical simulations. We find stellar mass functions broadly consistent with observations, with no scarcity of massive, quiescent galaxies at $z\sim2.7$, but with a higher quiescent galaxy fraction at high masses in IllustrisTNG. Average ages of simulated quiescent galaxies are between 0.8 and 1.0 Gyr, older by a factor $\sim2$ than observed in spectroscopically-confirmed quiescent galaxies at similar redshift. Besides being potentially indicative of issues with star-formation recipes in simulations, this discrepancy might also be partly explained by limitations in the estimation of observed ages. We investigate the purity of simulated UVJ rest-frame colorselected massive quiescent samples with photometric uncertainties typical of deep surveys (e.g., COSMOS). We find evidence for significant contamination (up to 60 percent) by dusty star-forming galaxies in the UVJ region that is typically populated by older quiescent sources. Furthermore, simulations suggest that the completeness of UVJ-selected quiescent samples at this redshift may be reduced by 30 percent due to a high fraction of young quiescent galaxies not entering the UVJ quiescent region. Massive, quiescent galaxies in simulations have on average lower angular momenta and higher projected axis ratios and concentrations than star-forming counterparts. Average sizes of simulated quiescent galaxies are relatively close to observed ones, and broadly consistent within the uncertainties. The average size ratio of quiescent and star-forming galaxies in the probed mass range is formally consistent with observations, although this result is partly affected by poor statistics.

(278)Mass determination of protoplanetary disks from dust evolution
• Riccardo Franceschi,
• Tilman Birnstiel,
• Thomas Henning,
• Paola Pinilla,
• Dmitry Semenov
• +1
Astronomy and Astrophysics, 657, p13 (01/2022) doi:10.1051/0004-6361/202141705
abstract + abstract -

Context. The mass of protoplanetary disks is arguably one of their most important quantities shaping their evolution toward planetary systems, but it remains a challenge to determine this quantity. Using the high spatial resolution now available on telescopes such as the Atacama Large Millimeter/submillimeter Array (ALMA), recent studies derived a relation between the disk surface density and the location of the "dust lines". This is a new concept in the field, linking the disk size at different continuum wavelengths with the radial distribution of grain populations of different sizes.
Aims: We aim to use a dust evolution model to test the dependence of the dust line location on disk gas mass. In particular, we are interested in the reliability of the method for disks showing radial substructures, as recent high-resolution observations revealed.
Methods: We performed dust evolution calculations, which included perturbations to the gas surface density with different amplitudes at different radii, to investigate their effect on the global drift timescale of dust grains. These models were then used to calibrate the relation between the dust grain drift timescale and the disk gas mass. We investigated under which condition the dust line location is a good mass estimator and tested how different stellar and disk properties (disk mass, stellar mass, disk age, and dust-to-gas ratio) affect the dust line properties. Finally, we show the applicability of this method to disks such as TW Hya and AS 209 that have been observed at high angular resolution with ALMA and show pronounced disk structures.
Results: Our models without pressure bumps confirm a strong dependence of the dust line location on the disk gas mass and its applicability as a reliable mass estimator. The other disk properties do not significantly affect the dust line location, except for the age of the system, which is the major source of uncertainty for this mass estimator. A population of synthetic disks was used to calibrate an analytic relation between the dust line location and the disk mass for smooth disks, finding that previous mass estimates based on dust lines overestimate disk masses by about one order of magnitude. Radial pressure bumps can alter the location of the dust line by up to ~10 au, while its location is mainly determined by the disk mass. Therefore, an accurate mass estimation requires a proper evaluation of the effect of bumps. However, when radial substructures act as traps for dust grains, the relation between the dust line location and disk mass becomes weaker, and other mass estimators need to be adopted.
Conclusions: Our models show that the determination of the dust line location is a promising approach to the mass estimate of protoplanetay disks, but the exact relation between the dust line location and disk mass depends on the structure of the particular disk. We calibrated the relation for disks without evidence of radial structures, while for more complex structures we ran a simple dust evolution model. However, this method fails when there is evidence of strong dust traps. It is possible to reveal when dust evolution is dominated by traps, providing the necessary information for when the method should be applied with caution.

(277)QCD static force in gradient flow
• Nora Brambilla,
• Hee Sok Chung,
• Antonio Vairo,
• Xiang-Peng Wang
Journal of High Energy Physics, 2022 (01/2022) doi:10.1007/JHEP01(2022)184
abstract + abstract -

We compute the QCD static force and potential using gradient flow at next-to-leading order in the strong coupling. The static force is the spatial derivative of the static potential: it encodes the QCD interaction at both short and long distances. While on the one side the static force has the advantage of being free of the O(ΛQCD) renormalon affecting the static potential when computed in perturbation theory, on the other side its direct lattice QCD computation suffers from poor convergence. The convergence can be improved by using gradient flow, where the gauge fields in the operator definition of a given quantity are replaced by flowed fields at flow time t, which effectively smear the gauge fields over a distance of order √{t }, while they reduce to the QCD fields in the limit t → 0. Based on our next-to-leading order calculation, we explore the properties of the static force for arbitrary values of t, as well as in the t → 0 limit, which may be useful for lattice QCD studies.

(276)Towards RNA life on Early Earth: From atmospheric HCN to biomolecule production in warm little ponds
• Ben K. D. Pearce,
• Karan Molaverdikhani,
• Ralph E. Pudritz,
• Thomas Henning,
• Kaitlin E. Cerrillo
arXiv e-prints (01/2022) e-Print:2201.00829
abstract + abstract -

The origin of life on Earth involves the early appearance of an information-containing molecule such as RNA. The basic building blocks of RNA could have been delivered by carbon-rich meteorites, or produced in situ by processes beginning with the synthesis of hydrogen cyanide (HCN) in the early Earth's atmosphere. Here, we construct a robust physical and non-equilibrium chemical model of the early Earth atmosphere. The atmosphere is supplied with hydrogen from impact degassing of meteorites, sourced with water evaporated from the oceans, carbon dioxide from volcanoes, and methane from undersea hydrothermal vents, and in which lightning and external UV-driven chemistry produce HCN. This allows us to calculate the rain-out of HCN into warm little ponds (WLPs). We then use a comprehensive sources and sinks numerical model to compute the resulting abundances of nucleobases, ribose, and nucleotide precursors such as 2-aminooxazole resulting from aqueous and UV-driven chemistry within them. We find that at 4.4 bya (billion years ago) the limits of adenine concentrations in ponds for habitable surfaces is 0.05$\mu$M in the absence of seepage. These concentrations can be maintained for over 100 Myr. Meteorite delivery of adenine to WLPs can provide boosts in concentration by 2-3 orders of magnitude, but these boosts deplete within months by UV photodissociation, seepage, and hydrolysis. The early evolution of the atmosphere is dominated by the decrease of hydrogen due to falling impact rates and atmospheric escape, and the rise of oxygenated species such as OH from H2O photolysis. Our work points to an early origin of RNA on Earth within ~200 Myr of the Moon-forming impact.

(275)Proca theory from the spinning worldline
• Matthias Carosi,
• Ivo Sachs
Journal of High Energy Physics, 2022 (01/2022) doi:10.1007/JHEP01(2022)135
abstract + abstract -

We obtain Proca field theory from the quantisation of the N = 2 supersymmetric worldline upon supplementing the graded BRST-algebra with an extra multiplet of oscillators. The linearised theory describes the BV-extended spectrum of Proca theory, together with a Stückelberg field. When coupling the theory to background fields we derive the Proca equations, arising as consistency conditions in the BRST procedure. We also explore non-abelian modifications, complexified vector fields as well as coupling to a dilaton field. We propose a cubic action on the space of BRST-operators which reproduces the known Proca action.

(274)Low-Energy Supernovae Severely Constrain Radiative Particle Decays
• Andrea Caputo,
• Hans-Thomas Janka,
• Georg Raffelt,
• Edoardo Vitagliano
arXiv e-prints (01/2022) e-Print:2201.09890
abstract + abstract -

The hot and dense core formed in the collapse of a massive star is a powerful source of hypothetical feebly-interacting particles such as sterile neutrinos, dark photons, axion-like particles (ALPs), and others. Radiative decays such as $a\to2\gamma$ deposit this energy in the surrounding material if the mean free path is less than the radius of the progenitor star. For the first time, we use a supernova (SN) population with particularly low explosion energies as the most sensitive calorimeters to constrain this possibility. These SNe are observationally identified as low-luminosity events with low ejecta velocities and low masses of ejected $^{56}$Ni. Their low energies limit the energy deposition from particle decays to less than about 0.1 B, where $1~{\rm B~(bethe)}=10^{51}~{\rm erg}$. For 1-500 MeV-mass ALPs, this generic argument excludes ALP-photon couplings $G_{a\gamma\gamma}$ in the $10^{-10}$-$10^{-8}~{\rm GeV}^{-1}$ range.

(273)Publishing statistical models: Getting the most out of particle physics experiments
• Kyle Cranmer,
• Sabine Kraml,
• Harrison Prosper,
• Philip Bechtle,
• Florian Bernlochner
• +28
• Itay M. Bloch,
• Enzo Canonero,
• Marcin Chrzaszcz,
• Andrea Coccaro,
• Jan Conrad,
• Glen Cowan,
• Matthew Feickert,
• Nahuel Ferreiro,
• Andrew Fowlie,
• Lukas A. Heinrich,
• Alexander Held,
• Thomas Kuhr,
• Anders Kvellestad,
• Maeve Madigan,
• Farvah Nazila Mahmoudi,
• Knut Dundas Morå,
• Mark S. Neubauer,
• Maurizio Pierini,
• Juan Rojo,
• Sezen Sekmen,
• Luca Silvestrini,
• Veronica Sanz,
• Giordon H. Stark,
• Riccardo Torre,
• Robert Thorne,
• Wolfgang Waltenberger,
• Nicholas Wardle,
• Jonas Wittbrodt
• (less)
SciPost Physics, 12 (01/2022) doi:10.21468/SciPostPhys.12.1.037
abstract + abstract -

The statistical models used to derive the results of experimental analyses are of incredible scientific value and are essential information for analysis preservation and reuse. In this paper, we make the scientific case for systematically publishing the full statistical models and discuss the technical developments that make this practical. By means of a variety of physics cases -- including parton distribution functions, Higgs boson measurements, effective field theory interpretations, direct searches for new physics, heavy flavor physics, direct dark matter detection, world averages, and beyond the Standard Model global fits -- we illustrate how detailed information on the statistical modelling can enhance the short- and long-term impact of experimental results.

(272)Production of Very Light Elements and Strontium in the Early Ejecta of Neutron Star Mergers
• Albino Perego,
• Diego Vescovi,
• Achille Fiore,
• Leonardo Chiesa,
• Christian Vogl
• +8
• Stefano Benetti,
• Sebastiano Bernuzzi,
• Marica Branchesi,
• Enrico Cappellaro,
• Sergio Cristallo,
• Andreas Flörs,
• Wolfgang E. Kerzendorf,
• David Radice
• (less)
The Astrophysical Journal, 925, p17 (01/2022) doi:10.3847/1538-4357/ac3751
abstract + abstract -

We study the production of very light elements (Z < 20) in the dynamical and spiral-wave wind ejecta of binary neutron star mergers by combining detailed nucleosynthesis calculations with the outcome of numerical relativity merger simulations. All our models are targeted to GW170817 and include neutrino radiation. We explore different finite-temperature, composition-dependent nuclear equations of state, and binary mass ratios, and find that hydrogen and helium are the most abundant light elements. For both elements, the decay of free neutrons is the driving nuclear reaction. In particular, ~0.5-2 × 10-6 M of hydrogen are produced in the fast expanding tail of the dynamical ejecta, while ~1.5-11 × 10-6 M of helium are synthesized in the bulk of the dynamical ejecta, usually in association with heavy r-process elements. By computing synthetic spectra, we find that the possibility of detecting hydrogen and helium features in kilonova spectra is very unlikely for fiducial masses and luminosities, even when including nonlocal thermodynamic equilibrium effects. The latter could be crucial to observe helium lines a few days after merger for faint kilonovae or for luminous kilonovae ejecting large masses of helium. Finally, we compute the amount of strontium synthesized in the dynamical and spiral-wave wind ejecta, and find that it is consistent with (or even larger than, in the case of a long-lived remnant) the one required to explain early spectral features in the kilonova of GW170817.

(271)Response approach to the integrated shear 3-point correlation function: the impact of baryonic effects on small scales
• Anik Halder,
• Alexandre Barreira
arXiv e-prints (01/2022) e-Print:2201.05607
abstract + abstract -

The integrated shear 3-point correlation function $\zeta_{\pm}$ is a higher-order statistic of the cosmic shear field that describes the modulation of the 2-point correlation function $\xi_{\pm}$ by long-wavelength features in the field. Here, we introduce a new theoretical model to calculate $\zeta_{\pm}$ 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 $\zeta_{\pm}$ is dominated by the nonlinear matter bispectrum in the squeezed limit, which can be evaluated accurately using the nonlinear 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 $\zeta_{\pm}$ measured in simulated cosmic shear maps. The impact of baryonic feedback enters effectively only through the corresponding impact on the nonlinear matter power spectrum, thereby permitting to account for these astrophysical effects on $\zeta_{\pm}$ similarly to how they are currently accounted for on $\xi_{\pm}$. Using a simple idealized Fisher matrix forecast for a DES-like survey we find that, compared to $\xi_{\pm}$, a combined $\xi_{\pm}\ \&\ \zeta_{\pm}$ analysis can lead to improvements of order $20-40\%$ on the constraints of cosmological parameters such as $\sigma_8$ or the dark energy equation of state parameter $w_0$. 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 are encouraging results that motivate future works on the integrated shear 3-point correlation function towards applications to real survey data.

(270)The velocity structure of the intracluster medium during a major merger: simulated microcalorimeter observations
• Veronica Biffi,
• John A. ZuHone,
• Tony Mroczkowski,
• Esra Bulbul,
• William Forman
arXiv e-prints (01/2022) e-Print:2201.12370
abstract + abstract -

Major mergers between galaxy clusters can produce large turbulent and bulk flow velocities in the intra-cluster medium and thus imprint diagnostic features in X-ray spectral emission lines from heavy ions. As demonstrated by Hitomi in observations of the Perseus cluster, measurements of gas velocities in clusters from high-resolution X-ray spectra will be achievable with upcoming X-ray calorimeters like those on board XRISM, Athena, or a Lynx like mission. We investigate this possibility for interesting locations across a major cluster merger from a hydrodynamical simulation, via X-ray synthetic spectra with a few eV energy resolution. We observe the system from directions perpendicular to the plane of the merger and along the merger axis. In these extreme geometrical configurations, we find clear non-Gaussian shapes of the iron He-like K_alpha line at 6.7keV. The velocity dispersion predicted from the simulations can be retrieved for the brightest 100ks pointings with XRISM Resolve, despite some discrepancy related to the complex non-Gaussian line shapes. Measurements in faint regions require however high S/N and the larger collecting area of the Athena X-IFU calorimeter is thus needed. With the latter, we also investigate the gas temperature and velocity gradient across the merger bow shock edge, from 20"-wide annuli extracted from a single 1Ms X-IFU pointing. We find best-fit temperature and velocity dispersion values that are consistent with predictions from the simulations within 1-sigma, but the uncertainties on the inferred velocity dispersion are too large to place any stringent constraints on the shallow gradient downstream of the shock. We also present simulated images of the thermal and kinetic Sunyaev-Zeldovich effects, using the above viewing configurations, and compare the results at angular resolutions appropriate for future observatories such as CMB-S4 and AtLAST.

(269)Variable structures in M87* from space, time and frequency resolved interferometry
• Philipp Arras,
• Philipp Frank,
• Philipp Haim,
• Jakob Knollmüller,
• Reimar Leike
• +2
• Martin Reinecke,
• Torsten Enßlin
• (less)
Nature Astronomy, 6, p11 (01/2022) doi:10.1038/s41550-021-01548-0
abstract + abstract -

The immediate vicinity of an active supermassive black hole—with its event horizon, photon ring, accretion disk and relativistic jets—is an appropriate place to study physics under extreme conditions, particularly general relativity and magnetohydrodynamics. Observing the dynamics of such compact astrophysical objects provides insights into their inner workings, and the recent observations of M87* by the Event Horizon Telescope1-6 using very-long-baseline interferometry techniques allows us to investigate the dynamical processes of M87* on timescales of days. Compared with most radio interferometers, very-long-baseline interferometry networks typically have fewer antennas and low signal-to-noise ratios. Furthermore, the source is variable, prohibiting integration over time to improve signal-to-noise ratio. Here, we present an imaging algorithm7,8 that copes with the data scarcity and temporal evolution, while providing an uncertainty quantification. Our algorithm views the imaging task as a Bayesian inference problem of a time-varying brightness, exploits the correlation structure in time and reconstructs (2 + 1 + 1)-dimensional time-variable and spectrally resolved images. We apply this method to the Event Horizon Telescope observations of M87*9 and validate our approach on synthetic data. The time- and frequency-resolved reconstruction of M87* confirms variable structures on the emission ring and indicates extended and time-variable emission structures outside the ring itself.

(268)Star formation near the Sun is driven by expansion of the Local Bubble
• Catherine Zucker,
• Alyssa A. Goodman,
• João Alves,
• Shmuel Bialy,
• Michael Foley
• +6
• Joshua S. Speagle,
• Josefa GroÎ²schedl,
• Douglas P. Finkbeiner,
• Andreas Burkert,
• Diana Khimey,
• Cameren Swiggum
• (less)
Nature, 601, p4 (01/2022) doi:10.1038/s41586-021-04286-5
abstract + abstract -

For decades we have known that the Sun lies within the Local Bubble, a cavity of low-density, high-temperature plasma surrounded by a shell of cold, neutral gas and dust1-3. However, the precise shape and extent of this shell4,5, the impetus and timescale for its formation6,7, and its relationship to nearby star formation8 have remained uncertain, largely due to low-resolution models of the local interstellar medium. Here we report an analysis of the three-dimensional positions, shapes and motions of dense gas and young stars within 200 pc of the Sun, using new spatial9-11 and dynamical constraints12. We find that nearly all of the star-forming complexes in the solar vicinity lie on the surface of the Local Bubble and that their young stars show outward expansion mainly perpendicular to the bubble's surface. Tracebacks of these young stars' motions support a picture in which the origin of the Local Bubble was a burst of stellar birth and then death (supernovae) taking place near the bubble's centre beginning approximately 14 Myr ago. The expansion of the Local Bubble created by the supernovae swept up the ambient interstellar medium into an extended shell that has now fragmented and collapsed into the most prominent nearby molecular clouds, in turn providing robust observational support for the theory of supernova-driven star formation.

(267)Unveiling the Universe with Emerging Cosmological Probes
• Michele Moresco,
• Lorenzo Amati,
• Luca Amendola,
• Simon Birrer,
• John P. Blakeslee
• +20
• Michele Cantiello,
• Andrea Cimatti,
• Jeremy Darling,
• Massimo Della Valle,
• Maya Fishbach,
• Claudio Grillo,
• Nico Hamaus,
• Daniel Holz,
• Luca Izzo,
• Raul Jimenez,
• Elisabeta Lusso,
• Massimo Meneghetti,
• Ester Piedipalumbo,
• Alice Pisani,
• Alkistis Pourtsidou,
• Lucia Pozzetti,
• Miguel Quartin,
• Guido Risaliti,
• Piero Rosati,
• Licia Verde
• (less)
arXiv e-prints (01/2022) e-Print:2201.07241
abstract + abstract -

The detection of the accelerated expansion of the Universe has been one of the major breakthroughs in modern cosmology. Several cosmological probes (CMB, SNe Ia, BAO) have been studied in depth to better understand the nature of the mechanism driving this acceleration, and they are being currently pushed to their limits, obtaining remarkable constraints that allowed us to shape the standard cosmological model. In parallel to that, however, the percent precision achieved has recently revealed apparent tensions between measurements obtained from different methods. These are either indicating some unaccounted systematic effects, or are pointing toward new physics. Following the development of CMB, SNe, and BAO cosmology, it is critical to extend our selection of cosmological probes. Novel probes can be exploited to validate results, control or mitigate systematic effects, and, most importantly, to increase the accuracy and robustness of our results. This review is meant to provide a state-of-art benchmark of the latest advances in emerging beyond-standard cosmological probes. We present how several different methods can become a key resource for observational cosmology. In particular, we review cosmic chronometers, quasars, gamma-ray bursts, standard sirens, lensing time-delay with galaxies and clusters, cosmic voids, neutral hydrogen intensity mapping, surface brightness fluctuations, secular redshift drift, and clustering of standard candles. The review describes the method, systematics, and results of each probe in a homogeneous way, giving the reader a clear picture of the available innovative methods that have been introduced in recent years and how to apply them. The review also discusses the potential synergies and complementarities between the various probes, exploring how they will contribute to the future of modern cosmology.

(266)Intrinsic alignments of galaxies around cosmic voids
• William d'Assignies D.,
• Nora Elisa Chisari,
• Nico Hamaus,
• Sukhdeep Singh
Monthly Notices of the Royal Astronomical Society, 509, p10 (01/2022) doi:10.1093/mnras/stab2986
abstract + abstract -

The intrinsic alignments of galaxies, i.e. the correlation between galaxy shapes and their environment, are a major source of contamination for weak gravitational lensing surveys. Most studies of intrinsic alignments have so far focused on measuring and modelling the correlations of luminous red galaxies with galaxy positions or the filaments of the cosmic web. In this work, we investigate alignments around cosmic voids. We measure the intrinsic alignments of luminous red galaxies detected by the Sloan Digital Sky Survey around a sample of voids constructed from those same tracers and with radii in the ranges: [20-30; 30-40; 40-50] h-1 Mpc and in the redshift range z = 0.4-0.8. We present fits to the measurements based on a linear model at large scales, and on a new model based on the void density profile inside the void and in its neighbourhood. We constrain the free scaling amplitude of our model at small scales, finding no significant alignment at 1σ for either sample. We observe a deviation from the null hypothesis, at large scales, of 2σ for voids with radii between 20 and 30 h-1 Mpc, and 1.5σ for voids with radii between 30 and 40 h-1 Mpc and constrain the amplitude of the model on these scales. We find no significant deviation at 1σ for larger voids. Our work is a first attempt at detecting intrinsic alignments of galaxy shapes around voids and provides a useful framework for their mitigation in future void lensing studies.

(265)Inclusive Hadroproduction of P-wave Heavy Quarkonia in pNRQCD
• Hee Sok Chung
EPJ Web Conf., 258 (2022) doi:10.1051/epjconf/202225804005
abstract + abstract -

We compute NRQCD long-distance matrix elements that appear in the inclusive production cross sections of P-wave heavy quarkonia in the framework of potential NRQCD. The formalism developed in this work applies to strongly coupled charmonia and bottomonia. This makes possible the determination of color-octet NRQCD long-distance matrix elements without relying on measured cross section data, which has not been possible so far. We obtain results for inclusive production cross sections of χcJ and χbJ at the LHC, which are in good agreement with measurements.

(264)Gamma-ray observations of cosmic nuclei
• Roland Diehl
EPJ Web Conf., 260 (2022) doi:10.1051/epjconf/202226010001
abstract + abstract -

Gamma rays from nuclear processes such as radioactive decay and de-excitations are among the most-direct tools to witness the production and existence of speciﬁc nuclei and isotopes in and near cosmic nucleosynthesis sites. With space-borne instrumentation such as NuSTAR and SPI/INTEGRAL, and experimental techniques to handle a substantial instrumental background from cosmic-ray activations of the spacecraft and instrument, unique results have been obtained, from diffuse emissions of nuclei and positrons in interstellar surroundings of sources, as well as from observations of cosmic explosions and their radioactive afterglows. These witness non-sphericity in supernova explosions and a ﬂow of nucleosynthesis ejecta through superbubbles as common source environments. Next-generation experiments that are awaiting space missions promise a next level of observational nuclear astrophysics.

(263)Symplectic quantization of multi-field Generalized Proca electrodynamics
• Verónica Errasti Díez,
• Marina Krstic Marinkovic
(12/2021) e-Print:2112.11477
abstract + abstract -

We explicitly carry out the symplectic quantization of a family of multi-field Generalized Proca (GP) electrodynamics theories. In the process, we provide an independent derivation of the so-called secondary constraint enforcing relations -- consistency conditions that significantly restrict the allowed interactions in multi-field settings already at the classical level. Additionally, we unveil the existence of quantum consistency conditions, which apply in both single- and multi-field GP scenarios. Our newly found conditions imply that not all classically well-defined (multi-)GP theories are amenable to quantization. The extension of our results to the most general multi-GP class is conceptually straightforward, albeit algebraically cumbersome.

(262)Combining Planck and SPT cluster catalogs: cosmological analysis and impact on Planck scaling relation calibration
• L. Salvati,
• A. Saro,
• S. Bocquet,
• M. Costanzi,
• B. Ansarinejad
• +39
• B.A. Benson,
• L.E. Bleem,
• M.S. Calzadilla,
• J.E. Carlstrom,
• C.L. Chang,
• R. Chown,
• A.T. Crites,
• T. de Haan,
• M.A. Dobbs,
• W.B. Everett,
• B. Floyd,
• S. Grandis,
• E.M. George,
• N.W. Halverson,
• G.P. Holder,
• W.L. Holzapfel,
• J.D. Hrubes,
• A.T. Lee,
• D. Luong-Van,
• M. McDonald,
• J.J. McMahon,
• S.S. Meyer,
• M. Millea,
• L.M. Mocanu,
• J.J. Mohr,
• T. Natoli,
• Y. Omori,
• S. Padin,
• C. Pryke,
• C.L. Reichardt,
• J.E. Ruhl,
• F. Ruppin,
• K.K. Schaffer,
• T. Schrabback,
• E. Shirokoff,
• Z. Staniszewski,
• A.A. Stark,
• J.D. Vieira,
• R. Williamson
• (less)
(12/2021) e-Print:2112.03606
abstract + abstract -

We provide the first combined cosmological analysis of South Pole Telescope (SPT) and Planck cluster catalogs. The aim is to provide an independent calibration for Planck scaling relations, exploiting the cosmological constraining power of the SPT-SZ cluster catalog and its dedicated weak lensing (WL) and X-ray follow-up observations. We build a new version of the Planck cluster likelihood. In the $\nu \Lambda$CDM scenario, focusing on the mass slope and mass bias of Planck scaling relations, we find $\alpha_{\text{SZ}} = 1.49 _{-0.10}^{+0.07}$ and $(1-b)_{\text{SZ}} = 0.69 _{-0.14}^{+0.07}$ respectively. The results for the mass slope show a $\sim 4 \, \sigma$ departure from the self-similar evolution, $\alpha_{\text{SZ}} \sim 1.8$. This shift is mainly driven by the matter density value preferred by SPT data, $\Omega_m = 0.30 \pm 0.03$, lower than the one obtained by Planck data alone, $\Omega_m = 0.37 _{-0.06}^{+0.02}$. The mass bias constraints are consistent both with outcomes of hydrodynamical simulations and external WL calibrations, $(1-b) \sim 0.8$, and with results required by the Planck cosmic microwave background cosmology, $(1-b) \sim 0.6$. From this analysis, we obtain a new catalog of Planck cluster masses $M_{500}$. We estimate the relation between the published Planck derived $M_{\text{SZ}}$ masses and our derived masses, as a measured mass bias. We analyse the mass, redshift and detection noise dependence of this quantity, finding an increasing trend towards high redshift and low mass. These results mimic the effect of departure from self-similarity in cluster evolution, showing different dependencies for the low-mass high-mass, low-z high-z regimes.

(261)Observation of $\Lambda_b^0\rightarrow D^+ p \pi^-\pi^-$ and $\Lambda_b^0\rightarrow D^{*+} p \pi^-\pi^-$ decays
• Roel Aaij,
• Ahmed Sameh Wagih Abdelmotteleb,
• Carlos Abellán Beteta,
• Fernando Jesus Abudinén,
• Thomas Ackernley
• +1008
• Bernardo Adeva,
• Marco Adinolfi,
• Hossein Afsharnia,
• Christina Agapopoulou,
• Christine Angela Aidala,
• Salvatore Aiola,
• Ziad Ajaltouni,
• Simon Akar,
• Johannes Albrecht,
• Federico Alessio,
• Michael Alexander,
• Alejandro Alfonso Albero,
• Zakariya Aliouche,
• Georgy Alkhazov,
• Paula Alvarez Cartelle,
• Sandra Amato,
• Jake Lewis Amey,
• Yasmine Amhis,
• Liupan An,
• Lucio Anderlini,
• Martin Andersson,
• Aleksei Andreianov,
• Mirco Andreotti,
• Flavio Archilli,
• Alexander Artamonov,
• Marina Artuso,
• Kenenbek Arzymatov,
• Elie Aslanides,
• Michele Atzeni,
• Benjamin Audurier,
• Sebastian Bachmann,
• Marie Bachmayer,
• John Back,
• Pablo Baladron Rodriguez,
• Vladislav Balagura,
• Wander Baldini,
• Juan Baptista de Souza Leite,
• Matteo Barbetti,
• Roger Barlow,
• Sergey Barsuk,
• William Barter,
• Matteo Bartolini,
• Fedor Baryshnikov,
• Jan-Marc Basels,
• Saliha Bashir,
• Giovanni Bassi,
• Baasansuren Batsukh,
• Alexander Battig,
• Aurelio Bay,
• Anja Beck,
• Maik Becker,
• Franco Bedeschi,
• Ignacio Bediaga,
• Andrew Beiter,
• Vladislav Belavin,
• Samuel Belin,
• Violaine Bellee,
• Konstantin Belous,
• Ilia Belov,
• Ivan Belyaev,
• Giovanni Bencivenni,
• Eli Ben-Haim,
• Alexander Berezhnoy,
• Roland Bernet,
• Daniel Berninghoff,
• Harris Conan Bernstein,
• Claudia Bertella,
• Alessandro Bertolin,
• Christopher Betancourt,
• Federico Betti,
• Ia. Bezshyiko,
• Iaroslava Bezshyiko,
• Srishti Bhasin,
• Jihyun Bhom,
• Lingzhu Bian,
• Martin Stefan Bieker,
• Nicolo Vladi Biesuz,
• Simone Bifani,
• Pierre Billoir,
• Alice Biolchini,
• Matthew Birch,
• Fionn Caitlin Ros Bishop,
• Alexander Bitadze,
• Andrea Bizzeti,
• Mikkel Bjørn,
• Michele Piero Blago,
• Thomas Blake,
• Frederic Blanc,
• Steven Blusk,
• Dana Bobulska,
• Julian Alexander Boelhauve,
• Oscar Boente Garcia,
• Thomas Boettcher,
• Alexey Boldyrev,
• Alexander Bondar,
• Nikolay Bondar,
• Silvia Borghi,
• Maxim Borisyak,
• Martino Borsato,
• Jozef Tomasz Borsuk,
• Sonia Amina Bouchiba,
• Themistocles Bowcock,
• Alexandre Boyer,
• Concezio Bozzi,
• Matthew John Bradley,
• Svende Braun,
• Alexandre Brea Rodriguez,
• Jolanta Brodzicka,
• Arnau Brossa Gonzalo,
• Davide Brundu,
• Annarita Buonaura,
• Laura Buonincontri,
• Aodhan Tomas Burke,
• Christopher Burr,
• Albert Bursche,
• Anatoly Butkevich,
• Jordy Sebastiaan Butter,
• Jan Buytaert,
• Wiktor Byczynski,
• Sandro Cadeddu,
• Hao Cai,
• Roberto Calabrese,
• Lukas Calefice,
• Stefano Cali,
• Ryan Calladine,
• Marta Calvi,
• Miriam Calvo Gomez,
• Patricia Camargo Magalhaes,
• Pierluigi Campana,
• Angel Fernando Campoverde Quezada,
• Simone Capelli,
• Lorenzo Capriotti,
• Angelo Carbone,
• Giovanni Carboni,
• Roberta Cardinale,
• Alessandro Cardini,
• Ina Carli,
• Paolo Carniti,
• Leon David Carus,
• Kazuyoshi Carvalho Akiba,
• Adrian Casais Vidal,
• Rowina Caspary,
• Gianluigi Casse,
• Marco Cattaneo,
• Giovanni Cavallero,
• Sara Celani,
• Jacopo Cerasoli,
• Daniel Cervenkov,
• Abbie Jane Chadwick,
• Matthew George Chapman,
• Matthew Charles,
• Philippe Charpentier,
• Ph. Charpentier,
• Carlos Alberto Chavez Barajas,
• Maximilien Chefdeville,
• Chen Chen,
• Shanzhen Chen,
• Aleksei Chernov,
• Veronika Chobanova,
• Serhii Cholak,
• Marcin Chrzaszcz,
• Alexsei Chubykin,
• Vladimir Chulikov,
• Paolo Ciambrone,
• Maria Flavia Cicala,
• Xabier Cid Vidal,
• Gregory Ciezarek,
• P.E. L. Clarke,
• Marco Clemencic,
• Harry Cliff,
• Joel Closier,
• John Leslie Cobbledick,
• Victor Coco,
• Joao A B Coelho,
• Julien Cogan,
• Eric Cogneras,
• Lucian Cojocariu,
• Paula Collins,
• Tommaso Colombo,
• Liliana Congedo,
• Andrea Contu,
• Naomi Cooke,
• George Coombs,
• Imanol Corredoira,
• Gloria Corti,
• Cayo Mar Costa Sobral,
• Benjamin Couturier,
• Daniel Charles Craik,
• Jana Crkovská,
• Melissa Maria Cruz Torres,
• Robert Currie,
• Cesar Luiz Da Silva,
• Shakhzod Dadabaev,
• Lingyun Dai,
• Elena Dall'Occo,
• Jeremy Dalseno,
• Carmelo D'Ambrosio,
• Anna Danilina,
• Philippe d'Argent,
• Aigerim Dashkina,
• Jonathan Edward Davies,
• Adam Davis,
• Oscar De Aguiar Francisco,
• Kristof De Bruyn,
• Stefano De Capua,
• Michel De Cian,
• Erika De Lucia,
• Jussara De Miranda,
• Leandro De Paula,
• Marilisa De Serio,
• Dario De Simone,
• Patrizia De Simone,
• Fabio De Vellis,
• Jacco de Vries,
• Cameron Thomas Dean,
• Francesco Debernardis,
• Daniel Decamp,
• Vlad-George Dedu,
• Luigi Del Buono,
• Blaise Delaney,
• Hans Peter Dembinski,
• Adam Dendek,
• Vadym Denysenko,
• Denis Derkach,
• Olivier Deschamps,
• Fabrice Desse,
• Francesco Dettori,
• Biplab Dey,
• Alessandro Di Cicco,
• Pasquale Di Nezza,
• Sergey Didenko,
• Lorena Dieste Maronas,
• Hans Dijkstra,
• Vasyl Dobishuk,
• Chenzhi Dong,
• Amanda May Donohoe,
• Francesca Dordei,
• Alberto dos Reis,
• Lauren Douglas,
• Anatoliy Dovbnya,
• Anthony Gavin Downes,
• Maciej Wojciech Dudek,
• Laurent Dufour,
• Viacheslav Duk,
• Paolo Durante,
• John Matthew Durham,
• Deepanwita Dutta,
• Agnieszka Dziurda,
• Alexey Dzyuba,
• Sajan Easo,
• Ulrik Egede,
• Victor Egorychev,
• Semen Eidelman,
• Stephan Eisenhardt,
• Surapat Ek-In,
• Lars Eklund,
• Scott Ely,
• Alexandru Ene,
• Eliane Epple,
• Stephan Escher,
• Jonas Nathanael Eschle,
• Sevda Esen,
• Timothy Evans,
• Lucas Falcao,
• Yanting Fan,
• Bo Fang,
• Stephen Farry,
• Davide Fazzini,
• Mauricio Féo,
• Antonio Fernandez Prieto,
• Alex Daniel Fernez,
• Fabio Ferrari,
• Lino Ferreira Lopes,
• Fernando Ferreira Rodrigues,
• Silvia Ferreres Sole,
• Martina Ferrillo,
• Massimiliano Ferro-Luzzi,
• Sergey Filippov,
• Rosa Anna Fini,
• Massimiliano Fiorini,
• Miroslaw Firlej,
• Kamil Leszek Fischer,
• K.M. Fischer,
• Dillon Scott Fitzgerald,
• Conor Fitzpatrick,
• Tomasz Fiutowski,
• Aristeidis Fkiaras,
• Frederic Fleuret,
• Marianna Fontana,
• Flavio Fontanelli,
• Roger Forty,
• Daniel Foulds-Holt,
• Vinicius Franco Lima,
• Manuel Franco Sevilla,
• Markus Frank,
• Edoardo Franzoso,
• Giulia Frau,
• Christoph Frei,
• David Anthony Friday,
• Jinlin Fu,
• Quentin Fuehring,
• Emmy Gabriel,
• Giuliana Galati,
• Abraham Gallas Torreira,
• Domenico Galli,
• Silvia Gambetta,
• Yuyue Gan,
• Miriam Gandelman,
• Paolo Gandini,
• Yuanning Gao,
• Michela Garau,
• Luis Miguel Garcia Martin,
• Paula Garcia Moreno,
• Julián García Pardiñas,
• Beatriz Garcia Plana,
• Felipe Andres Garcia Rosales,
• Lluis Garrido,
• Clara Gaspar,
• Robbert Erik Geertsema,
• David Gerick,
• Louis Lenard Gerken,
• Evelina Gersabeck,
• Marco Gersabeck,
• Timothy Gershon,
• Dawid Gerstel,
• Luca Giambastiani,
• Valerie Gibson,
• Henryk Karol Giemza,
• Alexander Leon Gilman,
• Matteo Giovannetti,
• Alessandra Gioventù,
• Pere Gironella Gironell,
• Carmen Giugliano,
• Konstantin Gizdov,
• Evangelos Leonidas Gkougkousis,
• Vladimir Gligorov,
• Carla Göbel,
• Elisabet Golobardes,
• Dmitry Golubkov,
• Andrey Golutvin,
• Alvaro Gomes,
• Sergio Gomez Fernandez,
• Fernanda Goncalves Abrantes,
• Mateusz Goncerz,
• Guanghua Gong,
• Petr Gorbounov,
• Igor Vladimirovich Gorelov,
• Claudio Gotti,
• Jascha Peter Grabowski,
• Thomas Grammatico,
• Luis Alberto Granado Cardoso,
• Eugeni Graugés,
• Elena Graverini,
• Giacomo Graziani,
• Alexandru Grecu,
• Lex Marinus Greeven,
• Nathan Allen Grieser,
• Lucia Grillo,
• Sergey Gromov,
• Barak Raimond Gruberg Cazon,
• Chenxi Gu,
• Marco Guarise,
• Manuel Guittiere,
• Paul Andre Günther,
• Abdul-Kerim Guseinov,
• Evgeny Gushchin,
• Andreas Guth,
• Yury Guz,
• Thierry Gys,
• Thomas Hadavizadeh,
• Guido Haefeli,
• Christophe Haen,
• Jakob Haimberger,
• Tabitha Halewood-leagas,
• Phoebe Meredith Hamilton,
• Jan Patrick Hammerich,
• Qundong Han,
• Xiaoxue Han,
• Thomas Henry Hancock,
• Eva Brottmann Hansen,
• Stephanie Hansmann-Menzemer,
• Neville Harnew,
• Thomas Harrison,
• Christoph Hasse,
• Mark Hatch,
• Jibo He,
• Malte Hecker,
• Kevin Heijhoff,
• Kevin Heinicke,
• Riley Dylan Leslie Henderson,
• Arthur Marius Hennequin,
• Karol Hennessy,
• Louis Henry,
• Johannes Heuel,
• Adlène Hicheur,
• Donal Hill,
• Martha Hilton,
• Sophie Elizabeth Hollitt,
• Ruiwe Hou,
• Yingrui Hou,
• Jiangqiao Hu,
• Jifeng Hu,
• Wenhua Hu,
• Xiaofan Hu,
• Wenqian Huang,
• Xiaotao Huang,
• Wouter Hulsbergen,
• Ross John Hunter,
• Mikhail Hushchyn,
• David Hutchcroft,
• Daniel Hynds,
• Philipp Ibis,
• Marek Idzik,
• Dmitrii Ilin,
• Philip Ilten,
• Alexander Inglessi,
• Artur Ishteev,
• Kuzma Ivshin,
• Richard Jacobsson,
• Hendrik Jage,
• Sune Jakobsen,
• Eddy Jans,
• Brij Kishor Jashal,
• Abolhassan Jawahery,
• Vukan Jevtic,
• Xiaojie Jiang,
• Malcolm John,
• Daniel Johnson,
• Christopher Jones,
• Thomas Peter Jones,
• Beat Jost,
• Nathan Jurik,
• Sabin Hashmi Kalavan Kadavath,
• Sergii Kandybei,
• Youen Kang,
• Matthias Karacson,
• Maksim Karpov,
• Jacob William Kautz,
• Floris Keizer,
• Dustin Michael Keller,
• Matthew Kenzie,
• Tjeerd Ketel,
• Basem Khanji,
• Anastasiia Kharisova,
• Sergei Kholodenko,
• Thomas Kirn,
• Veronica Soelund Kirsebom,
• Ouail Kitouni,
• Suzanne Klaver,
• Nico Kleijne,
• Konrad Klimaszewski,
• Mateusz Rafal Kmiec,
• Serhii Koliiev,
• Almagul Kondybayeva,
• Anatoly Konoplyannikov,
• Pawel Kopciewicz,
• Renata Kopecna,
• Patrick Koppenburg,
• Mikhail Korolev,
• Igor Kostiuk,
• Oleksander Kot,
• Sofia Kotriakhova,
• Polina Kravchenko,
• Leonid Kravchuk,
• Rafal Dominik Krawczyk,
• Michal Kreps,
• Felix Johannes Kress,
• Sophie Katharina Kretzschmar,
• Pavel Krokovny,
• Wojciech Krupa,
• Wojciech Krzemien,
• Jakub Kubat,
• Marcin Kucharczyk,
• Vasily Kudryavtsev,
• Hilbrand Steffen Kuindersma,
• Gerd Joachim Kunde,
• Tengiz Kvaratskheliya,
• Daniel Lacarrere,
• George Lafferty,
• Adriano Lai,
• Andrea Lampis,
• Davide Lancierini,
• John Jake Lane,
• Richard Lane,
• Gaia Lanfranchi,
• Christoph Langenbruch,
• Jan Langer,
• Oliver Lantwin,
• Thomas Latham,
• Federico Lazzari,
• Renaud Le Gac,
• Sook Hyun Lee,
• Regis Lefèvre,
• Alexander Leflat,
• Sergey Legotin,
• Olivier Leroy,
• Tadeusz Lesiak,
• Blake Leverington,
• Hengne Li,
• Peilian Li,
• Shiyang Li,
• Yiming Li,
• Yutong Li,
• Zhuoming Li,
• Xixin Liang,
• Tai-hua Lin,
• Rolf Lindner,
• Vitalii Lisovskyi,
• Roman Litvinov,
• Guoming Liu,
• Huanhuan Liu,
• Qian Liu,
• Shuaiyi Liu,
• Aniol Lobo Salvia,
• Angelo Loi,
• Julian Lomba Castro,
• Iain Longstaff,
• Jose Lopes,
• Saúl López Soliño,
• George Holger Lovell,
• Yu Lu,
• Chiara Lucarelli,
• Donatella Lucchesi,
• Stanislav Luchuk,
• Miriam Lucio Martinez,
• Valeriia Lukashenko,
• Yiheng Luo,
• Anna Lupato,
• Eleonora Luppi,
• Oliver Lupton,
• Alberto Lusiani,
• Xiao-Rui Lyu,
• Lishuang Ma,
• Ruiting Ma,
• Serena Maccolini,
• Frederic Machefert,
• Florin Maciuc,
• Vladimir Macko,
• Patrick Mackowiak,
• Samuel Maddrell-Mander,
• Olga Madejczyk,
• Lakshan Ram Madhan Mohan,
• Oleg Maev,
• Artem Maevskiy,
• Maciej Witold Majewski,
• Jakub Jacek Malczewski,
• Sneha Malde,
• Bartosz Malecki,
• Alexander Malinin,
• Timofei Maltsev,
• Hanna Malygina,
• Giulia Manca,
• Giampiero Mancinelli,
• Daniele Manuzzi,
• Daniele Marangotto,
• Jan Maratas,
• Jean François Marchand,
• Umberto Marconi,
• Saverio Mariani,
• Carla Marin Benito,
• Matthieu Marinangeli,
• Jörg Marks,
• Alexander Mclean Marshall,
• Phillip John Marshall,
• Gabriele Martelli,
• Giuseppe Martellotti,
• Loris Martinazzoli,
• Maurizio Martinelli,
• Diego Martinez Santos,
• Fernando Martinez Vidal,
• André Massafferri,
• Marcel Materok,
• Rosen Matev,
• Abhijit Mathad,
• Viacheslav Matiunin,
• Clara Matteuzzi,
• Kara Renee Mattioli,
• Andrea Mauri,
• Emilie Maurice,
• Juan Mauricio,
• Michal Kazimierz Mazurek,
• Michael McCann,
• Lucas Mcconnell,
• Tamaki Holly Mcgrath,
• Niall Thomas Mchugh,
• Andrew McNab,
• Ronan McNulty,
• James Vincent Mead,
• Brian Meadows,
• Gerwin Meier,
• Dmytro Melnychuk,
• Simone Meloni,
• Marcel Merk,
• Andrea Merli,
• Lucas Meyer Garcia,
• Mikhail Mikhasenko,
• Diego Alejandro Milanes,
• Edward James Millard,
• Marko Milovanovic,
• Marie-Noelle Minard,
• Alessandro Minotti,
• Luca Minzoni,
• Sara Elizabeth Mitchell,
• Biljana Mitreska,
• Dominik Stefan Mitzel,
• Antje Mödden,
• Rizwaan Adeeb Mohammed,
• Razvan Daniel Moise,
• Sergei Mokhnenko,
• Titus Mombächer,
• Igancio Alberto Monroy,
• Stephane Monteil,
• Mauro Morandin,
• Gianfranco Morello,
• Michael Joseph Morello,
• Jakub Moron,
• Adam Benjamin Morris,
• Andrew George Morris,
• Raymond Mountain,
• Hongjie Mu,
• Franz Muheim,
• Mick Mulder,
• Dominik Müller,
• Katharina Müller,
• Colm Harold Murphy,
• Donal Murray,
• Rebecca Murta,
• Piera Muzzetto,
• Paras Naik,
• Tatsuya Nakada,
• Raja Nandakumar,
• Tara Nanut,
• Irina Nasteva,
• Matthew Needham,
• Nicola Neri,
• Sebastian Neubert,
• Niko Neufeld,
• Ryan Newcombe,
• Elisabeth Maria Niel,
• Simon Nieswand,
• Nikolay Nikitin,
• Niklas Stefan Nolte,
• Camille Normand,
• Cynthia Nunez,
• Agnieszka Oblakowska-Mucha,
• Vladimir Obraztsov,
• Thomas Oeser,
• Daniel Patrick O'Hanlon,
• Shinichi Okamura,
• Rudolf Oldeman,
• Federica Oliva,
• Mario Edgardo Olivares,
• C.J. G. Onderwater,
• Ryunosuke Hugo O'Neil,
• Juan Martin Otalora Goicochea,
• Tatiana Ovsiannikova,
• Patrick Owen,
• Maria Aranzazu Oyanguren,
• Klaas Ole Padeken,
• Bhagyashree Pagare,
• Preema Rennee Pais,
• Tommaso Pajero,
• Antimo Palano,
• Matteo Palutan,
• Yue Pan,
• Gennady Panshin,
• Antonios Papanestis,
• Marco Pappagallo,
• Luciano Pappalardo,
• Cheryl Pappenheimer,
• William Parker,
• Christopher Parkes,
• Barbara Passalacqua,
• Giovanni Passaleva,
• Alessandra Pastore,
• Mitesh Patel,
• Claudia Patrignani,
• Christopher James Pawley,
• Alex Pearce,
• Antonio Pellegrino,
• Monica Pepe Altarelli,
• Stefano Perazzini,
• Dmitrii Pereima,
• Asier Pereiro Castro,
• Pascal Perret,
• Marko Petric,
• Konstantinos Petridis,
• Alessandro Petrolini,
• Aleksandr Petrov,
• Stefano Petrucci,
• Marco Petruzzo,
• Thi Thuy Hang Pham,
• Anton Philippov,
• Roberto Piandani,
• Lorenzo Pica,
• Mauro Piccini,
• Boleslaw Pietrzyk,
• Guillaume Pietrzyk,
• Martina Pili,
• Davide Pinci,
• Flavio Pisani,
• Marco Pizzichemi,
• P.K. Resmi,
• Vlad-Mihai Placinta,
• Jonathan Plews,
• Maximo Plo Casasus,
• Francesco Polci,
• Marco Poli Lener,
• Mariia Poliakova,
• Anton Poluektov,
• Natalia Polukhina,
• Ivan Polyakov,
• Erica Polycarpo,
• Sebastien Ponce,
• Dmitry Popov,
• Sergei Popov,
• Stanislav Poslavskii,
• Kodassery Prasanth,
• Laura Promberger,
• Claire Prouve,
• Valery Pugatch,
• Veronique Puill,
• Giovanni Punzi,
• Hongrong Qi,
• Wenbin Qian,
• Ning Qin,
• Renato Quagliani,
• Naomi Veronika Raab,
• Raul Iraq Rabadan Trejo,
• Bartlomiej Rachwal,
• Jonas Rademacker,
• Matteo Rama,
• Miguel Ramos Pernas,
• Murilo Rangel,
• Fedor Ratnikov,
• Gerhard Raven,
• Meril Reboud,
• Federico Redi,
• Florian Reiss,
• Clara Remon Alepuz,
• Zan Ren,
• Victor Renaudin,
• Roberto Ribatti,
• Alessandro Maria Ricci,
• Stefania Ricciardi,
• Kurt Rinnert,
• Patrick Robbe,
• Gary Robertson,
• Ana Barbara Rodrigues,
• Eduardo Rodrigues,
• Jairo Alexis Rodriguez Lopez,
• E.R. R. Rodriguez Rodriguez,
• Alexandra Paige Rollings,
• Philipp Roloff,
• Vladimir Romanovskiy,
• Marcos Romero Lamas,
• Antonio Romero Vidal,
• Jordan Daniel Roth,
• Marcello Rotondo,
• Matthew Scott Rudolph,
• Thomas Ruf,
• Ramon Angel Ruiz Fernandez,
• Joan Ruiz Vidal,
• Artem Ryzhikov,
• Jakub Ryzka,
• Juan Jose Saborido Silva,
• Naylya Sagidova,
• Niladribihari Sahoo,
• Biagio Saitta,
• Matteo Salomoni,
• Cristina Sanchez Gras,
• Roberta Santacesaria,
• Cibran Santamarina Rios,
• Marco Santimaria,
• Emanuele Santovetti,
• Danila Saranin,
• Gediminas Sarpis,
• Minaugas Sarpis,
• Alessio Sarti,
• Celestina Satriano,
• Alessia Satta,
• Miroslav Saur,
• Darya Savrina,
• Halime Sazak,
• Luke George Scantlebury Smead,
• Alessandro Scarabotto,
• Stefan Schael,
• Sigrid Scherl,
• Manuel Schiller,
• Heinrich Schindler,
• Michael Schmelling,
• Burkhard Schmidt,
• Sebastian Schmitt,
• Olivier Schneider,
• Andreas Schopper,
• Maxime Schubiger,
• Sebastian Schulte,
• Marie Helene Schune,
• Rainer Schwemmer,
• Barbara Sciascia,
• Sara Sellam,
• Alexander Semennikov,
• Mara Senghi Soares,
• Antonino Sergi,
• Nicola Serra,
• Lorenzo Sestini,
• Alex Seuthe,
• Yiduo Shang,
• Desmond Mzamo Shangase,
• Mikhail Shapkin,
• Ivan Shchemerov,
• Lesya Shchutska,
• Tara Shears,
• Lev Shekhtman,
• Zhihong Shen,
• Shuqi Sheng,
• Vladimir Shevchenko,
• Edward Brendan Shields,
• Yuya Shimizu,
• Evgenii Shmanin,
• Joseph David Shupperd,
• Benedetto Gianluca Siddi,
• Rafael Silva Coutinho,
• Gabriele Simi,
• Saverio Simone,
• Nicola Skidmore,
• Tomasz Skwarnicki,
• Mark Slater,
• Igor Slazyk,
• Jennifer Clare Smallwood,
• John Gordon Smeaton,
• Anastasia Smetkina,
• Eluned Smith,
• Mark Smith,
• Aleksandra Snoch,
• Lais Soares Lavra,
• Michael Sokoloff,
• F.J. P. Soler,
• Aleksandr Solovev,
• Ivan Solovyev,
• Felipe Luan Souza De Almeida,
• Bruno Souza De Paula,
• Bernhard Spaan,
• Elisabetta Spadaro Norella,
• Patrick Spradlin,
• Federico Stagni,
• Marian Stahl,
• Sascha Stahl,
• Seophine Stanislaus,
• Olaf Steinkamp,
• Oleg Stenyakin,
• Holger Stevens,
• Sheldon Stone,
• Daria Strekalina,
• Fidan Suljik,
• Jiayin Sun,
• Liang Sun,
• Yipeng Sun,
• Peter Svihra,
• Paul Nathaniel Swallow,
• Krzysztof Swientek,
• Adam Szabelski,
• Tomasz Szumlak,
• Maciej Pawel Szymanski,
• Shantam Taneja,
• Alastair Roger Tanner,
• Martin Duy Tat,
• Aleksandr Terentev,
• Frederic Teubert,
• Eric Thomas,
• Daniel James David Thompson,
• Kayleigh Anne Thomson,
• Hanae Tilquin,
• Vincent Tisserand,
• Stephane T'Jampens,
• Mark Tobin,
• Luca Tomassetti,
• Xingyu Tong,
• Diego Torres Machado,
• Da Yu Tou,
• Ekaterina Trifonova,
• Stoyan Miroslavov Trilov,
• Carina Trippl,
• Giulia Tuci,
• Alison Tully,
• Niels Tuning,
• Artur Ukleja,
• Daniel Joachim Unverzagt,
• Eduard Ursov,
• Andrii Usachov,
• Andrey Ustyuzhanin,
• Ulrich Uwer,
• Alexander Vagner,
• Vincenzo Vagnoni,
• Andrea Valassi,
• Giovanni Valenti,
• Nuria Valls Canudas,
• Martinus van Beuzekom,
• Maarten Van Dijk,
• Hubert Van Hecke,
• Eric van Herwijnen,
• Maarten van Veghel,
• Ricardo Vazquez Gomez,
• Pablo Vazquez Regueiro,
• Carlos Vázquez Sierra,
• Stefania Vecchi,
• Jaap Velthuis,
• Michele Veltri,
• Aravindhan Venkateswaran,
• Michele Veronesi,
• Mika Vesterinen,
• Daniel Vieira,
• Maria Vieites Diaz,
• Harald Viemann,
• Xavier Vilasis-Cardona,
• Eva Vilella Figueras,
• Andrea Villa,
• Pascal Vincent,
• Felicia Carolin Volle,
• Dorothea Vom Bruch,
• Alexey Vorobyev,
• Vitaly Vorobyev,
• Nikolai Voropaev,
• Kimberley Vos,
• Roland Waldi,
• John Walsh,
• Chishuai Wang,
• Jialu Wang,
• Jianchun Wang,
• Jianqiao Wang,
• Jike Wang,
• Mengzhen Wang,
• Rui Wang,
• Yilong Wang,
• Zhenzi Wang,
• Zirui Wang,
• Ziyi Wang,
• Jake Alexander Ward,
• Nigel Watson,
• Steffen Georg Weber,
• David Websdale,
• Constantin Weisser,
• Benedict Donald C Westhenry,
• Dylan Jaide White,
• Mark Whitehead,
• Aidan Richard Wiederhold,
• Dirk Wiedner,
• Guy Wilkinson,
• Michael Wilkinson,
• Ifan Williams,
• Mike Williams,
• Mark Richard James Williams,
• Fergus Wilson,
• Wojciech Wislicki,
• Mariusz Witek,
• Lukas Witola,
• Guy Wormser,
• Stephen Wotton,
• Hangyi Wu,
• Kenneth Wyllie,
• Zhiyu Xiang,
• Dong Xiao,
• Yuehong Xie,
• Ao Xu,
• Jingyi Xu,
• Li Xu,
• Menglin Xu,
• Qingnian Xu,
• Zehua Xu,
• Zhihao Xu,
• Di Yang,
• Shuangli Yang,
• Youhua Yang,
• Zhenwei Yang,
• Zishuo Yang,
• Yuezhe Yao,
• Lauren Emma Yeomans,
• Hang Yin,
• Jiesheng Yu,
• Xuhao Yuan,
• Oleg Yushchenko,
• Ettore Zaffaroni,
• Mikhail Zavertyaev,
• Milosz Zdybal,
• Oleksandr Zenaiev,
• Ming Zeng,
• Dongliang Zhang,
• Liming Zhang,
• Shulei Zhang,
• Shunan Zhang,
• Yanxi Zhang,
• Yu Zhang,
• Alina Zharkova,
• Alexey Zhelezov,
• Yangheng Zheng,
• Tianwen Zhou,
• Xiaokang Zhou,
• Yixiong Zhou,
• Valeriia Zhovkovska,
• Xianglei Zhu,
• Xiaoyu Zhu,
• Zhanwen Zhu,
• Valery Zhukov,
• Jennifer Brigitta Zonneveld,
• Quan Zou,
• Stefano Zucchelli,
• Davide Zuliani,
• Gianluca Zunica
• (less)
abstract + abstract -

The multihadron decays ${\Lambda}_b^0$ → D+pπ−π− and ${\Lambda}_b^0$ → D$^{*}$+pπ−π− are observed in data corresponding to an integrated luminosity of 3 fb$^{−1}$, collected in proton-proton collisions at centre-of-mass energies of 7 and 8 TeV by the LHCb detector. Using the decay ${\Lambda}_b^0$ → ${\Lambda}_c^{+}$π$^{+}$π$^{−}$π$^{−}$ as a normalisation channel, the ratio of branching fractions is measured to be$\frac{\mathcal{B}\left({\Lambda}_b^0\to {D}^{+}p{\pi}^{-}{\pi}^{-}\right)}{\mathcal{B}\left({\Lambda}_b^0\to {\Lambda}_c^0{\pi}^{+}{\pi}^{-}{\pi}^{-}\right)}\times \frac{\mathcal{B}\left({D}^{+}\to {K}^{-}{\pi}^{+}{\pi}^{+}\right)}{\mathcal{B}\left({\Lambda}_c^0\to {pK}^{-}{\pi}^{-}\right)}=\left(5.35\pm 0.21\pm 0.16\right)\%,$where the first uncertainty is statistical and the second systematic. The ratio of branching fractions for the ${\Lambda}_b^0$ → D$^{*+}$pπ$^{−}$π$^{−}$ and ${\Lambda}_b^0$ → D$^{+}$pπ$^{−}$π$^{−}$ decays is found to be$\frac{\mathcal{B}\left({\Lambda}_b^0\to {D}^{\ast +}p{\pi}^{-}{\pi}^{-}\right)}{\mathcal{B}\left({\Lambda}_b^0\to {D}^{+}p{\pi}^{-}{\pi}^{-}\right)}\times \left(\mathcal{B}\left({D}^{\ast +}\to {D}^{+}{\pi}^0\right)+\mathcal{B}\left({D}^{\ast +}\to {D}^{+}\gamma \right)\right)=\left(61.3\pm 4.3\pm 4.0\right)\%.$[graphic not available: see fulltext]

(260)CLMM: a LSST-DESC cluster weak lensing mass modeling library for cosmology
• M. Aguena,
• C. Avestruz,
• C. Combet,
• S. Fu,
• R. Herbonnet
• +20
• A. I. Malz,
• M. Penna-Lima,
• M. Ricci,
• S. D. P. Vitenti,
• L. Baumont,
• H. Fan,
• M. Fong,
• M. Ho,
• M. Kirby,
• C. Payerne,
• D. Boutigny,
• B. Lee,
• B. Liu,
• T. McClintock,
• H. Miyatake,
• C. Sifón,
• A. von der Linden,
• H. Wu,
• M. Yoon,
• LSST Dark Energy Science Collaboration
• (less)
Monthly Notices of the Royal Astronomical Society, 508, p19 (12/2021) doi:10.1093/mnras/stab2764
abstract + abstract -

We present the v1.0 release of CLMM, an open source PYTHON library for the estimation of the weak lensing masses of clusters of galaxies. CLMM is designed as a stand-alone toolkit of building blocks to enable end-to-end analysis pipeline validation for upcoming cluster cosmology analyses such as the ones that will be performed by the Vera C. Rubin Legacy Survey of Space and Time-Dark Energy Science Collaboration (LSST-DESC). Its purpose is to serve as a flexible, easy-to-install, and easy-to-use interface for both weak lensing simulators and observers and can be applied to real and mock data to study the systematics affecting weak lensing mass reconstruction. At the core of CLMM are routines to model the weak lensing shear signal given the underlying mass distribution of galaxy clusters and a set of data operations to prepare the corresponding data vectors. The theoretical predictions rely on existing software, used as backends in the code, that have been thoroughly tested and cross-checked. Combined theoretical predictions and data can be used to constrain the mass distribution of galaxy clusters as demonstrated in a suite of example Jupyter Notebooks shipped with the software and also available in the extensive online documentation.

(259)Taking off the edge -- simultaneous filament and end core formation
• Stefan Heigl,
• Elena Hoemann,
• Andreas Burkert
arXiv e-prints (12/2021) e-Print:2112.12640
abstract + abstract -

Simulations of idealised star-forming filaments of finite length typically show core growth which is dominated by two cores forming at its respective end. The end cores form due to a strong increasing acceleration at the filament ends which 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 often do not show this prevalence of cores at the filament edges. We use numerical simulations of accreting filaments forming in a finite converging flow to explore a possible mechanism which leads to a suppression of the end cores. While such a setup still leads to end cores that soon begin to move inwards, the continued accumulation of material outside of these makes a key difference: their positions now lie within the larger filamentary structure and not at its edges. This softens their inward gravitational acceleration as they are embedded by new material further out. As a result, these two cores do not grow as fast as expected for the edge effect and thus do not dominate over other core formation modes in the filament.

(258)Symplectic quantization of multi-field Generalized Proca electrodynamics
• Verónica Errasti Díez,
• Marina Krstic Marinkovic
arXiv e-prints (12/2021) e-Print:2112.11477
abstract + abstract -

We explicitly carry out the symplectic quantization of a family of multi-field Generalized Proca (GP) electrodynamics theories. In the process, we provide an independent derivation of the so-called secondary constraint enforcing relations -- consistency conditions that significantly restrict the allowed interactions in multi-field settings already at the classical level. Additionally, we unveil the existence of quantum consistency conditions, which apply in both single- and multi-field GP scenarios. Our newly found conditions imply that not all classically well-defined (multi-)GP theories are amenable to quantization. The extension of our results to the most general multi-GP class is conceptually straightforward, albeit algebraically cumbersome.

(257)Trade-offs and design principles in the spatial organization of catalytic particles
• Florian Hinzpeter,
• Filipe Tostevin,
• Alexander Buchner,
• Ulrich Gerland
Nature Physics, 18, p9 (12/2021) doi:10.1038/s41567-021-01444-4
abstract + abstract -

Catalytic particles are spatially organized in a number of biological systems across different length scales, from enzyme complexes to metabolically coupled cells. Despite operating on different scales, these systems all feature localized reactions involving partially hindered diffusive transport, which is determined by the collective arrangement of the catalysts. Yet it remains largely unexplored how different arrangements affect the interplay between the reaction and transport dynamics, which ultimately determines the flux through the reaction pathway. Here we show that two fundamental trade-offs arise, the first between efficient inter-catalyst transport and the depletion of substrate, and the second between steric confinement of intermediate products and the accessibility of catalysts to substrate. We use a model reaction pathway to characterize the general design principles for the arrangement of catalysts that emerge from the interplay of these trade-offs. We find that the question of optimal catalyst arrangements generalizes the well-known Thomson problem of electrostatics.

(256)Quantum probing of null singularities
• Ivo Sachs,
• Marc Schneider,
• Maximilian Urban
Physical Review D, 104 (12/2021) doi:10.1103/PhysRevD.104.125020
abstract + abstract -

We adapt the dual-null foliation to the functional Schrödinger representation of quantum field theory and study the behavior of quantum probes in plane-wave space-times near the null singularity. A comparison between the Einstein-Rosen and the Brinkmann patch, where the latter extends beyond the first, shows a seeming tension that can be resolved by comparing the configuration spaces. Our analysis concludes that Einstein-Rosen space-times support exclusively configurations with nonempty gravitational memory that are focused to a set of measure zero in the focal plane with respect to a Brinkmann observer. To conclude, we provide a rough framework to estimate the qualitative influence of backreactions on these results.

(255)Charge radii in covariant density functional theory: A global view
• U. C. Perera,
• A. V. Afanasjev,
• P. Ring
Physical Review C, 104 (12/2021) doi:10.1103/PhysRevC.104.064313
abstract + abstract -

A systematic global investigation of differential charge radii has been performed within the CDFT framework for the first time. Theoretical results obtained with conventional covariant energy density functionals and the separable pairing interaction of Tian et al. [Phys. Lett. B 676, 44 (2009), 10.1016/j.physletb.2009.04.067] are compared with experimental differential charge radii in the regions of the nuclear chart in which available experimental data crosses the neutron shell closures at N =28 ,50 ,82 , and 126. The analysis of absolute differential radii of different isotopic chains and their relative properties indicate clearly that such properties are reasonably well described in model calculations in the cases when the mean-field approximation is justified. However, while the observed clusterization of differential charge radii of different isotopic chains is well described above the N =50 and N =126 shell closures, it is more difficult to reproduce it above the N =28 and N =82 shell closures because of possible deficiencies in the underlying single-particle structure. The impact of the latter has been evaluated for spherical shapes and it was shown that the relative energies of the single-particle states and the patterns of their occupation with increasing neutron number have an appreciable impact on the evolution of the δ «r2»N ,N' values. These factors also limit the predictive power of model calculations in the regions of high densities of the single-particle states of different origin. It is shown that the kinks in the charge radii at neutron shell closures are due to the underlying single-particle structure and due to weakening or collapse of pairing at these closures. The regions of the nuclear chart in which the correlations beyond mean field are expected to have an impact on charge radii are indicated; the analysis shows that the assignment of a calculated excited prolate minimum to the experimental ground state allows us to understand the trends of the evolution of differential charge radii with neutron number in many cases of shape coexistence even at the mean-field level. It is usually assumed that pairing is a dominant contributor to odd-even staggering (OES) in charge radii. Our analysis paints a more complicated picture. It suggests a new mechanism in which the fragmentation of the single-particle content of the ground state in odd-mass nuclei due to particle-vibration coupling provides a significant contribution to OES in charge radii.

(254)The angular momentum structure of CR-driven galactic outflows triggered by stream accretion
• N. Peschken,
• M. Hanasz,
• T. Naab,
• D. Wóltański,
• A. Gawryszczak
Monthly Notices of the Royal Astronomical Society, 508, p13 (12/2021) doi:10.1093/mnras/stab2784
abstract + abstract -

We investigate the impact of gas accretion in streams on the evolution of disc galaxies, using magnetohydrodynamic simulations including advection and anisotropic diffusion of cosmic rays (CRs) generated by supernovae as the only source of feedback. Stream accretion has been suggested as an important galaxy growth mechanism in cosmological simulations and we vary their orientation and angular momentum in idealized setups. We find that accretion streams trigger the formation of galactic rings and enhanced star formation. The star formation rates and consequently the CR-driven outflow rates are higher for low angular momentum accretion streams, which also result in more compact, lower angular momentum discs. The CR generated outflows show a characteristic structure. At low outflow velocities (<50 km s-1), the angular momentum distribution is similar to the disc and the gas is in a fountain flow. Gas at high outflow velocities (>200 km s-1), penetrating deep into the halo, has close to zero angular momentum, and originates from the centre of the galaxies. As the mass loading factors of the CR-driven outflows are of the order of unity and higher, we conclude that this process is important for the removal of low angular momentum gas from evolving disc galaxies and the transport of, potentially metal enriched, material from galactic centres far into the galactic haloes.

(253)Interplanetary Dust as a Foreground for the LiteBIRD CMB Satellite Mission
• Ken Ganga,
• Michele Maris,
• Mathieu Remazeilles,
• LiteBIRD Collaboration
The Open Journal of Astrophysics, 4 (12/2021) doi:10.21105/astro.2110.13856
abstract + abstract -

As ever-more sensitive experiments are made in the quest for primordial CMB B Modes, the number of potentially significant astrophysical contaminants becomes larger as well. Thermal emission from interplanetary dust, for example, has been detected by the Planck satellite. While the polarization fraction of this Zodiacal, or interplanetary dust emission (IPDE) is expected to be low, it is bright enough to be detected in total power. Here, estimates of the magnitude of the effect as it might be seen by the LiteBIRD satellite are made. The COBE IPDE model from Kelsall et al. (1998) is combined with a model of the LiteBIRD experiment's scanning strategy to estimate potential contamination of the CMB in both total power and in polarization power spectra. LiteBIRD should detect IPDE in temperature across all of its bands, from 40 through 402 GHz, and should improve limits on the polarization fraction of IPDE at the higher end of this frequency range. If the polarization fraction of IPDE is of order 1%, the current limit from ISO/CAM measurements in the mid-infrared, it may induce large-scale polarization B Modes comparable to cosmological models with an r of order 0.001. In this case, the polarized IPDE would also need to be modeled and removed. As a CMB foreground, IPDE will always be subdominant to Galactic emissions, though because it caused by emission from grains closer to us, it appears variable as the Earth travels around the Sun, and may thereby complicate the data analysis somewhat. But with an understanding of some of the symmetries of the emission and some flexibility in the data processing, it should not be the primary impediment to the CMB polarization measurement.

(252)Finite-temperature linear response theory based on relativistic Hartree Bogoliubov model with point-coupling interaction
• A. Ravlić,
• Y. F. Niu,
• T. Nikšić,
• N. Paar,
• P. Ring
Physical Review C, 104 (12/2021) doi:10.1103/PhysRevC.104.064302
abstract + abstract -

The finite-temperature linear response theory based on the finite-temperature relativistic Hartree-Bogoliubov (FT-RHB) model is developed in the charge-exchange channel to study the temperature evolution of spin-isospin excitations. Calculations are performed self-consistently with relativistic point-coupling interactions DD-PC1 and DD-PCX. In the charge-exchange channel, the pairing interaction can be split into isovector (T =1 ) and isoscalar (T =0 ) parts. For the isovector component, the same separable form of the Gogny D1S pairing interaction is used both for the ground-state calculation as well as for the residual interaction, while the strength of the isoscalar pairing in the residual interaction is determined by comparison with experimental data on Gamow-Teller resonance (GTR) and isobaric analog resonance (IAR) centroid energy differences in even-even tin isotopes. The temperature effects are introduced by treating Bogoliubov quasiparticles within a grand-canonical ensemble. Thus, unlike the conventional formulation of the quasiparticle random-phase approximation (QRPA) based on the Bardeen-Cooper-Schrieffer (BCS) basis, our model is formulated within the Hartree-Fock-Bogoliubov (HFB) quasiparticle basis. Implementing a relativistic point-coupling interaction and a separable pairing force allows for the reduction of complicated two-body residual interaction matrix elements, which considerably decreases the dimension of the problem in the coordinate space. The main advantage of this method is to avoid the diagonalization of a large QRPA matrix, especially at finite temperature where the size of configuration space is significantly increased. The implementation of the linear response code is used to study the temperature evolution of IAR, GTR, and spin-dipole resonance (SDR) in even-even tin isotopes in the temperature range T =0 -1.5 MeV.

(251)The two phases of core formation - orbital evolution in the centres of ellipticals with supermassive black hole binaries
• M. Frigo,
• T. Naab,
• A. Rantala,
• P. H. Johansson,
• B. Neureiter
• +2
Monthly Notices of the Royal Astronomical Society, 508, p15 (12/2021) doi:10.1093/mnras/stab2754
abstract + abstract -

The flat stellar density cores of massive elliptical galaxies form rapidly due to sinking supermassive black holes (SMBHs) in gas-poor galaxy mergers. After the SMBHs form a bound binary, gravitational slingshot interactions with nearby stars drive the core regions towards a tangentially biased stellar velocity distribution. We use collisionless galaxy merger simulations with accurate collisional orbit integration around the central SMBHs to demonstrate that the removal of stars from the centre by slingshot kicks accounts for the entire change in velocity anisotropy. The rate of strong (unbinding) kicks is constant over several hundred Myr at $\sim 3 \ \mathrm{ M}_\odot\, \rm yr^{-1}$ for our most massive SMBH binary (MBH = 1.7 × 1010 M). Using a frequency-based orbit classification scheme (box, x-tube, z-tube, rosette), we demonstrate that slingshot kicks mostly affect box orbits with small pericentre distances, leading to a velocity anisotropy of β ≲ -0.6 within several hundred Myr as observed in massive ellipticals with large cores. We show how different SMBH masses affect the orbital structure of the merger remnants and present a kinematic tomography connecting orbit families to integral field kinematic features. Our direct orbit classification agrees remarkably well with a modern triaxial Schwarzschild analysis applied to simulated mock kinematic maps.

(250)The dispersal of protoplanetary discs - III. Influence of stellar mass on disc photoevaporation
• Giovanni Picogna,
• Barbara Ercolano,
• Catherine C. Espaillat
Monthly Notices of the Royal Astronomical Society, 508, p9 (12/2021) doi:10.1093/mnras/stab2883
abstract + abstract -

The strong X-ray irradiation from young solar-type stars may play a crucial role in the thermodynamics and chemistry of circumstellar discs, driving their evolution in the last stages of disc dispersal as well as shaping the atmospheres of newborn planets. In this paper, we study the influence of stellar mass on circumstellar disc mass-loss rates due to X-ray irradiation, extending our previous study of the mass-loss rate's dependence on the X-ray luminosity and spectrum hardness. We focus on stars with masses between 0.1 and 1 M, which are the main target of current and future missions to find potentially habitable planets. We find a linear relationship between the mass-loss rates and the stellar masses when changing the X-ray luminosity accordingly with the stellar mass. This linear increase is observed also when the X-ray luminosity is kept fixed because of the lower disc aspect ratio which allows the X-ray irradiation to reach larger radii. We provide new analytical relations for the mass-loss rates and profiles of photoevaporative winds as a function of the stellar mass that can be used in disc and planet population synthesis models. Our photoevaporative models correctly predict the observed trend of inner-disc lifetime as a function of stellar mass with an increased steepness for stars smaller than 0.3 M, indicating that X-ray photoevaporation is a good candidate to explain the observed disc dispersal process.

(249)The dispersal of protoplanetary discs - II: photoevaporation models with observationally derived irradiating spectra
• Barbara Ercolano,
• Giovanni Picogna,
• Kristina Monsch,
• Jeremy J. Drake,
• Thomas Preibisch
Monthly Notices of the Royal Astronomical Society, 508, p11 (12/2021) doi:10.1093/mnras/stab2590
abstract + abstract -

Young solar-type stars are known to be strong X-ray emitters and their X-ray spectra have been widely studied. X-rays from the central star may play a crucial role in the thermodynamics and chemistry of the circumstellar material as well as in the atmospheric evolution of young planets. In this paper, we present model spectra based on spectral parameters derived from the observations of young stars in the Orion nebula cluster from the Chandra Orion Ultradeep Project (COUP). The spectra are then used to calculate new photoevaporation prescriptions that can be used in disc and planet population synthesis models. Our models clearly show that disc wind mass loss rates are controlled by the stellar luminosity in the soft ($100\, \mathrm{eV}$ to $1\, \mathrm{keV}$) X-ray band. New analytical relations are provided for the mass loss rates and profiles of photoevaporative winds as a function of the luminosity in the soft X-ray band. The agreement between observed and predicted transition disc statistics moderately improved using the new spectra, but the observed population of strongly accreting large cavity discs can still not be reproduced by these models. Furthermore, our models predict a population of non-accreting transition discs that are not observed. This highlights the importance of considering the depletion of millimetre-sized dust grains from the outer disc, which is a likely reason why such discs have not been detected yet.

(248)Chromo-electric screening length in 2+1 flavor QCD
• Peter Petreczky,
• Sebastian Steinbeißer,
• Johannes Heinrich Weber
arXiv e-prints (12/2021) e-Print:2112.00788
abstract + abstract -

We study Polyakov loop as well as correlators of real and imaginary parts of the Polyakov loop in 2+1 flavor QCD at finite temperature. We use hypercubic (HYP) smearing to improve the signal in the lattice calculations and to obtain reliable results for the correlators at large distances. From the large distance behavior of the correlators we estimate the chromo-electric screening length to be (0.38-44)/T. Furthermore, we show that the short distance distortions due to HYP smearing do not affect the physics of interest

(247)Three-loop gluon scattering in QCD and the gluon Regge trajectory
• Fabrizio Caola,
• Amlan Chakraborty,
• Giulio Gambuti,
• Andreas von Manteuffel,
• Lorenzo Tancredi
arXiv e-prints (12/2021) e-Print:2112.11097
abstract + abstract -

We compute the three-loop helicity amplitudes for the scattering of four gluons in QCD. We employ projectors in the 't Hooft-Veltman scheme and construct the amplitudes from a minimal set of physical building blocks, which allows us to keep the computational complexity under control. We obtain relatively compact results that can be expressed in terms of harmonic polylogarithms. In addition, we consider the Regge limit of our amplitude and extract the gluon Regge trajectory in full three-loop QCD. This is the last missing ingredient required for studying single-Reggeon exchanges at next-to-next-to-leading logarithmic accuracy.

(246)From amino acid mixtures to peptides in liquid sulphur dioxide on early Earth
• Fabian Sauer,
• Maren Haas,
• Constanze Sydow,
• Alexander F. Siegle,
• Christoph A. Lauer
• +1
Nature Communications, 12 (12/2021) doi:10.1038/s41467-021-27527-7
abstract + abstract -

The formation of peptide bonds is one of the most important biochemical reaction steps. Without the development of structurally and catalytically active polymers, there would be no life on our planet. However, the formation of large, complex oligomer systems is prevented by the high thermodynamic barrier of peptide condensation in aqueous solution. Liquid sulphur dioxide proves to be a superior alternative for copper-catalyzed peptide condensations. Compared to water, amino acids are activated in sulphur dioxide, leading to the incorporation of all 20 proteinogenic amino acids into proteins. Strikingly, even extremely low initial reactant concentrations of only 50 mM are sufficient for extensive peptide formation, yielding up to 2.9% of dialanine in 7 days. The reactions carried out at room temperature and the successful use of the Hadean mineral covellite (CuS) as a catalyst, suggest a volcanic environment for the formation of the peptide world on early Earth.

(245)A general framework to test gravity using galaxy clusters IV: cluster and halo properties in DGP gravity
• Myles A. Mitchell,
• César Hernández-Aguayo,
• Christian Arnold,
• Baojiu Li
Monthly Notices of the Royal Astronomical Society, 508, p17 (12/2021) doi:10.1093/mnras/stab2817
abstract + abstract -

We study and model the properties of galaxy clusters in the normal-branch Dvali-Gabadadze-Porrati (nDGP) model of gravity, which is representative of a wide class of theories that exhibit the Vainshtein screening mechanism. Using the first cosmological simulations that incorporate both full baryonic physics and nDGP, we find that, despite being efficiently screened within clusters, the fifth force can raise the temperature of the intracluster gas, affecting the scaling relations between the cluster mass and three observable mass proxies: the gas temperature, the Compton Y-parameter of the Sunyaev-Zel'dovich effect, and the X-ray analogue of the Y-parameter. Therefore, unless properly accounted for, this could lead to biased measurements of the cluster mass in tests that use cluster observations, such as cluster number counts, to probe gravity. Using a suite of dark-matter-only simulations, which span a wide range of box sizes and resolutions, and which feature very different strengths of the fifth force, we also calibrate general fitting formulae that can reproduce the nDGP halo concentration at percent accuracy for 0 ≤ z ≤ 1, and halo mass function with ${\lesssim}3{{\ \rm per\ cent}}$ accuracy at 0 ≤ z ≤ 1 (increasing to ${\lesssim}5{{\ \rm per\ cent}}$ for 1 ≤ z ≤ 2), over a halo mass range spanning four orders of magnitude. Our model for the concentration can be used for converting between halo mass overdensities and predicting statistics such as the non-linear matter power spectrum. The results of this work will form part of a framework for unbiased constraints of gravity using the data from ongoing and upcoming cluster surveys.

(244)BSM master formula for ε'/ε in the WET basis at NLO in QCD
• Jason Aebischer,
• Christoph Bobeth,
• Andrzej J. Buras,
• Jacky Kumar
Journal of High Energy Physics, 2021 (12/2021) doi:10.1007/JHEP12(2021)043
abstract + abstract -

As an important step towards a complete next-to-leading (NLO) QCD analysis of the ratio ε'/ε within the Standard Model Effective Field Theory (SMEFT), we present for the first time the NLO master formula for the BSM part of this ratio expressed in terms of the Wilson coefficients of all contributing operators evaluated at the electroweak scale. To this end we use the common Weak Effective Theory (WET) basis (the so-called JMS basis) for which tree-level and one-loop matching to the SMEFT are already known. The relevant hadronic matrix elements of BSM operators at the electroweak scale are taken from Dual QCD approach and the SM ones from lattice QCD. It includes the renormalization group evolution and quark-flavour threshold effects at NLO in QCD from hadronic scales, at which these matrix elements have been calculated, to the electroweak scale.

(243)Rotation Curves in z 1-2 Star-forming Disks: Comparison of Dark Matter Fractions and Disk Properties for Different Fitting Methods
• S. H. Price,
• T. T. Shimizu,
• R. Genzel,
• H. Übler,
• N. M. Förster Schreiber
• +20
• L. J. Tacconi,
• R. I. Davies,
• R. T. Coogan,
• D. Lutz,
• S. Wuyts,
• E. Wisnioski,
• A. Nestor,
• A. Sternberg,
• A. Burkert,
• R. Bender,
• A. Contursi,
• R. L. Davies,
• R. Herrera-Camus,
• M. -J. Lee,
• T. Naab,
• R. Neri,
• A. Renzini,
• R. Saglia,
• A. Schruba,
• K. Schuster
• (less)
The Astrophysical Journal, 922, p20 (12/2021) doi:10.3847/1538-4357/ac22ad
abstract + abstract -

We present a follow-up analysis examining the dynamics and structures of 41 massive, large star-forming galaxies at z ~ 0.67 - 2.45 using both ionized and molecular gas kinematics. We fit the galaxy dynamics with models consisting of a bulge, a thick, turbulent disk, and an NFW dark matter halo, using code that fully forward-models the kinematics, including all observational and instrumental effects. We explore the parameter space using Markov Chain Monte Carlo (MCMC) sampling, including priors based on stellar and gas masses and disk sizes. We fit the full sample using extracted 1D kinematic profiles. For a subset of 14 well-resolved galaxies, we also fit the 2D kinematics. The MCMC approach robustly confirms the results from least-squares fitting presented in Paper I: the sample galaxies tend to be baryon-rich on galactic scales (within one effective radius). The 1D and 2D MCMC results are also in good agreement for the subset, demonstrating that much of the galaxy dynamical information is captured along the major axis. The 2D kinematics are more affected by the presence of noncircular motions, which we illustrate by constructing a toy model with constant inflow for one galaxy that exhibits residual signatures consistent with radial motions. This analysis, together with results from Paper I and other studies, strengthens the finding that massive, star-forming galaxies at z ~ 1 - 2 are baryon-dominated on galactic scales, with lower dark matter fractions toward higher baryonic surface densities. Finally, we present details of the kinematic fitting code used in this analysis.

(242)Mass-ratio and Magnetic Flux Dependence of Modulated Accretion from Circumbinary Disks
• Scott C. Noble,
• Julian H. Krolik,
• Manuela Campanelli,
• Yosef Zlochower,
• Bruno C. Mundim
• +2
• Hiroyuki Nakano,
• Miguel Zilhão
• (less)
The Astrophysical Journal, 922, p29 (12/2021) doi:10.3847/1538-4357/ac2229
abstract + abstract -

Accreting supermassive binary black holes (SMBBHs) are potential multimessenger sources because they emit both gravitational-wave and electromagnetic (EM) radiation. Past work has shown that their EM output may be periodically modulated by an asymmetric density distribution in the circumbinary disk, often called an "overdensity" or "lump;" this modulation could possibly be used to identify a source as a binary. We explore the sensitivity of the overdensity to SMBBH mass ratio and magnetic flux through the accretion disk. We find that the relative amplitude of the overdensity and its associated EM periodic signal both degrade with diminishing mass ratio, vanishing altogether somewhere between 1:2 and 1:5. Greater magnetization also weakens the lump and any modulation of the light output. We develop a model to describe how lump formation results from internal stress degrading faster in the lump region than it can be rejuvenated through accretion inflow, and predicts a threshold value in specific internal stress below which lump formation should occur and which all our lump-forming simulations satisfy. Thus, detection of such a modulation would provide a constraint on both mass ratio and magnetic flux piercing the accretion flow.

(241)The formation of wide exoKuiper belts from migrating dust traps
• E. Miller,
• S. Marino,
• S. M. Stammler,
• P. Pinilla,
• C. Lenz
• +2
Monthly Notices of the Royal Astronomical Society, 508, p19 (12/2021) doi:10.1093/mnras/stab2935
abstract + abstract -

The question of what determines the width of Kuiper belt analogues (exoKuiper belts) is an open one. If solved, this understanding would provide valuable insights into the architecture, dynamics, and formation of exoplanetary systems. Recent observations by ALMA have revealed an apparent paradox in this field, the presence of radially narrow belts in protoplanetary discs that are likely the birthplaces of planetesimals, and exoKuiper belts nearly four times as wide in mature systems. If the parent planetesimals of this type of debris disc indeed form in these narrow protoplanetary rings via streaming instability where dust is trapped, we propose that this width dichotomy could naturally arise if these dust traps form planetesimals whilst migrating radially, e.g. as caused by a migrating planet. Using the dust evolution software DUSTPY, we find that if the initial protoplanetary disc and trap conditions favour planetesimal formation, dust can still effectively accumulate and form planetesimals as the trap moves. This leads to a positive correlation between the inward radial speed and final planetesimal belt width, forming belts up to ~100AU over 10 Myr of evolution. We show that although planetesimal formation is most efficient in low-viscosity (α = 10-4) discs with steep dust traps to trigger the streaming instability, the large widths of most observed planetesimal belts constrain α to values ≥4 × 10-4 at tens of AU, otherwise the traps cannot migrate far enough. Additionally, the large spread in the widths and radii of exoKuiper belts could be due to different trap migration speeds (or protoplanetary disc lifetimes) and different starting locations, respectively. Our work serves as a first step to link exoKuiper belts and rings in protoplanetary discs.

(240)The DESI $N$-body Simulation Project I: Testing the Robustness of Simulations for the DESI Dark Time Survey
• Cameron Grove,
• Chia-Hsun Chuang,
• Ningombam Chandrachani Devi,
• Lehman Garrison,
• Benjamin L'Huillier
• +17
• Yu Feng,
• John Helly,
• César Hernández-Aguayo,
• Shadab Alam,
• Hanyu Zhang,
• Yu Yu,
• Shaun Cole,
• Daniel Eisenstein,
• Peder Norberg,
• Risa Wechsler,
• David Brooks,
• Kyle Dawson,
• Martin Landriau,
• Aaron Meisner,
• Claire Poppett,
• Gregory Tarlé,
• Octavio Valenzuela
• (less)
arXiv e-prints (12/2021) e-Print:2112.09138
abstract + abstract -

Analysis of large galaxy surveys requires confidence in the robustness of numerical simulation methods. The simulations are used to construct mock galaxy catalogs to validate data analysis pipelines and identify potential systematics. We compare three $N$-body simulation codes, ABACUS, GADGET, and SWIFT, to investigate the regimes in which their results agree. We run $N$-body simulations at three different mass resolutions, $6.25\times10^{8}$, $2.11\times10^{9}$, and $5.00\times10^{9}~h^{-1}$M$_{\odot}$, matching phases to reduce the noise within the comparisons. We find systematic errors in the halo clustering between different codes are smaller than the DESI statistical error for $s > 20\, h^{-1}$Mpc in the correlation function in redshift space. Through the resolution comparison we find that simulations run with a mass resolution of $2.1\times10^{9}~h^{-1}$M$_{\odot}$ are sufficiently converged for systematic effects in the halo clustering to be smaller than the DESI statistical error at scales larger than $20 \, h^{-1}$Mpc. These findings show that the simulations are robust for extracting cosmological information from large scales which is the key goal of the DESI survey. Comparing matter power spectra, we find the codes agree to within 1% for $k \leq 10~h$Mpc$^{-1}$. We also run a comparison of three initial condition generation codes and find good agreement. In addition, we include a quasi-$N$-body code, FastPM, since we plan use it for certain DESI analyses. The impact of the halo definition and galaxy-halo relation will be presented in a follow up study.

(239)Two-loop bispectrum of large-scale structure
• Tobias Baldauf,
• Mathias Garny,
• Petter Taule,
• Theo Steele
Physical Review D, 104 (12/2021) doi:10.1103/PhysRevD.104.123551
abstract + abstract -

The bispectrum is the leading non-Gaussian statistic in large-scale structure, carrying valuable information on cosmology that is complementary to the power spectrum. To access this information, we need to model the bispectrum in the weakly nonlinear regime. In this work we present the first two-loop, i.e. next-to-next-to-leading order perturbative description of the bispectrum within an effective field theory (EFT) framework. Using an analytic expansion of the perturbative kernels up to F6 we derive a renormalized bispectrum that is demonstrated to be independent of the UV cutoff. We show that the EFT parameters associated with the four independent second-order EFT operators known from the one-loop bispectrum are sufficient to absorb the UV sensitivity of the two-loop contributions in the double-hard region. In addition, we employ a simplified treatment of the single-hard region, introducing one extra EFT parameter at two-loop order. We compare our results to N -body simulations using the realization-based grid perturbation theory method and find good agreement within the expected range, as well as consistent values for the EFT parameters. The two-loop terms start to become relevant at k ≈0.07 h Mpc-1. The range of wave numbers with percent-level agreement, independently of the shape, extends from 0.08 to 0.15 h Mpc-1 when going from one to two loops at z =0 . In addition, we quantify the impact of using exact instead of Einstein-de-Sitter kernels for the one-loop bispectrum, and discuss in how far their impact can be absorbed into a shift of the EFT parameters.

(238)The local PNG bias of neutral Hydrogen, H$_{I}$
• Alexandre Barreira
abstract + abstract -

We use separate universe simulations with the IllustrisTNG galaxy formation model to predict the local PNG bias parameters bΦ and bΦδ of atomic neutral hydrogen, H$_{I}$. These parameters and their relation to the linear density bias parameter b

$_{1}$ play a key role in observational constraints of the local PNG parameter f

$_{NL}$ using the H$_{I}$ power spectrum and bispectrum. Our results show that the popular calculation based on the universality of the halo mass function overpredicts the bΦ(b

$_{1}$) and bΦδ(b

$_{1}$) relations measured in the simulations. In particular, our results show that at z ≲ 1 the H$_{I}$ power spectrum is more sensitive to f

$_{NL}$ compared to previously thought (bΦ is more negative), but is less sensitive at other epochs (bΦ is less positive). We discuss how this can be explained by the competition of physical effects such as that large-scale gravitational potentials with local PNG (i) accelerate the conversion of hydrogen to heavy elements by star formation, (ii) enhance the effects of baryonic feedback that eject the gas to regions more exposed to ionizing radiation, and (iii) promote the formation of denser structures that shield the H$_{I}$ more efficiently. Our numerical results can be used to revise existing forecast studies on f

$_{NL}$ using 21 cm line-intensity mapping data. Despite this first step towards predictions for the local PNG bias parameters of H$_{I}$, we emphasize that more work is needed to assess their sensitivity on the assumed galaxy formation physics and H$_{I}$ modeling strategy.

(237)EOS - A Software for Flavor Physics Phenomenology
• Danny van Dyk,
• Frederik Beaujean,
• Thomas Blake,
• Christoph Bobeth,
• Marzia Bordone
• +15
• Katarina Dugic,
• Eike Eberhard,
• Nico Gubernari,
• Elena Graverini,
• Martin Jung,
• Ahmet Kokulu,
• Stephan Kürten,
• Domagoj Leljak,
• Philip Lüghausen,
• Stefan Meiser,
• Muslem Rahimi,
• Méril Reboud,
• Rafael Silva Coutinho,
• Javier Virto,
• K. Keri Vos
• (less)
(11/2021) e-Print:2111.15428
abstract + abstract -

EOS is an open-source software for a variety of computational tasks in flavor physics. Its use cases include theory predictions within and beyond the Standard Model of particle physics, Bayesian inference of theory parameters from experimental and theoretical likelihoods, and simulation of pseudo events for a number of signal processes. EOS ensures high-performance computations through a C++ back-end and ease of usability through a Python front-end. To achieve this flexibility, EOS enables the user to select from a variety of implementations of the relevant decay processes and hadronic matrix elements at run time. In this article, we describe the general structure of the software framework and provide basic examples. Further details and in-depth interactive examples are provided as part of the EOS online documentation.

(236)The Pacific Ocean Neutrino Experiment
• Elisa Resconi
PoS, ICRC2021, p024 (11/2021) e-Print:2111.13133 doi:10.22323/1.395.0024
abstract + abstract -

Neutrino telescopes are unrivaled tools to explore the Universe at its most extreme. The current generation of telescopes has shown that very high energy neutrinos are produced in the cosmos, even with hints of their possible origin, and that these neutrinos can be used to probe our understanding of particle physics at otherwise inaccessible regimes. The fluxes, however, are low, which means newer, larger telescopes are needed. Here we present the Pacific Ocean Neutrino Experiment, a proposal to build a multi-cubic-kilometer neutrino telescope off the coast of Canada. The idea builds on the experience accumulated by previous sea-water missions, and the technical expertise of Ocean Networks Canada that would facilitate deploying such a large infrastructure. The design and physics potential of the first stage and a full-scale P-ONE are discussed.

(235)Searches for rare ${B}_s^0$ and B$^{0}$ decays into four muons
• R. Aaij,
• A.S.W. Abdelmotteleb,
• C. Abellán Beteta,
• F. Abudinén,
• T. Ackernley
• +1009
• B. Adeva,
• M. Adinolfi,
• H. Afsharnia,
• C. Agapopoulou,
• C.A. Aidala,
• S. Aiola,
• Z. Ajaltouni,
• S. Akar,
• J. Albrecht,
• F. Alessio,
• M. Alexander,
• A. Alfonso Albero,
• Z. Aliouche,
• G. Alkhazov,
• P. Alvarez Cartelle,
• S. Amato,
• J.L. Amey,
• Y. Amhis,
• L. An,
• L. Anderlini,
• M. Andersson,
• A. Andreianov,
• M. Andreotti,
• F. Archilli,
• A. Artamonov,
• M. Artuso,
• K. Arzymatov,
• E. Aslanides,
• M. Atzeni,
• B. Audurier,
• S. Bachmann,
• M. Bachmayer,
• J.J. Back,
• P. Baladron Rodriguez,
• V. Balagura,
• W. Baldini,
• J. Baptista de Souza Leite,
• M. Barbetti,
• R.J. Barlow,
• S. Barsuk,
• W. Barter,
• M. Bartolini,
• F. Baryshnikov,
• J.M. Basels,
• S. Bashir,
• G. Bassi,
• B. Batsukh,
• A. Battig,
• A. Bay,
• A. Beck,
• M. Becker,
• F. Bedeschi,
• I. Bediaga,
• A. Beiter,
• V. Belavin,
• S. Belin,
• V. Bellee,
• K. Belous,
• I. Belov,
• I. Belyaev,
• G. Bencivenni,
• E. Ben-Haim,
• A. Berezhnoy,
• R. Bernet,
• D. Berninghoff,
• H.C. Bernstein,
• C. Bertella,
• A. Bertolin,
• C. Betancourt,
• F. Betti,
• Ia. Bezshyiko,
• Iaroslava Bezshyiko,
• S. Bhasin,
• J. Bhom,
• L. Bian,
• M.S. Bieker,
• N.V. Biesuz,
• S. Bifani,
• P. Billoir,
• A. Biolchini,
• M. Birch,
• F.C.R. Bishop,
• A. Bitadze,
• A. Bizzeti,
• M. Bjørn,
• M.P. Blago,
• T. Blake,
• F. Blanc,
• S. Blusk,
• D. Bobulska,
• J.A. Boelhauve,
• O. Boente Garcia,
• T. Boettcher,
• A. Boldyrev,
• A. Bondar,
• N. Bondar,
• S. Borghi,
• M. Borisyak,
• M. Borsato,
• J.T. Borsuk,
• S.A. Bouchiba,
• T.J.V. Bowcock,
• A. Boyer,
• C. Bozzi,
• M.J. Bradley,
• S. Braun,
• A. Brea Rodriguez,
• J. Brodzicka,
• A. Brossa Gonzalo,
• D. Brundu,
• A. Buonaura,
• L. Buonincontri,
• A.T. Burke,
• C. Burr,
• A. Bursche,
• A. Butkevich,
• J.S. Butter,
• J. Buytaert,
• W. Byczynski,
• S. Cadeddu,
• H. Cai,
• R. Calabrese,
• L. Calefice,
• S. Cali,
• R. Calladine,
• M. Calvi,
• M. Calvo Gomez,
• P. Camargo Magalhaes,
• P. Campana,
• A.F. Campoverde Quezada,
• S. Capelli,
• L. Capriotti,
• A. Carbone,
• G. Carboni,
• R. Cardinale,
• A. Cardini,
• I. Carli,
• P. Carniti,
• L. Carus,
• K. Carvalho Akiba,
• A. Casais Vidal,
• R. Caspary,
• G. Casse,
• M. Cattaneo,
• G. Cavallero,
• S. Celani,
• J. Cerasoli,
• D. Cervenkov,
• A.J. Chadwick,
• M.G. Chapman,
• M. Charles,
• Philippe Charpentier,
• Ph. Charpentier,
• G. Chatzikonstantinidis,
• C.A. Chavez Barajas,
• M. Chefdeville,
• C. Chen,
• S. Chen,
• A. Chernov,
• V. Chobanova,
• S. Cholak,
• M. Chrzaszcz,
• A. Chubykin,
• V. Chulikov,
• P. Ciambrone,
• M.F. Cicala,
• X. Cid Vidal,
• G. Ciezarek,
• P.E. L. Clarke,
• M. Clemencic,
• H.V. Cliff,
• J. Closier,
• J.L. Cobbledick,
• V. Coco,
• J.A.B. Coelho,
• J. Cogan,
• E. Cogneras,
• L. Cojocariu,
• P. Collins,
• T. Colombo,
• L. Congedo,
• A. Contu,
• N. Cooke,
• G. Coombs,
• I. Corredoira,
• G. Corti,
• C.M. Costa Sobral,
• B. Couturier,
• D.C. Craik,
• J. Crkovská,
• M. Cruz Torres,
• R. Currie,
• C.L. Da Silva,
• S. Dadabaev,
• L. Dai,
• E. Dall'Occo,
• J. Dalseno,
• C. D'Ambrosio,
• A. Danilina,
• P. d'Argent,
• A. Dashkina,
• J.E. Davies,
• A. Davis,
• O. De Aguiar Francisco,
• K. De Bruyn,
• S. De Capua,
• M. De Cian,
• E. De Lucia,
• J.M. De Miranda,
• L. De Paula,
• M. De Serio,
• D. De Simone,
• P. De Simone,
• F. De Vellis,
• J.A. de Vries,
• C.T. Dean,
• F. Debernardis,
• D. Decamp,
• V. Dedu,
• L. Del Buono,
• B. Delaney,
• H.-P. Dembinski,
• A. Dendek,
• V. Denysenko,
• D. Derkach,
• O. Deschamps,
• F. Desse,
• F. Dettori,
• B. Dey,
• A. Di Cicco,
• P. Di Nezza,
• S. Didenko,
• L. Dieste Maronas,
• H. Dijkstra,
• V. Dobishuk,
• C. Dong,
• A.M. Donohoe,
• F. Dordei,
• A.C. dos Reis,
• L. Douglas,
• A. Dovbnya,
• A.G. Downes,
• M.W. Dudek,
• L. Dufour,
• V. Duk,
• P. Durante,
• J.M. Durham,
• D. Dutta,
• A. Dziurda,
• A. Dzyuba,
• S. Easo,
• U. Egede,
• V. Egorychev,
• S. Eidelman,
• S. Eisenhardt,
• S. Ek-In,
• L. Eklund,
• S. Ely,
• A. Ene,
• E. Epple,
• S. Escher,
• J. Eschle,
• S. Esen,
• T. Evans,
• L.N. Falcao,
• Y. Fan,
• B. Fang,
• S. Farry,
• D. Fazzini,
• M. Féo,
• A. Fernandez Prieto,
• A.D. Fernez,
• F. Ferrari,
• L. Ferreira Lopes,
• F. Ferreira Rodrigues,
• S. Ferreres Sole,
• M. Ferrillo,
• M. Ferro-Luzzi,
• S. Filippov,
• R.A. Fini,
• M. Fiorini,
• M. Firlej,
• Kamil Leszek Fischer,
• K.M. Fischer,
• D.S. Fitzgerald,
• C. Fitzpatrick,
• T. Fiutowski,
• A. Fkiaras,
• F. Fleuret,
• M. Fontana,
• F. Fontanelli,
• R. Forty,
• D. Foulds-Holt,
• V. Franco Lima,
• M. Franco Sevilla,
• M. Frank,
• E. Franzoso,
• G. Frau,
• C. Frei,
• D.A. Friday,
• J. Fu,
• Q. Fuehring,
• E. Gabriel,
• G. Galati,
• A. Gallas Torreira,
• D. Galli,
• S. Gambetta,
• Y. Gan,
• M. Gandelman,
• P. Gandini,
• Y. Gao,
• M. Garau,
• L.M. Garcia Martin,
• P. Garcia Moreno,
• J. García Pardiñas,
• B. Garcia Plana,
• F.A. Garcia Rosales,
• L. Garrido,
• C. Gaspar,
• R.E. Geertsema,
• D. Gerick,
• L.L. Gerken,
• E. Gersabeck,
• M. Gersabeck,
• T. Gershon,
• D. Gerstel,
• L. Giambastiani,
• V. Gibson,
• H.K. Giemza,
• A.L. Gilman,
• M. Giovannetti,
• A. Gioventù,
• P. Gironella Gironell,
• C. Giugliano,
• K. Gizdov,
• E.L. Gkougkousis,
• V.V. Gligorov,
• C. Göbel,
• E. Golobardes,
• D. Golubkov,
• A. Golutvin,
• A. Gomes,
• S. Gomez Fernandez,
• F. Goncalves Abrantes,
• M. Goncerz,
• G. Gong,
• P. Gorbounov,
• I.V. Gorelov,
• C. Gotti,
• E. Govorkova,
• J.P. Grabowski,
• T. Grammatico,
• L.A. Granado Cardoso,
• E. Graugés,
• E. Graverini,
• G. Graziani,
• A. Grecu,
• L.M. Greeven,
• N.A. Grieser,
• L. Grillo,
• S. Gromov,
• B.R. Gruberg Cazon,
• C. Gu,
• M. Guarise,
• M. Guittiere,
• P.A. Günther,
• E. Gushchin,
• A. Guth,
• Y. Guz,
• T. Gys,
• T. Hadavizadeh,
• G. Haefeli,
• C. Haen,
• J. Haimberger,
• T. Halewood-leagas,
• P.M. Hamilton,
• J.P. Hammerich,
• Q. Han,
• X. Han,
• T.H. Hancock,
• E.B. Hansen,
• S. Hansmann-Menzemer,
• N. Harnew,
• T. Harrison,
• C. Hasse,
• M. Hatch,
• J. He,
• M. Hecker,
• K. Heijhoff,
• K. Heinicke,
• R.D.L. Henderson,
• A.M. Hennequin,
• K. Hennessy,
• L. Henry,
• J. Heuel,
• A. Hicheur,
• D. Hill,
• M. Hilton,
• S.E. Hollitt,
• R. Hou,
• Y. Hou,
• Jiangqiao Hu,
• Jifeng Hu,
• W. Hu,
• X. Hu,
• W. Huang,
• X. Huang,
• W. Hulsbergen,
• R.J. Hunter,
• M. Hushchyn,
• D. Hutchcroft,
• D. Hynds,
• P. Ibis,
• M. Idzik,
• D. Ilin,
• P. Ilten,
• A. Inglessi,
• A. Ishteev,
• K. Ivshin,
• R. Jacobsson,
• H. Jage,
• S. Jakobsen,
• E. Jans,
• B.K. Jashal,
• A. Jawahery,
• V. Jevtic,
• X. Jiang,
• M. John,
• D. Johnson,
• C.R. Jones,
• T.P. Jones,
• B. Jost,
• N. Jurik,
• S.H. Kalavan Kadavath,
• S. Kandybei,
• Y. Kang,
• M. Karacson,
• M. Karpov,
• J.W. Kautz,
• F. Keizer,
• D.M. Keller,
• M. Kenzie,
• T. Ketel,
• B. Khanji,
• A. Kharisova,
• S. Kholodenko,
• T. Kirn,
• V.S. Kirsebom,
• O. Kitouni,
• S. Klaver,
• N. Kleijne,
• K. Klimaszewski,
• M.R. Kmiec,
• S. Koliiev,
• A. Kondybayeva,
• A. Konoplyannikov,
• P. Kopciewicz,
• R. Kopecna,
• P. Koppenburg,
• M. Korolev,
• I. Kostiuk,
• O. Kot,
• S. Kotriakhova,
• P. Kravchenko,
• L. Kravchuk,
• R.D. Krawczyk,
• M. Kreps,
• F. Kress,
• S. Kretzschmar,
• P. Krokovny,
• W. Krupa,
• W. Krzemien,
• J. Kubat,
• M. Kucharczyk,
• V. Kudryavtsev,
• H.S. Kuindersma,
• G.J. Kunde,
• T. Kvaratskheliya,
• D. Lacarrere,
• G. Lafferty,
• A. Lai,
• A. Lampis,
• D. Lancierini,
• J.J. Lane,
• R. Lane,
• G. Lanfranchi,
• C. Langenbruch,
• J. Langer,
• O. Lantwin,
• T. Latham,
• F. Lazzari,
• R. Le Gac,
• S.H. Lee,
• R. Lefèvre,
• A. Leflat,
• S. Legotin,
• O. Leroy,
• T. Lesiak,
• B. Leverington,
• H. Li,
• P. Li,
• S. Li,
• Yiming Li,
• Yutong Li,
• Z. Li,
• X. Liang,
• T. Lin,
• R. Lindner,
• V. Lisovskyi,
• R. Litvinov,
• G. Liu,
• H. Liu,
• Q. Liu,
• S. Liu,
• A. Lobo Salvia,
• A. Loi,
• J. Lomba Castro,
• I. Longstaff,
• J.H. Lopes,
• S. López Soliño,
• G.H. Lovell,
• Y. Lu,
• C. Lucarelli,
• D. Lucchesi,
• S. Luchuk,
• M. Lucio Martinez,
• V. Lukashenko,
• Y. Luo,
• A. Lupato,
• E. Luppi,
• O. Lupton,
• A. Lusiani,
• X. Lyu,
• L. Ma,
• R. Ma,
• S. Maccolini,
• F. Machefert,
• F. Maciuc,
• V. Macko,
• P. Mackowiak,
• S. Maddrell-Mander,
• O. Madejczyk,
• L.R. Madhan Mohan,
• O. Maev,
• A. Maevskiy,
• M.W. Majewski,
• J.J. Malczewski,
• S. Malde,
• B. Malecki,
• A. Malinin,
• T. Maltsev,
• H. Malygina,
• G. Manca,
• G. Mancinelli,
• D. Manuzzi,
• D. Marangotto,
• J. Maratas,
• J.F. Marchand,
• U. Marconi,
• S. Mariani,
• C. Marin Benito,
• M. Marinangeli,
• J. Marks,
• A.M. Marshall,
• P.J. Marshall,
• G. Martelli,
• G. Martellotti,
• L. Martinazzoli,
• M. Martinelli,
• D. Martinez Santos,
• F. Martinez Vidal,
• A. Massafferri,
• M. Materok,
• R. Matev,
• A. Mathad,
• V. Matiunin,
• C. Matteuzzi,
• K.R. Mattioli,
• A. Mauri,
• E. Maurice,
• J. Mauricio,
• M. Mazurek,
• M. McCann,
• L. Mcconnell,
• T.H. Mcgrath,
• N.T. Mchugh,
• A. McNab,
• R. McNulty,
• J.V. Mead,
• B. Meadows,
• G. Meier,
• D. Melnychuk,
• S. Meloni,
• M. Merk,
• A. Merli,
• L. Meyer Garcia,
• M. Mikhasenko,
• D.A. Milanes,
• E. Millard,
• M. Milovanovic,
• M.-N. Minard,
• A. Minotti,
• L. Minzoni,
• S.E. Mitchell,
• B. Mitreska,
• D.S. Mitzel,
• A. Mödden,
• R.A. Mohammed,
• R.D. Moise,
• S. Mokhnenko,
• T. Mombächer,
• I.A. Monroy,
• S. Monteil,
• M. Morandin,
• G. Morello,
• M.J. Morello,
• J. Moron,
• A.B. Morris,
• A.G. Morris,
• R. Mountain,
• H. Mu,
• F. Muheim,
• M. Mulder,
• D. Müller,
• K. Müller,
• C.H. Murphy,
• D. Murray,
• R. Murta,
• P. Muzzetto,
• P. Naik,
• T. Nakada,
• R. Nandakumar,
• T. Nanut,
• I. Nasteva,
• M. Needham,
• N. Neri,
• S. Neubert,
• N. Neufeld,
• R. Newcombe,
• E.M. Niel,
• S. Nieswand,
• N. Nikitin,
• N.S. Nolte,
• C. Normand,
• C. Nunez,
• A. Oblakowska-Mucha,
• V. Obraztsov,
• T. Oeser,
• D.P. O'Hanlon,
• S. Okamura,
• R. Oldeman,
• F. Oliva,
• M.E. Olivares,
• C.J. G. Onderwater,
• R.H. O'Neil,
• J.M. Otalora Goicochea,
• T. Ovsiannikova,
• P. Owen,
• A. Oyanguren,
• K.O. Padeken,
• B. Pagare,
• P.R. Pais,
• T. Pajero,
• A. Palano,
• M. Palutan,
• Y. Pan,
• G. Panshin,
• A. Papanestis,
• M. Pappagallo,
• L.L. Pappalardo,
• C. Pappenheimer,
• W. Parker,
• C. Parkes,
• B. Passalacqua,
• G. Passaleva,
• A. Pastore,
• M. Patel,
• C. Patrignani,
• C.J. Pawley,
• A. Pearce,
• A. Pellegrino,
• M. Pepe Altarelli,
• S. Perazzini,
• D. Pereima,
• A. Pereiro Castro,
• P. Perret,
• M. Petric,
• K. Petridis,
• A. Petrolini,
• A. Petrov,
• S. Petrucci,
• M. Petruzzo,
• T.T.H. Pham,
• A. Philippov,
• R. Piandani,
• L. Pica,
• M. Piccini,
• B. Pietrzyk,
• G. Pietrzyk,
• M. Pili,
• D. Pinci,
• F. Pisani,
• M. Pizzichemi,
• P.K. Resmi,
• V. Placinta,
• J. Plews,
• M. Plo Casasus,
• F. Polci,
• M. Poli Lener,
• M. Poliakova,
• A. Poluektov,
• N. Polukhina,
• I. Polyakov,
• E. Polycarpo,
• S. Ponce,
• D. Popov,
• S. Popov,
• S. Poslavskii,
• K. Prasanth,
• L. Promberger,
• C. Prouve,
• V. Pugatch,
• V. Puill,
• G. Punzi,
• H. Qi,
• W. Qian,
• N. Qin,
• R. Quagliani,
• N.V. Raab,
• R.I. Rabadan Trejo,
• B. Rachwal,
• J.H. Rademacker,
• M. Rama,
• M. Ramos Pernas,
• M.S. Rangel,
• F. Ratnikov,
• G. Raven,
• M. Reboud,
• F. Redi,
• F. Reiss,
• C. Remon Alepuz,
• Z. Ren,
• V. Renaudin,
• R. Ribatti,
• A.M. Ricci,
• S. Ricciardi,
• K. Rinnert,
• P. Robbe,
• G. Robertson,
• A.B. Rodrigues,
• E. Rodrigues,
• J.A. Rodriguez Lopez,
• E.R. R. Rodriguez Rodriguez,
• A. Rollings,
• P. Roloff,
• V. Romanovskiy,
• M. Romero Lamas,
• A. Romero Vidal,
• J.D. Roth,
• M. Rotondo,
• M.S. Rudolph,
• T. Ruf,
• R.A. Ruiz Fernandez,
• J. Ruiz Vidal,
• A. Ryzhikov,
• J. Ryzka,
• J.J. Saborido Silva,
• N. Sagidova,
• N. Sahoo,
• B. Saitta,
• M. Salomoni,
• C. Sanchez Gras,
• R. Santacesaria,
• C. Santamarina Rios,
• M. Santimaria,
• E. Santovetti,
• D. Saranin,
• G. Sarpis,
• M. Sarpis,
• A. Sarti,
• C. Satriano,
• A. Satta,
• M. Saur,
• D. Savrina,
• H. Sazak,
• L.G. Scantlebury Smead,
• A. Scarabotto,
• S. Schael,
• S. Scherl,
• M. Schiller,
• H. Schindler,
• M. Schmelling,
• B. Schmidt,
• S. Schmitt,
• O. Schneider,
• A. Schopper,
• M. Schubiger,
• S. Schulte,
• M.H. Schune,
• R. Schwemmer,
• B. Sciascia,
• S. Sellam,
• A. Semennikov,
• M. Senghi Soares,
• A. Sergi,
• N. Serra,
• L. Sestini,
• A. Seuthe,
• Y. Shang,
• D.M. Shangase,
• M. Shapkin,
• I. Shchemerov,
• L. Shchutska,
• T. Shears,
• L. Shekhtman,
• Z. Shen,
• S. Sheng,
• V. Shevchenko,
• E.B. Shields,
• Y. Shimizu,
• E. Shmanin,
• J.D. Shupperd,
• B.G. Siddi,
• R. Silva Coutinho,
• G. Simi,
• S. Simone,
• N. Skidmore,
• T. Skwarnicki,
• M.W. Slater,
• I. Slazyk,
• J.C.