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(269)Dislocations under gradient flow and their effect on the renormalized coupling
• Anna Hasenfratz,
• Oliver Witzel
Physical Review D, 103 (02/2021) doi:10.1103/PhysRevD.103.034505
abstract + abstract -

Nonzero topological charge is prohibited in the chiral limit of continuum gauge-fermion systems because any unpaired instanton would create a zero mode of the Dirac operator. On the lattice, however, the geometric Qgeom=⟨F F ∼ ⟩/32 π2 definition of the topological charge does not necessarily vanish in the chiral limit even when the gauge fields are smoothed for example with gradient flow. Small vacuum fluctuations (dislocations) not seen by the fermions may be promoted to instantonlike objects by the gradient flow. We demonstrate that these artifacts of the flow cause the gradient flow renormalized gauge coupling to increase and appear to run faster. In step-scaling studies such strong coupling artifacts contribute a term that might not follow perturbative scaling. The usual a /L →0 continuum limit extrapolations can hence lead to incorrect results. In this paper we investigate these topological lattice artifacts in the massless SU(3) 10-flavor system with domain wall fermions and the massless 8-flavor system with staggered fermions. For both systems we observe that in the range of strong coupling Symanzik gradient flow exhibits more lattice artifacts compared to Wilson gradient flow. We demonstrate how this artifact impacts the determination of the renormalized gauge coupling and the step-scaling β function.

(268)Symmetry energy investigation with pion production from Sn+Sn systems
• G. Jhang,
• J. Estee,
• J. Barney,
• G. Cerizza,
• M. Kaneko
• +76
• J. W. Lee,
• W. G. Lynch,
• T. Isobe,
• M. Kurata-Nishimura,
• T. Murakami,
• C. Y. Tsang,
• M. B. Tsang,
• R. Wang,
• D. S. Ahn,
• L. Atar,
• T. Aumann,
• H. Baba,
• K. Boretzky,
• J. Brzychczyk,
• N. Chiga,
• N. Fukuda,
• I. Gasparic,
• B. Hong,
• A. Horvat,
• K. Ieki,
• N. Inabe,
• Y. J. Kim,
• T. Kobayashi,
• Y. Kondo,
• H. S. Lee,
• Y. Leifels,
• J. Łukasik,
• J. Manfredi,
• A. B. McIntosh,
• P. Morfouace,
• T. Nakamura,
• N. Nakatsuka,
• S. Nishimura,
• R. Olsen,
• H. Otsu,
• P. Pawłowski,
• K. Pelczar,
• D. Rossi,
• H. Sakurai,
• C. Santamaria,
• H. Sato,
• H. Scheit,
• R. Shane,
• Y. Shimizu,
• H. Simon,
• A. Snoch,
• A. Sochocka,
• Z. Sosin,
• T. Sumikama,
• H. Suzuki,
• D. Suzuki,
• H. Takeda,
• S. Tangwancharoen,
• H. Toernqvist,
• Y. Togano,
• Z. G. Xiao,
• S. J. Yennello,
• J. Yurkon,
• Y. Zhang,
• Maria Colonna,
• Dan Cozma,
• Paweł Danielewicz,
• Hannah Elfner,
• Natsumi Ikeno,
• Che Ming Ko,
• Justin Mohs,
• Dmytro Oliinychenko,
• Akira Ono,
• Jun Su,
• Yong Jia Wang,
• Hermann Wolter,
• Jun Xu,
• Ying-Xun Zhang,
• Zhen Zhang,
• the SπRIT Collaboration
• (less)
Physics Letters B, 813 (02/2021) doi:10.1016/j.physletb.2020.136016
abstract + abstract -

In the past two decades, pions created in the high density regions of heavy ion collisions have been predicted to be sensitive at high densities to the symmetry energy term in the nuclear equation of state, a property that is key to our understanding of neutron stars. In a new experiment designed to study the symmetry energy, the multiplicities of negatively and positively charged pions have been measured with high accuracy for central 132Sn+124Sn, 112Sn+124Sn, and 108Sn+112Sn collisions at E / A = 270 MeV with the SπRIT Time Projection Chamber. While individual pion multiplicities are measured to 4% accuracy, those of the charged pion multiplicity ratios are measured to 2% accuracy. We compare these data to predictions from seven major transport models. The calculations reproduce qualitatively the dependence of the multiplicities and their ratios on the total neutron and proton number in the colliding systems. However, the predictions of the transport models from different codes differ too much to allow extraction of reliable constraints on the symmetry energy from the data. This finding may explain previous contradictory conclusions on symmetry energy constraints obtained from pion data in Au+Au system. These new results call for still better understanding of the differences among transport codes, and new observables that are more sensitive to the density dependence of the symmetry energy.

(267)Primordial gravitational waves in a minimal model of particle physics and cosmology
• Andreas Ringwald,
• Ken'ichi Saikawa,
• Carlos Tamarit
Journal of Cosmology and Astroparticle Physics, 2021 (02/2021) doi:10.1088/1475-7516/2021/02/046
abstract + abstract -

In this paper we analyze the spectrum of the primordial gravitational waves (GWs) predicted in the Standard Model*Axion*Seesaw*Higgs portal inflation (SMASH) model, which was proposed as a minimal extension of the Standard Model that addresses five fundamental problems of particle physics and cosmology (inflation, baryon asymmetry, neutrino masses, strong CP problem, and dark matter) in one stroke. The SMASH model has a unique prediction for the critical temperature of the second order Peccei-Quinn (PQ) phase transition Tc ~ 108 GeV up to the uncertainty in the calculation of the axion dark matter abundance, implying that there is a drastic change in the equation of state of the universe at that temperature. Such an event is imprinted on the spectrum of GWs originating from the primordial tensor fluctuations during inflation and entering the horizon at T ~ Tc, which corresponds to f ~ 1 Hz, pointing to a best frequency range covered by future space-borne GW interferometers. We give a precise estimation of the effective relativistic degrees of freedom across the PQ phase transition and use it to evaluate the spectrum of GWs observed today. It is shown that the future high sensitivity GW experiment—ultimate DECIGO—can probe the nontrivial feature resulting from the PQ phase transition in this model.

(266)Volume statistics as a probe of large-scale structure
• Kwan Chuen Chan,
• Nico Hamaus
Physical Review D, 103 (02/2021) doi:10.1103/PhysRevD.103.043502
abstract + abstract -

We investigate the application of volume statistics to probe the distribution of underdense regions in the large-scale structure of the Universe. This statistic measures the distortion of Eulerian volume elements relative to Lagrangian ones and can be built from tracer particles using tessellation methods. We apply Voronoi and Delaunay tessellation to study the clustering properties of density and volume statistics. Their level of shot-noise contamination is similar, as both methods take into account all available tracer particles in the field estimator. The tessellation causes a smoothing effect in the power spectrum, which can be approximated by a constant window function on large scales. The clustering bias of the volume statistic with respect to the dark matter density field is determined and found to be negative. We further identify the baryon acoustic oscillation (BAO) feature in the volume statistic. Apart from being smoothed out on small scales, the BAO is present in the volume power spectrum as well, without any systematic bias. These observations suggest that the exploitation of volume statistics as a complementary probe of cosmology is very promising.

(265)HOLISMOKES. III. Achromatic phase of strongly lensed Type Ia supernovae
• S. Huber,
• S. H. Suyu,
• U. M. Noebauer,
• J. H. H. Chan,
• M. Kromer
• +3
• S. A. Sim,
• D. Sluse,
• S. Taubenberger
• (less)
Astronomy and Astrophysics, 646, p16 (02/2021) doi:10.1051/0004-6361/202039218
abstract + abstract -

To use strongly lensed Type Ia supernovae (LSNe Ia) for cosmology, a time-delay measurement between the multiple supernova (SN) images is necessary. The sharp rise and decline of SN Ia light curves make them promising for measuring time delays, but microlensing can distort these light curves and therefore add large uncertainties to the measurements. An alternative approach is to use color curves where uncertainties due to microlensing are significantly reduced for a certain period of time known as the achromatic phase. In this work, we investigate in detail the achromatic phase, testing four different SN Ia models with various microlensing configurations. We find on average an achromatic phase of around three rest-frame weeks or longer for most color curves, but the spread in the duration of the achromatic phase (due to different microlensing maps and filter combinations) is quite large and an achromatic phase of just a few days is also possible. Furthermore, the achromatic phase is longer for smoother microlensing maps and lower macro-magnifications. From our investigations, we do not find a strong dependency on the SN model or on asymmetries in the SN ejecta. We find that six rest-frame LSST color curves exhibit features such as extreme points or turning points within the achromatic phase, which make them promising for time-delay measurements; however, only three of the color curves are independent. These curves contain combinations of rest-frame bands u, g, r, and i, and to observe them for typical LSN Ia redshifts, it would be ideal to cover (observer-frame) filters r, i, z, y, J, and H. If follow-up resources are restricted, we recommend r, i, and z as the bare minimum for using color curves and/or light curves since LSNe Ia are bright in these filters and observational uncertainties are lower than in the infrared regime. With additional resources, infrared observations in y, J, and H would be useful for obtaining color curves of SNe, especially at redshifts above ∼0.8 when they become critical.

(264)Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): Late Infall Causing Disk Misalignment and Dynamic Structures in SU Aur
• Christian Ginski,
• Stefano Facchini,
• Jane Huang,
• Myriam Benisty,
• Dennis Vaendel
• +17
• Lucas Stapper,
• Carsten Dominik,
• Jaehan Bae,
• François Ménard,
• Gabriela Muro-Arena,
• Michiel R. Hogerheijde,
• Melissa McClure,
• Rob G. van Holstein,
• Tilman Birnstiel,
• Yann Boehler,
• Alexander Bohn,
• Mario Flock,
• Eric E. Mamajek,
• Carlo F. Manara,
• Paola Pinilla,
• Christophe Pinte,
• Álvaro Ribas
• (less)
The Astrophysical Journal, 908, p13 (02/2021) doi:10.3847/2041-8213/abdf57
abstract + abstract -

Gas-rich circumstellar disks are the cradles of planet formation. As such, their evolution will strongly influence the resulting planet population. In the ESO DESTINYS large program, we study these disks within the first 10 Myr of their development with near-infrared scattered-light imaging. Here we present VLT/SPHERE polarimetric observations of the nearby class II system SU Aur in which we resolve the disk down to scales of ∼7 au. In addition to the new SPHERE observations, we utilize VLT/NACO, HST/STIS, and ALMA archival data. The new SPHERE data show the disk around SU Aur and extended dust structures in unprecedented detail. We resolve several dust tails connected to the Keplerian disk. By comparison with ALMA data, we show that these dust tails represent material falling onto the disk. The disk itself shows an intricate spiral structure and a shadow lane, cast by an inner, misaligned disk component. Our observations suggest that SU Aur is undergoing late infall of material, which can explain the observed disk structures. SU Aur is the clearest observational example of this mechanism at work and demonstrates that late accretion events can still occur in the class II phase, thereby significantly affecting the evolution of circumstellar disks. Constraining the frequency of such events with additional observations will help determine whether this process is responsible for the spin-orbit misalignment in evolved exoplanet systems. * Based on observations performed with VLT/SPHERE under program ID 1104.C-0415(E).

(263)Inclusive Hadroproduction of P -Wave Heavy Quarkonia in Potential Nonrelativistic QCD
• Nora Brambilla,
• Hee Sok Chung,
• Antonio Vairo
Physical Review Letters, 126 (02/2021) doi:10.1103/PhysRevLett.126.082003
abstract + abstract -

We compute the color-singlet and color-octet nonrelativistic QCD (NRQCD) long-distance matrix elements for inclusive production of P -wave quarkonia in the framework of potential NRQCD. In this way, the color-octet NRQCD long-distance matrix element can be determined without relying on measured cross section data, which has not been possible so far. We obtain inclusive cross sections of χc J and χb J at the LHC, which are in good agreement with data. In principle, the formalism developed in this Letter can be applied to all inclusive production processes of heavy quarkonia.

(262)Scaling relations of fuzzy dark matter haloes - I. Individual systems in their cosmological environment
• Matteo Nori,
• Marco Baldi
Monthly Notices of the Royal Astronomical Society, 501, p18 (02/2021) doi:10.1093/mnras/staa3772
abstract + abstract -

Dark matter models involving a very light bosonic particle, generally known as fuzzy dark matter (FDM), have been recently attracting great interest in the cosmology community, as their wave-like phenomenology would simultaneously explain the long-standing misdetection of a dark matter particle and help easing the small-scale issues related to the standard cold dark matter (CDM) scenario. With this work, we initiate a series of papers aiming at investigating the evolution of FDM structures in a cosmological framework performed with our N-body code AX-GADGET, detailing for the first time in the literature how the actual scaling relations between solitonic cores and host haloes properties are significantly affected by the dynamical state, morphology, and merger history of the individual systems. In particular, in this first paper we confirm the ability of AX-GADGET to correctly reproduce the typical FDM solitonic core and we employ it to study the non-linear evolution of eight FDM haloes in their cosmological context through the zoom-in simulation approach. We find that the scaling relations identified in previous works for isolated systems are generally modified for haloes evolving in a realistic cosmological environment, and appear to be valid only as a limit for the most relaxed and spherically symmetric systems.

(261)Dibaryons: Molecular versus compact hexaquarks
• H. Clement,
• T. Skorodko
Chinese Physics C, 45, p16 (02/2021) doi:10.1088/1674-1137/abcd8e
abstract + abstract -

Hexaquarks constitute a natural extension of complex quark systems, just as tetra- and pentaquarks do. To this end, the current status of $d^*(2380)$ in both experiment and theory is reviewed. Recent high-precision measurements in the nucleon-nucleon channel and analyses thereof have established $d^*(2380)$ as an indisputable resonance in the long-sought dibaryon channel. Important features of this $I(J^P) = 0(3^+)$ state are its narrow width and deep binding relative to the $\Delta(1232)\Delta(1232)$ threshold. Its decay branchings favor theoretical calculations predicting a compact hexaquark nature of this state. We review the current status of experimental and theoretical studies on $d^*(2380)$ as well as new physics aspects it may bring in future. In addition, we review the situation at the $\Delta(1232) N$ and $N^*(1440)N$ thresholds, where evidence for a number of resonances of presumably molecular nature has been found - similar to the situation in charmed and beauty sectors. Finally, we briefly discuss the situation of dibaryon searches in the flavored quark sectors. * This work has been supported by DFG (CL 214/3-3). H. Cl. appreciates the support by the Munich Institute for Astro- and Particle Physics (MIAPP) which is funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany's Excellence Strategy - EXC-2094 - 390783311

(260)Giant planet migration during the disc dispersal phase
• Kristina Monsch,
• Giovanni Picogna,
• Barbara Ercolano,
• Wilhelm Kley
Astronomy and Astrophysics, 646, p15 (02/2021) doi:10.1051/0004-6361/202039658
abstract + abstract -

Context. Transition discs are expected to be a natural outcome of the interplay between photoevaporation and giant planet formation. Massive planets reduce the inflow of material from the outer to the inner disc, therefore triggering an earlier onset of disc dispersal due to photoevaporation through a process known as Planet-Induced PhotoEvaporation. In this case, a cavity is formed as material inside the planetary orbit is removed by photoevaporation, leaving only the outer disc to drive the migration of the giant planet.
Aims: We investigate the impact of photoevaporation on giant planet migration and focus specifically on the case of transition discs with an evacuated cavity inside the planet location. This is important for determining under what circumstances photoevaporation is efficient at halting the migration of giant planets, thus affecting the final orbital distribution of a population of planets.
Methods: For this purpose, we use 2D FARGO simulations to model the migration of giant planets in a range of primordial and transition discs subject to photoevaporation. The results are then compared to the standard prescriptions used to calculate the migration tracks of planets in 1D planet population synthesis models.
Results: The FARGO simulations show that once the disc inside the planet location is depleted of gas, planet migration ceases. This contradicts the results obtained by the impulse approximation, which predicts the accelerated inward migration of planets in discs that have been cleared inside the planetary orbit.
Conclusions: These results suggest that the impulse approximation may not be suitable for planets embedded in transition discs. A better approximation that could be used in 1D models would involve halting planet migration once the material inside the planetary orbit is depleted of gas and the surface density at the 3:2 mean motion resonance location in the outer disc reaches a threshold value of 0.01 g cm−2.

(259)Fission fragment distributions and their impact on the r -process nucleosynthesis in neutron star mergers
• J. -F. Lemaître,
• S. Goriely,
• A. Bauswein,
• H. -T. Janka
Physical Review C, 103 (02/2021) doi:10.1103/PhysRevC.103.025806
abstract + abstract -

Neutron star (NS) merger ejecta offer viable sites for the production of heavy r -process elements with nuclear mass numbers A ≳140 . The crucial role of fission recycling is responsible for the robustness of this site against many astrophysical uncertainties. Here, we introduce improvements to our scission-point model, called SPY, to derive the fission fragment distribution for all neutron-rich fissioning nuclei of relevance in r -process calculations. These improvements include a phenomenological modification of the scission distance and a smoothing procedure of the distribution. Such corrections lead to much better agreement with experimental fission yields. Those yields are also used to estimate the number of neutrons emitted by the excited fragments on the basis of different neutron evaporation models. Our fission yields are extensively compared to those predicted by the GEF (general description of fission observables) model. The impact of fission on the r -process nucleosynthesis in binary neutron mergers is also reanalyzed. Two scenarios are considered, the first one with low initial electron fraction subject to intense fission recycling, in contrast to the second one, which includes weak interactions on nucleons. The various regions of the nuclear chart responsible for fission recycling during the neutron irradiation and after freeze-out are discussed. The contribution fission processes may have to the final abundance distribution is also studied in detail in the light of newly defined quantitative indicators describing the fission recycling, the fission seeds, and the fission progenitors. In particular, those allow us to estimate the contribution of fission to the final abundance distribution stemming from specific heavy nuclei. Calculations obtained with SPY and GEF fission fragment distributions are compared for both r -process scenarios.

(258)HOLISMOKES. IV. Efficient mass modeling of strong lenses through deep learning
• S. Schuldt,
• S. H. Suyu,
• T. Meinhardt,
• L. Leal-Taixé,
• R. Cañameras
• +2
Astronomy and Astrophysics, 646, p17 (02/2021) doi:10.1051/0004-6361/202039574
abstract + abstract -

Modeling the mass distributions of strong gravitational lenses is often necessary in order to use them as astrophysical and cosmological probes. With the large number of lens systems (≳105) expected from upcoming surveys, it is timely to explore efficient modeling approaches beyond traditional Markov chain Monte Carlo techniques that are time consuming. We train a convolutional neural network (CNN) on images of galaxy-scale lens systems to predict the five parameters of the singular isothermal ellipsoid (SIE) mass model (lens center x and y, complex ellipticity ex and ey, and Einstein radius θE). To train the network we simulate images based on real observations from the Hyper Suprime-Cam Survey for the lens galaxies and from the Hubble Ultra Deep Field as lensed galaxies. We tested different network architectures and the effect of different data sets, such as using only double or quad systems defined based on the source center and using different input distributions of θE. We find that the CNN performs well, and with the network trained on both doubles and quads with a uniform distribution of θE > 0.5″ we obtain the following median values with 1σ scatter: Δx = (0.00-0.30+0.30)″, Δy = (0.00-0.29+0.30)″, ΔθE = (0.07-0.12+0.29)″, Δex = -0.01-0.09+0.08, and Δey = 0.00-0.09+0.08. The bias in θE is driven by systems with small θE. Therefore, when we further predict the multiple lensed image positions and time-delays based on the network output, we apply the network to the sample limited to θE > 0.8″. In this case the offset between the predicted and input lensed image positions is (0.00-0.29+0.29)″ and (0.00-0.31+0.32)″ for the x and y coordinates, respectively. For the fractional difference between the predicted and true time-delay, we obtain 0.04-0.05+0.27. Our CNN model is able to predict the SIE parameter values in fractions of a second on a single CPU, and with the output we can predict the image positions and time-delays in an automated way, such that we are able to process efficiently the huge amount of expected galaxy-scale lens detections in the near future.

(257)On the Use of Field RR Lyrae as Galactic Probes. II. A New ΔS Calibration to Estimate Their Metallicity
• J. Crestani,
• M. Fabrizio,
• V. F. Braga,
• C. Sneden,
• G. Preston
• +31
• I. Ferraro,
• G. Iannicola,
• G. Bono,
• A. Alves-Brito,
• M. Nonino,
• V. D'Orazi,
• L. Inno,
• M. Monelli,
• J. Storm,
• G. Altavilla,
• B. Chaboyer,
• M. Dall'Ora,
• G. Fiorentino,
• C. Gilligan,
• E. K. Grebel,
• H. Lala,
• B. Lemasle,
• M. Marengo,
• S. Marinoni,
• P. M. Marrese,
• C. E. Martínez-Vázquez,
• N. Matsunaga,
• J. P. Mullen,
• J. Neeley,
• Z. Prudil,
• R. da Silva,
• P. B. Stetson,
• F. Thévenin,
• E. Valenti,
• A. Walker,
• M. Zoccali
• (less)
The Astrophysical Journal, 908, p19 (02/2021) doi:10.3847/1538-4357/abd183
abstract + abstract -

We performed the largest and most homogeneous spectroscopic survey of field RR Lyraes (RRLs). We secured ≍6300 high-resolution (HR, R ∼ 35,000) spectra for 143 RRLs (111 fundamental, RRab; 32 first-overtone, RRc). The atmospheric parameters were estimated by using the traditional approach and the iron abundances were measured by using an LTE line analysis. The resulting iron distribution shows a well-defined metal-rich tail approaching solar iron abundance. This suggests that field RRLs experienced a complex chemical enrichment in the early halo formation. We used these data to develop a new calibration of the ΔS method. This diagnostic, based on the equivalent widths of Ca II K and three Balmer (Hδ,γ,β) lines, traces the metallicity of RRLs. For the first time, the new empirical calibration: (i) includes spectra collected over the entire pulsation cycle; (ii) includes RRc variables; (iii) relies on spectroscopic calibrators covering more than three dex in iron abundance; and (iv) provides independent calibrations based on one/two/three Balmer lines. The new calibrations were applied to a data set of both SEGUE-SDSS and degraded HR spectra totalling 6451 low-resolution (R ∼ 2000) spectra for 5001 RRLs (3439 RRab, 1562 RRc). This resulted in an iron distribution with a median η = -1.55 ± 0.01 and σ = 0.51 dex, in good agreement with literature values. We also found that RRc are 0.10 dex more metal-poor than RRab variables, and have a distribution with a smoother metal-poor tail. This finding supports theoretical prescriptions suggesting a steady decrease in the RRc number when moving from metal-poor to metal-rich stellar environments. * Based on observations obtained with the du Pont telescope at Las Campanas Observatory, operated by Carnegie Institution for Science. Based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. Based partly on data obtained with the STELLA robotic telescopes in Tenerife, an AIP facility jointly operated by AIP and IAC. Some of the observations reported in this paper were obtained with the Southern African Large Telescope (SALT). Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere.

(256)KiDS-1000 methodology: Modelling and inference for joint weak gravitational lensing and spectroscopic galaxy clustering analysis
• B. Joachimi,
• C. -A. Lin,
• M. Asgari,
• T. Tröster,
• C. Heymans
• +22
• H. Hildebrandt,
• F. Köhlinger,
• A. G. Sánchez,
• A. H. Wright,
• M. Bilicki,
• C. Blake,
• J. L. van den Busch,
• M. Crocce,
• A. Dvornik,
• T. Erben,
• F. Getman,
• B. Giblin,
• H. Hoekstra,
• K. Kuijken,
• N. R. Napolitano,
• P. Schneider,
• R. Scoccimarro,
• E. Sellentin,
• H. Y. Shan,
• M. von Wietersheim-Kramsta,
• J. Zuntz
• (less)
Astronomy and Astrophysics, 646, p44 (02/2021) doi:10.1051/0004-6361/202038831
abstract + abstract -

We present the methodology for a joint cosmological analysis of weak gravitational lensing from the fourth data release of the ESO Kilo-Degree Survey (KiDS-1000) and galaxy clustering from the partially overlapping Baryon Oscillation Spectroscopic Survey (BOSS) and the 2-degree Field Lensing Survey (2dFLenS). Cross-correlations between BOSS and 2dFLenS galaxy positions and source galaxy ellipticities have been incorporated into the analysis, necessitating the development of a hybrid model of non-linear scales that blends perturbative and non-perturbative approaches, and an assessment of signal contributions by astrophysical effects. All weak lensing signals were measured consistently via Fourier-space statistics that are insensitive to the survey mask and display low levels of mode mixing. The calibration of photometric redshift distributions and multiplicative gravitational shear bias has been updated, and a more complete tally of residual calibration uncertainties was propagated into the likelihood. A dedicated suite of more than 20 000 mocks was used to assess the performance of covariance models and to quantify the impact of survey geometry and spatial variations of survey depth on signals and their errors. The sampling distributions for the likelihood and the χ2 goodness-of-fit statistic have been validated, with proposed changes for calculating the effective number of degrees of freedom. The prior volume was explicitly mapped, and a more conservative, wide top-hat prior on the key structure growth parameter S8 = σ8m/0.3)1/2 was introduced. The prevalent custom of reporting S8 weak lensing constraints via point estimates derived from its marginal posterior is highlighted to be easily misinterpreted as yielding systematically low values of S8, and an alternative estimator and associated credible interval are proposed. Known systematic effects pertaining to weak lensing modelling and inference are shown to bias S8 by no more than 0.1 standard deviations, with the caveat that no conclusive validation data exist for models of intrinsic galaxy alignments. Compared to the previous KiDS analyses, S8 constraints are expected to improve by 20% for weak lensing alone and by 29% for the joint analysis.

(255)Multipole expansion of gravitational waves: from harmonic to Bondi coordinates
• Luc Blanchet,
• Geoffrey Compère,
• Guillaume Faye,
• Roberto Oliveri,
• Ali Seraj
Journal of High Energy Physics, 2021 (02/2021) doi:10.1007/JHEP02(2021)029
abstract + abstract -

We transform the metric of an isolated matter source in the multipolar post-Minkowskian approximation from harmonic (de Donder) coordinates to radiative Newman-Unti (NU) coordinates. To linearized order, we obtain the NU metric as a functional of the mass and current multipole moments of the source, valid all-over the exterior region of the source. Imposing appropriate boundary conditions we recover the generalized Bondi-van der Burg-Metzner-Sachs residual symmetry group. To quadratic order, in the case of the mass-quadrupole interaction, we determine the contributions of gravitational-wave tails in the NU metric, and prove that the expansion of the metric in terms of the radius is regular to all orders. The mass and angular momentum aspects, as well as the Bondi shear, are read off from the metric. They are given by the radiative quadrupole moment including the tail terms.

(254)Neutrino parameters in the Planck-scale lepton number breaking scenario with extended scalar sectors
• Cesar Bonilla,
• Johannes Herms,
• Alejandro Ibarra,
• Patrick Strobl
Physical Review D, 103 (02/2021) doi:10.1103/PhysRevD.103.035010
abstract + abstract -

Two-loop effects on the right-handed neutrino masses can have an impact on the low-energy phenomenology, especially when the right-handed neutrino mass spectrum is very hierarchical at the cutoff scale. In this case, the physical masses of the lighter right-handed neutrinos can be dominated by quantum effects induced by the heavier ones. Further, if the heaviest right-handed neutrino mass is at around the Planck scale, two-loop effects on the right-handed neutrino masses generate, through the seesaw mechanism, an active neutrino mass that is in the ballpark of the experimental values. In this paper we investigate extensions of the Planck-scale lepton number breaking scenario by additional Higgs doublets (inert or not). We find that under reasonable assumptions these models lead simultaneously to an overall neutrino mass scale and to a neutrino mass hierarchy in qualitative agreement with observations.

(253)ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT). V. Sample, overview, and demography of disk molecular emission
• A. Garufi,
• L. Podio,
• C. Codella,
• D. Fedele,
• E. Bianchi
• +7
• C. Favre,
• F. Bacciotti,
• C. Ceccarelli,
• S. Mercimek,
• K. Rygl,
• R. Teague,
• L. Testi
• (less)
Astronomy and Astrophysics, 645, p16 (01/2021) doi:10.1051/0004-6361/202039483
abstract + abstract -

We present an overview of the ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT), a campaign devoted to the characterization of the molecular emission from partly embedded young stars. The project is aimed at attaining a better understanding of the gaseous products delivered to planets by means of high-resolution maps of the assorted lines probing disks at the time of planet formation (≲1 Myr). Nine different molecules are surveyed through our observations of six Class I/flat-spectrum sources. As part of a series of articles analyzing specific targets and molecules, in this work we describe the sample and provide a general overview of the results, focusing specifically on the spatial distribution, column densities, and abundance ratios of H2CO, CS, and CN. In these embedded sources, the 12CO emission is dominated by envelope and outflow emission while the CS and, especially, the H2CO are good tracers of the gaseous disk structure. The spatial distribution and brightness of the o-H2CO 31,2-21,1 and CS 5-4 lines are very similar to each other and across all targets. The CN 2-1 line emission is fainter and distributed over radii larger than the dust continuum. The H2CO and CS emission is always dimmed in the inner ~50 au. While the suppression by the dusty disk and absorption by the line-of-sight material significantly contributes to this inner depression, an actual decrease in the column density is plausible in most cases, making the observed ring-like morphology realistic. We also found that the gaseous disk extent, when traced by H2CO (150-390 au), is always 60% larger than the dust disk. This systematic discrepancy may, in principle, be explained by the different optical depth of continuum and line emission without invoking any dust radial drift. Finally, the o-H2CS 71,6-61,5 and CH3OH 50,5-40,4 line emission are detected in two disks and one disk, respectively, while the HDO is never detected. The H2CO column densities are 12-50 times larger than those inferred for Class II sources while they are in line with those of other Class 0/I. The CS column densities are lower than those of H2CO, which is an opposite trend with regard to Class II objects. We also inferred abundance ratios between the various molecular species finding, among others, a H2CS/H2CO ratio that is systematically lower than unity (0.4-0.7 in HL Tau, 0.1 - 0.2 in IRAS 04302+2247, and <0.4 in all other sources), as well as a CH3OH/H2CO ratio (<0.7 in HL Tau and 0.5-0.7 in IRAS 04302+2247) that is lower than the only available estimate in a protoplanetary disks (1.3 in TW Hya) and between one and two orders of magnitude lower than those of the hot corinos around Class 0 protostars. These results are a first step toward the characterization of the disk's chemical evolution, which ought to be complemented by subsequent observations of less exceptional disks and customized thermo-chemical modeling.

(252)Exploring the contamination of the DES-Y1 Cluster Sample with SPT-SZ selected clusters
• S. Grandis,
• J.J. Mohr,
• M. Costanzi,
• A. Saro,
• S. Bocquet
• +71
• M. Klein,
• M. Aguena,
• S. Allam,
• J. Annis,
• D. Bacon,
• E. Bertin,
• L. Bleem,
• D. Brooks,
• D.L. Burke,
• A. Carnero Rosel,
• M. Carrasco Kind,
• J. Carretero,
• F.J. Castander,
• A. Choi,
• L.N. da Costa,
• J. De Vincente,
• S. Desai,
• H.T. Diehl,
• J.P. Dietrich,
• P. Doel,
• T.F. Eifler,
• S. Everett,
• I. Ferrero,
• B. Floyd,
• P. Fosalba,
• J. Frieman,
• J. García-Bellido,
• E. Gaztanaga,
• D. Gruen,
• R.A. Gruendl,
• J. Gschwend,
• N. Gupta,
• G. Gutierrez,
• S.R. Hinton,
• D.L. Hollowood,
• K. Honscheid,
• D.J. James,
• T. Jeltema,
• K. Kuehn,
• O. Lahav,
• C. Lidman,
• M. Lima,
• M.A G. Maia,
• M. March,
• J.L. Marshall,
• P. Melchior,
• F. Menanteau,
• R. Miquel,
• R. Morgan,
• J. Myles,
• R. Ogando,
• A. Palmese,
• F. Paz-Chinchón,
• A.A. Plazas,
• C.L. Reichardt,
• A.K. Romer,
• E. Sanchez,
• V. Scarpine,
• S. Serrano,
• I. Sevilla-Noarbe,
• P. Singh,
• M. Smith,
• E. Suchyta,
• M.E C. Swanson,
• G. Tarle,
• D. Thomas,
• C. To,
• J. Weller,
• R.D. Wilkinson,
• H. Wu
• (less)
Mon.Not.Roy.Astron.Soc., 504, p1253 (01/2021) e-Print:2101.04984 doi:10.1093/mnras/stab869
abstract + abstract -

We perform a cross validation of the cluster catalogue selected by the red-sequence Matched-filter Probabilistic Percolation algorithm (redMaPPer) in Dark Energy Survey year 1 (DES-Y1) data by matching it with the Sunyaev–Zel’dovich effect (SZE) selected cluster catalogue from the South Pole Telescope SPT-SZ survey. Of the 1005 redMaPPer selected clusters with measured richness |$\hat{\lambda }\gt 40$| in the joint footprint, 207 are confirmed by SPT-SZ. Using the mass information from the SZE signal, we calibrate the richness–mass relation using a Bayesian cluster population model. We find a mass trend λ ∝ M^B consistent with a linear relation (B ∼ 1), no significant redshift evolution and an intrinsic scatter in richness of σ_λ = 0.22 ± 0.06. By considering two error models, we explore the impact of projection effects on the richness–mass modelling, confirming that such effects are not detectable at the current level of systematic uncertainties. At low richness SPT-SZ confirms fewer redMaPPer clusters than expected. We interpret this richness dependent deficit in confirmed systems as due to the increased presence at low richness of low-mass objects not correctly accounted for by our richness-mass scatter model, which we call contaminants. At a richness |$\hat{\lambda }=40$|⁠, this population makes up |${\gt}12{{\ \rm per\ cent}}$| (97.5 percentile) of the total population. Extrapolating this to a measured richness |$\hat{\lambda }=20$| yields |${\gt}22{{\ \rm per\ cent}}$| (97.5 percentile). With these contamination fractions, the predicted redMaPPer number counts in different plausible cosmologies are compatible with the measured abundance. The presence of such a population is also a plausible explanation for the different mass trends (B ∼ 0.75) obtained from mass calibration using purely optically selected clusters. The mean mass from stacked weak lensing (WL) measurements suggests that these low-mass contaminants are galaxy groups with masses ∼3–5 × 10^13 M_⊙ which are beyond the sensitivity of current SZE and X-ray surveys but a natural target for SPT-3G and eROSITA.

(251)CODEX Weak Lensing Mass Catalogue and implications on the mass-richness relation
• K. Kiiveri,
• D. Gruen,
• A. Finoguenov,
• T. Erben,
• L. van Waerbeke
• +17
• E. Rykoff,
• L. Miller,
• S. Hagstotz,
• R. Dupke,
• J. Patrick Henry,
• J-P. Kneib,
• G. Gozaliasl,
• C.C. Kirkpatrick,
• N. Cibirka,
• N. Clerc,
• M. Costanzi,
• E.S. Cypriano,
• E. Rozo,
• H. Shan,
• P. Spinelli,
• J. Valiviita,
• J. Weller
• (less)
Mon.Not.Roy.Astron.Soc., 502, p1494 (01/2021) e-Print:2101.02257 doi:10.1093/mnras/staa3936
abstract + abstract -

The COnstrain Dark Energy with X-ray clusters (CODEX) sample contains the largest flux limited sample of X-ray clusters at $0.35 < z < 0.65$. It was selected from ROSAT data in the 10,000 square degrees of overlap with BOSS, mapping a total number of 2770 high-z galaxy clusters. We present here the full results of the CFHT CODEX program on cluster mass measurement, including a reanalysis of CFHTLS Wide data, with 25 individual lensing-constrained cluster masses. We employ $lensfit$ shape measurement and perform a conservative colour-space selection and weighting of background galaxies. Using the combination of shape noise and an analytic covariance for intrinsic variations of cluster profiles at fixed mass due to large scale structure, miscentring, and variations in concentration and ellipticity, we determine the likelihood of the observed shear signal as a function of true mass for each cluster. We combine 25 individual cluster mass likelihoods in a Bayesian hierarchical scheme with the inclusion of optical and X-ray selection functions to derive constraints on the slope $\alpha$, normalization $\beta$, and scatter $\sigma_{\ln \lambda | \mu}$ of our richness-mass scaling relation model in log-space: $\left<\ln \lambda | \mu \right> = \alpha \mu + \beta$, with $\mu = \ln (M_{200c}/M_{\mathrm{piv}})$, and $M_{\mathrm{piv}} = 10^{14.81} M_{\odot}$. We find a slope $\alpha = 0.49^{+0.20}_{-0.15}$, normalization $\exp(\beta) = 84.0^{+9.2}_{-14.8}$ and $\sigma_{\ln \lambda | \mu} = 0.17^{+0.13}_{-0.09}$ using CFHT richness estimates. In comparison to other weak lensing richness-mass relations, we find the normalization of the richness statistically agreeing with the normalization of other scaling relations from a broad redshift range ($0.0<z<0.65$) and with different cluster selection (X-ray, Sunyaev-Zeldovich, and optical).

(250)Detector fabrication development for the LiteBIRD satellite mission
• Benjamin Westbrook,
• Christopher Raum,
• Shawn Beckman,
• Nicole Farias
• +22
• Trevor Sasse,
• Aritoki Suzuki,
• Elijah Kane,
• Jason E. Austermann,
• James A Beall,
• Shannon M. Duff,
• Johannes Hubmayr,
• Gene C. Hilton,
• Jeff Van Lanen,
• Michael R. Vissers,
• Greg Jaehnig,
• Nils Halverson,
• Tommaso Ghinga,
• Samantha Stever,
• Yuto Minami,
• Keith L. Thompson,
• Megan Russell,
• Kam Arnold,
• Joseph Siebert,
• Maximiliano Silva-Feaver,
• the LiteBIRD Joint Study Group
• (less)
arXiv e-prints (01/2021) e-Print:2101.05306
abstract + abstract -

LiteBIRD is a JAXA-led strategic Large-Class satellite mission designed to measure the polarization of the cosmic microwave background and cosmic foregrounds from 34 to 448 GHz across the entire sky from L2 in the late 2020's. The primary focus of the mission is to measure primordially generated B-mode polarization at large angular scales. Beyond its primary scientific objective LiteBIRD will generate a data-set capable of probing a number of scientific inquiries including the sum of neutrino masses. The primary responsibility of United States will be to fabricate the three flight model focal plane units for the mission. The design and fabrication of these focal plane units is driven by heritage from ground based experiments and will include both lenslet-coupled sinuous antenna pixels and horn-coupled orthomode transducer pixels. The experiment will have three optical telescopes called the low frequency telescope, mid frequency telescope, and high frequency telescope each of which covers a portion of the mission's frequency range. JAXA is responsible for the construction of the low frequency telescope and the European Consortium is responsible for the mid- and high- frequency telescopes. The broad frequency coverage and low optical loading conditions, made possible by the space environment, require development and adaptation of detector technology recently deployed by other cosmic microwave background experiments. This design, fabrication, and characterization will take place at UC Berkeley, NIST, Stanford, and Colorado University, Boulder. We present the current status of the US deliverables to the LiteBIRD mission.

(249)Redshift-space effects in voids and their impact on cosmological tests. Part I: the void size function
• Carlos M. Correa,
• Dante J. Paz,
• Ariel G. Sánchez,
• Andrés N. Ruiz,
• +1
Monthly Notices of the Royal Astronomical Society, 500, p15 (01/2021) doi:10.1093/mnras/staa3252
abstract + abstract -

Voids are promising cosmological probes. Nevertheless, every cosmological test based on voids must necessarily employ methods to identify them in redshift space. Therefore, redshift-space distortions (RSD) and the Alcock-Paczyński effect (AP) have an impact on the void identification process itself generating distortion patterns in observations. Using a spherical void finder, we developed a statistical and theoretical framework to describe physically the connection between the identification in real and redshift space. We found that redshift-space voids above the shot noise level have a unique real-space counterpart spanning the same region of space, they are systematically bigger and their centres are preferentially shifted along the line of sight. The expansion effect is a by-product of RSD induced by tracer dynamics at scales around the void radius, whereas the off-centring effect constitutes a different class of RSD induced at larger scales by the global dynamics of the whole region containing the void. The volume of voids is also altered by the fiducial cosmology assumed to measure distances, this is the AP change of volume. These three systematics have an impact on cosmological statistics. In this work, we focus on the void size function. We developed a theoretical framework to model these effects and tested it with a numerical simulation, recovering the statistical properties of the abundance of voids in real space. This description depends strongly on cosmology. Hence, we lay the foundations for improvements in current models of the abundance of voids in order to obtain unbiased cosmological constraints from redshift surveys.

(248)Learning multivariate new physics
• Raffaele Tito D'Agnolo,
• Gaia Grosso,
• Maurizio Pierini,
• Andrea Wulzer,
• Marco Zanetti
European Physical Journal C, 81 (01/2021) doi:10.1140/epjc/s10052-021-08853-y
abstract + abstract -

We discuss a method that employs a multilayer perceptron to detect deviations from a reference model in large multivariate datasets. Our data analysis strategy does not rely on any prior assumption on the nature of the deviation. It is designed to be sensitive to small discrepancies that arise in datasets dominated by the reference model. The main conceptual building blocks were introduced in D'Agnolo and Wulzer (Phys Rev D 99 (1), 015014. doi.org/10.1103/PhysRevD.99.015014. arXiv:1806.02350 [hep-ph], 2019). Here we make decisive progress in the algorithm implementation and we demonstrate its applicability to problems in high energy physics. We show that the method is sensitive to putative new physics signals in di-muon final states at the LHC. We also compare our performances on toy problems with the ones of alternative methods proposed in the literature.

(247)Measuring the spectrum of primordial gravitational waves with CMB, PTA and laser interferometers
• Paolo Campeti,
• Eiichiro Komatsu,
• Davide Poletti,
• Carlo Baccigalupi
Journal of Cosmology and Astroparticle Physics, 2021 (01/2021) doi:10.1088/1475-7516/2021/01/012
abstract + abstract -

We investigate the possibility of measuring the primordial gravitational wave (GW) signal across 21 decades in frequencies, using the cosmic microwave background (CMB), pulsar timing arrays (PTA), and laser and atomic interferometers. For the CMB and PTA experiments we consider the LiteBIRD mission and the Square Kilometer Array (SKA), respectively. For the interferometers we consider space mission proposals including the Laser Interferometer Space Antenna (LISA), the Big Bang Observer (BBO), the Deci-hertz Interferometer Gravitational wave Observatory (DECIGO), the μAres experiment, the Decihertz Observatory (DO), and the Atomic Experiment for Dark Matter and Gravity Exploration in Space (AEDGE), as well as the ground-based Einstein Telescope (ET) proposal. We implement the mathematics needed to compute sensitivities for both CMB and interferometers, and derive the response functions for the latter from the first principles. We also evaluate the effect of the astrophysical foreground contamination in each experiment. We present binned sensitivity curves and error bars on the energy density parameter, ΩGWh2, as a function of frequency for two representative classes of models for the stochastic background of primordial GW: the quantum vacuum fluctuation in the metric from single-field slow-roll inflation, and the source-induced tensor perturbation from the spectator axion-SU(2) inflation models. We find excellent prospects for joint measurements of the GW spectrum by CMB and space-borne interferometers mission proposals.

(246)The completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: BAO and RSD measurements from anisotropic clustering analysis of the quasar sample in configuration space between redshift 0.8 and 2.2
• Jiamin Hou,
• Ariel G. Sánchez,
• Ashley J. Ross,
• Alex Smith,
• Richard Neveux
• +25
• Julian Bautista,
• Etienne Burtin,
• Cheng Zhao,
• Román Scoccimarro,
• Kyle S. Dawson,
• Arnaud de Mattia,
• Axel de la Macorra,
• Hélion du Mas des Bourboux,
• Daniel J. Eisenstein,
• Héctor Gil-Marín,
• Eva-Maria Mueller,
• Will J. Percival,
• Graziano Rossi,
• Mariana Vargas Magaña,
• Pauline Zarrouk,
• Gong-Bo Zhao,
• Jonathan Brinkmann,
• Joel R. Brownstein,
• Chia-Hsun Chuang,
• Jeffrey A. Newman,
• Donald P. Schneider,
• M. Vivek
• (less)
Monthly Notices of the Royal Astronomical Society, 500, p21 (01/2021) doi:10.1093/mnras/staa3234
abstract + abstract -

We measure the anisotropic clustering of the quasar sample from Data Release 16 (DR16) of the Sloan Digital Sky Survey IV extended Baryon Oscillation Spectroscopic Survey (eBOSS). A sample of 343 708 spectroscopically confirmed quasars between redshift 0.8 < z < 2.2 are used as tracers of the underlying dark matter field. In comparison with DR14 sample, the final sample doubles the number of objects as well as the survey area. In this paper, we present the analysis in configuration space by measuring the two-point correlation function and decomposing it using the Legendre polynomials. For the full-shape analysis of the Legendre multipole moments, we measure the baryon acoustic oscillation (BAO) distance and the growth rate of the cosmic structure. At an effective redshift of zeff = 1.48, we measure the comoving angular diameter distance DM(zeff)/rdrag = 30.66 ± 0.88, the Hubble distance DH(zeff)/rdrag = 13.11 ± 0.52, and the product of the linear growth rate and the rms linear mass fluctuation on scales of $8 \, h^{-1}\, {\rm Mpc}$ , fσ8(zeff) = 0.439 ± 0.048. The accuracy of these measurements is confirmed using an extensive set of mock simulations developed for the quasar sample. The uncertainties on the distance and growth rate measurements have been reduced substantially (∼45 and ∼30 per cent) with respect to the DR14 results. We also perform a BAO-only analysis to cross check the robustness of the methodology of the full-shape analysis. Combining our analysis with the Fourier-space analysis, we arrive at $D^{{\bf c}}_{\rm M}(z_{\rm eff})/r_{\rm drag} = 30.21 \pm 0.79$ , $D^{{\bf c}}_{\rm H}(z_{\rm eff})/r_{\rm drag} = 13.23 \pm 0.47$ , and $f\sigma _8^{{\bf c}}(z_{\rm eff}) = 0.462 \pm 0.045$ .

(245)Cosmology dependence of halo masses and concentrations in hydrodynamic simulations
• Antonio Ragagnin,
• Alexandro Saro,
• Priyanka Singh,
• Klaus Dolag
Monthly Notices of the Royal Astronomical Society, 500, p16 (01/2021) doi:10.1093/mnras/staa3523
abstract + abstract -

We employ a set of Magneticum cosmological hydrodynamic simulations that span over 15 different cosmologies, and extract masses and concentrations of all well-resolved haloes between z = 0 and 1 for critical overdensities $\Delta _\textrm {vir}, \Delta _{200c}, \Delta _{500c}, \Delta _{2500c}$ and mean overdensity Δ200m. We provide the first mass-concentration (Mc) relation and sparsity relation (i.e. MΔ1 - MΔ2 mass conversion) of hydrodynamic simulations that is modelled by mass, redshift, and cosmological parameters Ωm, Ωb, σ8, h0 as a tool for observational studies. We also quantify the impact that the Mc relation scatter and the assumption of Navarro-Frank-White (NFW) density profiles have on the uncertainty of the sparsity relation. We find that converting masses with the aid of an Mc relation carries an additional fractional scatter ( $\approx 4{{\ \rm per\ cent}}$ ) originated from deviations from the assumed NFW density profile. For this reason, we provide a direct mass-mass conversion relation fit that depends on redshift and cosmological parameters. We release the package HYDRO_MC, a PYTHON tool that perform all kind of conversions presented in this paper.

(244)Determining the systemic redshift of Lyman α emitters with neural networks and improving the measured large-scale clustering
• Siddhartha Gurung-López,
• Shun Saito,
• Carlton M. Baugh,
• Silvia Bonoli,
• Cedric G. Lacey
• +1
Monthly Notices of the Royal Astronomical Society, 500, p24 (01/2021) doi:10.1093/mnras/staa3269
abstract + abstract -

We explore how to mitigate the clustering distortions in Lyman α emitter (LAE) samples caused by the misidentification of the Lyman α ( $\rm {Ly}\,\alpha$ ) wavelength in their $\rm {Ly}\,\alpha$ line profiles. We use the $\rm {Ly}\,\alpha$ line profiles from our previous LAE theoretical model that includes radiative transfer in the interstellar and intergalactic mediums. We introduce a novel approach to measure the systemic redshift of LAEs from their $\rm {Ly}\,\alpha$ line using neural networks. In detail, we assume that for a fraction of the whole LAE population their systemic redshift is determined precisely through other spectral features. We then use this subset to train a neural network that predicts the $\rm {Ly}\,\alpha$ wavelength given an $\rm {Ly}\,\alpha$ line profile. We test two different training sets: (i) the LAEs are selected homogeneously and (ii) only the brightest LAE is selected. In comparison with previous approaches in the literature, our methodology improves significantly the accuracy in determining the $\rm {Ly}\,\alpha$ wavelength. In fact, after applying our algorithm in ideal $\rm {Ly}\,\alpha$ line profiles, we recover the clustering unperturbed down to $1\, {\rm cMpc}\, h^{-1}$ . Then, we test the performance of our methodology in realistic $\rm {Ly}\,\alpha$ line profiles by downgrading their quality. The machine learning technique using the uniform sampling works well even if the $\rm {Ly}\,\alpha$ line profile quality is decreased considerably. We conclude that LAE surveys such as HETDEX would benefit from determining with high accuracy the systemic redshift of a subpopulation and applying our methodology to estimate the systemic redshift of the rest of the galaxy sample.

(243)Evidence for galaxy quenching in the green valley caused by a lack of a circumgalactic medium
• Glenn G. Kacprzak,
• Nikole M. Nielsen,
• Hasti Nateghi,
• Christopher W. Churchill,
• Stephanie K. Pointon
• +3
• Themiya Nanayakkara,
• Sowgat Muzahid,
• Jane C. Charlton
• (less)
Monthly Notices of the Royal Astronomical Society, 500, p13 (01/2021) doi:10.1093/mnras/staa3461
abstract + abstract -

The relationship between a galaxy's properties and its circumgalactic medium (CGM) provides a unique view of how galaxies evolve. We present an interesting edge-on (i = 86°) disc galaxy (G1547) where the CGM is probed by a background quasar at a distance of 84 kpc and within 10° of the galaxy major axis. G1547 does not have any detectable CGM absorption down to stringent limits, covering H I (EWr <0.02 Å, log(N(H I)/cm-2) < 12.6) and a range of low and high ionization absorption lines (O I, C II, N II, Si II, C III, N III, Si III, C IV, Si IV, N V, and O VI). This system is rare, given the covering fraction of $1.00_{-0.04}^{+0.00}$ for sub-L* galaxies within 50-100 kpc of quasar sightlines. G1547 has a low star formation rate (SFR, 1.1 M yr-1), specific SFR (sSFR, 1.5 × 10-10 yr-1), and ΣSFR (0.06 M yr-1 kpc-2) and does not exhibit active galactic nucleus or star-formation-driven outflows. Compared to the general population of galaxies, G1547 is in the green valley and has an above average metallicity with a negative gradient. When compared to other H I absorption-selected galaxies, we find that quiescent galaxies with log(sSFR/yr-1) < -11 have a low probability (4/12) of possessing detectable H I in their CGM, while all galaxies (40/40) with log(sSFR/yr-1) > -11 have H I absorption. We conclude that sSFR is a good indicator of the presence of H I CGM. Interestingly however, G1547 is the only galaxy with log(sSFR/yr-1) > -11 that has no detectable CGM. Given the properties of G1547, and its absent CGM, it is plausible that G1547 is undergoing quenching due to a lack of accreting fuel for star formation, with an estimated quenching time-scale of 4 ± 1 Gyr. G1547 provides a unique perspective into the external mechanisms that could explain the migration of galaxies into the green valley.

(242)Blind H I and OH Absorption Line Search: First Results with MALS and uGMRT Processed Using ARTIP
• N. Gupta,
• P. Jagannathan,
• R. Srianand,
• S. Bhatnagar,
• P. Noterdaeme
• +30
• F. Combes,
• P. Petitjean,
• J. Jose,
• S. Pandey,
• A. J. Baker,
• S. A. Balashev,
• E. Boettcher,
• H. -W. Chen,
• C. Cress,
• R. Dutta,
• S. Goedhart,
• G. Heald,
• G. I. G. Józsa,
• E. Kamau,
• P. Kamphuis,
• J. Kerp,
• H. -R. Klöckner,
• K. Knowles,
• V. Krishnan,
• J. -. K. Krogager,
• V. P. Kulkarni,
• E. Momjian,
• K. Moodley,
• S. Passmoor,
• A. Schröeder,
• S. Sekhar,
• S. Sikhosana,
• J. Wagenveld,
• O. I. Wong
• (less)
The Astrophysical Journal, 907, p24 (01/2021) doi:10.3847/1538-4357/abcb85
abstract + abstract -

We present details of the Automated Radio Telescope Imaging Pipeline (ARTIP) and the results of a sensitive blind search for H I and OH absorbers at z < 0.4 and z < 0.7, respectively. ARTIP is written in Python 3.6, extensively uses the Common Astronomy Software Application tools and tasks, and is designed to enable the geographically distributed MeerKAT Absorption Line Survey (MALS) team to collaboratively process large volumes of radio interferometric data. We apply it to the first MALS data set obtained using the 64-dish MeerKAT radio telescope and 32 K channel mode of the correlator. With merely 40 minutes on target, we present the most sensitive spectrum of PKS 1830-211 ever obtained and characterize the known H I (z = 0.19) and OH (z = 0.89) absorbers. We further demonstrate ARTIP's capabilities to handle realistic observing scenarios by applying it to a sample of 72 bright radio sources observed with the upgraded Giant Metrewave Radio Telescope (uGMRT) to blindly search for H I and OH absorbers. We estimate the numbers of H I and OH absorbers per unit redshift to be n21(z ∼ 0.18) < 0.14 and nOH(z ∼ 0.40) < 0.12, respectively, and constrain the cold gas covering factor of galaxies at large impact parameters (50 kpc < ρ < 150 kpc) to be less than 0.022. Due to the small redshift path, Δz ∼ 13 for H I with column density >5.4 × 1019 cm-2, the survey has probed only the outskirts of star-forming galaxies at ρ > 30 kpc. MALS with the expected Δz ∼ 103-4 will overcome this limitation and provide stringent constraints on the cold gas fraction of galaxies in diverse environments over 0 < z < 1.5.

(241)The diffuse interstellar band around 8620 Å. I. Methods and application to the GIBS data set
• H. Zhao,
• M. Schultheis,
• A. Recio-Blanco,
• G. Kordopatis,
• P. de Laverny
• +4
• M. Zoccali,
• F. Surot,
• E. Valenti
• (less)
Astronomy and Astrophysics, 645, p17 (01/2021) doi:10.1051/0004-6361/202039736
abstract + abstract -

Context. Diffuse interstellar bands (DIBs) are interstellar absorption features that widely exist in the optical and near-infrared wavelength range. DIBs play an important role in the lifecycle of the interstellar medium and can also be used to trace the Galactic structure.
Aims: We developed a set of procedures to automatically detect and measure the DIB around 8620 Å (the Gaia DIB) for a wide range of temperatures. The method was tested on ~5000 spectra from the Giraffe Inner Bulge Survey (GIBS) that has a spectral window similar to that of the Gaia-RVS spectra. Based on this sample, we studied the correlation between the equivalent width (EW) of the Gaia DIB and the interstellar reddening E(J - KS) toward the inner Galaxy, as well as the DIB intrinsic properties.
Methods: Our procedure automatically checks and eliminates invalid cases, and then applies a specific local normalization. The DIB profile is fit with a Gaussian function. Specifically, the DIB feature is extracted from the spectra of late-type stars by subtracting the corresponding synthetic spectra. For early-type stars we applied a specific model based on the Gaussian process that needs no prior knowledge of the stellar parameters. In addition, we provide the errors contributed by the synthetic spectra and from the random noise.
Results: After validation, we obtained 4194 reasonable fitting results from the GIBS database. An EW versus E(J - KS) relation is derived as E(J - KS) = 1.875 (±0.152) × EW - 0.011 (±0.048), according to E(B - V)/EW = 2.721, which is highly consistent with previous results toward similar sightlines. After a correction based on the Vista Variables in the Via Lactea (VVV) database for both EW and reddening, the coefficient derived from individual GIBS fields, E(J - KS)/EW = 1.884 ± 0.225, is also in perfect agreement with literature values. Based on a subsample of 1015 stars toward the Galactic center within - 3° < b < 3° and - 6° < l < 3°, we determined a rest-frame wavelength of the Gaia DIB as 8620.55 Å.
Conclusions: The procedures for automatic detection and measurement of the Gaia DIB are successfully developed and have been applied to the GIBS spectra. A Gaussian profile is proved to be a proper and stable assumption for the Gaia DIB as no intrinsic asymmetry is found. A tight linearity of its correlation with the reddening is derived toward the inner Milky Way, which is consistent with previous results.

The catalog is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/645/A14

(240)Covariance of the matter power spectrum including the survey window function effect: N -body simulations versus fifth-order perturbation theory on grids
• Atsushi Taruya,
• Takahiro Nishimichi,
• Donghui Jeong
Physical Review D, 103 (01/2021) doi:10.1103/PhysRevD.103.023501
abstract + abstract -

We present a next-to-next-to-leading (fifth or NNLO) order calculation for the covariance matrix of the matter power spectrum, taking into account the effect of survey window functions. Using the grid-based calculation scheme for the standard perturbation theory, GridSPT, we quickly generate multiple realizations of the nonlinear density fields to fifth order in perturbation theory, then estimate the power spectrum and the covariance matrix from the sample. To the end, we have obtained the non-Gaussian covariance originated from the one-loop trispectrum without explicitly computing the trispectrum. By comparing the GridSPT calculations with the N -body results, we show that NNLO GridSPT result reproduces the N -body results on quasilinear scales, where SPT accurately models nonlinear matter power spectrum. Incorporating the survey window function effect to GridSPT is rather straightforward, and the resulting NNLO covariance matrix also matches well with the N -body results.

(239)A new view of observed galaxies through 3D modelling and visualisation
• T. Dykes,
• C. Gheller,
• B. S. Koribalski,
• K. Dolag,
• M. Krokos
Astronomy and Computing, 34 (01/2021) doi:10.1016/j.ascom.2021.100448
abstract + abstract -

Observational astronomers survey the sky in great detail to gain a better understanding of many types of astronomical phenomena. In particular, the formation and evolution of galaxies, including our own, are a wide field of research. Three dimensional (spatial 3D) scientific visualisation is typically limited to simulated galaxies, due to the inherently two dimensional spatial resolution of Earth-based observations. However, with appropriate means of reconstruction, such visualisation can also be used to bring out the inherent 3D structure that exists in 2D observations of known galaxies, providing new views of these galaxies and visually illustrating the spatial relationships within galaxy groups that are not obvious in 2D. We present a novel approach to reconstruct and visualise 3D representations of nearby galaxies based on observational data using the scientific visualisation software Splotch. We apply our approach to a case study of the nearby barred spiral galaxy known as M83, presenting a new perspective of the M83 local group and highlighting the similarities between our reconstructed views of M83 and other known galaxies of similar inclinations.

(238)A new class of fossil fragments from the hierarchical assembly of the Galactic bulge
• F. R. Ferraro,
• C. Pallanca,
• B. Lanzoni,
• C. Crociati,
• E. Dalessandro
• +10
• L. Origlia,
• R. M. Rich,
• S. Saracino,
• A. Mucciarelli,
• E. Valenti,
• D. Geisler,
• F. Mauro,
• S. Villanova,
• C. Moni Bidin,
• G. Beccari
• (less)
Nature Astronomy, 5, p8 (01/2021) doi:10.1038/s41550-020-01267-y
abstract + abstract -

The formation and evolutionary processes of galaxy bulges are still unclear, and the presence of young stars in the bulge of the Milky Way is largely debated. We recently demonstrated that Terzan 5, in the Galactic bulge, is a complex stellar system hosting stars with very different ages and a striking chemical similarity to the field population. This indicates that its progenitor was probably one of the giant structures that are thought to generate bulges through coalescence. Here we show that another globular cluster-like system in the bulge (Liller 1) hosts two distinct stellar populations with remarkably different ages: only 1-3 Gyr for the youngest, and 12 Gyr for the oldest, which is impressively similar to the old component of Terzan 5. This discovery classifies Liller 1 and Terzan 5 as sites of recent star formation in the Galactic bulge and provides clear observational proof that the hierarchical assembly of primordial massive structures contributed to the formation of the Milky Way spheroid.

(237)The Connection between Mergers and AGN Activity in Simulated and Observed Massive Galaxies
• Ray S. Sharma,
• Ena Choi,
• Rachel S. Somerville,
• Gregory F. Snyder,
• Dale D. Kocevski
• +6
• Michaela Hirschmann,
• Benjamin P. Moster,
• Thorsten Naab,
• Desika Narayanan,
• Jeremiah P. Ostriker,
• David J. Rosario
• (less)
arXiv e-prints (01/2021) e-Print:2101.01729
abstract + abstract -

We analyze a suite of $30$ high resolution zoom-in cosmological hydrodynamic simulations of massive galaxies with stellar masses $M_{\ast} > 10^{10.9} M_\odot$, with the goal of better understanding merger activity in AGN, AGN activity in merging systems, SMBH growth during mergers, and the role of gas content. Using the radiative transfer code \textsc{Powderday}, we generate HST-WFC3 F160W synthetic observations of redshift $0.5 < z < 3$ central galaxies, add noise properties similar to the CANDELS survey, and measure morphological properties from the synthetic images using commonly adopted non-parametric statistics. We compare the distributions of morphological properties measured from the synthetic images with a sample of inactive galaxies and X-ray selected AGN hosts from CANDELS. We study the connection between mergers and AGN activity in the simulations, the synthetic images, and the observed CANDELS sample. We find that, in both the simulations and CANDELS, even the most luminous $(L_{\rm bol} > 10^{45}$ erg s$^{-1})$ AGN in our sample are no more likely than inactive galaxies $(L_{\rm bol} < 10^{43}$ erg s$^{-1})$ to be found in merging systems. We also find that AGN activity is not overall enhanced by mergers, nor enhanced at any specific time in the $1$ Gyr preceding and following a merger. Even gas rich major mergers (stellar mass ratio $>$1:4) do not necessarily enhance AGN activity or significantly grow the central SMBH. We conclude that in the simulated massive galaxies studied here, mergers are not the primary drivers of AGN.

(236)The fully developed remnant of a neutrino-driven supernova. Evolution of ejecta structure and asymmetries in SNR Cassiopeia A
• S. Orlando,
• A. Wongwathanarat,
• H. -T. Janka,
• M. Miceli,
• M. Ono
• +3
• S. Nagataki,
• F. Bocchino,
• G. Peres
• (less)
Astronomy and Astrophysics, 645, p32 (01/2021) doi:10.1051/0004-6361/202039335
abstract + abstract -

Context. The remnants of core-collapse supernovae (SNe) are probes of the physical processes associated with their parent SNe.
Aims: Here we aim to explore to which extent the remnant keeps memory of the asymmetries that develop stochastically in the neutrino-heating layer due to hydrodynamic instabilities (e.g., convective overturn and the standing accretion shock instability; SASI) during the first second after core bounce.
Methods: We coupled a three-dimensional (3D) hydrodynamic model of a neutrino-driven SN explosion, which has the potential to reproduce the observed morphology of the Cassiopeia A (Cas A) remnant, with 3D (magneto)-hydrodynamic simulations of the remnant formation. The simulations cover ≈2000 yr of expansion and include all physical processes relevant to describe the complexities in the SN evolution and the subsequent interaction of the stellar debris with the wind of the progenitor star.
Results: The interaction of large-scale asymmetries left from the earliest phases of the explosion with the reverse shock produces, at the age of ≈350 yr, an ejecta structure and a remnant morphology which are remarkably similar to those observed in Cas A. Small-scale structures in the large-scale Fe-rich plumes that were created during the initial stages of the SN, combined with hydrodynamic instabilities that develop after the passage of the reverse shock, naturally produce a pattern of ring- and crown-like structures of shocked ejecta. The consequence is a spatial inversion of the ejecta layers with Si-rich ejecta being physically interior to Fe-rich ejecta. The full-fledged remnant shows voids and cavities in the innermost unshocked ejecta, which are physically connected with ring-like features of shocked ejecta in the main shell in most cases, resulting from the expansion of Fe-rich plumes and their inflation due to the decay of radioactive species. The asymmetric distributions of 44Ti and 56Fe, which are mostly concentrated in the northern hemisphere, and pointing opposite to the kick velocity of the neutron star, as well as their abundance ratio are both compatible with those inferred from high-energy observations of Chandra and NuSTAR. Finally, the simulations show that the fingerprints of the SN can still be visible ≈2000 yr after the explosion.
Conclusions: The main asymmetries and features observed in the ejecta distribution of Cas A can be explained by the interaction of the reverse shock with the initial large-scale asymmetries that developed from stochastic processes (e.g., convective overturn and SASI activity) that originate during the first seconds of the SN blast.

Movies associated to Figs. 7, 8, 12, 15 are available at https://www.aanda.org

(235)The kinematics and dark matter fractions of TNG50 galaxies at z = 2 from an observational perspective
• Hannah Übler,
• Shy Genel,
• Amiel Sternberg,
• Reinhard Genzel,
• Sedona H. Price
• +11
• Natascha M. Förster Schreiber,
• Taro T. Shimizu,
• Annalisa Pillepich,
• Dylan Nelson,
• Andreas Burkert,
• Ric Davies,
• Lars Hernquist,
• Philipp Lang,
• Dieter Lutz,
• Rüdiger Pakmor,
• Linda J. Tacconi
• (less)
Monthly Notices of the Royal Astronomical Society, 500, p23 (01/2021) doi:10.1093/mnras/staa3464
abstract + abstract -

We contrast the gas kinematics and dark matter contents of z = 2 star-forming galaxies (SFGs) from state-of-the-art cosmological simulations within the ΛCDM framework to observations. To this end, we create realistic mock observations of massive SFGs ( $M_*\gt 4\times 10^{10} \, \mathrm{M}_{\odot}$ , SFR >50 M yr-1) from the TNG50 simulation of the IllustrisTNG suite, resembling near-infrared, adaptive-optics assisted integral-field observations from the ground. Using observational line fitting and modelling techniques, we analyse in detail the kinematics of seven TNG50 galaxies from five different projections per galaxy, and compare them to observations of twelve massive SFGs by Genzel et al. (2020). The simulated galaxies show clear signs of disc rotation but mostly exhibit more asymmetric rotation curves, partly due to large intrinsic radial and vertical velocity components. At identical inclination angle, their 1D velocity profiles can vary along different lines of sight by up to Δv = 200 km s-1. From dynamical modelling we infer rotation speeds and velocity dispersions that are broadly consistent with observational results. We find low central dark matter fractions compatible with observations ( $f_{\rm DM}^v(\lt R_e)=v_{\rm DM}^2(R_e)/v_{\rm circ}^2(R_e)\sim 0.32\pm 0.10$ ), however for disc effective radii Re that are mostly too small: at fixed Re the TNG50 dark matter fractions are too high by a factor of ∼2. We speculate that the differences in gas kinematics and dark matter content compared to the observations may be due to physical processes that are not resolved in sufficient detail with the numerical resolution available in current cosmological simulations.

(234)A diffusiophoretic mechanism for ATP-driven transport without motor proteins
• Beatrice Ramm,
• Andriy Goychuk,
• Alena Khmelinskaia,
• Philipp Blumhardt,
• Hiromune Eto
• +3
• Kristina A. Ganzinger,
• Erwin Frey,
• Petra Schwille
• (less)
Nature Physics, 17, p9 (2021) doi:10.1038/s41567-021-01213-3
abstract + abstract -

The healthy growth and maintenance of a biological system depends on the precise spatial organization of molecules within the cell through the dissipation of energy. Reaction-diffusion mechanisms can facilitate this organization, as can directional cargo transport orchestrated by motor proteins, by relying on specific protein interactions. However, transport of material through the cell can also be achieved by active processes based on non-specific, purely physical mechanisms, a phenomenon that remains poorly explored. Here, using a combined experimental and theoretical approach, we discover and describe a hidden function of the Escherichia coli MinDE protein system: in addition to forming dynamic patterns, this system accomplishes the directional active transport of functionally unrelated cargo on membranes. Remarkably, this mechanism enables the sorting of diffusive objects according to their effective size, as evidenced using modular DNA origami-streptavidin nanostructures. We show that the diffusive fluxes of MinDE and non-specific cargo couple via density-dependent friction. This non-specific process constitutes a diffusiophoretic mechanism, as yet unknown in a cell biology setting. This nonlinear coupling between diffusive fluxes could represent a generic physical mechanism for establishing intracellular organization.

(233)Searching for New Physics with (\bar {\mathcal {B}}(B_{s,d}\to \mu \bar \mu )/\Delta M_{s,d})
• C. Bobeth,
• A. J. Buras
Acta Physica Polonica B, 52 (2021) doi:10.5506/APhysPolB.52.1189
abstract + abstract -

We reemphasize that the ratio $R_{s\mu} \equiv \overline{\mathcal{B}}(B_s\to\mu\bar\mu)/\Delta M_s$ is a measure of the tension of the Standard Model (SM) with latest measurements of $\overline{\mathcal{B}}(B_s\to\mu\bar\mu)$ that does not suffer from the persistent puzzle on the $|V_{cb}|$ determinations from inclusive versus exclusive $b\to c\ell\bar\nu$ decays and which affects the value of the CKM element $|V_{ts}|$ that is crucial for the SM predictions of both $\overline{\mathcal{B}}(B_s\to\mu\bar\mu)$ and $\Delta M_s$, but cancels out in the ratio $R_{s\mu}$. In our analysis we include higher order electroweak and QED corrections und adapt the latest hadronic input to find a tension of about $2\sigma$ for $R_{s\mu}$ measurements with the SM independently of $|V_{ts}|$. We also discuss the ratio $R_{d\mu}$ which could turn out, in particular in correlation with $R_{s\mu}$, to be useful for the search for New Physics, when the data on both ratios improves. Also $R_{d\mu}$ is independent of $|V_{cb}|$ or more precisely $|V_{td}|$.

(232)The (\varepsilon '/\varepsilon )-story: 1976–2021
• A. J. Buras
Acta Physica Polonica B, 52 (2021) doi:10.5506/APhysPolB.52.7
abstract + abstract -

The ratio $\epsilon'/\epsilon$ measures the size of the direct CP violation in $K_L\to\pi\pi$ decays $(\epsilon^\prime)$ relative to the indirect one described by $\epsilon$ and is very sensitive to new sources of CP violation. As such it played a prominent role in particle physics already for 45 years. Due to the smallness of $\epsilon'/\epsilon$ its measurement required heroic efforts in the 1980s and the 1990s on both sides of the Atlantic with final results presented by NA48 and KTeV collaborations 20 years ago. Unfortunately, even 45 years after the first calculation of $\epsilon'/\epsilon$ we do not know to which degree the Standard Model agrees with this data and how large is the room left for new physics contributions to this ratio. This is due to significant non-perturbative (hadronic) uncertainties accompanied by partial cancellation between the QCD penguin contributions and electroweak penguin contributions. While the significant control over the short distance perturbative effects has been achieved already in the early 1990s, with several improvements since then, different views on the non-perturbative contributions to $\epsilon'/\epsilon$ have been expressed by different authors over last thirty years. In fact even today the uncertainty in the room left for NP contributions to $\epsilon'/\epsilon$ is very significant. My own work on $\epsilon'/\epsilon$ started in 1983 and involved both perturbative and non-perturbative calculations. This writing is a non-technical recollection of the steps which led to the present status of $\epsilon'/\epsilon$ including several historical remarks not known to everybody. The present status of the $\Delta I=1/2$ rule is also summarized. This story is dedicated to Jean-Marc Gerard on the occasion of the 35th anniversary of our collaboration and his 64th birthday.

(231)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
Mon.Not.Roy.Astron.Soc., 508, p4610 (2021) e-Print:2109.09996 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 (M_BH = 1.7 × 10^10 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.

(230)Planet migration, resonant locking, and accretion streams in PDS 70: comparing models and data
• Claudia Toci,
• Giuseppe Lodato,
• Valentin Christiaens,
• Davide Fedele,
• Christophe Pinte
• +2
• Daniel J. Price,
• Leonardo Testi
• (less)
Monthly Notices of the Royal Astronomical Society, 499, p13 (12/2020) doi:10.1093/mnras/staa2933
abstract + abstract -

The disc surrounding PDS 70, with two directly imaged embedded giant planets, is an ideal laboratory to study planet-disc interaction. We present 3D smoothed particle hydrodynamics simulations of the system. In our simulations, planets, which are free to migrate and accrete mass, end up in a locked resonant configuration that is dynamically stable. We show that features observed at infrared (scattered light) and millimetre (thermal continuum) wavelengths are naturally explained by the accretion stream on to the outer planet, without requiring a circumplanetary disc around Planet c. We post-processed our near-infrared synthetic images in order to account for observational biases known to affect high-contrast images. Our successful reproduction of the observations indicates that planet-disc dynamical interactions alone are sufficient to explain the observations of PDS 70.

(229)Deep learning Blazar classification based on multifrequency spectral energy distribution data
• Bernardo M.O. Fraga,
• Ulisses Barres de Almeida,
• Clecio R. Bom,
• Carlos H. Brandt,
• Paolo Giommi
• +2
• Patrick Schubert,
• Marcio P. de Albuquerque
• (less)
Mon.Not.Roy.Astron.Soc., 505, p1268 (12/2020) e-Print:2012.15340 doi:10.1093/mnras/stab1349
abstract + abstract -

Blazars are among the most studied sources in high-energy astrophysics as they form the largest fraction of extragalactic gamma-ray sources and are considered prime candidates for being the counterparts of high-energy astrophysical neutrinos. Their reliable identification amid the many faint radio sources is a crucial step for multimessenger counterpart associations. As the astronomical community prepares for the coming of a number of new facilities able to survey the non-thermal sky at unprecedented depths, from radio to gamma-rays, machine-learning techniques for fast and reliable source identification are ever more relevant. The purpose of this work was to develop a deep learning architecture to identify Blazar within a population of active galactic nucleus (AGN) based solely on non-contemporaneous spectral energy distribution information, collected from publicly available multifrequency catalogues. This study uses an unprecedented amount of data, with spectral energy distributions (SEDs) for ≈14 000 sources collected with the Open Universe VOU-Blazars tool. It uses a convolutional long short-term memory neural network purposefully built for the problem of SED classification, which we describe in detail and validate. The network was able to distinguish Blazars from other types of active galactic nuclei (AGNs) to a satisfying degree (achieving a receiver operating characteristic area under curve of 0.98), even when trained on a reduced subset of the whole sample. This initial study does not attempt to classify Blazars among their different sub-classes, or quantify the likelihood of any multifrequency or multimessenger association, but is presented as a step towards these more practically oriented applications.

(228)Responses of Halo Occupation Distributions: a new ingredient in the halo model & the impact on galaxy bias
• Rodrigo Voivodic,
• Alexandre Barreira
abstract + abstract -

Halo occupation distribution (HOD) models describe the number of galaxies that reside in different haloes, and are widely used in galaxy-halo connection studies using the halo model (HM). Here, we introduce and study HOD response functions R

(227)Higgs-mass predictions in the MSSM and beyond
• P. Slavich,
• S. Heinemeyer,
• E. Bagnaschi,
• H. Bahl,
• M. Goodsell
• +34
• H.E. Haber,
• T. Hahn,
• R. Harlander,
• W. Hollik,
• G. Lee,
• M. Mühlleitner,
• S. Paßehr,
• H. Rzehak,
• D. Stöckinger,
• A. Voigt,
• C.E.M. Wagner,
• G. Weiglein,
• B.C. Allanach,
• T. Biekötter,
• S. Borowka,
• J. Braathen,
• M. Carena,
• T.N. Dao,
• G. Degrassi,
• F. Domingo,
• P. Drechsel,
• U. Ellwanger,
• M. Gabelmann,
• R. Gröber,
• J. Klappert,
• T. Kwasnitza,
• D. Meuser,
• L. Mihaila,
• N. Murphy,
• K. Nickel,
• W. Porod,
• E.A. Reyes Rojas,
• I. Sobolev,
• F. Staub
• (less)
Eur.Phys.J.C, 81, p450 (12/2020) e-Print:2012.15629 doi:10.1140/epjc/s10052-021-09198-2
abstract + abstract -

Predictions for the Higgs masses are a distinctive feature of supersymmetric extensions of the Standard Model, where they play a crucial role in constraining the parameter space. The discovery of a Higgs boson and the remarkably precise measurement of its mass at the LHC have spurred new efforts aimed at improving the accuracy of the theoretical predictions for the Higgs masses in supersymmetric models. The “Precision SUSY Higgs Mass Calculation Initiative” (KUTS) was launched in 2014 to provide a forum for discussions between the different groups involved in these efforts. This report aims to present a comprehensive overview of the current status of Higgs-mass calculations in supersymmetric models, to document the many advances that were achieved in recent years and were discussed during the KUTS meetings, and to outline the prospects for future improvements in these calculations.

(226)On the characteristics of fast neutrino flavor instabilities in three-dimensional core-collapse supernova models
• Francesco Capozzi,
• Robert Glas,
• H.-Thomas Janka,
• Irene Tamborra
abstract + abstract -

We assess the occurrence of fast neutrino flavor instabilities in two three-dimensional state-of-the-art core-collapse supernova simulations performed using a two-moment three-species neutrino transport scheme: one with an exploding 9M⊙ and one with a nonexploding 20M⊙ model. Apart from confirming the presence of fast instabilities occurring within the neutrino decoupling and the supernova pre-shock regions, we detect flavor instabilities in the post-shock region for the exploding model. These instabilities are likely to be scattering-induced. In addition, the failure in achieving a successful explosion in the heavier supernova model seems to seriously hinder the occurrence of fast instabilities in the post-shock region. This is a consequence of the large matter densities behind the stalled or retreating shock, which implies high neutrino scattering rates and thus more isotropic distributions of neutrinos and antineutrinos. Our findings suggest that the supernova model properties and the fate of the explosion can remarkably affect the occurrence of fast instabilities. Hence, a larger set of realistic hydrodynamical simulations of the stellar collapse is needed in order to make reliable predictions on the flavor conversion physics.

(225)Mu-Tau Neutrinos: Influencing Fast Flavor Conversions in Supernovae
• Francesco Capozzi,
• Sovan Chakraborty,
• Manibrata Sen
Physical Review Letters, 125 (12/2020) doi:10.1103/PhysRevLett.125.251801
abstract + abstract -

Neutrinos in a core-collapse supernova can undergo fast flavor conversions with a possible impact on the explosion mechanism and nucleosynthesis. We perform the first nonlinear simulations of fast conversions in the presence of three neutrino flavors. The recent supernova simulations with muon production call for such an analysis, as they relax the standard νμ ,τ¯ μ ,τ (two-flavor) assumption. Our results show the significance of muon and tau lepton number angular distributions, together with the traditional electron lepton number ones. Indeed, our three-flavor results are potentially very different from two-flavor ones. These results strengthen the need to further investigate the occurrence of fast conversions in supernova simulation data, including the degeneracy breaking of mu and tau neutrinos.

(224)Polarization angle measurement of LiteBIRD low frequency telescope scaled model
• Hayato Takakura,
• Yutaro Sekimoto,
• Junji Inatani,
• Shingo Kashima,
• Masahiro Sugimoto
Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 11443, p14 (12/2020) doi:10.1117/12.2560419
abstract + abstract -

LiteBIRD is JAXA Strategic Large Mission for the late 2020s that aims to observe the large-scale B-mode polarization pattern of the cosmic microwave background. One of its telescopes, the Low Frequency Telescope (LFT), has a crossed-Dragone design and observes at 34-161 GHz with a field of view of 18° x 9°. Because a miscalibration of the polarization angles mixes E- and B-mode polarization, we have measured the variation of the polarization angles in the field of view of a 1/4-scaled LFT antenna at 140-220 GHz, which corresponds to 35-55 GHz for the full-scale LFT, considering a scaling of the wavelength. We placed a collimated-wave source near the scaled-LFT aperture and rotated the polarization angle of the LFT feed. The measurements were explained well with a simple Jones matrix calculation, and the fitting errors of the polarization angles were less than 0.1'. We also measured the polarization angles by rotating the polarization direction in the scaled-LFT aperture, and the results were consistent with the angles measured by rotating the feed polarization at the +/-10" level, except at the lowest frequencies. The polarization angle at the edges of the focal plane varied from that at the center by up to around a degree, with larger variation at lower frequencies. We evaluated the polarization angles for both Pol-X and Pol-Y feeds, and the results with Pol-Y showed a trend consistent with ray-tracing simulations. The results for Pol-X showed the opposite trend of the polarization rotation direction and larger angle variations.

(223)Simulation of the cosmic ray effects for the LiteBIRD satellite observing the CMB B-mode polarization
• Mayu Tominaga,
• Masahiro Tsujimoto,
• Samantha Lynn Stever,
• Tommaso Ghigna,
• HIrokazu Ishino
• +1
Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 11453, p15 (12/2020) doi:10.1117/12.2576127
abstract + abstract -

The LiteBIRD satellite is planned to be launched by JAXA in the late 2020s. Its main purpose is to observe the large-scale B-mode polarization in the Cosmic Microwave Background (CMB) anticipated from the Inflation theory. LiteBIRD will observe the sky for three years at the second Lagrangian point (L2) of the Sun-Earth system. Planck was the predecessor for observing the CMB at L2, and the onboard High Frequency Instrument (HFI) suffered contamination by glitches caused by the cosmic-ray (CR) hits. We consider the CR hits can also be a serious source of the systematic uncertainty for LiteBIRD. Thus, we have started a comprehensive end-to-end simulation study to assess impact of the CR hits for the LiteBIRD detectors. Here, we describe procedures to make maps and power spectra from the simulated time-ordered data, and present initial results. Our initial estimate is that ClBB by CR is ~ 2 ×10-6 μK2CMB in a one-year observation with 12 detectors assuming that the noise is 1 aW/ √ Hz for the differential mode of two detectors constituting a polarization pair.

(222)Biasing Relation, Environmental Dependencies, and Estimation of the Growth Rate from Star-forming Galaxies
• Gustavo Yepes,
• Enzo Branchini
The Astrophysical Journal, 905, p21 (12/2020) doi:10.3847/1538-4357/abc42f
abstract + abstract -

The connection between galaxy star formation rate (SFR) and dark matter (DM) is of paramount importance for the extraction of cosmological information from next-generation spectroscopic surveys that will target emission line star-forming galaxies. Using publicly available mock galaxy catalogs obtained from various semianalytic models (SAMs), we explore the SFR-DM connection in relation to the speed-from-light method for inferring the growth rate, f, from luminosity/SFR shifts. Emphasis is given to the dependence of the SFR distribution on the environmental density on scales of 10-100 s Mpc. We show that the application of the speed-from-light method to a Euclid-like survey is not biased by environmental effects. In all models, the precision on the measured β = f/b parameter is σβ ≲ 0.17 at z = 1. This translates into errors of σf ∼ 0.22 and ${\sigma }_{(f{\sigma }_{8})}\sim 0.1$ without invoking assumptions on the mass power spectrum. These errors are in the same ballpark as recent analyses of the redshift space distortions in galaxy clustering. In agreement with previous studies, the bias factor, b, is roughly a scale-independent, constant function of the SFR for star-forming galaxies. Its value at z = 1 ranges from 1.2 to 1.5 depending on the SAM recipe. Although in all SAMs, denser environments host galaxies with higher stellar masses, the dependence of the SFR on the environment is more involved. In most models, the SFR probability distribution is skewed to larger values in denser regions. One model exhibits an inverted trend, where high SFR is suppressed in dense environments.

(221)Detector fabrication development for the LiteBIRD satellite mission
• B. Westbrook,
• C. Raum,
• S. Beckman,
• A. T. Lee,
• N. Farias
• +21
• T. Sasse,
• A. Suzuki,
• E. Kane,
• J. E. Austermann,
• J. A. Beall,
• S. M. Duff,
• J. Hubmayr,
• G. C. Hilton,
• J. Van Lanen,
• M. R. Vissers,
• N. Halverson,
• G. Jaehnig,
• T. Ghinga,
• S. Stever,
• Y. Minami,
• K. L. Thompson,
• M. Russell,
• K. Arnold,
• J. Seibert,
• M. Silva-Feaver
• (less)
Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 11443, p22 (12/2020) doi:10.1117/12.2562978
abstract + abstract -

LiteBIRD is a JAXA-led strategic Large-Class satellite mission designed to measure the polarization of the cosmic microwave background and cosmic foregrounds from 34 to 448 GHz across the entire sky from L2 in the late 2020's. The primary focus of the mission is to measure primordially generated B-mode polarization at large angular scales. Beyond its primary scientific objective LiteBIRD will generate a data-set capable of probing a number of scientific inquiries including the sum of neutrino masses. The primary responsibility of United States will be to fabricate the three flight model focal plane units for the mission. The design and fabrication of these focal plane units is driven by heritage from ground based experiments and will include both lenslet-coupled sinuous antenna pixels and horn-coupled orthomode transducer pixels. The experiment will have three optical telescopes called the low frequency telescope, mid frequency telescope, and high frequency telescope each of which covers a portion of the mission's frequency range. JAXA is responsible for the construction of the low frequency telescope and the European Consortium is responsible for the mid- and high- frequency telescopes. The broad frequency coverage and low optical loading conditions, made possible by the space environment, require development and adaptation of detector technology recently deployed by other cosmic microwave background experiments. This design, fabrication, and characterization will take place at UC Berkeley, NIST, Stanford, and Colorado University, Boulder. We present the current status of the US deliverables to the LiteBIRD mission.

(220)MS renormalization of S-wave quarkonium wavefunctions at the origin
• Hee Sok Chung
Journal of High Energy Physics, 2020 (12/2020) doi:10.1007/JHEP12(2020)065
abstract + abstract -

We compute S-wave quarkonium wavefunctions at the origin in the MS ¯ scheme based on nonrelativistic effective field theories. We include the effects of nonperturbative long-distance behaviors of the potentials, while we determine the short-distance behaviors of the potentials in perturbative QCD. We obtain MS ¯-renormalized quarkonium wavefunctions at the origin that have the correct scale dependences that are expected from perturbative QCD, so that the scale dependences cancel in physical quantities. Based on the calculation of the wavefunctions at the origin, we make model-independent predictions of decay constants and electromagnetic decay rates of S-wave charmonia and bottomonia, and compare them with measurements. We find that the poor convergence of perturbative QCD corrections are substantially improved when we include corrections to the wavefunctions at the origin in the calculation of decay constants and decay rates.

(219)New constraints on supersymmetry using neutrino telescopes
• S. Meighen-Berger,
• M. Agostini,
• A. Ibarra,
• K. Krings,
• H. Niederhausen
• +3
• A. Rappelt,
• E. Resconi,
• A. Turcati
• (less)
Physics Letters B, 811 (12/2020) doi:10.1016/j.physletb.2020.135929
abstract + abstract -

We demonstrate that megaton-mass neutrino telescopes are able to observe the signal from long-lived particles beyond the Standard Model, in particular the stau, the supersymmetric partner of the tau lepton. Its signature is an excess of charged particle tracks with horizontal arrival directions and energy deposits between 0.1 and 1 TeV inside the detector. We exploit this previously-overlooked signature to search for stau particles in the publicly available IceCube data. The data shows no evidence of physics beyond the Standard Model. We derive a new lower limit on the stau mass of 320 GeV (95% C.L.) and estimate that this new approach, when applied to the full data set available to the IceCube collaboration, will reach word-leading sensitivity to the stau mass (mτ∼ = 450 GeV).

(218)Concept design of low frequency telescope for CMB B-mode polarization satellite LiteBIRD
• Y. Sekimoto,
• E. Allys,
• K. Arnold
• +232
• D. Auguste,
• J. Aumont,
• R. Aurlien,
• J. Austermann,
• C. Baccigalupi,
• A. J. Banday,
• R. Banerji,
• R. B. Barreiro,
• S. Basak,
• J. Beall,
• D. Beck,
• S. Beckman,
• J. Bermejo,
• P. de Bernardis,
• M. Bersanelli,
• J. Bonis,
• J. Borrill,
• F. Boulanger,
• S. Bounissou,
• M. Brilenkov,
• M. Brown,
• M. Bucher,
• E. Calabrese,
• P. Campeti,
• A. Carones,
• F. J. Casas,
• A. Challinor,
• V. Chan,
• K. Cheung,
• Y. Chinone,
• J. F. Cliche,
• L. Colombo,
• F. Columbro,
• J. Cubas,
• A. Cukierman,
• D. Curtis,
• G. D'Alessandro,
• N. Dachlythra,
• M. De Petris,
• C. Dickinson,
• P. Diego-Palazuelos,
• M. Dobbs,
• T. Dotani,
• L. Duband,
• S. Duff,
• J. M. Duval,
• K. Ebisawa,
• T. Elleflot,
• H. K. Eriksen,
• J. Errard,
• T. Essinger-Hileman,
• F. Finelli,
• R. Flauger,
• C. Franceschet,
• U. Fuskeland,
• M. Galloway,
• K. Ganga,
• J. R. Gao,
• R. Genova-Santos,
• M. Gerbino,
• M. Gervasi,
• T. Ghigna,
• E. Gjerløw,
• J. Grain,
• F. Grupp,
• A. Gruppuso,
• J. E. Gudmundsson,
• T. de Haan,
• N. W. Halverson,
• P. Hargrave,
• T. Hasebe,
• M. Hasegawa,
• M. Hattori,
• M. Hazumi,
• S. Henrot-Versillé,
• D. Herman,
• D. Herranz,
• C. A. Hill,
• G. Hilton,
• Y. Hirota,
• E. Hivon,
• R. A. Hlozek,
• Y. Hoshino,
• E. de la Hoz,
• J. Hubmayr,
• K. Ichiki,
• T. iida,
• K. Ishimura,
• H. Ishino,
• G. Jaehnig,
• T. Kaga,
• S. Kashima,
• N. Katayama,
• A. Kato,
• T. Kawasaki,
• R. Keskitalo,
• T. Kisner,
• Y. Kobayashi,
• N. Kogiso,
• A. Kogut,
• K. Kohri,
• E. Komatsu,
• K. Komatsu,
• K. Konishi,
• N. Krachmalnicoff,
• I. Kreykenbohm,
• C. L. Kuo,
• A. Kushino,
• L. Lamagna,
• J. V. Lanen,
• M. Lattanzi,
• A. T. Lee,
• C. Leloup,
• F. Levrier,
• E. Linder,
• T. Louis,
• G. Luzzi,
• T. Maciaszek,
• B. Maffei,
• D. Maino,
• M. Maki,
• S. Mandelli,
• E. Martinez-Gonzalez,
• S. Masi,
• T. Matsumura,
• A. Mennella,
• M. Migliaccio,
• Y. Minanmi,
• K. Mitsuda,
• J. Montgomery,
• L. Montier,
• G. Morgante,
• B. Mot,
• Y. Murata,
• J. A. Murphy,
• M. Nagai,
• Y. Nagano,
• T. Nagasaki,
• R. Nagata,
• S. Nakamura,
• T. Namikawa,
• P. Natoli,
• S. Nerval,
• T. Nishibori,
• H. Nishino,
• C. O'Sullivan,
• H. Ogawa,
• H. Ogawa,
• S. Oguri,
• H. Ohsaki,
• I. S. Ohta,
• L. Pagano,
• A. Paiella,
• D. Paoletti,
• G. Patanchon,
• J. Peloton,
• F. Piacentini,
• G. Pisano,
• 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. Sandri,
• M. Sasaki,
• G. Savini,
• D. Scott,
• J. Seibert,
• B. Sherwin,
• K. Shinozaki,
• M. Shiraishi,
• P. Shirron,
• G. Signorelli,
• G. Smecher,
• S. Stever,
• R. Stompor,
• H. Sugai,
• S. Sugiyama,
• A. Suzuki,
• J. Suzuki,
• T. L. Svalheim,
• E. Switzer,
• R. Takaku,
• H. Takakura,
• S. Takakura,
• Y. Takase,
• Y. Takeda,
• A. Tartari,
• E. Taylor,
• Y. Terao,
• H. Thommesen,
• K. L. Thompson,
• B. Thorne,
• T. Toda,
• M. Tomasi,
• M. Tominaga,
• N. Trappe,
• M. Tristram,
• M. Tsuji,
• M. Tsujimoto,
• C. Tucker,
• J. Ullom,
• G. Vermeulen,
• P. Vielva,
• F. Villa,
• M. Vissers,
• N. Vittorio,
• I. Wehus,
• J. Weller,
• B. Westbrook,
• J. Wilms,
• B. Winter,
• E. J. Wollack,
• N. Y. Yamasaki,
• T. Yoshida,
• J. Yumoto,
• M. Zannoni,
• A. Zonca
• (less)
Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 11453, p21 (12/2020) doi:10.1117/12.2561841
abstract + abstract -

LiteBIRD has been selected as JAXA's strategic large mission in the 2020s, to observe the cosmic microwave background (CMB) B-mode polarization over the full sky at large angular scales. The challenges of LiteBIRD are the wide field-of-view (FoV) and broadband capabilities of millimeter-wave polarization measurements, which are derived from the system requirements. The possible paths of stray light increase with a wider FoV and the far sidelobe knowledge of -56 dB is a challenging optical requirement. A crossed-Dragone configuration was chosen for the low frequency telescope (LFT : 34-161 GHz), one of LiteBIRD's onboard telescopes. It has a wide field-of-view (18° x 9°) with an aperture of 400 mm in diameter, corresponding to an angular resolution of about 30 arcminutes around 100 GHz. The focal ratio f/3.0 and the crossing angle of the optical axes of 90° are chosen after an extensive study of the stray light. The primary and secondary reflectors have rectangular shapes with serrations to reduce the diffraction pattern from the edges of the mirrors. The reflectors and structure are made of aluminum to proportionally contract from warm down to the operating temperature at 5 K. A 1/4 scaled model of the LFT has been developed to validate the wide field-of-view design and to demonstrate the reduced far sidelobes. A polarization modulation unit (PMU), realized with a half-wave plate (HWP) is placed in front of the aperture stop, the entrance pupil of this system. A large focal plane with approximately 1000 AlMn TES detectors and frequency multiplexing SQUID amplifiers is cooled to 100 mK. The lens and sinuous antennas have broadband capability. Performance specifications of the LFT and an outline of the proposed verification plan are presented.

(217)[N II] Fine-structure Emission at 122 and 205 μm in a Galaxy at z = 2.6: A Globally Dense Star-forming Interstellar Medium
• M. J. Doherty,
• J. E. Geach,
• R. J. Ivison,
• S. Dye
The Astrophysical Journal, 905, p7 (12/2020) doi:10.3847/1538-4357/abc5b9
abstract + abstract -

We present new observations with the Atacama Large Millimeter/submillimeter Array of the 122 and 205 μm fine-structure line emission of singly ionized nitrogen in a strongly lensed starburst galaxy at z = 2.6. The 122/205 μm [N II] line ratio is sensitive to electron density, ${n}_{{\rm{e}}}$, in the ionized interstellar medium, and we use this to measure ne ≍ 300 cm-3, averaged across the galaxy. This is over an order of magnitude higher than the Milky Way average, comparable to localized Galactic star-forming regions. Combined with observations of the atomic carbon (C I) and carbon monoxide (CO J = 4-3) in the same system, we reveal the conditions in this intensely star-forming system. The majority of the molecular interstellar medium has been driven to high density, and the resultant conflagration of star formation produces a correspondingly dense ionized phase, presumably colocated with myriad H II regions that litter the gas-rich disk.

(216)Breadboard model of the polarization modulator unit based on a continuously rotating half-wave plate for the low-frequency telescope of the LiteBIRD space mission
• Yuki Sakurai,
• Tomotake Matsumura,
• Nobuhiko Katayama,
• Kunimoto Komatsu,
• Ryota Takaku
• +21
• Shinya Sugiyama,
• Yoshiki Nomura,
• Takayuki Toda,
• Tommaso Ghigna,
• Teruhito Iida,
• Hajime Sugai,
• Masashi Hazumi,
• Hirokazu Ishino,
• Hiroyuki Ohsaki,
• Yutaka Terao,
• Hisashi Enokida,
• Yusuke Ishida,
• Yosuke Iwata,
• Kuniaki Konishi,
• Haruyuki Sakurai,
• Junji Yumoto,
• Makoto Kuwata-Gonokami,
• Akito Kusaka,
• Charles Hill
• (less)
Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 11453, p20 (12/2020) doi:10.1117/12.2560289
abstract + abstract -

We present a breadboard model development status of the polarization modulator unit (PMU) for a low-frequency telescope (LFT) of the LiteBIRD space mission. LiteBIRD is a next-generation cosmic microwave background polarization satellite to measure the primordial B-mode with the science goal of σr < 0.001. The baseline design of LiteBIRD consists of reflective low-frequency and refractive medium-and-high-frequency telescopes. Each telescope employs the PMU based on a continuous rotating half-wave plate (HWP) at the aperture. The PMU is a critical instrument for the LiteBIRD to achieve the science goal because it significantly suppresses 1/f noise and mitigates systematic uncertainties. The LiteBIRD LFT PMU consists of a broadband achromatic HWP and a cryogenic rotation mechanism. In this presentation, we discuss requirements, design and systematic studies of the PMU, and we report the development status of the broadband HWP and the space-compatible cryogenic rotation mechanism.

(215)A polarization modulator unit for the mid- and high-frequency telescopes of the LiteBIRD mission
• Fabio Columbro,
• Paolo de Bernardis,
• Luca Lamagna,
• Silvia Masi,
• Alessandro Paiella
• +2
• Francesco Piacentini,
• Giampaolo Pisano
• (less)
Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 11443, p16 (12/2020) doi:10.1117/12.2577818
abstract + abstract -

The LiteBIRD mission is a JAXA strategic L-class mission for all sky CMB surveys which will be launched in the 2020s. The main target of the mission is the detection of primordial gravitational waves with a sensitivity of the tensor-to-scalar ratio δr<0.001. The polarization modulator unit (PMU) represents a critical and powerful component to suppress 1/f noise contribution and mitigate systematic uncertainties induced by detector gain drift, both for the high-frequency telescope (HFT) and for the mid-frequency telescope (MFT). Each PMU is based on a continuously-rotating transmissive half-wave plate (HWP) held by a superconducting magnetic bearing in a 5K environment. In this contribution we will present the design and expected performance of the LiteBIRD PMUs and testing performed on every PMU subsystem with a room-temperature rotating disk used as a stand-in for the cryogenic HWP rotor.

(214)Simulating electromagnetic transfer function from the transmission antennae to the sensors vicinity in LiteBIRD
• M. Tsuji,
• M. Tsujimoto,
• Y. Sekimoto,
• T. Dotani,
• M. Shiraishi
Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 11443, p9 (12/2020) doi:10.1117/12.2560899
abstract + abstract -

The electromagnetic interference (EMI) is becoming an increasingly important factor in the spacecraft design equipped with highly sensitive detectors. This is particularly the case for LiteBIRD, in which the TES bolometers are exposed to space through the optical path. A particular concern is radiative interference caused by the X-band transmission during the ground communication. As the end-to-end verification test will be conducted in a later phase of the development, we need to derisk the concern early using simulation. In this report, we present the result of the EMI effects in the 1-GHz frequency range based on the electromagnetic simulation using a finite difference time domain (FDTD) solver. We modeled the dominant large structures of the spacecraft, calculated the spatial transmission of the antenna power, and estimated the electric field strength at the detector focal plane. The simulation results helped constrain aspects of the LiteBIRD satellite, such as the forward/backward ratio of the transmission antenna, to reduce the coupling between the antenna and the detectors.

(213)The optical design of the Litebird middle and high frequency telescope
• L. Lamagna,
• J. E. Gudmundsson,
• P. Hargrave,
• C. Franceschet
• +24
• M. De Petris,
• J. Austermann,
• S. Bounissou,
• F. Columbro,
• P. de Bernardis,
• S. Henrot-Versillé,
• J. Hubmayr,
• G. Jaehnig,
• R. Keskitalo,
• B. Maffei,
• S. Masi,
• T. Matsumura,
• L. Montier,
• B. Mot,
• F. Noviello,
• C. O'Sullivan,
• A. Paiella,
• G. Pisano,
• S. Realini,
• A. Ritacco,
• G. Savini,
• A. Suzuki,
• N. Trappe,
• B. Winter
• (less)
Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 11443, p17 (12/2020) doi:10.1117/12.2579233
abstract + abstract -

LiteBIRD is a JAXA strategic L-class mission devoted to the measurement of polarization of the Cosmic Microwave Background, searching for the signature of primordial gravitational waves in the B-modes pattern of the polarization. The onboard instrumentation includes a Middle and High Frequency Telescope (MHFT), based on a pair of cryogenically cooled refractive telescopes covering, respectively, the 89-224 GHz and the 166-448 GHz bands. Given the high target sensitivity and the careful systematics control needed to achieve the scientific goals of the mission, optical modeling and characterization are performed with the aim to capture most of the physical effects potentially affecting the real performance of the two refractors. We describe the main features of the MHFT, its design drivers and the major challenges in system optimization and characterization. We provide the current status of the development of the optical system and we describe the current plan of activities related to optical performance simulation and validation.

(212)Study of the strong interaction among hadrons with correlations at the LHC
• L. Fabbietti,
• V. Mantovani Sarti,
• O. Vazquez Doce
arXiv e-prints (12/2020) e-Print:2012.09806
abstract + abstract -

The strong interaction among hadrons has been measured in the past by scattering experiments. Although this technique has been extremely successful in providing information about the nucleon-nucleon and pion-nucleon interactions, when unstable hadrons are considered the experiments become more challenging. In the last few years, the analysis of correlations in the momentum space for pairs of stable and unstable hadrons measured in pp and p-Pb collisions by the ALICE Collaboration at the LHC has provided a new method to investigate the strong interaction among hadrons. In this article, we review the numerous results recently achieved for hyperon-nucleon, hyperon-hyperon, and kaon-nucleon pairs, which show that this new method opens the possibility of measuring the residual strong interaction of any hadron pair.

(211)HOLISMOKES. I. Highly Optimised Lensing Investigations of Supernovae, Microlensing Objects, and Kinematics of Ellipticals and Spirals
• S. H. Suyu,
• S. Huber,
• R. Cañameras,
• M. Kromer,
• S. Schuldt
• +8
• S. Taubenberger,
• A. Yıldırım,
• V. Bonvin,
• J. H. H. Chan,
• F. Courbin,
• U. Nöbauer,
• S. A. Sim,
• D. Sluse
• (less)
Astronomy and Astrophysics, 644, p15 (12/2020) doi:10.1051/0004-6361/202037757
abstract + abstract -

We present the HOLISMOKES programme on strong gravitational lensing of supernovae (SNe) as a probe of SN physics and cosmology. We investigate the effects of microlensing on early-phase SN Ia spectra using four different SN explosion models. We find that distortions of SN Ia spectra due to microlensing are typically negligible within ten rest-frame days after a SN explosion (< 1% distortion within the 1σ spread and ≲10% distortion within the 2σ spread). This shows the great prospects of using lensed SNe Ia to obtain intrinsic early-phase SN spectra for deciphering SN Ia progenitors. As a demonstration of the usefulness of lensed SNe Ia for cosmology, we simulate a sample of mock lensed SN Ia systems that are expected to have accurate and precise time-delay measurements in the era of the Rubin Observatory Legacy Survey of Space and Time (LSST). Adopting realistic yet conservative uncertainties on their time-delay distances and lens angular diameter distances, of 6.6% and 5%, respectively, we find that a sample of 20 lensed SNe Ia would allow us to constrain the Hubble constant (H0) with 1.3% uncertainty in the flat ΛCDM cosmology. We find a similar constraint on H0 in an open ΛCDM cosmology, while the constraint degrades to 3% in a flat wCDM cosmology. We anticipate lensed SNe to be an independent and powerful probe of SN physics and cosmology in the upcoming LSST era.

(210)Another SMEFT story: Z' facing new results on ɛ'/ɛ, ΔM<SUB>K</SUB> and K → πν ν ¯
• Jason Aebischer,
• Andrzej J. Buras,
• Jacky Kumar
Journal of High Energy Physics, 2020 (12/2020) doi:10.1007/JHEP12(2020)097
abstract + abstract -

Recently the RBC-UKQCD lattice QCD collaboration presented new results for the hadronic matrix elements relevant for the ratio ɛ'/ɛ in the Standard Model (SM) albeit with significant uncertainties. With the present knowledge of the Wilson coefficients and isospin breaking effects there is still a sizable room left for new physics (NP) contributions to ɛ'/ɛ which could both enhance or suppress this ratio to agree with the data. The new SM value for the K0 - K¯0 mass difference ΔMK from RBC-UKQCD is on the other hand by 2σ above the data hinting for NP required to suppress ΔMK. Simultaneously the most recent results for K+ → π+ν ν ¯ from NA62 and for KL → π0ν ν ¯ from KOTO still allow for significant NP contributions. We point out that the suppression of ΔMK by NP requires the presence of new CP-violating phases with interesting implications for K → πν ν ¯, KS → μ+μ- and KL → π0+- decays. Considering a Z'-scenario within the SMEFT we analyze the dependence of all these observables on the size of NP still allowed by the data on ɛ'/ɛ. The hinted ΔMK anomaly together with the ɛK constraint implies in the presence of only left-handed (LH) or right-handed (RH) flavour-violating Z' couplings strict correlation between K+ → π+ν ν ¯ and KL → π0ν ν ¯ branching ratios so that they are either simultaneously enhanced or suppressed relative to SM predictions. An anticorrelation can only be obtained in the presence of both LH and RH couplings. Interestingly, the NP QCD penguin scenario for ɛ'/ɛ is excluded by SMEFT renormalization group effects in ɛK so that NP effects in ɛ'/ɛ are governed by electroweak penguins. We also investigate for the first time whether the presence of a heavy Z' with flavour violating couplings could generate through top Yukawa renormalization group effects FCNCs mediated by the SM Z-boson. The outcome turns out to be very interesting.

(209)Classical Yang-Mills observables from amplitudes
• Leonardo de la Cruz,
• Ben Maybee,
• Donal O'Connell,
• Alasdair Ross
Journal of High Energy Physics, 2020 (12/2020) doi:10.1007/JHEP12(2020)076
abstract + abstract -

The double copy suggests that the basis of the dynamics of general relativity is Yang-Mills theory. Motivated by the importance of the relativistic two-body problem, we study the classical dynamics of colour-charged particle scattering from the perspective of amplitudes, rather than equations of motion. We explain how to compute the change of colour, and the radiation of colour, during a classical collision. We apply our formalism at next-to-leading order for the colour change and at leading order for colour radiation.

(208)Topological Phase Transition in Coupled Rock-Paper-Scissors Cycles
• Johannes Knebel,
• Philipp M. Geiger,
• Erwin Frey
Physical Review Letters, 125 (12/2020) doi:10.1103/PhysRevLett.125.258301
abstract + abstract -

A hallmark of topological phases is the occurrence of topologically protected modes at the system's boundary. Here, we find topological phases in the antisymmetric Lotka-Volterra equation (ALVE). The ALVE is a nonlinear dynamical system and describes, for example, the evolutionary dynamics of a rock-paper-scissors cycle. On a one-dimensional chain of rock-paper-scissor cycles, topological phases become manifest as robust polarization states. At the transition point between left and right polarization, solitary waves are observed. This topological phase transition lies in symmetry class D within the "tenfold way" classification as also realized by 1D topological superconductors.

(207)Broadband electrical action sensing techniques with conducting wires for low-mass dark matter axion detection
• Michael E. Tobar,
• Ben T. McAllister,
• Maxim Goryachev
Physics of the Dark Universe, 30 (12/2020) doi:10.1016/j.dark.2020.100624
abstract + abstract -

Due to the inverse Primakoff effect, it has been shown that when axions mix with a DC B →-field, the resulting electrical action will produce an AC electromotive force, which oscillates at the Compton frequency of the axion. As in standard electrodynamics, this electromotive force may be modelled as an oscillating effective impressed magnetic current boundary source. We use this result to calculate the sensitivity of new experiments to low-mass axions using the quasi-static technique, defined as when the Compton wavelength of the axion is greater than the dimensions of the experiment. First, we calculate the current induced in a straight conducting wire (electric dipole antenna) in the limit where the DC B →-field can be considered as spatially constant and show that it has a sensitivity proportional to the axion mass. Following this we extend the topology by making use of the full extent of the spatially varying DC B →-field of the electromagnet. This is achieved by transforming the 1D conducting wire to a 2D winding with inductance, to fully link the effective magnetic current boundary source and hence couple to the full axion induced electrical action (or electromotive force). We investigate two different topologies: The first uses a single winding, and couples to the effective short circuit current generated in the winding, which is optimally read out using a sensitive low impedance SQUID amplifier: The second technique uses multiple windings, with every turn effectively increasing the induced voltage, which is proportional to the winding number. The read out of this configuration is optimised by implementing a cryogenic low-noise high input impedance voltage amplifier. The end result is the realisation of new Broadband Electrical Action Sensing Techniques with orders of magnitude improved sensitivity over current low-mass axion experiments, with a sensitivity linearly proportional to the axion-photon coupling and capable of detecting QCD dark matter axions in the mass range of 10-12 - 10-8 eV and below.

(206)Precision cosmology with voids in the final BOSS data
• Nico Hamaus,
• Alice Pisani,
• Jin-Ah Choi,
• Guilhem Lavaux,
• Benjamin D. Wandelt
• +1
Journal of Cosmology and Astroparticle Physics, 2020 (12/2020) doi:10.1088/1475-7516/2020/12/023
abstract + abstract -

We report novel cosmological constraints obtained from cosmic voids in the final BOSS DR12 dataset. They arise from the joint analysis of geometric and dynamic distortions of average void shapes (i.e., the stacked void-galaxy cross-correlation function) in redshift space. Our model uses tomographic deprojection to infer real-space void profiles and self-consistently accounts for the Alcock-Paczynski (AP) effect and redshift-space distortions (RSD) without any prior assumptions on cosmology or structure formation. It is derived from first physical principles and provides an extremely good description of the data at linear perturbation order. We validate this model with the help of mock catalogs and apply it to the final BOSS data to constrain the RSD and AP parameters f/b and DA H/c, where f is the linear growth rate, b the linear galaxy bias, DA the comoving angular diameter distance, H the Hubble rate, and c the speed of light. In addition, we include two nuisance parameters in our analysis to marginalize over potential systematics. We obtain f/b=0.540±0.091 and DA H/c=0.588±0.004 from the full void sample at a mean redshift of z=0.51. In a flat ΛCDM cosmology, this implies Ωm=0.312±0.020 for the present-day matter density parameter. When we use additional information from the survey mocks to calibrate our model, these constraints improve to f/b=0.347±0.023, DA H/c=0.588±0.003, and Ωm = 0.310 ± 0.017. However, we emphasize that the calibration depends on the specific model of cosmology and structure formation assumed in the mocks, so the calibrated results should be considered less robust. Nevertheless, our calibration-independent constraints are among the tightest of their kind to date, demonstrating the immense potential of using cosmic voids for cosmology in current and future data.

(205)Mapping the stellar age of the Milky Way bulge with the VVV. III. High-resolution reddening map
• F. Surot,
• E. Valenti,
• O. A. Gonzalez,
• M. Zoccali,
• E. Sökmen
• +2
Astronomy and Astrophysics, 644, p11 (12/2020) doi:10.1051/0004-6361/202038346
abstract + abstract -

Context. A detailed study of the Galactic bulge stellar population necessarily requires an accurate representation of the interstellar extinction, particularly toward the Galactic plane and center, where severe and differential reddening is expected to vary on sub-arcmin scales. Although recent infrared surveys have addressed this problem by providing extinction maps across the whole Galactic bulge area, dereddened color-magnitude diagrams near the plane and center appear systematically undercorrected, prompting the need for higher resolution. These undercorrections affect any stellar study sensitive to color (e.g., star formation history analyses via color-magnitude diagram fitting), either making them inaccurate or limiting them to small and relatively stable extinction windows where this value is low and better constrained.
Aims: This study is aimed at providing a high-resolution (2 arcmin to ∼10 arcsec) color excess map for the VVV bulge area in J - Ks color.
Methods: We used the MW-BULGE-PSFPHOT catalogs, sampling ∼300 deg2 across the Galactic bulge (|l| < 10° and -10° < b < 5°) to isolate a sample of red clump and red giant branch stars, for which we calculated the average J - Ks color in a fine spatial grid in (l, b) space.
Results: We obtained an E(J - Ks) map spanning the VVV bulge area of roughly 300 deg2, with the equivalent of a resolution between ∼1 arcmin for bulge outskirts (l < 6°) to below 20 arcsec within the central |l| < 1°, and below 10 arcsec for the innermost area (|l| < 1° and |b| < 3°).

The map is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/644/A140

Based on observations taken within the ESO VISTA Public Survey VVV, Program ID 179.B-2002 (PI: Minniti, Lucas).

The result is publicly available at http://basti-iac.oa-teramo.inaf.it/vvvexmap/

(204)SMEFT atlas of ΔF = 2 transitions
• Jason Aebischer,
• Christoph Bobeth,
• Andrzej J. Buras,
• Jacky Kumar
Journal of High Energy Physics, 2020 (12/2020) doi:10.1007/JHEP12(2020)187
abstract + abstract -

We present a model-independent anatomy of the ΔF = 2 transitions K0-K¯0, Bs,d-B¯s ,d and D0-D¯0 in the context of the Standard Model Effective Field Theory (SMEFT). We present two master formulae for the mixing amplitude [M12]BSM. One in terms of the Wilson coefficients (WCs) of the Low-Energy Effective Theory (LEFT) operators evaluated at the electroweak scale μew and one in terms of the WCs of the SMEFT operators evaluated at the BSM scale Λ. The coefficients Paij entering these formulae contain all the information below the scales μew and Λ, respectively. Renormalization group effects from the top-quark Yukawa coupling play the most important role. The collection of the individual contributions of the SMEFT operators to [M12]BSM can be considered as the SMEFT atlas of ΔF = 2 transitions and constitutes a travel guide to such transitions far beyond the scales explored by the LHC. We emphasize that this atlas depends on whether the down-basis or the up-basis for SMEFT operators is considered. We illustrate this technology with tree-level exchanges of heavy gauge bosons (Z', G') and corresponding heavy scalars.

(203)Responses of Halo Occupation Distributions: a new ingredient in the halo model &amp; the impact on galaxy bias
• Rodrigo Voivodic,
• Alexandre Barreira
arXiv e-prints (12/2020) e-Print:2012.04637
abstract + abstract -

Halo occupation distribution (HOD) models describe the number of galaxies that reside in different haloes, and are widely used in galaxy-halo connection studies using the halo model (HM). Here, we introduce and study HOD response functions $R_\mathcal{O}^g$ that describe the response of the HODs to long-wavelength perturbations $\mathcal{O}$. The linear galaxy bias parameters $b_\mathcal{O}^g$ are a weighted version of $b_\mathcal{O}^h + R_\mathcal{O}^g$, where $b_\mathcal{O}^h$ is the halo bias, but the contribution from $R_\mathcal{O}^g$ is routinely ignored in the literature. We investigate the impact of this by measuring the $R_\mathcal{O}^g$ in separate universe simulations of the IllustrisTNG model for three types of perturbations: total matter perturbations, $\mathcal{O}=\delta_m$; baryon-CDM compensated isocurvature perturbations, $\mathcal{O}=\sigma$; and potential perturbations with local primordial non-Gaussianity, $\mathcal{O}\propto f_{\rm NL}\phi$. Our main takeaway message is that the $R_\mathcal{O}^g$ are not negligible in general and their size should be estimated on a case-by-case basis. For stellar-mass selected galaxies, the responses $R_\phi^g$ and $R_\sigma^g$ are sizeable and cannot be neglected in HM calculations of the bias parameters $b_\phi^g$ and $b_\sigma^g$; this is relevant to constrain inflation using galaxies. On the other hand, we do not detect a strong impact of the HOD response $R_1^g$ on the linear galaxy bias $b_1^g$. These results can be explained by the impact that the perturbations have on stellar-to-total-mass relations. We also look into the impact on the bias of the gas distribution and find similar conclusions. We show that a single extra parameter describing the overall amplitude of $R_\mathcal{O}^g$ recovers the measured $b_\mathcal{O}^g$ well, which indicates that $R_\mathcal{O}^g$ can be easily added to HM/HOD studies as a new ingredient.

(202)LiteBIRD satellite: JAXA's new strategic L-class mission for all-sky surveys of cosmic microwave background polarization
• M. Hazumi,
• E. Allys,
• K. Arnold
• +233
• D. Auguste,
• J. Aumont,
• R. Aurlien,
• J. Austermann,
• C. Baccigalupi,
• A. J. Banday,
• R. Banjeri,
• R. B. Barreiro,
• S. Basak,
• J. Beall,
• D. Beck,
• S. Beckman,
• J. Bermejo,
• P. de Bernardis,
• M. Bersanelli,
• J. Bonis,
• J. Borrill,
• F. Boulanger,
• S. Bounissou,
• M. Brilenkov,
• M. Brown,
• M. Bucher,
• E. Calabrese,
• P. Campeti,
• A. Carones,
• F. J. Casas,
• A. Challinor,
• V. Chan,
• K. Cheung,
• Y. Chinone,
• J. F. Cliche,
• L. Colombo,
• F. Columbro,
• J. Cubas,
• A. Cukierman,
• D. Curtis,
• G. D'Alessandro,
• N. Dachlythra,
• M. De Petris,
• C. Dickinson,
• P. Diego-Palazuelos,
• M. Dobbs,
• T. Dotani,
• L. Duband,
• S. Duff,
• J. M. Duval,
• K. Ebisawa,
• T. Elleflot,
• H. K. Eriksen,
• J. Errard,
• T. Essinger-Hileman,
• F. Finelli,
• R. Flauger,
• C. Franceschet,
• U. Fuskeland,
• M. Galloway,
• K. Ganga,
• J. R. Gao,
• R. Genova-Santos,
• M. Gerbino,
• M. Gervasi,
• T. Ghigna,
• E. Gjerløw,
• J. Grain,
• F. Grupp,
• A. Gruppuso,
• J. E. Gudmundsson,
• T. de Haan,
• N. W. Halverson,
• P. Hargrave,
• T. Hasebe,
• M. Hasegawa,
• M. Hattori,
• S. Henrot-Versillé,
• D. Herman,
• D. Herranz,
• C. A. Hill,
• G. Hilton,
• Y. Hirota,
• E. Hivon,
• R. A. Hlozek,
• Y. Hoshino,
• E. de la Hoz,
• J. Hubmayr,
• K. Ichiki,
• T. Iida,
• K. Ishimura,
• H. Ishino,
• G. Jaehnig,
• T. Kaga,
• S. Kashima,
• N. Katayama,
• A. Kato,
• T. Kawasaki,
• R. Keskitalo,
• T. Kisner,
• Y. Kobayashi,
• N. Kogiso,
• A. Kogut,
• K. Kohri,
• E. Komatsu,
• K. Komatsu,
• K. Konishi,
• N. Krachmalnicoff,
• I. Kreykenbohm,
• C. L. Kuo,
• A. Kushino,
• L. Lamagna,
• J. V. Lanen,
• M. Lattanzi,
• A. T. Lee,
• C. Leloup,
• F. Levrier,
• E. Linder,
• T. Louis,
• G. Luzzi,
• T. Maciaszek,
• B. Maffei,
• D. Maino,
• M. Maki,
• S. Mandelli,
• E. Martinez-Gonzalez,
• S. Masi,
• T. Matsumura,
• A. Mennella,
• M. Migliaccio,
• Y. Minami,
• K. Mitsuda,
• J. Montgomery,
• L. Montier,
• G. Morgante,
• B. Mot,
• Y. Murata,
• J. A. Murphy,
• M. Nagai,
• Y. Nagano,
• T. Nagasaki,
• R. Nagata,
• S. Nakamura,
• T. Namikawa,
• P. Natoli,
• S. Nerval,
• T. Nishibori,
• H. Nishino,
• F. Noviello,
• C. O'Sullivan,
• H. Ogawa,
• H. Ogawa,
• S. Oguri,
• H. Ohsaki,
• I. S. Ohta,
• L. Pagano,
• A. Paiella,
• D. Paoletti,
• G. Patanchon,
• J. Peloton,
• F. Piacentini,
• G. Pisano,
• 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. Sandri,
• M. Sasaki,
• G. Savini,
• D. Scott,
• J. Seibert,
• Y. Sekimoto,
• B. Sherwin,
• K. Shinozaki,
• M. Shiraishi,
• P. Shirron,
• G. Signorelli,
• G. Smecher,
• S. Stever,
• R. Stompor,
• H. Sugai,
• S. Sugiyama,
• A. Suzuki,
• J. Suzuki,
• T. L. Svalheim,
• E. Switzer,
• R. Takaku,
• H. Takakura,
• S. Takakura,
• Y. Takase,
• Y. Takeda,
• A. Tartari,
• E. Taylor,
• Y. Terao,
• H. Thommesen,
• K. L. Thompson,
• B. Thorne,
• T. Toda,
• M. Tomasi,
• M. Tominaga,
• N. Trappe,
• M. Tristram,
• M. Tsuji,
• M. Tsujimoto,
• C. Tucker,
• J. Ullom,
• G. Vermeulen,
• P. Vielva,
• F. Villa,
• M. Vissers,
• N. Vittorio,
• I. Wehus,
• J. Weller,
• B. Westbrook,
• J. Wilms,
• B. Winter,
• E. J. Wollack,
• N. Y. Yamasaki,
• T. Yoshida,
• J. Yumoto,
• M. Zannoni,
• A. Zonca
• (less)
Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 11443, p20 (12/2020) doi:10.1117/12.2563050
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. JAXA selected LiteBIRD in May 2019 as a strategic large-class (L-class) mission, with its expected launch in the late 2020s using JAXA's H3 rocket. LiteBIRD plans to map the cosmic microwave background (CMB) polarization over the full sky with unprecedented precision. Its main scientific objective is to carry out a definitive 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 an insight into the quantum nature of gravity and other new physics beyond the standard models of particle physics and cosmology. To this end, LiteBIRD will perform full-sky surveys for three years at the Sun-Earth Lagrangian point L2 for 15 frequency bands between 34 and 448 GHz with three telescopes, to achieve a total sensitivity of 2.16 μK-arcmin with a typical angular resolution of 0.5° at 100 GHz. We provide an overview of the LiteBIRD project, including scientific objectives, mission requirements, top-level system requirements, operation concept, and expected scientific outcomes.

(201)Arguments against using h<SUP>-1</SUP> Mpc units in observational cosmology
• Ariel G. Sánchez
Physical Review D, 102 (12/2020) doi:10.1103/PhysRevD.102.123511
abstract + abstract -

It is common to express cosmological measurements in units of h-1 Mpc . Here, we review some of the complications that originate from this practice. A crucial problem caused by these units is related to the normalization of the matter power spectrum, which is commonly characterized in terms of the linear-theory rms mass fluctuation in spheres of radius 8 h-1 Mpc , σ8. This parameter does not correctly capture the impact of h on the amplitude of density fluctuations. We show that the use of σ8 has caused critical misconceptions for both the so-called σ8 tension regarding the consistency between low-redshift probes and cosmic microwave background data and the way in which growth-rate estimates inferred from redshift-space distortions are commonly expressed. We propose to abandon the use of h-1 Mpc units in cosmology and to characterize the amplitude of the matter power spectrum in terms of σ12, defined as the mass fluctuation in spheres of radius 12 Mpc, whose value is similar to the standard σ8 for h ∼0.67 .

(200)Driving galactic winds with magnetic fields at low and high redshift
• Ulrich P. Steinwandel,
• Klaus Dolag,
• Harald Lesch,
• Andreas Burkert
arXiv e-prints (12/2020) e-Print:2012.12905
abstract + abstract -

Although playing a key role for our understanding of the evolution of galaxies, the exact way how observed 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-axis-symmetric instabilities in galaxies (bars, spiral-arms, warps) can lead to local exponential magnetic field growth by a radial flows beyond the equipartition value by at least two orders of magnitude on a time-scale 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 $\eta \approx 0.1$, in agreement with our numerical simulations. Moreover, our outflow mechanism could contribute to an understanding of the large fraction of bared 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 (SFR) in our model together with cross-correlated masses from the star-forming main-sequence at redshifts $z\sim2$ allow us to estimate the outflow rate and mass loading factors by non-axis-symmetric instabilities and a subsequent radial inflow dynamo, giving mass loading factors of $\eta \approx 0.1$ for galaxies in the range of M$_{\star}=10^9 - 10^{12}$ M$_{\odot}$, in good agreement with recent results of Sinfoni and KMOS$^{3\mathrm{D}}$.

(199)Overview of the medium and high frequency telescopes of the LiteBIRD space mission
• L. Montier,
• B. Mot,
• P. de Bernardis,
• B. Maffei,
• G. Pisano
• +232
• F. Columbro,
• J. E. Gudmundsson,
• S. Henrot-Versillé,
• L. Lamagna,
• J. Montgomery,
• T. Prouvé,
• M. Russell,
• G. Savini,
• S. Stever,
• K. L. Thompson,
• M. Tsujimoto,
• C. Tucker,
• B. Westbrook,
• E. Allys,
• K. Arnold,
• D. Auguste,
• J. Aumont,
• R. Aurlien,
• J. Austermann,
• C. Baccigalupi,
• A. J. Banday,
• R. Banerji,
• R. B. Barreiro,
• S. Basak,
• J. Beall,
• D. Beck,
• S. Beckman,
• J. Bermejo,
• M. Bersanelli,
• J. Bonis,
• J. Borrill,
• F. Boulanger,
• S. Bounissou,
• M. Brilenkov,
• M. Brown,
• M. Bucher,
• E. Calabrese,
• P. Campeti,
• A. Carones,
• F. J. Casas,
• A. Challinor,
• V. Chan,
• K. Cheung,
• Y. Chinone,
• J. F. Cliche,
• L. Colombo,
• J. Cubas,
• A. Cukierman,
• D. Curtis,
• G. D'Alessandro,
• N. Dachlythra,
• M. De Petris,
• C. Dickinson,
• P. Diego-Palazuelos,
• M. Dobbs,
• T. Dotani,
• L. Duband,
• S. Duff,
• J. M. Duval,
• K. Ebisawa,
• T. Elleflot,
• H. K. Eriksen,
• J. Errard,
• T. Essinger-Hileman,
• F. Finelli,
• R. Flauger,
• C. Franceschet,
• U. Fuskeland,
• M. Galloway,
• K. Ganga,
• J. R. Gao,
• R. Genova-Santos,
• M. Gerbino,
• M. Gervasi,
• T. Ghigna,
• E. Gjerløw,
• J. Grain,
• F. Grupp,
• A. Gruppuso,
• T. de Haan,
• N. W. Halverson,
• P. Hargrave,
• T. Hasebe,
• M. Hasegawa,
• M. Hattori,
• M. Hazumi,
• D. Herman,
• D. Herranz,
• C. A. Hill,
• G. Hilton,
• Y. Hirota,
• E. Hivon,
• R. A. Hlozek,
• Y. Hoshino,
• E. de la Hoz,
• J. Hubmayr,
• K. Ichiki,
• T. Iida,
• K. Ishimura,
• H. Ishino,
• G. Jaehnig,
• T. Kaga,
• S. Kashima,
• N. Katayama,
• A. Kato,
• T. Kawasaki,
• R. Keskitalo,
• T. Kisner,
• Y. Kobayashi,
• N. Kogiso,
• A. Kogut,
• K. Kohri,
• E. Komatsu,
• K. Komatsu,
• K. Konishi,
• N. Krachmalnicoff,
• I. Kreykenbohm,
• C. L. Kuo,
• A. Kushino,
• J. V. Lanen,
• M. Lattanzi,
• A. T. Lee,
• C. Leloup,
• F. Levrier,
• E. Linder,
• T. Louis,
• G. Luzzi,
• T. Maciaszek,
• D. Maino,
• M. Maki,
• S. Mandelli,
• E. Martinez-Gonzalez,
• S. Masi,
• T. Matsumura,
• A. Mennella,
• M. Migliaccio,
• Y. Minami,
• K. Mitsuda,
• G. Morgante,
• Y. Murata,
• J. A. Murphy,
• M. Nagai,
• Y. Nagano,
• T. Nagasaki,
• R. Nagata,
• S. Nakamura,
• T. Namikawa,
• P. Natoli,
• S. Nerval,
• T. Nishibori,
• H. Nishino,
• C. O'Sullivan,
• H. Ogawa,
• H. Ogawa,
• S. Oguri,
• H. Ohsaki,
• I. S. Ohta,
• L. Pagano,
• A. Paiella,
• D. Paoletti,
• G. Patanchon,
• J. Peloton,
• F. Piacentini,
• G. Polenta,
• D. Poletti,
• G. Puglisi,
• D. Rambaud,
• C. Raum,
• S. Realini,
• M. Reinecke,
• M. Remazeilles,
• A. Ritacco,
• G. Roudil,
• J. A. Rubino-Martin,
• H. Sakurai,
• Y. Sakurai,
• M. Sandri,
• M. Sasaki,
• D. Scott,
• J. Seibert,
• Y. Sekimoto,
• B. Sherwin,
• K. Shinozaki,
• M. Shiraishi,
• P. Shirron,
• G. Signorelli,
• G. Smecher,
• R. Stompor,
• H. Sugai,
• S. Sugiyama,
• A. Suzuki,
• J. Suzuki,
• T. L. Svalheim,
• E. Switzer,
• R. Takaku,
• H. Takakura,
• S. Takakura,
• Y. Takase,
• Y. Takeda,
• A. Tartari,
• E. Taylor,
• Y. Terao,
• H. Thommesen,
• B. Thorne,
• T. Toda,
• M. Tomasi,
• M. Tominaga,
• N. Trappe,
• M. Tristram,
• M. Tsuji,
• J. Ullom,
• G. Vermeulen,
• P. Vielva,
• F. Villa,
• M. Vissers,
• N. Vittorio,
• I. Wehus,
• J. Weller,
• J. Wilms,
• B. Winter,
• E. J. Wollack,
• N. Y. Yamasaki,
• T. Yoshida,
• J. Yumoto,
• M. Zannoni,
• A. Zonca
• (less)
Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 11443, p21 (12/2020) doi:10.1117/12.2562243
abstract + abstract -

LiteBIRD is a JAXA-led Strategic Large-Class mission designed to search for the existence of the primordial gravitational waves produced during the inflationary phase of the Universe, through the measurements of their imprint onto the polarization of the cosmic microwave background (CMB). These measurements, requiring unprecedented sensitivity, will be performed over the full sky, at large angular scales, and over 15 frequency bands from 34 GHz to 448 GHz. The LiteBIRD instruments consist of three telescopes, namely the Low-, Medium-and High-Frequency Telescope (respectively LFT, MFT and HFT). We present in this paper an overview of the design of the Medium-Frequency Telescope (89{224 GHz) and the High-Frequency Telescope (166{448 GHz), the so-called MHFT, under European responsibility, which are two cryogenic refractive telescopes cooled down to 5 K. They include a continuous rotating half-wave plate as the first optical element, two high-density polyethylene (HDPE) lenses and more than three thousand transition-edge sensor (TES) detectors cooled to 100 mK. We provide an overview of the concept design and the remaining specific challenges that we have to face in order to achieve the scientific goals of LiteBIRD.

(198)Fuzzy Dark Matter and Dark Matter Halo Cores
• A. Burkert
The Astrophysical Journal, 904, p6 (12/2020) doi:10.3847/1538-4357/abb242
abstract + abstract -

Whereas cold dark matter (CDM) simulations predict central dark matter cusps with densities that diverge as ρ(r) ∼ 1/r, observations often indicate constant-density cores with finite central densities ρ0 and a flat density distribution within a core radius r0. This paper investigates whether this core-cusp problem can be solved by fuzzy dark matter (FDM), a hypothetical particle with a mass of the order of m ≍ 10-22 eV and a corresponding de Broglie wavelength on astrophysical scales. We show that galaxies with CDM halo virial masses Mvir ≤ 1011M follow two core-scaling relations. In addition to the well-known universal core column density Σ0 ≡ ρ0 × r0 = 75 ${M}_{\odot }$ pc-2, core radii increase with virial masses as r0 ∼ ${M}_{\mathrm{vir}}^{\gamma }$ with γ of order unity. Using the simulations by Schive et al. we demonstrate that FDM can explain the r0-Mvir scaling relation if the virial masses of the observed galaxy sample scale with the formation redshift z as Mvir ∼ (1 + z)-0.4. The observed constant Σ0 is however in complete disagreement with FDM cores which are characterized by a steep dependence Σ0 ∼ r ${}_{0}^{-3}$ , independent of z. More high-resolution simulations are now required to confirm the simulations of Schive et al. and explore the transition region between the soliton core and the surrounding halo. If these results hold, FDM can be ruled out as the origin of observed dark matter cores and other physical processes are required to account for their formation.

(197)Measuring Dark Matter in Galaxies: The Mass Fraction within Five Effective Radii
• William E. Harris,
• Rhea-Silvia Remus,
• Gretchen L. H. Harris,
• Iu. V. Babyk
The Astrophysical Journal, 905, p17 (12/2020) doi:10.3847/1538-4357/abc429
abstract + abstract -

Large galaxies may contain an "atmosphere" of hot interstellar X-ray gas, and the temperature and radial density profile of this gas can be used to measure the total mass of the galaxy contained within a given radius r. We use this technique for 102 early-type galaxies with stellar masses M > 1010M, to evaluate the mass fraction of dark matter (DM) within the fiducial radius r = 5re, denoted f5 = fDM(5re). On average, these systems have a median $\overline{{f}_{5}}\simeq 0.8\mbox{--}0.9$ with a typical galaxy-to-galaxy scatter ±0.15. Comparisons with mass estimates made through the alternative techniques of satellite dynamics (e.g., velocity distributions of globular clusters, planetary nebulae, satellite dwarfs) as well as strong lensing show encouraging consistency over the same range of stellar mass. We find that many of the disk galaxies (S0/SA0/SB0) have a significantly higher mean f5 than do the pure ellipticals, by Δf5 ≃ 0.1. We suggest that this higher level may be a consequence of sparse stellar haloes and quieter histories with fewer major episodes of feedback or mergers. Comparisons are made with the Magneticum Pathfinder suite of simulations for both normal and centrally dominant "Brightest Cluster" galaxies. Though the observed data exhibit somewhat larger scatter at a given galaxy mass than do the simulations, the mean level of DM mass fraction for all classes of galaxies is in good first-order agreement with the simulations. Finally, we find that the group galaxies with stellar masses near M ∼ 1011M have relatively more outliers at low f5 than in other mass ranges, possibly the result of especially effective AGN feedback in that mass range leading to expansion of their DM halos.

(196)Galaxy power spectrum multipoles covariance in perturbation theory
• Román Scoccimarro
Physical Review D, 102 (12/2020) doi:10.1103/PhysRevD.102.123517
abstract + abstract -

We compute the covariance of the galaxy power spectrum multipoles in perturbation theory, including the effects of nonlinear evolution, nonlinear and nonlocal bias, radial redshift-space distortions, arbitrary survey window, and shot noise. We rewrite the power spectrum FKP estimator in terms of the usual windowed galaxy fluctuations and the fluctuations in the number of galaxies inside the survey volume. We show that this leads to a stronger supersample covariance than assumed in the literature and causes a substantial leakage of Gaussian information. We decompose the covariance matrix into several contributions that provide an insight into its behavior for different biased tracers. We show that for realistic surveys, the covariance of power spectrum multipoles is already dominated by shot noise and super survey mode coupling in the weakly nonlinear regime. Both these effects can be accurately modeled analytically, making a perturbative treatment of the covariance very compelling. Our method allows for the covariance to be varied as a function of cosmology and bias parameters very efficiently, with survey geometry entering as fixed kernels that can be computed separately using fast fourier transforms (FFTs). We find excellent agreement between our analytic covariance and that estimated from BOSS DR12 Patchy mock catalogs in the whole range we tested, up to k =0.6 h /Mpc . This bodes well for application to future surveys such as DESI and Euclid.

(195)EMERGE - empirical constraints on the formation of passive galaxies
• Benjamin P. Moster,
• Thorsten Naab,
• Simon D. M. White
Monthly Notices of the Royal Astronomical Society, 499, p20 (12/2020) doi:10.1093/mnras/staa3019
abstract + abstract -

We present constraints on the emergence and evolution of passive galaxies with the empirical model EMERGE, which reproduces the evolution of stellar mass functions (SMFs), specific and cosmic star formation rates since $z$ ≍ 10, 'quenched' galaxy fractions, and correlation functions. At fixed halo mass, present-day passive galaxies are more massive than active galaxies, whereas at fixed stellar mass passive galaxies populate more massive haloes in agreement with observations. This effect naturally results from the shape and scatter of the stellar-to-halo mass relation. The stellar mass assembly of present-day passive galaxies is dominated by 'in situ' star formation below ∼3 × 1011 M and by merging and accretion of 'ex situ' formed stars at higher mass. The mass dependence is in tension with current cosmological simulations. Lower mass passive galaxies show extended star formation towards low redshift in agreement with IFU surveys. All passive galaxies have main progenitors on the 'main sequence of star formation' with the 'red sequence' appearing at $z$ ≍ 2. Above this redshift, over 95 per cent of the progenitors of passive galaxies are active. More than 90 per cent of $z$ ≍ 2 'main sequence' galaxies with m* > 1010 M evolve into present-day passive galaxies. Above redshift 6, more than 80 per cent of the observed SMFs above 109 M can be accounted for by progenitors of passive galaxies with m* > 1010 M. This implies that high-redshift observations mainly probe the birth of present-day passive galaxies. EMERGE is available at github.com/bmoster/emerge.

(194)Environmental stability achieved for the Manfred Hirt Planet Spectrograph
• Vanessa Fahrenschon,
• Hanna Kellermann,
• Liang Wang,
• Frank Grupp,
• Claus Gössl
• +7
• Ulrich Hopp,
• Wolfgang Mitsch,
• Michael Schmidt,
• Christoph Ries,
• Jana Steuer,
• Roberto Saglia,
• Ralf Bender
• (less)
Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 11447, p20 (12/2020) doi:10.1117/12.2560944
abstract + abstract -

The Manfred Hirt Planet Spectrograph (MaHPS) — formerly also referred to as FOCES — is a high-resolution echelle spectrograph at the 2m telescope of the Wendelstein Observatory. One of its main scientific goals is the detection of planets at the few m/s level. To achieve such high precisions on a long-term scale, environmental stabilization of the instrument is required. The currently used temperature and pressure control systems are introduced and we present two different temperature control setups, with two and three actively controlled layers respectively. A series of measurements with an Astro Frequency Comb (AFC) as calibrator is shown to illustrate the system performance.

(193)Verification observations of the Manfred Hirt Planet Spectrograph
• Hanna Kellermann,
• Liang Wang,
• Vanessa Fahrenschon,
• Jana Steuer,
• Fei Zhao
• +7
• Frank Grupp,
• Michael Schmidt,
• Christoph Ries,
• Claus Goessel,
• Wolfgang Mitsch,
• Ulrich Hopp,
• Ralf Bender
• (less)
Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 11447, p10 (12/2020) doi:10.1117/12.2562495
abstract + abstract -

The Manfred Hirt Planet Spectrograph - formerly operated under the name FOCES - started its regular scientific observation program in fall 2019 at the 2m telescope of the Wendelstein Observatory, operated by the University Observatory of the LMU Munich. We present the first radial velocity stability measurements of an astronomical target, the 51 Pegasi b exoplanet system, utilizing our Astro Frequency Comb (ACF) for wavelength calibration. For computing RV shifts from orderwisely extracted Echelle spectra we have developed a new software pipeline. In this proceeding we will introduce the most important features of our pipeline: wavelength calibration with simultaneously recorded spectra of the AFC, generation of spectral templates, and an optional fit or cross- correlation function (CCF) for the calculation of the relative RV signals. Finally, the performance of the pipeline real data is demonstrated.

(192)The strange case of the transient HBL blazar 4FGL J1544.3-0649
• N. Sahakyan,
• P. Giommi
Mon.Not.Roy.Astron.Soc., 502, p836 (11/2020) e-Print:2011.10237 doi:10.1093/mnras/stab011
abstract + abstract -

We present a multifrequency study of the transient γ-ray source 4FGL J1544.3−0649, a blazar that exhibited a remarkable behaviour raising from the state of an anonymous mid-intensity radio source, never detected at high energies, to that of one of the brightest extreme blazars in the X-ray and γ-ray sky. Our analysis shows that the averaged γ-ray spectrum is well described by a power law with a photon index of 1.87 ± 0.04, while the flux above 100 MeV is (8.0 ± 0.9) × 10^−9 photon cm^−2 s^−1, which increases during the active state of the source. The X-ray flux and spectral slope are both highly variable, with the highest 2–10 keV flux reaching (1.28 ± 0.05) × 10^−10 erg cm^−2 s^−1. On several observations, the X-ray spectrum hardened to the point implying as SED peak moving to energies larger than 10 keV. As in many extreme blazars the broad-band spectral energy distribution can be described by a homogeneous one-zone synchrotron-self-Compton leptonic model. We briefly discuss the potential implications for high-energy multimessenger astrophysics in case the dual behaviour shown by 4FGL J1544.3−0649 does not represent an isolated case, but rather a manifestation of a so far unnoticed relatively common phenomenon.

(191)Towards testing the theory of gravity with DESI: summary statistics, model predictions and future simulation requirements
• Christian Arnold,
• Alejandro Aviles,
• Rachel Bean,
• Yan-Chuan Cai
• +31
• Marius Cautun,
• Jorge L. Cervantes-Cota,
• Carolina Cuesta-Lazaro,
• N. Chandrachani Devi,
• Alexander Eggemeier,
• Sebastien Fromenteau,
• Alma X. Gonzalez-Morales,
• Vitali Halenka,
• Jian-hua He,
• Wojciech A. Hellwing,
• César Hernández-Aguayo,
• Mustapha Ishak,
• Kazuya Koyama,
• Baojiu Li,
• Axel de la Macorra,
• Jennifer Menesses Rizo,
• Christopher Miller,
• Eva-Maria Mueller,
• Gustavo Niz,
• Pierros Ntelis,
• Matias Rodríguez Otero,
• Cristiano G. Sabiu,
• Zachary Slepian,
• Alejo Stark,
• Octavio Valenzuela,
• Georgios Valogiannis,
• Mariana Vargas-Magaña,
• Hans A. Winther,
• Pauline Zarrouk,
• Gong-Bo Zhao,
• Yi Zheng
• (less)
abstract + abstract -

Shortly after its discovery, General Relativity (GR) was applied to predict the behavior of our Universe on the largest scales, and later became the foundation of modern cosmology. Its validity has been verified on a range of scales and environments from the Solar system to merging black holes. However, experimental confirmations of GR on cosmological scales have so far lacked the accuracy one would hope for — its applications on those scales being largely based on extrapolation and its validity there sometimes questioned in the shadow of the discovery of the unexpected cosmic acceleration. Future astronomical instruments surveying the distribution and evolution of galaxies over substantial portions of the observable Universe, such as the Dark Energy Spectroscopic Instrument (DESI), will be able to measure the fingerprints of gravity and their statistical power will allow strong constraints on alternatives to GR.In this paper, based on a set of N-body simulations and mock galaxy catalogs, we study the predictions of a number of traditional and novel

summary statistics beyond linear redshift distortions in two well-studied modified gravity models — chameleon f(R) gravity and a braneworld model — and the potential of testing these deviations from GR using DESI. These

summary statistics employ a wide array of statistical properties of the galaxy and the underlying dark matter field, including two-point and higher-order statistics, environmental dependence, redshift space distortions and weak lensing. We find that they hold promising power for testing GR to unprecedented precision. The major future challenge is to make realistic, simulation-based mock galaxy catalogs for both GR and alternative models to fully exploit the statistic power of the DESI survey (by matching the volumes and galaxy number densities of the mocks to those in the real survey) and to better understand the impact of key systematic effects. Using these, we identify future simulation and analysis needs for gravity tests using DESI.

(190)Gravitational-wave signals from 3D supernova simulations with different neutrino-transport methods
• H. Andresen,
• R. Glas,
• H.Th. Janka
Mon.Not.Roy.Astron.Soc., 503, p3552 (11/2020) e-Print:2011.10499 doi:10.1093/mnras/stab675
abstract + abstract -

We compare gravitational-wave (GW) signals from eight 3D simulations of core-collapse supernovae, using two different progenitors with zero-age main-sequence masses of 9 and 20 solar masses (M_⊙). The collapse of each progenitor was simulated four times, at two different grid resolutions and with two different neutrino transport methods, using the aenus-alcar code. The main goal of this study is to assess the validity of recent concerns that the so-called ‘Ray-by-Ray+’ (RbR+) approximation is problematic in core-collapse simulations and can adversely affect theoretical GW predictions. Therefore, signals from simulations using RbR+ are compared to signals from corresponding simulations using a fully multidimensional (FMD) transport scheme. The 9 M_⊙ progenitor successfully explodes, whereas the 20 M_⊙ model does not. Both the standing accretion shock instability and hot-bubble convection develop in the post-shock layer of the non-exploding models. In the exploding models, neutrino-driven convection in the post-shock flow is established around 100 ms after core bounce and lasts until the onset of shock revival. We can, therefore, judge the impact of the numerical resolution and neutrino transport under all conditions typically seen in non-rotating core-collapse simulations. We find excellent qualitative agreement in all GW features. We find minor quantitative differences between simulations, but find no systematic differences between simulations using different transport schemes. Resolution-dependent differences in the hydrodynamic behaviour of low-resolution and high-resolution models have a greater impact on the GW signals than consequences of the different transport methods. Furthermore, increasing the resolution decreases the discrepancies between models with different neutrino transport.

(189)First all-flavor search for transient neutrino emission using 3-years of IceCube DeepCore data
• R. Abbasi,
• M. Ackermann,
• J.A. Aguilar,
• M. Ahlers
• +361
• M. Ahrens,
• C. Alispach,
• A.A.,
• Jr. Alves,
• N.M. Amin,
• K. Andeen,
• T. Anderson,
• I. Ansseau,
• G. Anton,
• C. Argüelles,
• S. Axani,
• X. Bai,
• A.,
• V. Balagopal,
• A. Barbano,
• S.W. Barwick,
• B. Bastian,
• V. Basu,
• V. Baum,
• S. Baur,
• R. Bay,
• J.J. Beatty,
• K.-H. Becker,
• J. Becker Tjus,
• C. Bellenghi,
• S. BenZvi,
• D. Berley,
• E. Bernardini,
• D.Z. Besson,
• G. Binder,
• D. Bindig,
• E. Blaufuss,
• S. Blot,
• S. Böser,
• O. Botner,
• J. Böttcher,
• E. Bourbeau,
• J. Bourbeau,
• J. Braun,
• S. Bron,
• J. Brostean-Kaiser,
• A. Burgman,
• R.S. Busse,
• M.A. Campana,
• C. Chen,
• D. Chirkin,
• S. Choi,
• B.A. Clark,
• K. Clark,
• L. Classen,
• A. Coleman,
• G.H. Collin,
• P. Coppin,
• P. Correa,
• D.F. Cowen,
• R. Cross,
• P. Dave,
• C. De Clercq,
• J.J. DeLaunay,
• H. Dembinski,
• K. Deoskar,
• S. De Ridder,
• A. Desai,
• P. Desiati,
• K.D. de Vries,
• G. de Wasseige,
• M. de With,
• T. DeYoung,
• S. Dharani,
• A. Diaz,
• J.C. Díaz-Vélez,
• H. Dujmovic,
• M. Dunkman,
• M.A. DuVernois,
• E. Dvorak,
• T. Ehrhardt,
• P. Eller,
• R. Engel,
• J. Evans,
• P.A. Evenson,
• S. Fahey,
• A.R. Fazely,
• S. Fiedlschuster,
• A.T. Fienberg,
• K. Filimonov,
• C. Finley,
• L. Fischer,
• D. Fox,
• A. Franckowiak,
• E. Friedman,
• A. Fritz,
• P. Fürst,
• T.K. Gaisser,
• J. Gallagher,
• E. Ganster,
• S. Garrappa,
• L. Gerhardt,
• T. Glauch,
• T. Glüsenkamp,
• A. Goldschmidt,
• J.G. Gonzalez,
• S. Goswami,
• D. Grant,
• T. Grégoire,
• Z. Griffith,
• S. Griswold,
• M. Gündüz,
• C. Haack,
• A. Hallgren,
• R. Halliday,
• L. Halve,
• F. Halzen,
• M. Ha Minh,
• K. Hanson,
• J. Hardin,
• A. Haungs,
• S. Hauser,
• D. Hebecker,
• K. Helbing,
• F. Henningsen,
• S. Hickford,
• J. Hignight,
• C. Hill,
• G.C. Hill,
• K.D. Hoffman,
• R. Hoffmann,
• T. Hoinka,
• B. Hokanson-Fasig,
• K. Hoshina,
• F. Huang,
• M. Huber,
• T. Huber,
• K. Hultqvist,
• M. Hünnefeld,
• R. Hussain,
• S. In,
• N. Iovine,
• A. Ishihara,
• M. Jansson,
• G.S. Japaridze,
• M. Jeong,
• B.J.P. Jones,
• R. Joppe,
• D. Kang,
• W. Kang,
• X. Kang,
• A. Kappes,
• D. Kappesser,
• T. Karg,
• M. Karl,
• A. Karle,
• U. Katz,
• M. Kauer,
• M. Kellermann,
• J.L. Kelley,
• A. Kheirandish,
• J. Kim,
• K. Kin,
• T. Kintscher,
• J. Kiryluk,
• S.R. Klein,
• R. Koirala,
• H. Kolanoski,
• L. Köpke,
• C. Kopper,
• S. Kopper,
• D.J. Koskinen,
• P. Koundal,
• M. Kovacevich,
• M. Kowalski,
• K. Krings,
• G. Krückl,
• N. Kurahashi,
• A. Kyriacou,
• C. Lagunas Gualda,
• J.L. Lanfranchi,
• M.J. Larson,
• F. Lauber,
• J.P. Lazar,
• K. Leonard,
• A. Leszczyńska,
• Y. Li,
• Q.R. Liu,
• E. Lohfink,
• C.J. Lozano Mariscal,
• L. Lu,
• F. Lucarelli,
• A. Ludwig,
• W. Luszczak,
• Y. Lyu,
• W.Y. Ma,
• K.B.M. Mahn,
• Y. Makino,
• P. Mallik,
• S. Mancina,
• I.C. Mariş,
• R. Maruyama,
• K. Mase,
• F. McNally,
• K. Meagher,
• M. Medici,
• A. Medina,
• M. Meier,
• S. Meighen-Berger,
• J. Merz,
• J. Micallef,
• D. Mockler,
• G. Momenté,
• T. Montaruli,
• R.W. Moore,
• R. Morse,
• M. Moulai,
• R. Naab,
• R. Nagai,
• U. Naumann,
• J. Necker,
• G. Neer,
• L.V. Nguyễn,
• L.V. Nguỹ̂{{e}}}}n,
• H. Niederhausen,
• M.L. Nielsen,
• M.U. Nisa,
• S.C. Nowicki,
• D.R. Nygren,
• A. Obertacke Pollmann,
• M. Oehler,
• A. Olivas,
• E. O'Sullivan,
• H. Pandya,
• D.V. Pankova,
• N. Park,
• G.K. Parker,
• E.N. Paudel,
• P. Peiffer,
• C. Pérez de los Heros,
• S. Philippen,
• D. Pieloth,
• S. Pieper,
• A. Pizzuto,
• M. Plum,
• Y. Popovych,
• A. Porcelli,
• P.B. Price,
• G.T. Przybylski,
• C. Raab,
• A. Raissi,
• M. Rameez,
• K. Rawlins,
• I.C. Rea,
• A. Rehman,
• R. Reimann,
• M. Renschler,
• G. Renzi,
• E. Resconi,
• S. Reusch,
• W. Rhode,
• M. Richman,
• B. Riedel,
• S. Robertson,
• G. Roellinghoff,
• M. Rongen,
• C. Rott,
• T. Ruhe,
• D. Ryckbosch,
• D. Rysewyk Cantu,
• I. Safa,
• S.E. Sanchez Herrera,
• A. Sandrock,
• J. Sandroos,
• M. Santander,
• Subir Sarkar,
• Sourav Sarkar,
• K. Satalecka,
• M. Scharf,
• M. Schaufel,
• H. Schieler,
• P. Schlunder,
• T. Schmidt,
• A. Schneider,
• J. Schneider,
• F.G. Schröder,
• L. Schumacher,
• S. Sclafani,
• D. Seckel,
• S. Seunarine,
• S. Shefali,
• M. Silva,
• B. Smithers,
• R. Snihur,
• J. Soedingrekso,
• D. Soldin,
• G.M. Spiczak,
• C. Spiering,
• J. Stachurska,
• M. Stamatikos,
• T. Stanev,
• R. Stein,
• J. Stettner,
• A. Steuer,
• T. Stezelberger,
• N.L. Strotjohann,
• T. Stuttard,
• G.W. Sullivan,
• F. Tenholt,
• S. Ter-Antonyan,
• S. Tilav,
• F. Tischbein,
• K. Tollefson,
• L. Tomankova,
• C. Tönnis,
• S. Toscano,
• D. Tosi,
• A. Trettin,
• M. Tselengidou,
• C.F. Tung,
• A. Turcati,
• R. Turcotte,
• C.F. Turley,
• J.P. Twagirayezu,
• B. Ty,
• E. Unger,
• M.A. Unland Elorrieta,
• J. Vandenbroucke,
• D. van Eijk,
• N. van Eijndhoven,
• D. Vannerom,
• J. van Santen,
• S. Verpoest,
• M. Vraeghe,
• C. Walck,
• A. Wallace,
• T.B. Watson,
• C. Weaver,
• A. Weindl,
• M.J. Weiss,
• J. Weldert,
• C. Wendt,
• J. Werthebach,
• M. Weyrauch,
• B.J. Whelan,
• N. Whitehorn,
• K. Wiebe,
• C.H. Wiebusch,
• D.R. Williams,
• M. Wolf,
• K. Woschnagg,
• G. Wrede,
• J. Wulff,
• X.W. Xu,
• Y. Xu,
• J.P. Yanez,
• S. Yoshida,
• T. Yuan,
• Z. Zhang
• (less)
abstract + abstract -

Since the discovery of a flux of high-energy astrophysical neutrinos, searches for their origins have focused primarily at TeV-PeV energies. Compared to sub-TeV searches, high-energy searches benefit from an increase in the neutrino cross section, improved angular resolution on the neutrino direction, and a reduced background from atmospheric neutrinos and muons. However, the focus on high energy does not preclude the existence of sub-TeV neutrino emission where IceCube retains sensitivity. Here we present the first all-flavor search from IceCube for transient emission of low-energy neutrinos, focusing on the energy region of 5.6-100 GeV using three years of data obtained with the IceCube-DeepCore detector. We find no evidence of transient neutrino emission in the data, thus leading to a constraint on the volumetric rate of astrophysical transient sources in the range of ∼ 705-2301 Gpc$^{-3}$ yr$^{-1}$ for sources following a subphotospheric energy spectrum with a mean energy of 100 GeV and a bolometric energy of 10$^{52}$ erg.

(188)New Extraction of the Cosmic Birefringence from the Planck 2018 Polarization Data
• Yuto Minami,
• Eiichiro Komatsu
Physical Review Letters, 125 (11/2020) doi:10.1103/PhysRevLett.125.221301
abstract + abstract -

We search for evidence of parity-violating physics in the Planck 2018 polarization data and report on a new measurement of the cosmic birefringence angle β . The previous measurements are limited by the systematic uncertainty in the absolute polarization angles of the Planck detectors. We mitigate this systematic uncertainty completely by simultaneously determining β and the angle miscalibration using the observed cross-correlation of the E - and B -mode polarization of the cosmic microwave background and the Galactic foreground emission. We show that the systematic errors are effectively mitigated and achieve a factor-of-2 smaller uncertainty than the previous measurement, finding β =0.35 ±0.14 deg (68% C.L.), which excludes β =0 at 99.2% C.L. This corresponds to the statistical significance of 2.4 σ .

(187)Classical gravitational self-energy from double copy
• Gabriel Luz Almeida,
• Stefano Foffa,
• Riccardo Sturani
Journal of High Energy Physics, 2020 (11/2020) doi:10.1007/JHEP11(2020)165
abstract + abstract -

We apply the classical double copy to the calculation of self-energy of composite systems with multipolar coupling to gravitational field, obtaining next-to-leading order results in the gravitational coupling GN by generalizing color to kinematics replacement rules known in literature. When applied to the multipolar description of the two-body system, the self-energy diagrams studied in this work correspond to tail processes, whose physical interpretation is of radiation being emitted by the non-relativistic source, scattered by the curvature generated by the binary system and then re-absorbed by the same source. These processes contribute to the conservative two-body dynamics and the present work represents a decisive step towards the systematic use of double copy within the multipolar post-Minkowskian expansion.

(186)Structure and Rotation of Young Massive Star Clusters in a Simulated Dwarf Starburst
• Natalia Lahén,
• Thorsten Naab,
• Peter H. Johansson,
• Bruce Elmegreen,
• Chia-Yu Hu
• +1
The Astrophysical Journal, 904, p17 (11/2020) doi:10.3847/1538-4357/abc001
abstract + abstract -

We analyze the three-dimensional shapes and kinematics of the young star cluster population forming in a high-resolution GRIFFIN project simulation of a metal-poor dwarf galaxy starburst. The star clusters, which follow a power-law mass distribution, form from the cold phase interstellar medium with an initial mass function sampled with individual stars down to four solar masses at sub-parsec spatial resolution. Massive stars and their important feedback mechanisms are modeled in detail. The simulated clusters follow a surprisingly tight relation between the specific angular momentum and mass with indications of two sub-populations. Massive clusters (Mcl ≳ 3 × 104 M) have the highest specific angular momenta at low ellipticities (ɛ ∼ 0.2) and show alignment between their shapes and rotation. Lower mass clusters have lower specific angular momenta with larger scatter, show a broader range of elongations, and are typically misaligned indicating that they are not shaped by rotation. The most massive clusters (M ≳ 105 M) accrete gas and protoclusters from a ≲100 pc scale local galactic environment on a t ≲ 10 Myr timescale, inheriting the ambient angular momentum properties. Their two-dimensional kinematic maps show ordered rotation at formation, up to v ∼ 8.5 km s-1, consistent with observed young massive clusters and old globular clusters, which they might evolve into. The massive clusters have angular momentum parameters λR ≲ 0.5 and show Gauss-Hermite coefficients h3 that are anti-correlated with the velocity, indicating asymmetric line-of-sight velocity distributions as a signature of a dissipative formation process.

(185)A Distance Determination to the Small Magellanic Cloud with an Accuracy of Better than Two Percent Based on Late-type Eclipsing Binary Stars
• Dariusz Graczyk,
• Grzegorz Pietrzyński,
• Ian B. Thompson,
• Wolfgang Gieren,
• Bartłomiej Zgirski
• +15
• Sandro Villanova,
• Marek Górski,
• Piotr Wielgórski,
• Paulina Karczmarek,
• Weronika Narloch,
• Bogumił Pilecki,
• Monica Taormina,
• Ksenia Suchomska,
• Alexandre Gallenne,
• Nicolas Nardetto,
• Jesper Storm,
• Rolf-Peter Kudritzki,
• Mikołaj Kałuszyński,
• Wojciech Pych
• (less)
The Astrophysical Journal, 904, p14 (11/2020) doi:10.3847/1538-4357/abbb2b
abstract + abstract -

We present a new study of late-type eclipsing binary stars in the Small Magellanic Cloud (SMC) undertaken with the aim of improving the distance determination to this important galaxy. A sample of 10 new detached, double-lined eclipsing binaries identified from the OGLE variable star catalogs and consisting of F- and G-type giant components has been analyzed. The absolute physical parameters of the individual components have been measured with a typical accuracy of better than 3%. All but one of the systems consist of young and intermediate population stars with masses in the range of 1.4 to 3.8 M. This new sample has been combined with five SMC eclipsing binaries previously published by our team. Distances to the binary systems were calculated using a surface brightness—color calibration. The targets form an elongated structure, highly inclined to the plane of the sky. The distance difference between the nearest and most-distant system amounts to 10 kpc with the line-of-sight depth reaching 7 kpc. We find tentative evidence of the existence of a spherical stellar substructure (core) in the SMC coinciding with its stellar center, containing about 40% of the young and intermediate age stars in the galaxy. The radial extension of this substructure is ∼1.5 kpc. We derive a distance to the SMC center of DSMC = 62.44 ± 0.47 (stat.) ± 0.81 (syst.) kpc corresponding to a distance modulus (m - M)SMC = 18.977 ± 0.016 ± 0.028 mag, representing an accuracy of better than 2%.

(184)Testing one-loop galaxy bias: Power spectrum
• Alexander Eggemeier,
• Román Scoccimarro,
• Martin Crocce,
• Andrea Pezzotta,
• Ariel G. Sánchez
Physical Review D, 102 (11/2020) doi:10.1103/PhysRevD.102.103530
abstract + abstract -

We test the regime of validity of the one-loop galaxy bias for a wide variety of biased tracers. Our most stringent test asks the bias model to simultaneously match the galaxy-galaxy and galaxy-mass spectrum, using the measured nonlinear matter spectrum from the simulations to test the one-loop effects from the bias expansion alone. In addition, we investigate the relevance of short-range nonlocality and halo exclusion through higher-derivative and scale-dependent noise terms, as well as the impact of using coevolution relations to reduce the number of free fitting parameters. From comparing the validity and merit of these assumptions, we find that a four-parameter model (linear, quadratic, cubic nonlocal bias, and constant shot noise) with a fixed quadratic tidal bias provides a robust modeling choice for the auto power spectrum of the less massive halos in our set of samples and their galaxy populations [up to kmax=0.35 h /Mpc for a sample volume of 6 (Gpc /h )3 ]. For the more biased tracers, it is most beneficial to include scale-dependent noise. This is also the preferred option when considering combinations of the auto and cross power spectrum, which might be relevant in joint studies of galaxy clustering and weak lensing. We also test the use of perturbation theory to account for matter loops through gRPT, EFT, and the hybrid approach RESPRESSO. While all these have similar performance, we find the latter to be the best in terms of validity and recovered mean posterior values, in accordance with it being based partially on simulations.

(183)FeynOnium: using FeynCalc for automatic calculations in Nonrelativistic Effective Field Theories
• Nora Brambilla,
• Hee Sok Chung,
• Antonio Vairo
Journal of High Energy Physics, 2020 (11/2020) doi:10.1007/JHEP11(2020)130
abstract + abstract -

We present new results on FEYNONIUM, an ongoing project to develop a general purpose software toolkit for semi-automatic symbolic calculations in nonrelativistic Effective Field Theories (EFTs). Building upon FEYNCALC, an existing MATHEMATICA package for symbolic evaluation of Feynman diagrams, we have created a powerful framework for automatizing calculations in nonrelativistic EFTs (NREFTs) at tree- and 1-loop level. This is achieved by exploiting the novel features of FEYNCALC that support manipulations of Cartesian tensors, Pauli matrices and nonstandard loop integrals. Additional operations that are common in nonrelativistic EFT calculations are implemented in a dedicated add-on called FEYNONIUM. While our current focus is on EFTs for strong interactions of heavy quarks, extensions to other systems that admit a nonrelativistic EFT description are planned for the future. All our codes are open-source and publicly available. Furthermore, we provide several example calculations that demonstrate how FEYNONIUM can be employed to reproduce known results from the literature.

(182)Fast neutrino flavor conversion, ejecta properties, and nucleosynthesis in newly-formed hypermassive remnants of neutron-star mergers
• Manu George,
• Meng-Ru Wu,
• Irene Tamborra,
• Ricard Ardevol-Pulpillo,
• Hans-Thomas Janka
Physical Review D, 102 (11/2020) doi:10.1103/PhysRevD.102.103015
abstract + abstract -

Neutrinos emitted in the coalescence of two neutron stars affect the dynamics of the outflow ejecta and the nucleosynthesis of heavy elements. In this work, we analyze the neutrino emission properties and the conditions leading to the growth of flavor instabilities in merger remnants consisting of a hypermassive neutron star and an accretion disk during the first 10 ms after the merger. The analyses are based on hydrodynamical simulations that include a modeling of neutrino emission and absorption effects via the "improved leakage-equilibration-absorption scheme" (ILEAS). We also examine the nucleosynthesis of the heavy elements via the rapid neutron-capture process (r -process) inside the material ejected during this phase. The dominant emission of ν¯e over νe from the merger remnant leads to favorable conditions for the occurrence of fast pairwise flavor conversions of neutrinos, independent of the chosen equation of state or the mass ratio of the binary. The nucleosynthesis outcome is very robust, ranging from the first to the third r -process peaks. In particular, more than 10-5 M of strontium are produced in these early ejecta that may account for the GW170817 kilonova observation. We find that the amount of ejecta containing free neutrons after the r -process freeze-out, which may power early-time UV emission, is reduced by roughly a factor of 10 when compared to simulations that do not include weak interactions. Finally, the potential flavor equipartition between all neutrino flavors is mainly found to affect the nucleosynthesis outcome in the polar ejecta within ≲3 0 ° , by changing the amount of the produced iron-peak and first-peak nuclei, but it does not alter the lanthanide mass fraction therein.

(181)How much H and He is 'hidden' in SNe Ib/c? - II. Intermediate-mass objects: a 22-=M<SUB>⊙</SUB> progenitor case study
• Jacob Teffs,
• Thomas Ertl,
• Paolo Mazzali,
• Stephan Hachinger,
• H. -Thomas Janka
Monthly Notices of the Royal Astronomical Society, 499, p18 (11/2020) doi:10.1093/mnras/staa2549
abstract + abstract -

Stripped envelope supernovae are a sub-class of core-collapse supernovae showing several stages of H/He shell stripping that determines the type: H-free/He-poor SNe are classified as Type Ic, H-poor/He-rich are Type Ib, and H/He-rich are Type IIb. Stripping H/He with only stellar wind requires significantly higher mass-loss rates than observed while binary-involved mass transfer may usually not strip enough to produce H/He free SNe. Type Ib/c SNe are sometimes found to include weak H/He transient lines as a product of a trace amount of H/He left over from stripping processes. The extent and mass of the H/He required to produce these lines is not well known. In this work, a 22 M progenitor model is stripped of the H/He shells in five steps prior to collapse and then exploded at four explosion energies. Requiring both optical and near-infrared He-=I lines for helium identification does not allow much He mass to be hidden in SE-SNE. Increasing the mass of He above the CO core delays the visibility of O-=I-=7774 in early spectra. Our SN-=Ib-like models are capable of reproducing the spectral evolution of a set of observed SNe with reasonable estimated Ek accuracy. Our SN-=IIb-like models can partially reproduce low energy observed SN-=IIb, but we find no observed comparison for the SN-=IIb-like models with high Ek.

(180)The molecular mass function of the local Universe
• P. Andreani,
• Y. Miyamoto,
• H. Kaneko,
• A. Boselli,
• K. Tatematsu
• +2
Astronomy and Astrophysics, 643, p5 (11/2020) doi:10.1051/0004-6361/202038675
abstract + abstract -

Aims: We construct the molecular mass function using the bivariate K-band-mass function (BMF) of the Herschel Reference Survey (HRS), which is a volume-limited sample that has already been widely studied at the entire electromagnetic spectrum.
Methods: The molecular mass function was derived from the K-band and the gas mass cumulative distribution using a copula method, which is described in detail in our previous papers.
Results: The H2 mass is relatively strongly correlated with the K-band luminosity because of the tight relation between the stellar mass and the molecular gas mass within the sample with a scatter, which is likely due to those galaxies which have lost their molecular content because of environmental effects or because of a larger gas consumption due to past star formation processes. The derived H2 MF samples the molecular mass range from ∼4 × 106 M to ∼1010 M, and when compared with theoretical models, it agrees well with the theoretical predictions at the lower end of the mass values; whereas at masses larger than 1010 M, the HRS sample may miss galaxies with a large content of molecular hydrogen and the outcomes are not conclusive. The value of the local density of the molecular gas mass inferred from our analysis is ∼1.5 × 107 M Mpc-3, and it is compared with the results at larger redshifts, confirming the lack of strong evolution for the molecular mass density between z = 0 and z = 4.
Conclusions: This is the first molecular mass function that has been derived on a complete sample in the local Universe, which can be used as a reliable calibration at redshift z = 0 for models aiming to predict the evolution of the molecular mass density.

(179)ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT). II. Vertical stratification of CO, CS, CN, H<SUB>2</SUB>CO, and CH<SUB>3</SUB>OH in a Class I disk
• L. Podio,
• A. Garufi,
• C. Codella,
• D. Fedele,
• E. Bianchi
• +6
• F. Bacciotti,
• C. Ceccarelli,
• C. Favre,
• S. Mercimek,
• K. Rygl,
• L. Testi
• (less)
Astronomy and Astrophysics, 642, p7 (10/2020) doi:10.1051/0004-6361/202038952
abstract + abstract -

The chemical composition of planets is inherited from that of the natal protoplanetary disk at the time of planet formation. Increasing observational evidence suggests that planet formation occurs in less than 1-2 Myr. This motivates the need for spatially resolved spectral observations of young Class I disks, as carried out by the ALMA chemical survey of Disk-Outflow sources in Taurus (ALMA-DOT). In the context of ALMA-DOT, we observe the edge-on disk around the Class I source IRAS 04302+2247 (the butterfly star) in the 1.3 mm continuum and five molecular lines. We report the first tentative detection of methanol (CH3OH) in a Class I disk and resolve, for the first time, the vertical structure of a disk with multiple molecular tracers. The bulk of the emission in the CO 2-1, CS 5-4, and o-H2CO 31, 2 - 21, 1 lines originates from the warm molecular layer, with the line intensity peaking at increasing disk heights, z, for increasing radial distances, r. Molecular emission is vertically stratified, with CO observed at larger disk heights (aperture z/r ∼ 0.41-0.45) compared to both CS and H2CO, which are nearly cospatial (z/r ∼ 0.21-0.28). In the outer midplane, the line emission decreases due to molecular freeze-out onto dust grains (freeze-out layer) by a factor of > 100 (CO) and 15 (CS). The H2CO emission decreases by a factor of only about 2, which is possibly due to H2CO formation on icy grains, followed by a nonthermal release into the gas phase. The inferred [CH3OH]/[H2CO] abundance ratio is 0.5-0.6, which is 1-2 orders of magnitude lower than for Class 0 hot corinos, and a factor ∼2.5 lower than the only other value inferred for a protoplanetary disk (in TW Hya, 1.3-1.7). Additionally, it is at the lower edge but still consistent with the values in comets. This may indicate that some chemical reprocessing occurs in disks before the formation of planets and comets.

The reduced images and datacubes are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/642/L7

(178)The impact of modified gravity on the Sunyaev–Zeldovich effect
• Myles A. Mitchell,
• Christian Arnold,
• César Hernández-Aguayo,
• Baojiu Li
Mon.Not.Roy.Astron.Soc., 501, p4565 (10/2020) e-Print:2011.00013 doi:10.1093/mnras/staa3941
abstract + abstract -

We study the effects of two popular modified gravity theories, which incorporate very different screening mechanisms, on the angular power spectra of the thermal (tSZ) and kinematic (kSZ) components of the Sunyaev–Zeldovich effect. Using the first cosmological simulations that simultaneously incorporate both screened modified gravity and a complete galaxy formation model, we find that the tSZ and kSZ power spectra are significantly enhanced by the strengthened gravitational forces in Hu-Sawicki f(R) gravity and the normal-branch Dvali–Gabadadze–Porrati model. Employing a combination of non-radiative and full-physics simulations, we find that the extra baryonic physics present in the latter acts to suppress the tSZ power on angular scales l ≳ 3000 and the kSZ power on all tested scales, and this is found to have a substantial effect on the model differences. Our results indicate that the tSZ and kSZ power can be used as powerful probes of gravity on large scales, using data from current and upcoming surveys, provided sufficient work is conducted to understand the sensitivity of the constraints to baryonic processes that are currently not fully understood.

(177)How to suppress exponential growth—on the parametric resonance of photons in an axion background
• Ariel Arza,
• Thomas Schwetz,
• Elisa Todarello
Journal of Cosmology and Astroparticle Physics, 2020 (10/2020) doi:10.1088/1475-7516/2020/10/013
abstract + abstract -

Axion-photon interactions can lead to an enhancement of the electromagnetic field by parametric resonance in the presence of a cold axion background, for modes with a frequency close to half the axion mass. In this paper, we study the role of the axion momentum dispersion as well as the effects of a background gravitational potential, which can detune the resonance due to gravitational redshift. We show, by analytical as well as numerical calculations, that the resonance leads to an exponential growth of the photon field only if (a) the axion momentum spread is smaller than the inverse resonance length, and (b) the gravitational detuning distance is longer than the resonance length. For realistic parameter values, both effects strongly suppress the resonance and prevent the exponential growth of the photon field. In particular, the redshift due to the gravitational potential of our galaxy prevents the resonance from developing for photons in the observable frequency range, even assuming that all the dark matter consists of a perfectly cold axion condensate. For axion clumps with masses below ~ 10-13 Msolar, the momentum spread condition is more restrictive, whereas, for more massive clumps, the redshift condition dominates.

(176)Self-consistent 3D Supernova Models From −7 Minutes to +7 s: A 1-bethe Explosion of a ∼19 $M_\odot$ Progenitor
• Robert Bollig,
• Daniel Kresse,
• H.-Th. Janka,
• Bernhard Müller
• +1
Astrophys.J., 915, p28 (10/2020) e-Print:2010.10506 doi:10.3847/1538-4357/abf82e
abstract + abstract -

To date, modern three-dimensional (3D) supernova (SN) simulations have not demonstrated that explosion energies of 1051 erg (=1 bethe=1 B) or more are possible for neutrino-driven SNe of non/slow-rotating M < 20 M ⊙ progenitors. We present the first such model, considering a nonrotating, solar-metallicity 18.88 M ⊙ progenitor, whose final 7 minutes of convective oxygen-shell burning were simulated in 3D and showed a violent oxygen–neon shell merger prior to collapse. A large set of 3D SN models was computed with the Prometheus-Vertex code, whose improved convergence of the two-moment equations with Boltzmann closure allows now to fully exploit the implicit neutrino-transport treatment. Nuclear burning is treated with a 23-species network. We vary the angular grid resolution and consider different nuclear equations of state and muon formation in the proto-neutron star (PNS), which requires six-species transport with coupling of all neutrino flavors across all energy–momentum groups. Elaborate neutrino transport was applied until ∼2 s after bounce. In one case, the simulation was continued to >7 s with an approximate treatment of neutrino effects that allows for seamless continuation without transients. A spherically symmetric neutrino-driven wind does not develop. Instead, accretion downflows to the PNS and outflows of neutrino-heated matter establish a monotonic rise of the explosion energy until ∼7 s post-bounce, when the outgoing shock reaches ∼50,000 km and enters the He layer. The converged value of the explosion energy at infinity (with overburden subtracted) is ∼1 B and the ejected 56Ni mass ≲0.087 M ⊙, both within a few 10% of the SN 1987A values. The final NS mass and kick are ∼1.65 M ⊙ and >450 km s−1, respectively.

(175)Toward Bayesian Data Compression
• Johannes Harth‐Kitzerow,
• Reimar H. Leike,
• Philipp Arras,
• Torsten A. Enßlin
Annalen Phys., 533 (10/2020) e-Print:2010.10375 doi:10.1002/andp.202000508
abstract + abstract -

In order to handle large datasets omnipresent in modern science, efficient compression algorithms are necessary. Here, a Bayesian data compression (BDC) algorithm that adapts to the specific measurement situation is derived in the context of signal reconstruction. BDC compresses a dataset under conservation of its posterior structure with minimal information loss given the prior knowledge on the signal, the quantity of interest. Its basic form is valid for Gaussian priors and likelihoods. For constant noise standard deviation, basic BDC becomes equivalent to a Bayesian analog of principal component analysis. Using metric Gaussian variational inference, BDC generalizes to non‐linear settings. In its current form, BDC requires the storage of effective instrument response functions for the compressed data and corresponding noise encoding the posterior covariance structure. Their memory demand counteract the compression gain. In order to improve this, sparsity of the compressed responses can be obtained by separating the data into patches and compressing them separately. The applicability of BDC is demonstrated by applying it to synthetic data and radio astronomical data. Still the algorithm needs further improvement as the computation time of the compression and subsequent inference exceeds the time of the inference with the original data.

(174)How to interpret observations of neutron-star mergers?
• Oliver Just,
• Andreas Bauswein,
• Stephane Goriely,
• Hirotaka Ito,
• Hans-Thomas Janka
• +1
Journal of Physics Conference Series, 1667 (10/2020) doi:10.1088/1742-6596/1667/1/012018
abstract + abstract -

The recent first multi-messenger observation of a neutron-star merger, GW170817 and its electromagnetic counterparts, has sparked tremendous excitement particularly because long-standing questions related to heavy-element nucleosynthesis and the nuclear equation of state could finally be tested with unprecedented capabilities. This proceedings article briefly reviews the main observation channels of neutron-star mergers and how those can be used to obtain insight about questions related to nucleosynthesis and the nuclear equation of state.

(173)Learning the non-equilibrium dynamics of Brownian movies
• Federico S. Gnesotto,
• Pierre Ronceray,
• Chase P. Broedersz
Nature Communications, 11 (10/2020) doi:10.1038/s41467-020-18796-9
abstract + abstract -

Time-lapse microscopy imaging provides direct access to the dynamics of soft and living systems. At mesoscopic scales, such microscopy experiments reveal intrinsic thermal and non-equilibrium fluctuations. These fluctuations, together with measurement noise, pose a challenge for the dynamical analysis of these Brownian movies. Traditionally, methods to analyze such experimental data rely on tracking embedded or endogenous probes. However, it is in general unclear, especially in complex many-body systems, which degrees of freedom are the most informative about their non-equilibrium nature. Here, we introduce an alternative, tracking-free approach that overcomes these difficulties via an unsupervised analysis of the Brownian movie. We develop a dimensional reduction scheme selecting a basis of modes based on dissipation. Subsequently, we learn the non-equilibrium dynamics, thereby estimating the entropy production rate and time-resolved force maps. After benchmarking our method against a minimal model, we illustrate its broader applicability with an example inspired by active biopolymer gels.

(172)Simultaneous determination of the cosmic birefringence and miscalibrated polarization angles II: Including cross-frequency spectra
• Yuto Minami,
• Eiichiro Komatsu
Progress of Theoretical and Experimental Physics, 2020 (10/2020) doi:10.1093/ptep/ptaa130
abstract + abstract -

We develop a strategy to determine the cosmic birefringence and miscalibrated polarization angles simultaneously using the observed $EB$ polarization power spectra of the cosmic microwave background and the Galactic foreground emission. We extend the methodology of Y. Minami et al. (Prog. Theor. Exp. Phys. 2019, 083E02, 2019), which was developed for auto-frequency power spectra, by including cross-frequency spectra. By fitting one global birefringence angle and independent miscalibration angles at different frequency bands, we determine both angles with significantly smaller uncertainties (by more than a factor of two) compared to the auto spectra.

(171)Anomalous Dimensions of Effective Theories from Partial Waves
• Pietro Baratella,
• Clara Fernandez,
• Benedict von Harling,
• Alex Pomarol
arXiv e-prints (10/2020) e-Print:2010.13809
abstract + abstract -

On-shell amplitude methods have proven to be extremely efficient for calculating anomalous dimensions. We further elaborate on these methods to show that, by the use of an angular momentum decomposition, the one-loop anomalous dimensions can be reduced to essentially a sum of products of partial waves. We apply this to the SM EFT, and show how certain classes of anomalous dimensions have their origin in the same partial-wave coefficients. We also use our result to obtain a generic formula for the one-loop anomalous dimensions of nonlinear sigma models at any order in the energy expansion, and apply our method to gravity, where it proves to be very advantageous even in the presence of IR divergencies.

(170)Constraining the origin and models of chemical enrichment in galaxy clusters using the Athena X-IFU
• F. Mernier,
• E. Cucchetti,
• L. Tornatore,
• V. Biffi,
• E. Pointecouteau
• +13
• N. Clerc,
• P. Peille,
• E. Rasia,
• D. Barret,
• S. Borgani,
• E. Bulbul,
• T. Dauser,
• K. Dolag,
• S. Ettori,
• M. Gaspari,
• F. Pajot,
• M. Roncarelli,
• J. Wilms
• (less)
Astronomy and Astrophysics, 642, p17 (10/2020) doi:10.1051/0004-6361/202038638
abstract + abstract -

Chemical enrichment of the Universe at all scales is related to stellar winds and explosive supernovae phenomena. Metals produced by stars and later spread throughout the intracluster medium (ICM) at the megaparsec scale become a fossil record of the chemical enrichment of the Universe and of the dynamical and feedback mechanisms determining their circulation. As demonstrated by the results of the soft X-ray spectrometer onboard Hitomi, high-resolution X-ray spectroscopy is the path to differentiating among the models that consider different metal-production mechanisms, predict the outcoming yields, and are a function of the nature, mass, and/or initial metallicity of their stellar progenitor. Transformational results shall be achieved through improvements in the energy resolution and effective area of X-ray observatories, allowing them to detect rarer metals (e.g. Na, Al) and constrain yet-uncertain abundances (e.g. C, Ne, Ca, Ni). The X-ray Integral Field Unit (X-IFU) instrument onboard the next-generation European X-ray observatory Athena is expected to deliver such breakthroughs. Starting from 100 ks of synthetic observations of 12 abundance ratios in the ICM of four simulated clusters, we demonstrate that the X-IFU will be capable of recovering the input chemical enrichment models at both low (z = 0.1) and high (z = 1) redshifts, while statistically excluding more than 99.5% of all the other tested combinations of models. By fixing the enrichment models which provide the best fit to the simulated data, we also show that the X-IFU will constrain the slope of the stellar initial mass function within ∼12%. These constraints will be key ingredients in our understanding of the chemical enrichment of the Universe and its evolution.