page 6 of 20
CN-4
RU-C
RU-D
(1429)The powerful lens galaxy cluster PLCK G287.0+32.9 (θ_E∼43″)
  • Maurizio D'Addona,
  • Amata Mercurio,
  • Piero Rosati,
  • Claudio Grillo,
  • Gabriel Caminha
  • +15
  • Ana Acebron,
  • Giuseppe Angora,
  • Pietro Bergamini,
  • Valerio Bozza,
  • Giovanni Granata,
  • Marianna Annunziatella,
  • Adriana Gargiulo,
  • Raphael Gobat,
  • Paolo Tozzi,
  • Marisa Girardi,
  • Marco Lombardi,
  • Massimo Meneghetti,
  • Pietro Schipani,
  • Luca Tortorelli,
  • Eros Vanzella
  • (less)
arXiv e-prints (01/2024) e-Print:2401.16473
abstract + abstract -

We present a new high-precision strong lensing model of PLCK G287.0+32.9, a massive lens galaxy cluster at z=0.383, with the aim to get an accurate estimation of its effective Einstein radius and total mass distribution. We also present a spectroscopic catalog containing accurate redshift measurements for 490 objects, including multiply-lensed sources and cluster member galaxies. We exploit high-quality spectroscopic data from three pointings of the VLT Multi Unit Spectroscopic Explorer, covering a central 3 arcmin2 region of the cluster. We complete the spectroscopic catalog by including redshift measurements from VLT-VIMOS and KECK-DEIMOS. We identify 129 spectroscopic cluster member galaxies, with redshift values 0.360≤z≤0.405 and mF160W≤21, and 24 photometric ones identified with a Convolutional Neural Network from ancillary HST imaging. We also identify 114 multiple images from 28 background sources, of which 84 images from 16 sources are new and the remaining ones were identified in previous work. The best-fitting lens model shows a root mean square separation value between the predicted and observed positions of the multiple images of 0.75″, corresponding to an improvement in reconstructing the observed positions of the multiple images of a factor of 2.5 with respect to previous models. Using the predictive power of our new lens model we find 3 new multiple images and we confirm the configuration of three systems of multiple images that were not used for the optimization of the model. The derived total mass distribution confirms this cluster to be a very prominent gravitational lens with an effective Einstein θE=43.4″±0.1″, that is in agreement with previous estimates and corresponds to a total mass enclosed in the critical curve of ME=3.33+0.02−0.07×1014M⊙.


RU-D
(1428)A parsec-scale Galactic 3D dust map out to 1.25 kpc from the Sun
  • Gordian Edenhofer,
  • Catherine Zucker,
  • Philipp Frank,
  • Andrew K. Saydjari,
  • Joshua S. Speagle
  • +2
  • Douglas Finkbeiner,
  • Torsten Enßlin
  • (less)
abstract + abstract -

High-resolution 3D maps of interstellar dust are critical for probing the underlying physics shaping the structure of the interstellar medium, and for foreground correction of astrophysical observations affected by dust. We aim to construct a new 3D map of the spatial distribution of interstellar dust extinction out to a distance of 1.25 kpc from the Sun. We leveraged distance and extinction estimates to 54 million nearby stars derived from the Gaia BP/RP spectra. Using the stellar distance and extinction information, we inferred the spatial distribution of dust extinction. We modeled the logarithmic dust extinction with a Gaussian process in a spherical coordinate system via iterative charted refinement and a correlation kernel inferred in previous work. In total, our posterior has over 661 million degrees of freedom. We probed the posterior distribution using the variational inference method MGVI. Our 3D dust map has an angular resolution of up to 14' (Nside = 256), and we achieve parsec-scale distance resolution, sampling the dust in 516 logarithmically spaced distance bins spanning 69 pc to 1250 pc. We generated 12 samples from the variational posterior of the 3D dust distribution and release the samples alongside the mean 3D dust map and its corresponding uncertainty. Our map resolves the internal structure of hundreds of molecular clouds in the solar neighborhood and will be broadly useful for studies of star formation, Galactic structure, and young stellar populations. It is available for download in a variety of coordinate systems online and can also be queried via the publicly available dustmaps Python package.


CN-7
RU-A
(1427)Nuclear ground-state properties probed by the relativistic Hartree-Bogoliubov approach
  • Zi Xin Liu,
  • Yi Hua Lam,
  • Ning Lu,
  • Peter Ring
At. Data Nucl. Data Tables (01/2024) e-Print:2309.06371 doi:10.1016/j.adt.2023.101635
abstract + abstract -

Using the relativistic Hartree-Bogoliubov framework with separable pairing force coupled with the latest covariant density functionals, i.e., PC-L3R, PC-X, DD-PCX, and DD-MEX, we systematically explore the ground-state properties of all isotopes of Z=8-110. These properties consist of the binding energies, one- and two-neutron separation energies (Sn and S2n), root-mean-square radius of matter, of neutron, of proton, and of charge distributions, Fermi surfaces, ground-state spins and parities. We then predict the edges of nuclear landscape and bound nuclei for the isotopic chains from oxygen (Z=8) to darmstadtium (Z=110) based on these latest covariant density functionals. The number of bound nuclei predicted by PC-L3R, PC-X, DD-PCX, and DD-MEX, are 9004, 9162, 6799, and 7112, respectively. The root-mean-square deviations of Sn (S2n) yielded from PC-L3R, PCX, DD-PCX, and DD-MEX are 0.962 (1.300) MeV, 0.920 (1.483) MeV, 0.993 (1.753) MeV, and 1.010 (1.544) MeV, respectively. The root-mean-square deviations of charge radius distributions of comparing the available experimental values with the theoretical counterparts resulted from PC-L3R, PC-X, DD-PCX, and DD-MEX are 0.035 fm, 0.037 fm, 0.035 fm, and 0.034 fm, respectively. We notice pronounced differences between the empirical and theoretical root-mean-square radii of neutron at nuclei near the neutron drip line of the Mg, Ca, and Kr isotopic chains, suggesting the possible existence of the halo or giant halo phenomena.


(1426)Emergent M-theory limit
  • Ralph Blumenhagen,
  • Niccolò Cribiori,
  • Aleksandar Gligovic,
  • Antonia Paraskevopoulou
Physical Review D (01/2024) doi:10.1103/PhysRevD.109.L021901
abstract + abstract -

It has been recently proposed that at each infinite distance limit in the moduli space of quantum gravity a perturbative description emerges with fundamental degrees of freedom given by those infinite towers of states whose typical mass scale is parametrically not larger than the ultraviolet cutoff, identified with the species scale. This proposal is applied to the familiar ten-dimensional type IIA and IIB superstring theories, when considering the limit of infinite string coupling. For type IIB, the light towers of states are given by excitations of the D 1 -brane, as expected from self-duality. Instead, for type IIA at strong coupling, which is dual to M-theory on S1, we make the observation that the emergent degrees of freedom are bound states of transversal M 2 - and M 5 -branes with Kaluza-Klein momentum along the circle. We speculate on the interpretation of the necessity of including all these states for a putative quantum formulation of M-theory.


CN-3
CN-4
RU-C
(1425)Optimal 1D Ly α forest power spectrum estimation - III. DESI early data
  • Naim Göksel Karaçaylı,
  • Paul Martini,
  • Julien Guy,
  • Corentin Ravoux,
  • Marie Lynn Abdul Karim
  • +57
  • Eric Armengaud,
  • Michael Walther,
  • J. Aguilar,
  • S. Ahlen,
  • S. Bailey,
  • J. Bautista,
  • S.F. Beltran,
  • D. Brooks,
  • L. Cabayol-Garcia,
  • S. Chabanier,
  • E. Chaussidon,
  • J. Chaves-Montero,
  • K. Dawson,
  • R. de la Cruz,
  • A. de la Macorra,
  • P. Doel,
  • A. Font-Ribera,
  • J. E. Forero-Romero,
  • S. Gontcho A Gontcho,
  • A.X. Gonzalez-Morales,
  • C. Gordon,
  • H.K Herrera-Alcantar,
  • K. Honscheid,
  • V. Iršič,
  • M. Ishak,
  • R. Kehoe,
  • T. Kisner,
  • A. Kremin,
  • M. Landriau,
  • L. Le Guillou,
  • M.E. Levi,
  • Z. Lukić,
  • A. Meisner,
  • R. Miquel,
  • J. Moustakas,
  • E. Mueller,
  • A. Muñoz-Gutiérrez,
  • L. Napolitano,
  • J. Nie,
  • G. Niz,
  • N. Palanque-Delabrouille,
  • W.J. Percival,
  • M. Pieri,
  • C. Poppett,
  • F. Prada,
  • I. Pérez-Ràfols,
  • C. Ramírez-Pérez,
  • G. Rossi,
  • E. Sanchez,
  • H. Seo,
  • F. Sinigaglia,
  • T. Tan,
  • G. Tarlé,
  • B. Wang,
  • B.A. Weaver,
  • C. Yèche,
  • Z. Zhou
  • (less)
abstract + abstract -

The 1D power spectrum P1D of the Ly α forest provides important information about cosmological and astrophysical parameters, including constraints on warm dark matter models, the sum of the masses of the three neutrino species, and the thermal state of the intergalactic medium. We present the first measurement of P1D with the quadratic maximum likelihood estimator (QMLE) from the Dark Energy Spectroscopic Instrument (DESI) survey early data sample. This early sample of 54 600 quasars is already comparable in size to the largest previous studies, and we conduct a thorough investigation of numerous instrumental and analysis systematic errors to evaluate their impact on DESI data with QMLE. We demonstrate the excellent performance of the spectroscopic pipeline noise estimation and the impressive accuracy of the spectrograph resolution matrix with 2D image simulations of raw DESI images that we processed with the DESI spectroscopic pipeline. We also study metal line contamination and noise calibration systematics with quasar spectra on the red side of the Ly α emission line. In a companion paper, we present a similar analysis based on the Fast Fourier Transform estimate of the power spectrum. We conclude with a comparison of these two approaches and discuss the key sources of systematic error that we need to address with the upcoming DESI Year 1 analysis.


CN-3
CN-4
RU-C
(1424)Validation of the Scientific Program for the Dark Energy Spectroscopic Instrument
  • DESI Collaboration: A. G. Adame,
  • J. Aguilar,
  • S. Ahlen,
  • S. Alam,
  • G. Aldering
  • +94
  • D. M. Alexander,
  • R. Alfarsy,
  • C. Allende Prieto,
  • M. Alvarez,
  • O. Alves,
  • A. Anand,
  • F. Andrade-Oliveira,
  • E. Armengaud,
  • J. Asorey,
  • S. Avila,
  • A. Aviles,
  • S. Bailey,
  • A. Balaguera-Antolínez,
  • O. Ballester,
  • C. Baltay,
  • A. Bault,
  • J. Bautista,
  • J. Behera,
  • S. F. Beltran,
  • S. BenZvi,
  • L. Beraldo e Silva,
  • J. R. Bermejo-Climent,
  • A. Berti,
  • R. Besuner,
  • F. Beutler,
  • D. Bianchi,
  • C. Blake,
  • R. Blum,
  • A. S. Bolton,
  • S. Brieden,
  • A. Brodzeller,
  • D. Brooks,
  • Z. Brown,
  • E. Buckley-Geer,
  • E. Burtin,
  • L. Cabayol-Garcia,
  • Z. Cai,
  • R. Canning,
  • L. Cardiel-Sas,
  • A. Carnero Rosell,
  • F. J. Castander,
  • J.L. Cervantes-Cota,
  • S. Chabanier,
  • E. Chaussidon,
  • J. Chaves-Montero,
  • S. Chen,
  • C. Chuang,
  • T. Claybaugh,
  • S. Cole,
  • A. P. Cooper,
  • A. Cuceu,
  • T. M. Davis,
  • K. Dawson,
  • R. de Belsunce,
  • R. de la Cruz,
  • A. de la Macorra,
  • A. de Mattia,
  • R. Demina,
  • U. Demirbozan,
  • J. DeRose,
  • A. Dey,
  • B. Dey,
  • G. Dhungana,
  • J. Ding,
  • Z. Ding,
  • P. Doel,
  • R. Doshi,
  • K. Douglass,
  • A. Edge,
  • S. Eftekharzadeh,
  • D. J. Eisenstein,
  • A. Elliott,
  • S. Escoffier,
  • P. Fagrelius,
  • X. Fan,
  • K. Fanning,
  • V. A. Fawcett,
  • S. Ferraro,
  • J. Ereza,
  • B. Flaugher,
  • A. Font-Ribera,
  • D. Forero-Sánchez,
  • J. E. Forero-Romero,
  • C. S. Frenk,
  • B. T. Gänsicke,
  • L. Á. García,
  • J. García-Bellido,
  • C. Garcia-Quintero,
  • L. H. Garrison,
  • H. Gil-Marín,
  • J. Golden-Marx,
  • S. Gontcho A Gontcho,
  • A. X. Gonzalez-Morales,
  • V. Gonzalez-Perez et al. (164 additional authors not shown)
  • (less)
The Astronomical Journal (01/2024) doi:10.3847/1538-3881/ad0b08
abstract + abstract -

The Dark Energy Spectroscopic Instrument (DESI) was designed to conduct a survey covering 14,000 deg2 over five years to constrain the cosmic expansion history through precise measurements of Baryon Acoustic Oscillations (BAO). The scientific program for DESI was evaluated during a five month Survey Validation (SV) campaign before beginning full operations. This program produced deep spectra of tens of thousands of objects from each of the stellar (MWS), bright galaxy (BGS), luminous red galaxy (LRG), emission line galaxy (ELG), and quasar target classes. These SV spectra were used to optimize redshift distributions, characterize exposure times, determine calibration procedures, and assess observational overheads for the five-year program. In this paper, we present the final target selection algorithms, redshift distributions, and projected cosmology constraints resulting from those studies. We also present a `One-Percent survey' conducted at the conclusion of Survey Validation covering 140 deg2 using the final target selection algorithms with exposures of a depth typical of the main survey. The Survey Validation indicates that DESI will be able to complete the full 14,000 deg2 program with spectroscopically-confirmed targets from the MWS, BGS, LRG, ELG, and quasar programs with total sample sizes of 7.2, 13.8, 7.46, 15.7, and 2.87 million, respectively. These samples will allow exploration of the Milky Way halo, clustering on all scales, and BAO measurements with a statistical precision of 0.28% over the redshift interval z<1.1, 0.39% over the redshift interval 1.1<z<1.9, and 0.46% over the redshift interval 1.9<z<3.5.


CN-3
CN-4
RU-C
(1423)Can the low-redshift Lyman alpha forest constrain AGN feedback models?
  • Vikram Khaire,
  • Teng Hu,
  • Joseph F. Hennawi,
  • Michael Walther,
  • Frederick Davies
abstract + abstract -

We investigate the potential of low-redshift Lyman alpha (Lyα) forest for constraining active galactic nuclei (AGN) feedback models by analyzing the Illustris and IllustrisTNG simulation at z=0.1. These simulations are ideal for studying the impact of AGN feedback on the intergalactic medium (IGM) as they share initial conditions with significant differences in the feedback prescriptions. Both simulations reveal that the IGM is significantly impacted by AGN feedback. Specifically, feedback is stronger in Illustris and results in reducing cool baryon fraction to 23% relative to 39% in IllustrisTNG. However, when comparing various statistics of Lyα forest such as 2D and marginalized distributions of Doppler widths and H I column density, line density, and flux power spectrum with real data, we find that most of these statistics are largely insensitive to the differences in feedback models. This lack of sensitivity arises because of the fundamental degeneracy between the fraction of cool baryons and the H I photoionization rate (ΓHI) as their product determines the optical depth of the Lyα forest. Since the ΓHI cannot be precisely predicted from first principles, it needs to be treated as a nuisance parameter adjusted to match the observed Lyα line density. After adjusting ΓHI, the distinctions in the considered statistics essentially fade away. Only the Lyα flux power spectrum at small spatial scales exhibits potentially observable differences, although this may be specific to the relatively extreme feedback model employed in Illustris. Without independent constraints on either ΓHI or cool baryon fraction, constraining AGN feedback with low-redshift Lyα forest will be very challenging.


MIAPbP
(1422)Oscillations of atomic energy levels induced by QCD axion dark matter
  • Hyungjin Kim,
  • Gilad Perez
Physical Review D (01/2024) doi:10.1103/PhysRevD.109.015005
abstract + abstract -

Axion-gluon interaction induces quadratic couplings between the axion and the matter fields. We find that, if the axion is an ultralight dark matter field, it induces small oscillations of the mass of the hadrons as well as other nuclear quantities. As a result, atomic energy levels oscillate. We use currently available atomic spectroscopy data to constrain such axion-gluon coupling. We also project the sensitivities of future experiments, such as ones using molecular and nuclear clock transitions. We show that current and near-future experiments constrain a finely tuned parameter space of axion models. These can compete with or dominate the already-existing constraints from oscillating neutron electric dipole moment and supernova bound, in addition to those expected from near future magnetometer-based experiments. We also briefly discuss the reach of accelerometers and interferometers.


(1421)Detecting fast neutrino flavor conversions with machine learning
  • Sajad Abbar,
  • Hiroki Nagakura
Physical Review D (01/2024) doi:10.1103/PhysRevD.109.023033
abstract + abstract -

Neutrinos in dense environments like core-collapse supernovae (CCSNe) and neutron star mergers (NSMs) can undergo fast flavor conversions (FFCs) once the angular distribution of neutrino lepton number crosses zero along a certain direction. Recent advancements have demonstrated the effectiveness of machine learning (ML) in detecting these crossings. In this study, we enhance prior research in two significant ways. First, we utilize realistic data from CCSN simulations, where neutrino transport is solved using the full Boltzmann equation. We evaluate the ML methods' adaptability in a real-world context, enhancing their robustness. In particular, we demonstrate that when working with artificial data, simpler models outperform their more complex counterparts, a noteworthy illustration of the bias-variance tradeoff in the context of ML. We also explore methods to improve artificial datasets for ML training. In addition, we extend our ML techniques to detect the crossings in the heavy-leptonic channels, accommodating scenarios where νx and ν¯x may differ. Our research highlights the extensive versatility and effectiveness of ML techniques, presenting an unparalleled opportunity to evaluate the occurrence of FFCs in CCSN and NSM simulations.


(1420)Oscillations of high-energy cosmic neutrinos in the copious MeV neutrino background
  • Sajad Abbar,
  • Jose Alonso Carpio,
  • Kohta Murase
Physical Review D (01/2024) doi:10.1103/PhysRevD.109.023025
abstract + abstract -

The core-collapse of massive stars and the merger of neutron star binaries are among the most promising candidate sites for the production of high-energy cosmic neutrinos. We demonstrate that the high-energy neutrinos produced in such extreme environments can experience efficient flavor conversions on scales much shorter than those expected in vacuum, due to their coherent forward scatterings with the bath of decohered low-energy neutrinos emitted from the central engine. These low-energy neutrinos, which exist as mass eigenstates, provide a very special and peculiar dominant background for the propagation of the high-energy ones. We point out that the high-energy neutrino flavor ratio is modified to a value independent of neutrinos energies, which is distinct from the conventional prediction with the matter effect. We also suggest that the signals can be used as a novel probe of new neutrino interactions beyond the Standard Model. This is yet another context where neutrino-neutrino interactions can play a crucial role in their flavor evolution.


(1419)Adjoint chromoelectric and -magnetic correlators with gradient flow
  • Viljami Leino
abstract + abstract -

When QCD is described by a nonrelativistic effective field theory, operators consisting of gluonic correlators of two chromoelectric or -magnetic fields will often appear in descriptions of quarkonium physics. At zero T, these correlators give the masses of gluelumps and the moments of these correlators can be used to understand the inclusive P-wave decay of quarkonium. At finite T these correlators define the diffusion of the heavy quarkonium. However, these correlators come with a divergent term in lattice spacing which needs to be taken care of. We inspect these correlators in pure gauge theory with gradient flow smearing, which should allow us to reduce and remove the divergence more carefully. In these proceedings, we focus on the effect of gradient flow to these correlators and the reduction of this divergence.


RU-A
(1418)PartonDensity.jl: a novel parton density determination code
  • Francesca Capel,
  • Ritu Aggarwal,
  • Michiel Botje,
  • Allen Caldwell,
  • Oliver Schulz
  • +1
abstract + abstract -

We introduce our novel Bayesian parton density determination code, PartonDensity.jl. The motivation for this new code, the framework and its validation are described. As we show, PartonDensity.jl provides both a flexible environment for the determination of parton densities and a wealth of information concerning the knowledge update provided by the analyzed data set.


(1417)Dust-gas dynamics driven by the streaming instability with various pressure gradients
  • Stanley A. Baronett,
  • Chao-Chin Yang,
  • Zhaohuan Zhu
Monthly Notices of the Royal Astronomical Society (01/2024) doi:10.1093/mnras/stae272
abstract + abstract -

The streaming instability, a promising mechanism to drive planetesimal formation in dusty protoplanetary discs, relies on aerodynamic drag naturally induced by the background radial pressure gradient. This gradient should vary in disks, but its effect on the streaming instability has not been sufficiently explored. For this purpose, we use numerical simulations of an unstratified disc to study the non-linear saturation of the streaming instability with mono-disperse dust particles and survey a wide range of gradients for two distinct combinations of the particle stopping time and the dust-to-gas mass ratio. As the gradient increases, we find most kinematic and morphological properties increase but not always in linear proportion. The density distributions of tightly-coupled particles are insensitive to the gradient whereas marginally-coupled particles tend to concentrate by more than an order of magnitude as the gradient decreases. Moreover, dust-gas vortices for tightly-coupled particles shrink as the gradient decreases, and we note higher resolutions are required to trigger the instability in this case. In addition, we find various properties at saturation that depend on the gradient may be observable and may help reconstruct models of observed discs dominated by streaming turbulence. In general, increased dust diffusion from stronger gradients can lower the concentration of dust filaments and can explain the higher solid abundances needed to trigger strong particle clumping and the reduced planetesimal formation efficiency previously found in vertically-stratified simulations.


(1416)Flat F-theory and friends
  • Peng Cheng,
  • Ilarion V. Melnikov,
  • Ruben Minasian
Journal of High Energy Physics (01/2024) doi:10.1007/JHEP01(2024)027
abstract + abstract -

We discuss F-theory backgrounds associated to flat torus bundles over Ricci-flat manifolds. In this setting the F-theory background can be understood as a IIB orientifold with a large radius limit described by a supersymmetric compactification of IIB supergravity on a smooth, Ricci flat, but in general non-spin geometry. When compactified on an additional circle these backgrounds are T-dual to IIA compactifications on smooth non-orientable manifolds with a Pin structure.


RU-D
(1415)The TYPHOON Stellar Population Synthesis Survey. I. The Young Stellar Population of the Great Barred Spiral NGC 1365
  • Eva Sextl,
  • Rolf-Peter Kudritzki,
  • Andreas Burkert,
  • I. -Ting Ho,
  • H. Jabran Zahid
  • +4
  • Mark Seibert,
  • Andrew J. Battisti,
  • Barry F. Madore,
  • Jeffrey A. Rich
  • (less)
The Astrophysical Journal (01/2024) doi:10.3847/1538-4357/ad08b3
abstract + abstract -

We analyze TYPHOON long-slit-absorption line spectra of the starburst barred spiral galaxy NGC 1365 obtained with the Progressive Integral Step Method covering an area of 15 kpc2. Applying a population synthesis technique, we determine the spatial distribution of ages and metallicities of the young and old stellar populations together with star formation rates, reddening, extinction, and the ratio R V of extinction to reddening. We detect a clear indication of inside-out growth of the stellar disk beyond 3 kpc characterized by an outward increasing luminosity fraction of the young stellar population, a decreasing average age, and a history of mass growth, which was finished 2 Gyr later in the outermost disk. The metallicity of the young stellar population is clearly super solar but decreases toward larger galactocentric radii with a gradient of -0.02 dex kpc-1. On the other hand, the metal content of the old population does not show a gradient and stays constant at a level roughly 0.4 dex lower than that of the young population. In the center of NGC 1365, we find a confined region where the metallicity of the young population drops dramatically and becomes lower than that of the old population. We attribute this to the infall of metal-poor gas, and additionally, to interrupted chemical evolution where star formation is stopped by active galactic nuclei and supernova feedback and then after several gigayears resumes with gas ejected by stellar winds from earlier generations of stars. We provide a simple model calculation as support for the latter.


CN-7
RU-A
(1414)Indication of a p-ϕ bound state from a correlation function analysis
  • Emma Chizzali,
  • Yuki Kamiya,
  • Raffaele Del Grande,
  • Takumi Doi,
  • Laura Fabbietti
  • +2
Physics Letters B (01/2024) doi:10.1016/j.physletb.2023.138358
abstract + abstract -

The existence of a nucleon-ϕ (N-ϕ) bound state has been subject of theoretical and experimental investigations for decades. In this letter, indication of a p-ϕ bound state is found, using for the first time two-particle correlation functions as alternative to invariant mass spectra. Newly available lattice calculations for the spin 3/2 N-ϕ interaction by the HAL QCD collaboration are used to constrain the spin 1/2 counterpart from the fit of the experimental p-ϕ correlation function measured by ALICE. The corresponding scattering length and effective range are f0(1/2) = (-1.54-0.53+0.53 (stat .)-0.09+0.16 (syst .) + i ⋅0.00-0.00+0.35 (stat .)-0.00+0.16 (syst .)) fm and d0(1/2) = (0.39-0.09+0.09 (stat .)-0.03+0.02 (syst .) + i ⋅ 0.00-0.04+0.00 (stat .)-0.02+0.00 (syst .)) fm, respectively. The results imply the appearance of a p-ϕ bound state with an estimated binding energy in the range of 12.8 - 56.1 MeV.


CN-7
(1413)Dense nuclear matter equation of state from heavy-ion collisions
  • Agnieszka Sorensen,
  • Kshitij Agarwal,
  • Kyle W. Brown,
  • Zbigniew Chajęcki,
  • Paweł Danielewicz
  • +131
  • Christian Drischler,
  • Stefano Gandolfi,
  • Jeremy W. Holt,
  • Matthias Kaminski,
  • Che-Ming Ko,
  • Rohit Kumar,
  • Bao-An Li,
  • William G. Lynch,
  • Alan B. McIntosh,
  • William G. Newton,
  • Scott Pratt,
  • Oleh Savchuk,
  • Maria Stefaniak,
  • Ingo Tews,
  • ManYee Betty Tsang,
  • Ramona Vogt,
  • Hermann Wolter,
  • Hanna Zbroszczyk,
  • Navid Abbasi,
  • Jörg Aichelin,
  • Anton Andronic,
  • Steffen A. Bass,
  • Francesco Becattini,
  • David Blaschke,
  • Marcus Bleicher,
  • Christoph Blume,
  • Elena Bratkovskaya,
  • B. Alex Brown,
  • David A. Brown,
  • Alberto Camaiani,
  • Giovanni Casini,
  • Katerina Chatziioannou,
  • Abdelouahad Chbihi,
  • Maria Colonna,
  • Mircea Dan Cozma,
  • Veronica Dexheimer,
  • Xin Dong,
  • Travis Dore,
  • Lipei Du,
  • José A. Dueñas,
  • Hannah Elfner,
  • Wojciech Florkowski,
  • Yuki Fujimoto,
  • Richard J. Furnstahl,
  • Alexandra Gade,
  • Tetyana Galatyuk,
  • Charles Gale,
  • Frank Geurts,
  • Fabiana Gramegna,
  • Sašo Grozdanov,
  • Kris Hagel,
  • Steven P. Harris,
  • Wick Haxton,
  • Ulrich Heinz,
  • Michal P. Heller,
  • Or Hen,
  • Heiko Hergert,
  • Norbert Herrmann,
  • Huan Zhong Huang,
  • Xu-Guang Huang,
  • Natsumi Ikeno,
  • Gabriele Inghirami,
  • Jakub Jankowski,
  • Jiangyong Jia,
  • José C. Jiménez,
  • Joseph Kapusta,
  • Behruz Kardan,
  • Iurii Karpenko,
  • Declan Keane,
  • Dmitri Kharzeev,
  • Andrej Kugler,
  • Arnaud Le Fèvre,
  • Dean Lee,
  • Hong Liu,
  • Michael A. Lisa,
  • William J. Llope,
  • Ivano Lombardo,
  • Manuel Lorenz,
  • Tommaso Marchi,
  • Larry McLerran,
  • Ulrich Mosel,
  • Anton Motornenko,
  • Berndt Müller,
  • Paolo Napolitani,
  • Joseph B. Natowitz,
  • Witold Nazarewicz,
  • Jorge Noronha,
  • Jacquelyn Noronha-Hostler,
  • Grażyna Odyniec,
  • Panagiota Papakonstantinou,
  • Zuzana Paulínyová,
  • Jorge Piekarewicz,
  • Robert D. Pisarski,
  • Christopher Plumberg,
  • Madappa Prakash,
  • Jørgen Randrup,
  • Claudia Ratti,
  • Peter Rau,
  • Sanjay Reddy,
  • Hans-Rudolf Schmidt,
  • Paolo Russotto,
  • Radoslaw Ryblewski,
  • Andreas Schäfer,
  • Björn Schenke,
  • Srimoyee Sen,
  • Peter Senger,
  • Richard Seto,
  • Chun Shen,
  • Bradley Sherrill,
  • Mayank Singh,
  • Vladimir Skokov,
  • Michał Spaliński,
  • Jan Steinheimer,
  • Mikhail Stephanov,
  • Joachim Stroth,
  • Christian Sturm,
  • Kai-Jia Sun,
  • Aihong Tang,
  • Giorgio Torrieri,
  • Wolfgang Trautmann,
  • Giuseppe Verde,
  • Volodymyr Vovchenko,
  • Ryoichi Wada,
  • Fuqiang Wang,
  • Gang Wang,
  • Klaus Werner,
  • Nu Xu,
  • Zhangbu Xu,
  • Ho-Ung Yee,
  • Sherry Yennello,
  • Yi Yin
  • (less)
Progress in Particle and Nuclear Physics (01/2024) doi:10.1016/j.ppnp.2023.104080
abstract + abstract -

The nuclear equation of state (EOS) is at the center of numerous theoretical and experimental efforts in nuclear physics. With advances in microscopic theories for nuclear interactions, the availability of experiments probing nuclear matter under conditions not reached before, endeavors to develop sophisticated and reliable transport simulations to interpret these experiments, and the advent of multi-messenger astronomy, the next decade will bring new opportunities for determining the nuclear matter EOS, elucidating its dependence on density, temperature, and isospin asymmetry. Among controlled terrestrial experiments, collisions of heavy nuclei at intermediate beam energies (from a few tens of MeV/nucleon to about 25 GeV/nucleon in the fixed-target frame) probe the widest ranges of baryon density and temperature, enabling studies of nuclear matter from a few tenths to about 5 times the nuclear saturation density and for temperatures from a few to well above a hundred MeV, respectively. Collisions of neutron-rich isotopes further bring the opportunity to probe effects due to the isospin asymmetry. However, capitalizing on the enormous scientific effort aimed at uncovering the dense nuclear matter EOS, both at RHIC and at FRIB as well as at other international facilities, depends on the continued development of state-of-the-art hadronic transport simulations. This white paper highlights the essential role that heavy-ion collision experiments and hadronic transport simulations play in understanding strong interactions in dense nuclear matter, with an emphasis on how these efforts can be used together with microscopic approaches and neutron star studies to uncover the nuclear EOS.


CN-3
RU-B
(1412)Matter-antimatter asymmetry and dark matter stability from baryon number conservation
  • Mar Císcar-Monsalvatje,
  • Alejandro Ibarra,
  • Jérôme Vandecasteele
abstract + abstract -

There is currently no evidence for a baryon asymmetry in our Universe. Instead, cosmological observations have only demonstrated the existence of a quark-antiquark asymmetry, which does not necessarily imply a baryon asymmetric Universe, since the baryon number of the dark sector particles is unknown. In this paper we discuss a framework where the total baryon number of the Universe is equal to zero, and where the observed quark-antiquark asymmetry arises from neutron portal interactions with a dark sector fermion N that carries baryon number. In order to render a baryon symmetric universe throughout the whole cosmological history, we introduce a complex scalar χ, with opposite baryon number and with the same initial abundance as N. Notably, due to the baryon number conservation, χ is absolutely stable and could have an abundance today equal to the observed dark matter abundance. Therefore, in this simple framework, the existence of a quark-antiquark asymmetry is intimately related to the existence (and the stability) of dark matter.


CN-7
(1411)Astrophysical Axion Bounds: The 2024 Edition
  • Andrea Caputo,
  • Georg Raffelt
abstract + abstract -

We review the current status of astrophysical bounds on QCD axions, primarily based on the observational effects of nonstandard energy losses on stars, including black-hole superradiance. Over the past few years, many of the traditional arguments have been reexamined both theoretically and using modern data and new ideas have been put forth. This compact review updates similar Lecture Notes written by one of us in 2006 [Lect. Notes Phys. 741 (2008) 51-71].


(1410)Search for Supernova Progenitor Stars with ZTF and LSST
  • Nora L. Strotjohann,
  • Eran O. Ofek,
  • Avishay Gal-Yam,
  • Jesper Sollerman,
  • Ping Chen
  • +7
  • Ofer Yaron,
  • Barak Zackay,
  • Nabeel Rehemtulla,
  • Phillipe Gris,
  • Frank J. Masci,
  • Ben Rusholme,
  • Josiah Purdum
  • (less)
The Astrophysical Journal (01/2024) doi:10.3847/1538-4357/ad06b6
abstract + abstract -

The direct detection of core-collapse supernova (SN) progenitor stars is a powerful way of probing the last stages of stellar evolution. However, detections in archival Hubble Space Telescope images are limited to about one detection per year. Here, we explore whether we can increase the detection rate by using data from ground-based wide-field surveys. Due to crowding and atmospheric blurring, progenitor stars can typically not be identified in preexplosion images alone. Instead, we combine many pre-SN and late-time images to search for the disappearance of the progenitor star. As a proof of concept, we implement our search of ZTF data. For a few hundred images, we achieve limiting magnitudes of ~23 mag in the g and r bands. However, no progenitor stars or long-lived outbursts are detected for 29 SNe within z ≤ 0.01, and the ZTF limits are typically several magnitudes less constraining than detected progenitors in the literature. Next, we estimate progenitor detection rates for the Legacy Survey of Space and Time (LSST) with the Vera C. Rubin telescope by simulating a population of nearby SNe. The background from bright host galaxies reduces the nominal LSST sensitivity by, on average, 0.4 mag. Over the 10 yr survey, we expect the detection of ~50 red supergiant progenitors and several yellow and blue supergiants. The progenitors of Type Ib and Ic SNe will be detectable if they are brighter than -4.7 or -4.0 mag in the LSST i band, respectively. In addition, we expect the detection of hundreds of pre-SN outbursts depending on their brightness and duration.


(1409)Buzzard to Cardinal: Improved Mock Catalogs for Large Galaxy Surveys
  • Chun-Hao To,
  • Joseph DeRose,
  • Risa H. Wechsler,
  • Eli Rykoff,
  • Hao-Yi Wu
  • +4
  • Susmita Adhikari,
  • Elisabeth Krause,
  • Eduardo Rozo,
  • David H. Weinberg
  • (less)
The Astrophysical Journal (01/2024) doi:10.3847/1538-4357/ad0e61
abstract + abstract -

We present the Cardinal mock galaxy catalogs, a new version of the Buzzard simulation that has been updated to support ongoing and future cosmological surveys, including the Dark Energy Survey (DES), DESI, and LSST. These catalogs are based on a one-quarter sky simulation populated with galaxies out to a redshift of z = 2.35 to a depth of m r = 27. Compared to the Buzzard mocks, the Cardinal mocks include an updated subhalo abundance matching model that considers orphan galaxies and includes mass-dependent scatter between galaxy luminosity and halo properties. This model can simultaneously fit galaxy clustering and group-galaxy cross-correlations measured in three different luminosity threshold samples. The Cardinal mocks also feature a new color assignment model that can simultaneously fit color-dependent galaxy clustering in three different luminosity bins. We have developed an algorithm that uses photometric data to further improve the color assignment model and have also developed a novel method to improve small-scale lensing below the ray-tracing resolution. These improvements enable the Cardinal mocks to accurately reproduce the abundance of galaxy clusters and the properties of lens galaxies in the DES data. As such, these simulations will be a valuable tool for future cosmological analyses based on large sky surveys.


(1408)First JWST Observations of JAGB Stars in the SN Ia Host Galaxies: NGC 7250, NGC 4536, NGC 3972
  • Abigail J. Lee,
  • Wendy L. Freedman,
  • In Sung Jang,
  • Barry F. Madore,
  • Kayla A. Owens
The Astrophysical Journal (01/2024) doi:10.3847/1538-4357/ad12c7
abstract + abstract -

The J-region Asymptotic Giant Branch (JAGB) method is a standard candle that leverages the constant luminosities of color-selected, carbon-rich AGB stars, measured in the near-infrared at 1.2 μm. The Chicago-Carnegie Hubble Program has obtained JWST imaging of the SN Ia host galaxies NGC 7250, NGC 4536, and NGC 3972. With these observations, the JAGB method can be studied for the first time using JWST. Lee et al. demonstrated the JAGB magnitude is optimally measured in the outer disks of galaxies, because in the inner regions the JAGB magnitude can vary significantly due to a confluence of reddening, blending, and crowding effects. However, determining where the "outer disk" lies can be subjective. Therefore, we introduce a novel method for systematically selecting the outer disk. In a given galaxy, the JAGB magnitude is first separately measured in concentric regions, and the "outer disk" is then defined as the first radial bin where the JAGB magnitude stabilizes to a few hundredths of a magnitude. After successfully employing this method in our JWST galaxy sample, we find the JAGB stars are well segregated from other stellar populations in color-magnitude space, and have observed dispersions about their individual F115W modes of σ N7250 = 0.32 mag, σ N4536 = 0.34 mag, and σ N3972 = 0.35 mag. These measured dispersions are similar to the scatter measured for the JAGB stars in the LMC using 2MASS data (σ = 0.33 mag). In conclusion, the JAGB stars as observed with JWST clearly demonstrate their considerable power both as high-precision extragalactic distance indicators and as SN Ia supernova calibrators.


(1407)Machine Learning-Based Detection of Non-Axisymmetric Fast Neutrino Flavor Instabilities in Core-Collapse Supernovae
  • Sajad Abbar,
  • Akira Harada,
  • Hiroki Nagakura
abstract + abstract -

In dense neutrino environments like core-collapse supernovae (CCSNe) and neutron star mergers (NSMs), neutrinos can undergo fast flavor conversions (FFC) when their angular distribution of neutrino electron lepton number ($\nu$ELN) crosses zero along some directions. While previous studies have demonstrated the detection of axisymmetric $\nu$ELN crossings in these extreme environments, non-axisymmetric crossings have remained elusive, mostly due to the absence of models for their angular distributions. In this study, we present a pioneering analysis of the detection of non-axisymmetric $\nu$ELN crossings using machine learning (ML) techniques. Our ML models are trained on data from two CCSN simulations, one with rotation and one without, where non-axisymmetric features in neutrino angular distributions play a crucial role. We demonstrate that our ML models achieve detection accuracies exceeding 90\%. This is an important improvement, especially considering that a significant portion of $\nu$ELN crossings in these models eluded detection by earlier methods.


(1406)Vortex creep heating vs. dark matter heating in neutron stars
  • Motoko Fujiwara,
  • Koichi Hamaguchi,
  • Natsumi Nagata,
  • Maura E. Ramirez-Quezada
Physics Letters B (01/2024) doi:10.1016/j.physletb.2023.138341
abstract + abstract -

Dark matter particles captured in neutron stars deposit their energy as heat. This DM heating effect can be observed only if it dominates over other internal heating effects in neutron stars. In this work, as an example of such an internal heating source, we consider the frictional heating caused by the creep motion of neutron superfluid vortex lines in the neutron star crust. The luminosity of this heating effect is controlled by the strength of the interaction between the vortex lines and nuclei in the crust, which can be estimated from the many-body calculation of a high-density nuclear system as well as through the temperature observation of old neutron stars. We show that both the temperature observation and theoretical calculation suggest that the vortex creep heating dominates over the DM heating. The vortex-nuclei interaction must be smaller than the estimated values by several orders of magnitude to overturn this.


CN-7
(1405)Large Neutrino Secret Interactions Have a Small Impact on Supernovae
  • Damiano F. G. Fiorillo,
  • Georg G. Raffelt,
  • Edoardo Vitagliano
Physical Review Letters (01/2024) e-Print:2307.15115 doi:10.1103/PhysRevLett.132.021002
abstract + abstract -

When hypothetical neutrino secret interactions (ν SI ) are large, they form a fluid in a supernova (SN) core, flow out with sonic speed, and stream away as a fireball. For the first time, we tackle the complete dynamical problem and solve all steps, systematically using relativistic hydrodynamics. The impact on SN physics and the neutrino signal is remarkably small. For complete thermalization within the fireball, the observable spectrum changes in a way that is independent of the coupling strength. One potentially large effect beyond our study is quick deleptonization if ν SI violate lepton number. By present evidence, however, SN physics leaves open a large region in parameter space, where laboratory searches and future high-energy neutrino telescopes will probe ν SI .


CN-7
(1404)Supernova emission of secretly interacting neutrino fluid: Theoretical foundations
  • Damiano F. G. Fiorillo,
  • Georg G. Raffelt,
  • Edoardo Vitagliano
abstract + abstract -

Neutrino-neutrino scattering could have a large secret component that would turn neutrinos within a supernova (SN) core into a self-coupled fluid. Neutrino transport within the SN core, emission from its surface, expansion into space, and the flux spectrum and time structure at Earth might all be affected. We examine these questions from first principles. First, diffusive transport differs only by a modified spectral average of the interaction rate. We next study the fluid energy transfer between a hot and a cold blackbody surface in plane-parallel and spherical geometry. The key element is the decoupling process within the radiating bodies, which themselves are taken to be isothermal. For a zero-temperature cold plate, mimicking radiation into free space by the hot plate, the energy flux is 3%-4% smaller than the usual Stefan-Boltzmann law. The fluid energy density just outside the hot plate is numerically 0.70 of the standard case, the outflow velocity is the speed of sound vs=c /√{3 } , conspiring to a nearly unchanged energy flux. Our results provide the crucial boundary condition for the expansion of the self-interacting fluid into space, assuming an isothermal neutrino sphere. We also derive a dynamical solution, assuming the emission suddenly begins at some instant. A neutrino front expands in space with luminal speed, whereas the outflow velocity at the radiating surface asymptotically approaches vs from above. Asymptotically, one thus recovers the steady-state emission found in the two-plate model. A sudden end to neutrino emission leads to a fireball with constant thickness equal to the duration of neutrino emission.


(1403)The DRAGON-II simulations - III. Compact binary mergers in clusters with up to 1 million stars: Mass, spin, eccentricity, merger rate and pair instability supernovae rate.
  • Manuel Arca Sedda,
  • Albrecht W. H. Kamlah,
  • Rainer Spurzem,
  • Francesco Paolo Rizzuto,
  • Mirek Giersz
  • +2
Monthly Notices of the Royal Astronomical Society (01/2024) doi:10.1093/mnras/stad3951
abstract + abstract -

Compact binary mergers forming in star clusters may exhibit distinctive features that can be used to identify them among observed gravitational-wave (GW) sources. Such features likely depend on the host cluster structure and the physics of massive star evolution. Here, we dissect the population of compact binary mergers in the DRAGON-II simulation database, a suite of 19 direct N-body models representing dense star clusters with up to 106 stars and $<33~{{\%}}$ of stars in primordial binaries. We find a substantial population of black hole binary (BBH) mergers, some of them involving an intermediate-mass BH (IMBH), and a handful mergers involving a stellar BH and either a neutron star (NS) or a white dwarf (WD). Primordial binary mergers, $\sim 30~{{\%}}$ of the whole population, dominate ejected mergers. Dynamical mergers, instead, dominate the population of in-cluster mergers and are systematically heavier than primordial ones. Around 20 % of DRAGON-II mergers are eccentric in the LISA band and 5 % in the LIGO band. We infer a mean cosmic merger rate of $\mathcal {R}\sim 30(4.4)(1.2)$ yr-1 Gpc-3 for BBHs, NS-BH, and WD-BH binary mergers, respectively, and discuss the prospects for multimessenger detection of WD-BH binaries with LISA. We model the rate of pair-instability supernovae (PISNe) in star clusters and find that surveys with a limiting magnitude mbol = 25 can detect ~1 - 15 yr-1 PISNe. Comparing these estimates with future observations could help to pin down the impact of massive star evolution on the mass spectrum of compact stellar objects in star clusters.


(1402)The Uchuu-SDSS galaxy lightcones: A clustering, Redshift Space Distortion and Baryonic Acoustic Oscillation study
  • C. A. Dong-Páez,
  • A. Smith,
  • A. O. Szewciw,
  • J. Ereza,
  • M. H. Abdullah
  • +9
  • C. Hernández-Aguayo,
  • S. Trusov,
  • F. Prada,
  • A. Klypin,
  • T. Ishiyama,
  • A. Berlind,
  • P. Zarrouk,
  • J. López Cacheiro,
  • J. Ruedas
  • (less)
Monthly Notices of the Royal Astronomical Society (01/2024) doi:10.1093/mnras/stae062
abstract + abstract -

We present the data release of the Uchuu-SDSS galaxies: a set of 32 high-fidelity galaxy lightcones constructed from the large Uchuu 2.1 trillion particles N-body simulation using Planck cosmology. We adopt subhalo abundance matching to populate the Uchuu-box halo catalogues with SDSS galaxy luminosities. These box catalogues generated at several redshifts are combined to create a set of lightcones with redshift-evolving galaxy properties. The Uchuu-SDSS galaxy lightcones are built to reproduce the footprint and statistical properties of the SDSS main galaxy survey, along with stellar masses and star formation rates. This facilitates a direct comparison of the observed SDSS and simulated Uchuu-SDSS data. Our lightcones reproduce a large number of observational results, such as the distribution of galaxy properties, galaxy clustering, stellar mass functions, and halo occupation distributions. Using simulated and real data we select samples of bright red galaxies at zeff = 0.15 to explore Redshift Space Distortions and Baryon Acoustic Oscillations (BAO) by fitting the full two-point correlation function and the BAO peak. We create a set of 5100 galaxy lightcones using GLAM N-body simulations to compute covariance errors. We report a $\sim 30~{{\%}}$ precision increase on fσ8 and the pre-reconstruction BAO scale, due to our better estimate of the covariance matrix. From our BAO-inferred α and α parameters, we obtain the first SDSS measurements of the Hubble and angular diameter distances $D_\mathrm{H}(z=0.15) / r_d = 27.9^{+3.1}_{-2.7}$, $D_\mathrm{M}(z=0.15) / r_d = 5.1^{+0.4}_{-0.4}$. Overall, we conclude that the Planck Λ CDM cosmology nicely explains the observed large-scale structure statistics of SDSS. All data sets are made publicly available.


(1401)Tracing the ejecta from cosmic nucleosynthesis
  • Roland Diehl
abstract + abstract -

Long-lived radioactive by-products of nucleosynthesis provide an opportunity to trace the flow of ejecta away from its sources for times beyond where ejecta can be seen otherwise. Gamma rays from such radioactive decay in interstellar space can be measured with space-borne telescopes. A prominent useful example is 26Al with a radioactive decay time of one My. Such observations have revealed that typical surroundings of massive stars are composed of large cavities, extending to kpc sizes. Implications are that material recycling into new stars is twofold: rather direct as parental clouds are hosts to new star formation triggered by feedback, and more indirect as these large cavities merge with ambient interstellar gas after some delay. Kinematic measurements of hot interstellar gas carrying such ejecta promises important measurements complementing stellar and dense gas kinematics.


ODSL
(1400)Combined track finding with GNN & CKF
  • Lukas Heinrich,
  • Benjamin Huth,
  • Andreas Salzburger,
  • Tilo Wettig
abstract + abstract -

The application of Graph Neural Networks (GNN) in track reconstruction is a promising approach to cope with the challenges arising at the High-Luminosity upgrade of the Large Hadron Collider (HL-LHC). GNNs show good track-finding performance in high-multiplicity scenarios and are naturally parallelizable on heterogeneous compute architectures. Typical high-energy-physics detectors have high resolution in the innermost layers to support vertex reconstruction but lower resolution in the outer parts. GNNs mainly rely on 3D space-point information, which can cause reduced track-finding performance in the outer regions. In this contribution, we present a novel combination of GNN-based track finding with the classical Combinatorial Kalman Filter (CKF) algorithm to circumvent this issue: The GNN resolves the track candidates in the inner pixel region, where 3D space points can represent measurements very well. These candidates are then picked up by the CKF in the outer regions, where the CKF performs well even for 1D measurements. Using the ACTS infrastructure, we present a proof of concept based on truth tracking in the pixels as well as a dedicated GNN pipeline trained on $t\bar{t}$ events with pile-up 200 in the OpenDataDetector.


(1399)Quenched Static force from generalized Wilson loops with gradient flow
  • Julian Mayer-Steudte
abstract + abstract -

We compute the static force on the lattice in the quenched case directly through generalized Wilson loops. We modify the Wilson loop by inserting an $E$-field component on one of the temporal Wilson lines. However, chromo-field components prevent us from performing the continuum limit properly, hence, we use gradient flow to renormalize the field insertion. As a result, we obtain continuum results and compare them to perturbative expression to extract $\Lambda_0$, and we predict the value $\sqrt{8t_0} \Lambda_{\overline{\textrm{MS}}}^{n_f=0} =0.629^{+22}_{-26}$. This work serves as preparation for similar operators with field insertions required in nonrelativistic effective field theories.


RU-D
(1398)Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): HD 34700 A unveils an inner ring
  • G. Columba,
  • E. Rigliaco,
  • R. Gratton,
  • D. Mesa,
  • V. D'Orazi
  • +16
  • C. Ginski,
  • N. Engler,
  • J. P. Williams,
  • J. Bae,
  • M. Benisty,
  • T. Birnstiel,
  • P. Delorme,
  • C. Dominik,
  • S. Facchini,
  • F. Menard,
  • P. Pinilla,
  • C. Rab,
  • Á. Ribas,
  • V. Squicciarini,
  • R. G. van Holstein,
  • A. Zurlo
  • (less)
Astronomy and Astrophysics (01/2024) doi:10.1051/0004-6361/202347109
abstract + abstract -

Context. The study of protoplanetary disks is fundamental to understand their evolution and interaction with the surrounding environment, and to constrain planet formation mechanisms.
Aims: We aim to characterise the young binary system HD 34700 A, which shows a wealth of structures.
Methods: Taking advantage of the high-contrast imaging instruments SPHERE at the VLT, LMIRCam at the LBT, and of ALMA observations, we analyse this system at multiple wavelengths. We study the morphology of the rings and spiral arms and the scattering properties of the dust. We discuss the possible causes of all the observed features.
Results: We detect for the first time, in the Hα band, a ring extending from ~65 au to ~120 au, inside the ring which is already known from recent studies. These two have different physical and geometrical properties. Based on the scattering properties, the outer ring may consist of grains with a typical size of aout ≥ 4 µm, while the inner ring has a smaller typical size of ain ≤ 0.4 µm. Two extended logarithmic spiral arms stem from opposite sides of the disk. The outer ring appears as a spiral arm itself, with a variable radial distance from the centre and extended substructures. ALMA data confirm the presence of a millimetric dust substructure centred just outside the outer ring, and detect misaligned gas rotation patterns for HD 34700 A and B.
Conclusions: The complexity of HD 34700 A, revealed by the variety of observed features, suggests the existence of one or more disk-shaping physical mechanisms. Our findings are compatible with the presence inside the disk of an as of yet undetected planet of several Jupiter masses and the system interaction with the surroundings, by means of gas cloudlet capture or flybys. Further observations with JWST/MIRI or ALMA (gas kinematics) could shed more light on them.


(1397)Bulge-disc decomposition of the Hydra cluster galaxies in 12 bands
  • Ciria Lima-Dias,
  • Antonela Monachesi,
  • Sergio Torres-Flores,
  • Arianna Cortesi,
  • Daniel Hernández-Lang
  • +13
  • Gissel P. Montaguth,
  • Yolanda Jiménez-Teja,
  • Swayamtrupta Panda,
  • Karín Menéndez-Delmestre,
  • Thiago S. Gonçalves,
  • Hugo Méndez-Hernández,
  • Eduardo Telles,
  • Paola Dimauro,
  • Clécio R. Bom,
  • Claudia Mendes de Oliveira,
  • Antonio Kanaan,
  • Tiago Ribeiro,
  • William Schoenell
  • (less)
Monthly Notices of the Royal Astronomical Society (01/2024) doi:10.1093/mnras/stad3571
abstract + abstract -

When a galaxy falls into a cluster, its outermost parts are the most affected by the environment. In this paper, we are interested in studying the influence of a dense environment on different galaxy's components to better understand how this affects the evolution of galaxies. We use, as laboratory for this study, the Hydra cluster which is close to virialization; yet it still shows evidence of substructures. We present a multiwavelength bulge-disc decomposition performed simultaneously in 12 bands from S-PLUS (Southern Photometric Local Universe Survey) data for 52 galaxies brighter than mr = 16. We model the galaxies with a Sérsic profile for the bulge and an exponential profile for the disc. We find that the smaller, more compact, and bulge-dominated galaxies tend to exhibit a redder colour at a fixed stellar mass. This suggests that the same mechanisms (ram-pressure and tidal stripping) that are causing the compaction in these galaxies are also causing them to stop forming stars. The bulge size is unrelated to the galaxy's stellar mass, while the disc size increases with greater stellar mass, indicating the dominant role of the disc in the overall galaxy mass-size relation found. Furthermore, our analysis of the environment unveils that quenched galaxies are prevalent in regions likely associated with substructures. However, these areas also harbour a minority of star-forming galaxies, primarily resulting from galaxy interactions. Lastly, we find that ~37 per cent of the galaxies exhibit bulges that are bluer than their discs, indicative of an outside-in quenching process in this type of dense environments.


CN-2
(1396)Active droplets through enzyme-free, dynamic phosphorylation
  • Job Boekhoven,
  • Simone Poprawa,
  • Michele Stasi,
  • Monika Wenisch,
  • Brigitte Kriebisch
  • +1
Nature Portfolio (01/2024) doi:10.21203/rs.3.rs-3788577/v1
abstract + abstract -

Life continuously transduces energy to perform critical functions using energy stored in reactive molecules like ATP or NADH. ATP dynamically phosphorylates active sites on proteins and thereby regulates their function. Inspired by such machinery, regulating supramolecular functions using energy stored in reactive molecules has gained traction. Enzyme-free, synthetic systems that use dynamic phosphorylation to regulate supramolecular processes do not exist.

 

We present an enzyme-free reaction cycle that consumes phosphorylating agents by transiently phosphorylating amino acids. The phosphorylated amino acids are labile and deactivate through hydrolysis. The cycle exhibits versatility and tunability, allowing for the dynamic phosphorylation of multiple precursors with a tunable half-life. Notably, we show the resulting phosphorylated products can regulate the peptide’s phase separation, leading to active droplets that require the continuous conversion of fuel to sustain. Our new reaction cycle will be valuable as a model for biological phosphorylation but can also offer insights into protocell formation.


CN-6
(1395)Insights into the broad-band emission of the TeV blazar Mrk 501 during the first X-ray polarization measurements
  • S. Abe,
  • J. Abhir,
  • V. A. Acciari,
  • A. Aguasca-Cabot,
  • I. Agudo
  • +259
  • T. Aniello,
  • S. Ansoldi,
  • L. A. Antonelli,
  • A. Arbet Engels,
  • C. Arcaro,
  • K. Asano,
  • A. Babić,
  • A. Baquero,
  • U. Barres de Almeida,
  • J. A. Barrio,
  • I. Batković,
  • A. Bautista,
  • J. Baxter,
  • J. Becerra González,
  • W. Bednarek,
  • E. Bernardini,
  • M. Bernardos,
  • J. Bernete,
  • A. Berti,
  • J. Besenrieder,
  • C. Bigongiari,
  • A. Biland,
  • O. Blanch,
  • G. Bonnoli,
  • Ž. Bošnjak,
  • I. Burelli,
  • G. Busetto,
  • A. Campoy-Ordaz,
  • A. Carosi,
  • R. Carosi,
  • M. Carretero-Castrillo,
  • A. J. Castro-Tirado,
  • G. Ceribella,
  • Y. Chai,
  • A. Cifuentes,
  • E. Colombo,
  • J. L. Contreras,
  • J. Cortina,
  • S. Covino,
  • G. D'Amico,
  • V. D'Elia,
  • P. Da Vela,
  • F. Dazzi,
  • A. De Angelis,
  • B. De Lotto,
  • R. de Menezes,
  • A. Del Popolo,
  • M. Delfino,
  • J. Delgado,
  • C. Delgado Mendez,
  • F. Di Pierro,
  • L. Di Venere,
  • D. Dominis Prester,
  • A. Donini,
  • D. Dorner,
  • M. Doro,
  • D. Elsaesser,
  • G. Emery,
  • J. Escudero,
  • L. Fariña,
  • A. Fattorini,
  • L. Foffano,
  • L. Font,
  • S. Fröse,
  • Y. Fukazawa,
  • R. J. García López,
  • M. Garczarczyk,
  • S. Gasparyan,
  • M. Gaug,
  • J. G. Giesbrecht Paiva,
  • N. Giglietto,
  • F. Giordano,
  • P. Gliwny,
  • N. Godinović,
  • T. Gradetzke,
  • R. Grau,
  • D. Green,
  • J. G. Green,
  • P. Günther,
  • D. Hadasch,
  • A. Hahn,
  • T. Hassan,
  • L. Heckmann,
  • J. Herrera,
  • D. Hrupec,
  • M. Hütten,
  • R. Imazawa,
  • K. Ishio,
  • I. Jiménez Mart'inez,
  • T. Kayanoki,
  • D. Kerszberg,
  • G. W. Kluge,
  • Y. Kobayashi,
  • P. M. Kouch,
  • H. Kubo,
  • J. Kushida,
  • M. Láinez Lezáun,
  • A. Lamastra,
  • F. Leone,
  • E. Lindfors,
  • L. Linhoff,
  • S. Lombardi,
  • F. Longo,
  • R. López-Coto,
  • M. López-Moya,
  • A. López-Oramas,
  • S. Loporchio,
  • A. Lorini,
  • E. Lyard,
  • B. Machado de Oliveira Fraga,
  • P. Majumdar,
  • M. Makariev,
  • G. Maneva,
  • N. Mang,
  • M. Manganaro,
  • S. Mangano,
  • K. Mannheim,
  • M. Mariotti,
  • M. Martínez,
  • M. Martínez-Chicharro,
  • A. Mas-Aguilar,
  • D. Mazin,
  • S. Menchiari,
  • S. Mender,
  • D. Miceli,
  • T. Miener,
  • J. M. Miranda,
  • R. Mirzoyan,
  • M. Molero González,
  • E. Molina,
  • H. A. Mondal,
  • A. Moralejo,
  • D. Morcuende,
  • T. Nakamori,
  • C. Nanci,
  • V. Neustroev,
  • C. Nigro,
  • L. Nikolić,
  • K. Nilsson,
  • K. Nishijima,
  • T. Njoh Ekoume,
  • K. Noda,
  • S. Nozaki,
  • Y. Ohtani,
  • A. Okumura,
  • J. Otero-Santos,
  • S. Paiano,
  • M. Palatiello,
  • D. Paneque,
  • R. Paoletti,
  • J. M. Paredes,
  • M. Peresano,
  • M. Persic,
  • M. Pihet,
  • G. Pirola,
  • F. Podobnik,
  • P. G. Prada Moroni,
  • E. Prandini,
  • G. Principe,
  • C. Priyadarshi,
  • W. Rhode,
  • M. Ribó,
  • J. Rico,
  • C. Righi,
  • N. Sahakyan,
  • T. Saito,
  • K. Satalecka,
  • F. G. Saturni,
  • B. Schleicher,
  • K. Schmidt,
  • F. Schmuckermaier,
  • J. L. Schubert,
  • T. Schweizer,
  • A. Sciaccaluga,
  • G. Silvestri,
  • J. Sitarek,
  • D. Sobczynska,
  • A. Spolon,
  • A. Stamerra,
  • J. Strišković,
  • D. Strom,
  • Y. Suda,
  • S. Suutarinen,
  • H. Tajima,
  • M. Takahashi,
  • R. Takeishi,
  • F. Tavecchio,
  • P. Temnikov,
  • K. Terauchi,
  • T. Terzić,
  • M. Teshima,
  • L. Tosti,
  • S. Truzzi,
  • A. Tutone,
  • S. Ubach,
  • J. van Scherpenberg,
  • S. Ventura,
  • I. Viale,
  • C. F. Vigorito,
  • V. Vitale,
  • I. Vovk,
  • R. Walter,
  • M. Will,
  • C. Wunderlich,
  • T. Yamamoto,
  • I. Liodakis,
  • F. J. Aceituno,
  • B. Agís-González,
  • H. Akitaya,
  • M. I. Bernardos,
  • D. Blinov,
  • I. G. Bourbah,
  • C. Casadio,
  • V. Casanova,
  • F. D'Ammando,
  • V. Fallah Ramazani,
  • E. Fernández-García,
  • Y. Fukazawa,
  • M. García-Comas,
  • E. Gau,
  • A. Gokus,
  • M. Gurwell,
  • P. Hakala,
  • T. Hovatta,
  • Y. -D. Hu,
  • C. Husillos,
  • J. Jormanainen,
  • S. G. Jorstad,
  • K. S. Kawabata,
  • G. K. Keating,
  • S. Kiehlmann,
  • E. Kontopodis,
  • H. Krawczynski,
  • A. Lähteenmäki,
  • C. Leto,
  • L. Lisalda,
  • N. Mandarakas,
  • A. Marchini,
  • A. P. Marscher,
  • W. Max-Moerbeck,
  • R. Middei,
  • T. Mizuno,
  • I. Myserlis,
  • T. Nakaoka,
  • M. Perri,
  • S. Puccetti,
  • R. Rao,
  • A. C. S. Readhead,
  • R. Reeves,
  • N. Rodriguez Cavero,
  • Q. Salomé,
  • M. Sasada,
  • R. Skalidis,
  • A. Sota,
  • I. Syrjärinne,
  • M. Tornikoski,
  • M. Uemura,
  • F. Verrecchia,
  • A. Vervelaki
  • (less)
abstract + abstract -

We present the first multi-wavelength study of Mrk 501 including very-high-energy (VHE) gamma-ray observations simultaneous to X-ray polarization measurements from the Imaging X-ray Polarimetry Explorer (IXPE). We use radio-to-VHE data from a multi-wavelength campaign organized between 2022-03-01 and 2022-07-19. The observations were performed by MAGIC, Fermi-LAT, NuSTAR, Swift (XRT and UVOT), and several instruments covering the optical and radio bands. During the IXPE pointings, the VHE state is close to the average behavior with a 0.2-1 TeV flux of 20%-50% the emission of the Crab Nebula. Despite the average VHE activity, an extreme X-ray behavior is measured for the first two IXPE pointings in March 2022 with a synchrotron peak frequency >1 keV. For the third IXPE pointing in July 2022, the synchrotron peak shifts towards lower energies and the optical/X-ray polarization degrees drop. The X-ray polarization is systematically higher than at lower energies, suggesting an energy-stratification of the jet. While during the IXPE epochs the polarization angle in the X-ray, optical and radio bands align well, we find a clear discrepancy in the optical and radio polarization angles in the middle of the campaign. We model the broad-band spectra simultaneous to the IXPE pointings assuming a compact zone dominating in the X-rays and VHE, and an extended zone stretching further downstream the jet dominating the emission at lower energies. NuSTAR data allow us to precisely constrain the synchrotron peak and therefore the underlying electron distribution. The change between the different states observed in the three IXPE pointings can be explained by a change of magnetization and/or emission region size, which directly connects the shift of the synchrotron peak to lower energies with the drop in polarization degree.


RU-A
(1394)Constraint characterization and degree of freedom counting in Lagrangian field theory
  • Verónica Errasti Díez,
  • Markus Maier,
  • Julio A. Méndez-Zavaleta
Physical Review D (01/2024) doi:10.1103/PhysRevD.109.025010
abstract + abstract -

We present a Lagrangian approach to counting degrees of freedom in first-order field theories. The emphasis is on the systematic attainment of a complete set of constraints. In particular, we provide the first comprehensive procedure to ensure the functional independence of all constraints and discuss in detail the possible closures of the constraint algorithm. We argue degrees of freedom can but need not correspond to physical modes. The appendix comprises fully worked out, physically relevant examples of varying complexity.


(1393)Unveiling the white dwarf in J191213.72 - 441045.1 through ultraviolet observations
  • Ingrid Pelisoli,
  • Snehalata Sahu,
  • Maxim Lyutikov,
  • Maxim Barkov,
  • Boris T. Gänsicke
  • +5
  • Jaco Brink,
  • David A. H. Buckley,
  • Stephen B. Potter,
  • Axel Schwope,
  • S. H. Ramírez
  • (less)
Monthly Notices of the Royal Astronomical Society (01/2024) doi:10.1093/mnras/stad3442
abstract + abstract -

J191213.72 - 441045.1 is a binary system composed of a white dwarf and an M-dwarf in a 4.03-h orbit. It shows emission in radio, optical, and X-ray, all modulated at the white dwarf spin period of 5.3 min, as well as various orbital sideband frequencies. Like in the prototype of the class of radio-pulsing white dwarfs, AR Scorpii, the observed pulsed emission seems to be driven by the binary interaction. In this work, we present an analysis of far-ultraviolet spectra obtained with the Cosmic Origins Spectrograph at the Hubble Space Telescope, in which we directly detect the white dwarf in J191213.72 - 441045.1. We find that the white dwarf has a temperature of Teff = 11485 ± 90 K and mass of 0.59 ± 0.05 M. We place a tentative upper limit on the magnetic field of ≈50 MG. If the white dwarf is in thermal equilibrium, its physical parameters would imply that crystallization has not started in the core of the white dwarf. Alternatively, the effective temperature could have been affected by compressional heating, indicating a past phase of accretion. The relatively low upper limit to the magnetic field and potential lack of crystallization that could generate a strong field pose challenges to pulsar-like models for the system and give preference to propeller models with a low magnetic field. We also develop a geometric model of the binary interaction which explains many salient features of the system.


RU-D
(1392)TIPSY: Trajectory of Infalling Particles in Streamers around Young stars. Dynamical analysis of the streamers around S CrA and HL Tau
  • Aashish Gupta,
  • Anna Miotello,
  • Jonathan P. Williams,
  • Til Birnstiel,
  • Michael Kuffmeier
  • +1
abstract + abstract -

Context. Elongated trails of infalling gas, often referred to as "streamers," have recently been observed around young stellar objects (YSOs) at different evolutionary stages. This asymmetric infall of material can significantly alter star and planet formation processes, especially in the more evolved YSOs. Aims. In order to ascertain the infalling nature of observed streamer-like structures and then systematically characterize their dynamics, we developed the code TIPSY (Trajectory of Infalling Particles in Streamers around Young stars). Methods. Using TIPSY, the streamer molecular line emission is first isolated from the disk emission. Then the streamer emission, which is effectively a point cloud in three-dimensional (3D) position-position-velocity space, is simplified to a curve-like representation. The observed streamer curve is then compared to the theoretical trajectories of infalling material. The best-fit trajectories are used to constrain streamer features, such as the specific energy, the specific angular momenta, the infall timescale, and the 3D morphology. Results. We used TIPSY to fit molecular-line ALMA observations of streamers around a Class II binary system, S CrA, and a Class I/II protostar, HL Tau. Our results indicate that both of the streamers are consistent with infalling motion. TIPSY results and mass estimates suggest that S CrA and HL Tau are accreting material at a rate of $\gtrsim27$ M$_{jupiter}$ Myr$^{-1}$ and $\gtrsim5$ M$_{jupiter}$ Myr$^{-1}$, respectively, which can significantly increase the mass budget available to form planets. Conclusions. TIPSY can be used to assess whether the morphology and kinematics of observed streamers are consistent with infalling motion and to characterize their dynamics, which is crucial for quantifying their impact on the protostellar systems.


RU-A
(1391)Planar three-loop QCD helicity amplitudes for V+jet production at hadron colliders
  • Thomas Gehrmann,
  • Petr Jakubčík,
  • Cesare Carlo Mella,
  • Nikolaos Syrrakos,
  • Lorenzo Tancredi
Physics Letters B (01/2024) doi:10.1016/j.physletb.2023.138369
abstract + abstract -

We compute the planar three-loop Quantum Chromodynamics (QCD) corrections to the helicity amplitudes involving a vector boson V = Z ,W±, two quarks and a gluon. These amplitudes are relevant to vector-boson-plus-jet production at hadron colliders and other precision QCD observables. The planar corrections encompass the leading colour factors N3, N2Nf, NNf2 and Nf3 . We provide the finite remainders of the independent helicity amplitudes in terms of multiple polylogarithms, continued to all kinematic regions and in a form which is compact and lends itself to efficient numerical evaluation. The presented amplitude respects the conjectured symbol-adjacency constraints for amplitudes with three massless and one massive leg.


(1390)The SRG/eROSITA all-sky survey: Hard X-ray selected Active Galactic Nuclei
  • Sophia G. H. Waddell,
  • J. Buchner,
  • K. Nandra,
  • M. Salvato,
  • A. Merloni
  • +10
  • I. Gauger,
  • Th. Boller,
  • R. Seppi,
  • J. Wolf,
  • T. Liu,
  • M. Brusa,
  • J. Comparat,
  • T. Dwelly,
  • Z. Igo,
  • B. Musiimenta
  • (less)
abstract + abstract -

The eROSITA instrument aboard the Spectrum Roentgen Gamma (SRG) satellite has performed its first all-sky survey between December 2019 and June 2020. This paper presents the resulting hard X-ray (2.3-5 keV) sample, the first created from an all-sky imaging survey in the 2-8 keV band, for sources within western galactic sky. The 5466 hard X-ray selected sources detected with eROSITA are presented and discussed. The Bayesian statistics-based code NWAY is used to identify the counterparts for the X-ray sources. These sources are classified based on their multiwavelength properties, and the literature is searched to identify spectroscopic redshifts, which further inform the source classification. A total of 2547 sources are found to have good-quality counterparts, and 111 of these are detected only in the hard band. Comparing with other hard X-ray selected surveys, the eROSITA hard sample covers a larger redshift range and probes dimmer sources, providing a complementary and expanded sample as compared to Swift-BAT. Examining the column density distribution of missed and detected eROSITA sources present in the follow-up catalog of Swift BAT 70 month sources, it is demonstrated that eROSITA can detect obscured sources with column densities $>10^{24}$ cm$^{-2}$, but that the completeness drops rapidly after $10^{23}$ cm$^{-2}$. A sample of hard-only sources, many of which are likely to be heavily obscured AGN, is also presented and discussed. X-ray spectral fitting reveals that these sources have extremely faint soft X-ray emission and their optical images suggest that they are found in more edge-on galaxies with lower b/a. The resulting X-ray catalog is demonstrated to be a powerful tool for understanding AGN, in particular heavily obscured AGN found in the hard-only sample.


(1389)Spectrum of global string networks and the axion dark matter mass
  • Ken'ichi Saikawa,
  • Javier Redondo,
  • Alejandro Vaquero,
  • Mathieu Kaltschmidt
abstract + abstract -

Cold dark matter axions produced in the post-inflationary Peccei-Quinn symmetry breaking scenario serve as clear targets for their experimental detection, since it is in principle possible to give a sharp prediction for their mass once we understand precisely how they are produced from the decay of global cosmic strings in the early Universe. In this paper, we perform a dedicated analysis of the spectrum of axions radiated from strings based on large scale numerical simulations of the cosmological evolution of the Peccei-Quinn field on a static lattice. Making full use of the massively parallel code and computing resources, we executed the simulations with up to $11264^3$ lattice sites, which allows us to improve our understanding of the dependence on the parameter controlling the string tension and thus give a more accurate extrapolation of the numerical results. We found that there are several systematic effects that have been overlooked in previous works, such as the dependence on the initial conditions, contaminations due to oscillations in the spectrum, and discretisation effects, some of which could explain the discrepancy in the literature. We confirmed the trend that the spectral index of the axion emission spectrum increases with the string tension, but did not find a clear evidence of whether it continues to increase or saturates to a constant at larger values of the string tension due to the severe discretisation effects. Taking this uncertainty into account and performing the extrapolation with a simple power law assumption on the spectrum, we find that the dark matter mass is predicted in the range of $m_a \approx 95$-$450\,\mu\mathrm{eV}$.


(1388)The eROSITA view of the Abell 3391/95 field. Cluster outskirts and filaments
  • Angie Veronica,
  • Thomas H. Reiprich,
  • Florian Pacaud,
  • Naomi Ota,
  • Jann Aschersleben
  • +15
  • Veronica Biffi,
  • Esra Bulbul,
  • Nicolas Clerc,
  • Klaus Dolag,
  • Thomas Erben,
  • Efrain Gatuzz,
  • Vittorio Ghirardini,
  • Jürgen Kerp,
  • Matthias Klein,
  • Ang Liu,
  • Teng Liu,
  • Konstantinos Migkas,
  • Miriam E. Ramos-Ceja,
  • Jeremy Sanders,
  • Claudia Spinelli
  • (less)
Astronomy and Astrophysics (01/2024) doi:10.1051/0004-6361/202347037
abstract + abstract -

Context. About 30% - 40% of the baryons in the local Universe remain unobserved. Many of these "missing" baryons are expected to reside in the warm-hot intergalactic medium (WHIM) of the cosmic web filaments that connect clusters of galaxies. SRG/eROSITA performance verification (PV) observations covered about 15 square degrees of the A3391/95 system and have revealed a ~15 Mpc continuous soft emission connecting several galaxy groups and clusters.
Aims: We aim to characterize the gas properties in the cluster outskirts (R500 < r < R200) and in the detected inter-cluster filaments (> R200) and to compare them to predictions.
Methods: We performed X-ray image and spectral analyses using the eROSITA PV data in order to assess the gas morphology and properties in the outskirts and the filaments in the directions of the previously detected Northern and Southern Filament of the A3391/95 system. We constructed surface brightness profiles using particle-induced background-subtracted, exposure- and Galactic absorption-corrected eROSITA products in the soft band (0.3-2.0 keV). We constrained the temperatures, metallicities, and electron densities through X-ray spectral fitting and compared them with the expected properties of the WHIM. We took particular care of the foreground.
Results: In the filament-facing outskirts of A3391 and the Northern Clump, we find higher temperatures than typical cluster outskirts profiles, with a significance of between 1.6 and 2.8σ, suggesting heating due to their connections with the filaments. We confirm surface brightness excess in the profiles of the Northern, Eastern, and Southern Filaments. From spectral analysis, we detect hot gas of 0.96−0.14+0.17 keV and 1.09−0.06+0.09 for the Northern and Southern Filament, respectively, which are close to the upper WHIM temperature limit. The filament metallicities are below 10% solar metallicity and the electron densities are ranging between 2.6 and 6.3 × 10−5 cm−3. The characteristic properties of the Little Southern Clump (LSC), which is located at a distance of ~1.5R200 from A3395S in the Southern Filament, suggest that it is a small galaxy group. Excluding the LSC from the analysis of the Southern Filament does not significantly change the temperature or metallicity of the gas, but it decreases the gas density by 30%. This shows the importance of taking into account any clumps in order to avoid overestimation of the gas measurement in the outskirts and filament regions.
Conclusions: We present measurements of morphology, temperature, metallicity, and density of individual warm-hot filaments. The electron densities of the filaments are consistent with the WHIM properties as predicted by cosmological simulations, but the temperatures are higher. As both filaments are short (1.8 and 2.7 Mpc) and located in a denser environment, stronger gravitational heating may be responsible for this temperature enhancement. The metallicities are low, but still within the expected range from the simulations.

Image that is displayed in Fig. 1 is available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (ftp://130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/681/A108


(1387)Exploring High-Purity Multiparton Scattering at Hadron Colliders
  • Jeppe R. Andersen,
  • Pier Francesco Monni,
  • Luca Rottoli,
  • Gavin P. Salam,
  • Alba Soto-Ontoso
Physical Review Letters (01/2024) doi:10.1103/PhysRevLett.132.041901
abstract + abstract -

Multiparton interactions are a fascinating phenomenon that occur in almost every high-energy hadron-hadron collision yet are remarkably difficult to study quantitatively. In this Letter, we present a strategy to optimally disentangle multiparton interactions from the primary scattering in a collision. That strategy enables probes of multiparton interactions that are significantly beyond the state of the art, including their characteristic momentum scale, the interconnection between primary and secondary scatters, and the pattern of three and potentially even more simultaneous hard scatterings. This opens a path to powerful new constraints on multiparton interactions for LHC phenomenology and to the investigation of their rich field-theoretical structure.


RU-C
(1386)The SRG/eROSITA All-Sky Survey: Constraints on AGN Feedback in Galaxy Groups
  • Y. E. Bahar,
  • E. Bulbul,
  • V. Ghirardini,
  • J. S. Sanders,
  • X. Zhang
  • +23
  • A. Liu,
  • N. Clerc,
  • E. Artis,
  • F. Balzer,
  • V. Biffi,
  • S. Bose,
  • J. Comparat,
  • K. Dolag,
  • C. Garrel,
  • B. Hadzhiyska,
  • C. Hernández-Aguayo,
  • L. Hernquist,
  • M. Kluge,
  • S. Krippendorf,
  • A. Merloni,
  • K. Nandra,
  • R. Pakmor,
  • P. Popesso,
  • M. Ramos-Ceja,
  • R. Seppi,
  • V. Springel,
  • J. Weller,
  • S. Zelmer
  • (less)
abstract + abstract -

We investigate the impact of AGN feedback, on the entropy and characteristic temperature measurements of galaxy groups detected in the SRG/eROSITA's first All-Sky Survey (eRASS1) to shed light on the characteristics of the feedback mechanisms. We analyze deeper eROSITA observations of 1178 galaxy groups detected in eRASS1. We divide the sample into 271 subsamples and extract average thermodynamic properties, including electron density, temperature, and entropy at three characteristic radii along with the integrated temperature by jointly analyzing X-ray images and spectra following a Bayesian approach. We present the tightest constraints on the impact of AGN feedback through our average entropy and characteristic temperature measurements of the largest group sample used in X-ray studies, incorporating major systematics in our analysis. We find that entropy shows an increasing trend with temperature in the form of a power-law-like relation at the higher intra-group medium temperatures, while for the low mass groups, a slight flattening is observed on the average entropy. Overall, the observed entropy measurements agree well with the earlier measurements in the literature. The comparisons with the state-of-the-art cosmological hydrodynamic simulations (MillenniumTNG, Magneticum, OWL simulations) after the applications of the selection function calibrated for our galaxy groups reveal that observed entropy profiles in the cores are below the predictions of simulations. At the mid-region, the entropy measurements agree well with the Magneticum simulations, whereas the predictions of MillenniumTNG and OWL simulations fall below observations. At the outskirts, the overall agreement between the observations and simulations improves, with Magneticum simulations reproducing the observations the best. Our measurements will pave the way for more realistic AGN feedback implementations in simulations.


(1385)Establishing the impact of luminous AGN with multi-wavelength observations and simulations
  • C. M. Harrison,
  • A. Girdhar,
  • S. R. Ward
Black Hole Winds at All Scales (2024) doi:10.1017/S1743921323002806
abstract + abstract -

Cosmological simulations fail to reproduce realistic galaxy populations without energy injection from active galactic nuclei (AGN) into the interstellar medium (ISM) and circumgalactic medium (CGM); a process called `AGN feedback'. Consequently, observational work searches for evidence that luminous AGN impact their host galaxies. Here, we review some of this work. Multi-phase AGN outflows are common, some with potential for significant impact. Additionally, multiple feedback channels can be observed simultaneously; e.g., radio jets from `radio quiet' quasars can inject turbulence on ISM scales, and displace CGM-scale molecular gas. However, caution must be taken comparing outflows to simulations (e.g., kinetic coupling efficiencies) to infer feedback potential, due to a lack of comparable predictions. Furthermore, some work claims limited evidence for feedback because AGN live in gas-rich, star-forming galaxies. However, simulations do not predict instantaneous, global impact on molecular gas or star formation. The impact is expected to be cumulative, over multiple episodes.


ODSL
RU-B
(1384)Fitting neutrino flares: Applying expectation maximization on neutrino data
  • Martina Karl,
  • Philipp Eller
abstract + abstract -

We present a new approach for identifying neutrino flares. Using the unsupervised machine learning algorithm expectation maximization, we reduce computing times compared to conventional approaches by a factor of 105 on a single CPU. Expectation maximization is also easily expandable to multiple flares. We explain the application of the algorithm and fit the neutrino flare of TXS 0506+056 as an example.


CN-8
(1383)Attention to Entropic Communication
  • Torsten Enßlin,
  • Carolin Weidinger,
  • Philipp Frank
Annalen der Physik (2024) e-Print:2307.11423
abstract + abstract -

The concept of attention, numerical weights that emphasize the importance of particular data, has proven to be very relevant in artificial intelligence. Relative entropy (RE, aka Kullback-Leibler divergence) plays a central role in communication theory. Here we combine these concepts, attention and RE. RE guides optimal encoding of messages in bandwidth-limited communication as well as optimal message decoding via the maximum entropy principle (MEP). In the coding scenario, RE can be derived from four requirements, namely being analytical, local, proper, and calibrated. Weighted RE, used for attention steering in communications, turns out to be improper. To see how proper attention communication can emerge, we analyze a scenario of a message sender who wants to ensure that the receiver of the message can perform well-informed actions. If the receiver decodes the message using the MEP, the sender only needs to know the receiver's utility function to inform optimally, but not the receiver's initial knowledge state. In case only the curvature of the utility function maxima are known, it becomes desirable to accurately communicate an attention function, in this case a by this curvature weighted and re-normalized probability function. Entropic attention communication is here proposed as the desired generalization of entropic communication that permits weighting while being proper, thereby aiding the design of optimal communication protocols in technical applications and helping to understand human communication. For example, our analysis shows how to derive the level of cooperation expected under misaligned interests of otherwise honest communication partners.


CN-3
CN-4
RU-C
(1382)Searching for the Imprints of AGN Feedback on the Lyman Alpha Forest Around Luminous Red Galaxies
  • Vikram Khaire,
  • Teng Hu,
  • Joseph F. Hennawi,
  • Joseph N. Burchett,
  • Michael Walther
  • +1
abstract + abstract -

We explore the potential of using the low-redshift Lyman-α (Lyα) forest surrounding luminous red galaxies (LRGs) as a tool to constrain active galactic nuclei (AGN) feedback models. Our analysis is based on snapshots from the Illustris and IllustrisTNG simulations at a redshift of z=0.1. These simulations offer an ideal platform for studying the influence of AGN feedback on the gas surrounding galaxies, as they share the same initial conditions and underlying code but incorporate different feedback prescriptions. Both simulations show significant impacts of feedback on the temperature and density of the gas around massive halos. Following our previous work, we adjusted the UV background in both simulations to align with the observed number density of Lyα lines (dN/dz) in the intergalactic medium and study the Lyα forest around massive halos hosting LRGs, at impact parameters (r⊥) ranging from 0.1 to 100 pMpc. Our findings reveal that dN/dz, as a function of r⊥, is approximately 1.5 to 2 times higher in IllustrisTNG compared to Illustris up to r⊥ of ∼10 pMpc. To further assess whether existing data can effectively discern these differences, we search for archival data containing spectra of background quasars probing foreground LRGs. Through a feasibility analysis based on this data, we demonstrate that dN/dz(r⊥) measurements can distinguish between feedback models of IllustrisTNG and Illustris with a precision exceeding 12σ. This underscores the potential of dN/dz(r⊥) measurements around LRGs as a valuable benchmark observation for discriminating between different feedback models.


CN-3
CN-4
RU-C
(1381)Measurements of the Thermal and Ionization State of the Intergalactic Medium during the Cosmic Afternoon
  • Teng Hu,
  • Vikram Khaire,
  • Joseph F. Hennawi,
  • Todd M. Tripp,
  • Jose Oñorbe
  • +2
abstract + abstract -

We perform the first measurement of the thermal and ionization state of the intergalactic medium (IGM) across 0.9 < z < 1.5 using 301 \lya absorption lines fitted from 12 HST STIS quasar spectra, with a total pathlength of \Delta z=2.1. We employ the machine-learning-based inference method that uses joint b-N distributions obtained from \lyaf decomposition. Our results show that the HI photoionization rates, \Gamma, are in good agreement with the recent UV background synthesis models, with \log (\Gamma/s^{-1})={-11.79}^{0.18}_{-0.15}, -11.98}^{0.09}_{-0.09}, and {-12.32}^{0.10}_{-0.12} at z=1.4, 1.2, and 1 respectively. We obtain the IGM temperature at the mean density, T_0, and the adiabatic index, \gamma, as [\log (T_0/K), \gamma]= [{4.13}^{+0.12}_{-0.10}, {1.34}^{+0.10}_{-0.15}], [{3.79}^{+0.11}_{-0.11}, {1.70}^{+0.09}_{-0.09}] and [{4.12}^{+0.15}_{-0.25}, {1.34}^{+0.21}_{-0.26}] at z=1.4, 1.2 and 1 respectively. Our measurements of T_0 at z=1.4 and 1.2 are consistent with the expected trend from z<3 temperature measurements as well as theoretical expectations that, in the absence of any non-standard heating, the IGM should cool down after HeII reionization. Whereas, our T_0 measurements at z=1 show unexpectedly high IGM temperature. However, because of the relatively large uncertainty in these measurements of the order of \Delta T_0~5000 K, mostly emanating from the limited redshift path length of available data in these bins, we can not definitively conclude whether the IGM cools down at z<1.5. Lastly, we generate a mock dataset to test the constraining power of future measurement with larger datasets. The results demonstrate that, with redshift pathlength \Delta z \sim 2 for each redshift bin, three times the current dataset, we can constrain the T_0 of IGM within 1500K. Such precision would be sufficient to conclusively constrain the history of IGM thermal evolution at z < 1.5.


CN-3
CN-4
RU-C
(1380)The Early Data Release of the Dark Energy Spectroscopic Instrument
  • DESI Collaboration: A. G. Adame,
  • J. Aguilar,
  • S. Ahlen,
  • S. Alam,
  • G. Aldering
  • +94
  • D. M. Alexander,
  • R. Alfarsy,
  • C. Allende Prieto,
  • M. Alvarez,
  • O. Alves,
  • A. Anand,
  • F. Andrade-Oliveira,
  • E. Armengaud,
  • J. Asorey,
  • S. Avila,
  • A. Aviles,
  • S. Bailey,
  • A. Balaguera-Antolínez,
  • O. Ballester,
  • C. Baltay,
  • A. Bault,
  • J. Bautista,
  • J. Behera,
  • S. F. Beltran,
  • S. BenZvi,
  • L. Beraldo e Silva,
  • J. R. Bermejo-Climent,
  • A. Berti,
  • R. Besuner,
  • F. Beutler,
  • D. Bianchi,
  • C. Blake,
  • R. Blum,
  • A. S. Bolton,
  • S. Brieden,
  • A. Brodzeller,
  • D. Brooks,
  • Z. Brown,
  • E. Buckley-Geer,
  • E. Burtin,
  • L. Cabayol-Garcia,
  • Z. Cai,
  • R. Canning,
  • L. Cardiel-Sas,
  • A. Carnero Rosell,
  • F. J. Castander,
  • J.L. Cervantes-Cota,
  • S. Chabanier,
  • E. Chaussidon,
  • J. Chaves-Montero,
  • S. Chen,
  • C. Chuang,
  • T. Claybaugh,
  • S. Cole,
  • A. P. Cooper,
  • A. Cuceu,
  • T. M. Davis,
  • K. Dawson,
  • R. de Belsunce,
  • R. de la Cruz,
  • A. de la Macorra,
  • A. de Mattia,
  • R. Demina,
  • U. Demirbozan,
  • J. DeRose,
  • A. Dey,
  • B. Dey,
  • G. Dhungana,
  • J. Ding,
  • Z. Ding,
  • P. Doel,
  • R. Doshi,
  • K. Douglass,
  • A. Edge,
  • S. Eftekharzadeh,
  • D. J. Eisenstein,
  • A. Elliott,
  • S. Escoffier,
  • P. Fagrelius,
  • X. Fan,
  • K. Fanning,
  • V. A. Fawcett,
  • S. Ferraro,
  • J. Ereza,
  • B. Flaugher,
  • A. Font-Ribera,
  • D. Forero-Sánchez,
  • J. E. Forero-Romero,
  • C. S. Frenk,
  • B. T. Gänsicke,
  • L. Á. García,
  • J. García-Bellido,
  • C. Garcia-Quintero,
  • L. H. Garrison,
  • H. Gil-Marín,
  • J. Golden-Marx,
  • S. Gontcho A Gontcho,
  • A. X. Gonzalez-Morales,
  • V. Gonzalez-Perez et al. (165 additional authors not shown)
  • (less)
abstract + abstract -

The Dark Energy Spectroscopic Instrument (DESI) completed its five-month Survey Validation in May 2021. Spectra of stellar and extragalactic targets from Survey Validation constitute the first major data sample from the DESI survey. This paper describes the public release of those spectra, the catalogs of derived properties, and the intermediate data products. In total, the public release includes good-quality spectral information from 466,447 objects targeted as part of the Milky Way Survey, 428,758 as part of the Bright Galaxy Survey, 227,318 as part of the Luminous Red Galaxy sample, 437,664 as part of the Emission Line Galaxy sample, and 76,079 as part of the Quasar sample. In addition, the release includes spectral information from 137,148 objects that expand the scope beyond the primary samples as part of a series of secondary programs. Here, we describe the spectral data, data quality, data products, Large-Scale Structure science catalogs, access to the data, and references that provide relevant background to using these spectra.


CN-3
CN-4
RU-C
(1379)Mock data sets for the Eboss and DESI Lyman-α forest surveys
  • Thomas Etourneau,
  • Jean-Marc Le Goff,
  • James Rich,
  • Ting Tan,
  • Andrei Cuceu
  • +30
  • S. Ahlen,
  • E. Armengaud,
  • D. Brooks,
  • T. Claybaugh,
  • A. de la Macorra,
  • P. Doel,
  • A. Font-Ribera,
  • J.E. Forero-Romero,
  • S. Gontcho A Gontcho,
  • A. X. Gonzalez-Morales,
  • H. K. Herrera-Alcantar,
  • K. Honscheid,
  • T. Kisner,
  • M. Landriau,
  • M. Manera,
  • P. Martini,
  • R. Miquel,
  • A. Muñoz-Gutiérrez,
  • J. Nie,
  • I. Pérez-Ràfols,
  • C. Poppett,
  • C. Ravoux,
  • M. Rezaie,
  • G. Rossi,
  • E. Sanchez,
  • M. Schubnell,
  • J. Stermer,
  • G. Tarlé,
  • M. Walther,
  • Z. Zhou
  • (less)
abstract + abstract -

We present a publicly-available code to generate mock Lyman-α (\lya) forest data sets. The code is based on the Fluctuating Gunn-Peterson Approximation (FGPA) applied to Gaussian random fields and on the use of fast Fourier transforms (FFT). The output includes spectra of lya transmitted flux fraction, F, a quasar catalog, and a catalog of high-column-density systems. While these three elements have realistic correlations, additional code is then used to generate realistic quasar spectra, to add absorption by high-column-density systems and metals, and to simulate instrumental effects. Redshift space distortions (RSD) are implemented by including the large-scale velocity-gradient field in the FGPA resulting in a correlation function of F that can be accurately predicted. One hundred realizations have been produced over the 14,000 deg2 Dark Energy Spectroscopy Instrument (DESI) survey footprint with 100 quasars per deg2, and they are being used for the Extended Baryon Oscillation Survey (eBOSS) and DESI surveys. The analysis of these realizations shows that the correlation of F follows the prediction within the accuracy of eBOSS survey. The most time-consuming part of the production occurs before application of the FGPA, and the existing pre-FGPA forests can be used to easily produce new mock sets with modified redshift-dependent bias parameters or observational conditions.


CN-7
RU-A
(1378)Partial-wave analysis of τ − → π−π−π+ντ at BELLE
  • Andrei Rabusov,
  • Daniel Greenwald,
  • Stephan Paul
Il Nuovo Cimento C (2024) e-Print:2310.09155
abstract + abstract -

We present preliminary results of a partial-wave analysis of τ−→π−π−π+νττ−→π−π−π+ντ​ in data from the Belle experiment at the KEKB e+e−e+e− collider. We demonstrate the presence of the a1(1420)a1​(1420) and a1(1640)a1​(1640) resonances in tauon decays and measure their masses and widths. We also present validation of our findings using a model-independent approach. Our results can improve modeling in simulation studies necessary for measuring the tauon electric and magnetic dipole moments and Michel parameters.

 


CN-3
RU-A
(1377)Constructing model-agnostic likelihoods, a method for the reinterpretation of particle physics results
  • Lorenz Gärtner,
  • Nikolai Hartmann,
  • Lukas Heinrich,
  • Malin Horstmann,
  • Thomas Kuhr
  • +3
  • Méril Reboud,
  • Slavomira Stefkova,
  • Danny van Dyk
  • (less)
arXiv e-prints (2024) e-Print:2402.08417
abstract + abstract -

Experimental High Energy Physics has entered an era of precision measurements. However, measurements of many of the accessible processes assume that the final states' underlying kinematic distribution is the same as the Standard Model prediction. This assumption introduces an implicit model-dependency into the measurement, rendering the reinterpretation of the experimental analysis complicated without reanalysing the underlying data. We present a novel reweighting method in order to perform reinterpretation of particle physics measurements. It makes use of reweighting the Standard Model templates according to kinematic signal distributions of alternative theoretical models, prior to performing the statistical analysis. The generality of this method allows us to perform statistical inference in the space of theoretical parameters, assuming different kinematic distributions, according to a beyond Standard Model prediction. We implement our method as an extension to the pyhf software and interface it with the EOS software, which allows us to perform flavor physics phenomenology studies. Furthermore, we argue that, beyond the pyhf or HistFactory likelihood specification, only minimal information is necessary to make a likelihood model-agnostic and hence easily reinterpretable. We showcase that publishing such likelihoods is crucial for a full exploitation of experimental results.


C2PAP
CN-2
RU-D
(1376)The interplay between forming planets and photoevaporating discs II: Wind-driven gas redistribution
  • Michael L. Weber,
  • Giovanni Picogna,
  • Barbara Ercolano
arXiv e-prints (2024) e-Print:2402.12053
abstract + abstract -

Disc winds and planet-disc interactions are two crucial mechanisms that define the structure, evolution and dispersal of protoplanetary discs. While winds are capable of removing material from discs, eventually leading to their dispersal, massive planets can shape their disc by creating sub-structures such as gaps and spiral arms. We study the interplay between an X-ray photoevaporative disc wind and the substructures generated due to planet-disc interactions to determine how their mutual interactions affect the disc's and the planet's evolution. We perform three-dimensional hydrodynamic simulations of viscous (α=6.9⋅10−4) discs that host a Jupiter-like planet and undergo X-ray photoevaporation. We trace the gas flows within the disc and wind and measure the accretion rate onto the planet, as well as the gravitational torque that is acting on it. Our results show that the planetary gap takes away the wind's pressure support, allowing wind material to fall back into the gap. This opens new pathways for material from the inner disc (and part of the outer disc) to be redistributed through the wind towards the gap. Consequently, the gap becomes shallower, and the flow of mass across the gap in both directions is significantly increased, as well as the planet's mass-accretion rate (by factors ≈5 and ≈2, respectively). Moreover, the wind-driven redistribution results in a denser inner disc and less dense outer disc, which, combined with the recycling of a significant portion of the inner wind, leads to longer lifetimes of the inner disc, contrary to the expectation in a planet-induced photoevaporation (PIPE) scenario that has been proposed in the past.


CN-7
RU-A
(1375)Impact of isovector pairing fluctuation on neutrinoless double-beta decay in multi-reference covariant density functional theory
  • C. R. Ding,
  • X. Zhang,
  • J. M. Yao,
  • P. Ring,
  • and J. Meng
Physical Review C (November/2023) e-Print:2305.00742 doi:10.1103/PhysRevC.108.054304
abstract + abstract -

We extend the multireference covariant density-functional theory (MR-CDFT) by including fluctuations in quadrupole deformations and average isovector pairing gaps simultaneously for the nuclear matrix elements (NMEs) of neutrinoless double-beta (0νββ) decay in the candidate nuclei 76Ge, 82Se, 100Mo, 130Te, and 136Xe assuming the exchange of either light or heavy neutrinos. The results indicate a linear correlation between the predicted NMEs and the isovector pairing strengths, as well as the excitation energies of 2+1 and 4+1 states. By adjusting the pairing strengths based on the excitation energies of the 2+1 states, we calculate the NMEs for 0νββ decay, which are reduced by approximately 12% to 62% compared with the results obtained in the previous studies by Song et al. [Phys. Rev. C 95, 024305 (2017)]. Additionally, upon introducing the average isovector pairing gap as an additional generator coordinate in the calculation, the NMEs increase by a factor ranging from 56% to 218%.


ODSL
RU-B
(1374)GraphNeT: Graph neural networks for neutrino telescope event reconstruction
  • Andreas Søgaard,
  • Rasmus F. Ørsøe,
  • Leon Bozianu,
  • Morten Holm,
  • Kaare Endrup Iversen
  • +4
  • Tim Guggenmos,
  • Martin Ha Minh,
  • Philipp Eller,
  • Troels C. Petersen
  • (less)
The Journal of open Source Software (May/2023) e-Print:2210.12194 doi:10.21105/joss.04971
abstract + abstract -

GraphNeT is an open-source python framework aimed at providing high quality, user friendly, end-to-end functionality to perform reconstruction tasks at neutrino telescopes using graph neural networks (GNNs). GraphNeT makes it fast and easy to train complex models that can provide event reconstruction with state-of-the-art performance, for arbitrary detector configurations, with inference times that are orders of magnitude faster than traditional reconstruction techniques. GNNs from GraphNeT are flexible enough to be applied to data from all neutrino telescopes, including future projects such as IceCube extensions or P-ONE. This means that GNN-based reconstruction can be used to provide state-of-the-art performance on most reconstruction tasks in neutrino telescopes, at real-time event rates, across experiments and physics analyses, with vast potential impact for neutrino and astro-particle physics.


ODSL
RU-B
(1373)A goodness-of-fit test based on a recursive product of spacings
  • Philipp Eller,
  • Lolian Shtembari
Journal of Intstrumentation (March/2023) e-Print:2111.02252v2 doi:10.48550/arXiv.2111.02252
abstract + abstract -

We introduce a new statistical test based on the observed spacings of ordered data. The statistic is sensitive to detect non-uniformity in random samples, or short-lived features in event time series. Under some conditions, this new test can outperform existing ones, such as the well known Kolmogorov-Smirnov or Anderson-Darling tests, in particular when the number of samples is small and differences occur over a small quantile of the null hypothesis distribution. A detailed description of the test statistic is provided including a detailed discussion of the parameterization of its distribution via asymptotic bootstrapping as well as a novel per-quantile error estimation of the empirical distribution. Two example applications are provided, using the test to boost the sensitivity in generic "bump hunting", and employing the test to detect supernovae. The article is rounded off with an extended performance comparison to other, established goodness-of-fit tests.


ODSL
RU-B
(1372)A flexible event reconstruction based on machine learning and likelihood principles
  • Philipp Eller,
  • Aaron Fienberg,
  • Jan Weldert,
  • Garrett Wendel,
  • Sebastian Böser
  • +1
Nuclear Instruments and Methods in Physics Research - section A (March/2023) e-Print:2208.10166 doi:10.1016/j.nima.2023.168011
abstract + abstract -

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


ODSL
RU-B
(1371)Public Kaggle Competition "IceCube -- Neutrinos in Deep Ice"
  • Philipp Eller (for the IceCube Collaboration)
Proceedings of Science (July/2023) e-Print:2307.15289 doi:10.5445/IR/1000163437
abstract + abstract -

The reconstruction of neutrino events in the IceCube experiment is crucial for many scientific analyses, including searches for cosmic neutrino sources. The Kaggle competition "IceCube -- Neutrinos in Deep ice" was a public machine learning challenge designed to encourage the development of innovative solutions to improve the accuracy and efficiency of neutrino event reconstruction. Participants worked with a dataset of simulated neutrino events and were tasked with creating a suitable model to predict the direction vector of incoming neutrinos. From January to April 2023, hundreds of teams competed for a total of $50k prize money, which was awarded to the best performing few out of the many thousand submissions. In this contribution I will present some insights into the organization of this large outreach project, and summarize some of the main findings, results and takeaways.


PhD Thesis
RU-A
(1370)Precision Measurement of the Chiral Anomaly and Improvements of the Data Acquisition System at the COMPASS experiment at CERN
  • Dominik Ecker - Advisor: Stephan Paul
Thesis (9/2023) link
abstract + abstract -

The chiral anomaly, a fundamental property of QCD, relates the coupling of an odd number of Goldstone bosons to vector bosons, e.g. of the coupling of three pions to one photon. This coupling can experimentally be measured in pion-photon scattering. We report on a precision experiment using the COMPASS experiment at CERN where pion-photon scattering is mediated via the Primakoff effect. We present also improvements of monitoring beam stability and of controlling the DAQ of COMPASS.


PhD Thesis
RU-D
(1369)Tracing the evolution of super-massive black holes through cosmic time with luminous active galactic nuclei
  • Julien Wolf - Advisor: Kirpal Nandra
Thesis (6/2023) doi:10.5282/edoc.31872
abstract + abstract -

Black holes are an essential building block of the baryonic structure in the Universe. Their masses range from a few times to a few billion times the mass of our Sun. Super-massive black holes (SMBHs), the largest form of compact objects, are believed to reside at the centre of all galaxies. Scaling relations between host properties and SMBH masses hint at a tight co-evolution between galaxies and their central black holes. In the deep nuclear gravitational potential, matter is accreted onto the SMBH. Under certain conditions, the viscous flow in the accretion disk releases extreme amounts of energy in the form of radiation. The galactic cores irradiating their environment under the effect of accretion are called active galactic nuclei (AGN). Over the last 20 years, quasars, the most luminous sub-species of AGN, have been discovered at ever-increasing distances. [...]


CN-7
PhD Thesis
RU-A
(1368)First measurement of the absorption of anti-3He and anti-3H in matter and its impact on anti-3He propagation in the galaxy
  • Stephan Königstorfer - Advisor: Laura Fabbietti
Thesis (4/2023) link
abstract + abstract -

This work contains the first measurement of the anti-3He and anti-3H inelastic cross sections on matter, measured with the ALICE experiment at the LHC. It also evaluates the effect of the measurements of inelastic cross sections on matter on the propagation of antinuclei through the galaxy, and thus determines the transparency of the galaxy to antinuclei from different sources.


CN-3
CN-4
RU-C
RU-D
(1367)Time Delay Cosmography: Analysis of Quadruply Lensed QSO SDSSJ1433 from Wendelstein Observatory
  • G. Queirolo,
  • S. Seitz,
  • A. Riffeser,
  • M. Kluge,
  • R. Bender
  • +5
  • C. Gössl,
  • U. Hopp,
  • C. Ries,
  • M. Schmidt,
  • R. Zöller
  • (less)
abstract + abstract -

The goal of this work is to obtain a Hubble constant estimate through the study of the quadruply lensed, variable QSO SDSSJ1433+6007. To achieve this we combine multi-filter, archival $\textit{HST}$ data for lens modelling and a dedicated time delay monitoring campaign with the 2.1m Fraunhofer telescope at the $\textit{Wendelstein Observatory}$. The lens modelling is carried out with the public $\texttt{lenstronomy}$ Python package for each of the filters individually. Through this approach, we find that the data in one of the $\textit{HST}$ filters (F160W) contain a light contaminant, that would, if remained undetected, have severely biased the lensing potentials and thus our cosmological inference. After rejecting these data we obtain a combined posterior for the Fermat potential differences from the lens modelling in the remaining filters (F475X, F814W, F105W and F140W) with a precision of $\sim6\%$. The analysis of the $\textit{g'}$-band Wendelstein light curve data is carried out with a free-knot spline fitting method implemented in the public Python $\texttt{PyCS3}$ tools. The precision of the time delays between the QSO images has a range between 7.5 and 9.8$\%$ depending on the brightness of the images and their time delay. We then combine the posteriors for the Fermat potential differences and time delays. Assuming a flat $\Lambda$CDM cosmology, we infer a Hubble parameter of $H_0=76.6^{+7.7}_{-7.0}\frac{\mathrm{km}}{\mathrm{Mpc\;s}}$, reaching $9.6\%$ uncertainty for a single system.


RU-B
(1366)The static force from generalized Wilson loops on the lattice using gradient flow
  • Nora Brambilla,
  • Viljami Leino,
  • Julian Mayer-Steudte,
  • Antonio Vairo
abstract + abstract -

The static QCD force from the lattice can be used to extract $\Lambda_{\overline{\textrm{MS}}}$, which determines the running of the strong coupling. Usually, this is done with a numerical derivative of the static potential. However, this introduces additional systematic uncertainties; thus, we use another observable to measure the static force directly. This observable consists of a Wilson loop with a chromoelectric field insertion. We work in the pure SU(3) gauge theory. We use gradient flow to improve the signal-to-noise ratio and to address the field insertion. We extract $\Lambda_{\overline{\textrm{MS}}}^{n_f=0}$ from the data by exploring different methods to perform the zero flow time limit. We obtain the value $\sqrt{8t_0} \Lambda_{\overline{\textrm{MS}}}^{n_f=0} =0.629^{+22}_{-26}$, where $t_0$ is a flow time reference scale. We also obtain precise determinations of several scales: $r_0/r_1$, $\sqrt{8 t_0}/r_0$, $\sqrt{8 t_0}/r_1$ and we compare to the literature. The gradient flow appears to be a promising method for calculations of Wilson loops with chromolectric and chromomagnetic insertions in quenched and unquenched configurations.


CN-6
(1365)Filamentation of a Relativistic Proton Bunch in Plasma
  • L. Verra,
  • C. Amoedo,
  • N. Torrado,
  • A. Clairembaud,
  • J. Mezger
  • +10
  • F. Pannell,
  • J. Pucek,
  • N. van Gils,
  • M. Bergamaschi,
  • G. Zevi Della Porta,
  • N. Lopes,
  • A. Sublet,
  • M. Turner,
  • E. Gschwendtner,
  • P. Muggli (AWAKE Collaboration)
  • (less)
arXiv e-prints (12/2023) e-Print:2312.13883
abstract + abstract -

We show in experiments that a long, underdense, relativistic proton bunch propagating in plasma undergoes the oblique instability, that we observe as filamentation. We determine a threshold value for the ratio between the bunch transverse size and plasma skin depth for the instability to occur. At the threshold, the outcome of the experiment alternates between filamentation and self-modulation instability (evidenced by longitudinal modulation into microbunches). Time-resolved images of the bunch density distribution reveal that filamentation grows to an observable level late along the bunch, confirming the spatio-temporal nature of the instability. We calculate the amplitude of the magnetic field generated in the plasma by the instability and show that the associated magnetic energy increases with plasma density.


RU-A
(1364)Soft-photon spectra and the LBK theorem
  • Roger Balsach,
  • Domenico Bonocore,
  • Anna Kulesza
abstract + abstract -

The study of next-to-leading-power (NLP) corrections in soft emissions continues to attract interest both in QCD and in QED. Soft-photon spectra in particular provide a clean case-study for the experimental verification of the Low-Burnett-Kroll (LBK) theorem. In this paper we study the consistency of the LBK theorem in the context of an ambiguity arising from momentum-conservation constraints in the computation of non-radiative amplitudes. We clarify that this ambiguity leads to various possible formulations of the LBK theorem, which are all equivalent up to power-suppressed effects (i.e. beyond the formal accuracy of the LBK theorem). We also propose a new formulation of the LBK theorem with a modified shifted kinematics which facilitates the numerical computation of non-radiative amplitudes with publicly available tools. Furthermore, we present numerical results for soft-photon spectra in the associated production of a muon pair with a photon, both in $e^+e^-$ annihilation and proton-proton collisions.


CN-2
RU-D
(1363)Linking Circumstellar Disk Lifetimes to the Rotational Evolution of Low-mass Stars
  • K. Monsch,
  • J. J. Drake,
  • C. Garraffo,
  • G. Picogna,
  • B. Ercolano
The Astrophysical Journal (12/2023) doi:10.3847/1538-4357/ad0a60
abstract + abstract -

The high-energy radiation emitted by young stars can have a strong influence on their rotational evolution at later stages. This is because internal photoevaporation is one of the major drivers of the dispersal of circumstellar disks, which surround all newly born low-mass stars during the first few million years of their evolution. Employing an internal EUV/X-ray photoevaporation model, we have derived a simple recipe for calculating realistic inner disk lifetimes of protoplanetary disks. This prescription was implemented into a magnetic-morphology-driven rotational evolution model and is used to investigate the impact of disk locking on the spin evolution of low-mass stars. We find that the length of the disk locking phase has a profound impact on the subsequent rotational evolution of a young star, and the implementation of realistic disk lifetimes leads to an improved agreement of model outcomes with observed rotation period distributions for open clusters of various ages. However, for both young star-forming regions tested in our model, the strong bimodality in rotation periods that is observed in h Per could not be recovered. h Per is only successfully recovered if the model is started from a double-peaked distribution with an initial disk fraction of 65%. However, at an age of only ~1 Myr, such a low disk fraction can only be achieved if an additional disk dispersal process, such as external photoevaporation, is invoked. These results therefore highlight the importance of including realistic disk dispersal mechanisms in rotational evolution models of young stars.


(1362)SUNRISE: The rich molecular inventory of high-redshift dusty galaxies revealed by broadband spectral line surveys
  • Chentao Yang,
  • Alain Omont,
  • Sergio Martín,
  • Thomas G. Bisbas,
  • Pierre Cox
  • +19
  • Alexandre Beelen,
  • Eduardo González-Alfonso,
  • Raphaël Gavazzi,
  • Susanne Aalto,
  • Paola Andreani,
  • Cecilia Ceccarelli,
  • Yu Gao,
  • Mark Gorski,
  • Michel Guélin,
  • Hai Fu,
  • R. J. Ivison,
  • Kirsten K. Knudsen,
  • Matthew Lehnert,
  • Hugo Messias,
  • Sebastien Muller,
  • Roberto Neri,
  • Dominik Riechers,
  • Paul van der Werf,
  • Zhi-Yu Zhang
  • (less)
Astronomy and Astrophysics (12/2023) doi:10.1051/0004-6361/202347610
abstract + abstract -

Understanding the nature of high-redshift dusty galaxies requires a comprehensive view of their interstellar medium (ISM) and molecular complexity. However, the molecular ISM at high redshifts is commonly studied using only a few species beyond 12C16O, limiting our understanding. In this paper, we present the results of deep 3 mm spectral line surveys using the NOrthern Extended Millimeter Array (NOEMA) targeting two strongly lensed dusty galaxies observed when the Universe was less than 1.8 Gyr old: APM 08279+5255, a quasar at redshift z = 3.911, and NCv1.143 (H-ATLAS J125632.7+233625), a z = 3.565 starburst galaxy. The spectral line surveys cover rest-frame frequencies from about 330 to 550 GHz for both galaxies. We report the detection of 38 and 25 emission lines in APM 08279+5255 and NCv1.143, respectively. These lines originate from 17 species, namely CO, 13CO, C18O, CN, CCH, HCN, HCO+, HNC, CS, C34S, H2O, H3O+, NO, N2H+, CH, c-C3H2, and the vibrationally excited HCN and neutral carbon. The spectra reveal the chemical richness and the complexity of the physical properties of the ISM. By comparing the spectra of the two sources and combining the analysis of the molecular gas excitation, we find that the physical properties and the chemical imprints of the ISM are different: the molecular gas is more excited in APM 08279+5255, which exhibits higher molecular gas temperatures and densities compared to NCv1.143; the molecular abundances in APM 08279+5255 are akin to the values of local active galactic nuclei (AGN), showing boosted relative abundances of the dense gas tracers that might be related to high-temperature chemistry and/or the X-ray-dominated regions, while NCv1.143 more closely resembles local starburst galaxies. The most significant differences between the two sources are found in H2O: the 448 GHz ortho-H2O(423 − 330) line is significantly brighter in APM 08279+5255, which is likely linked to the intense far-infrared radiation from the dust powered by AGN. Our astrochemical model suggests that, at such high column densities, far-ultraviolet radiation is less important in regulating the ISM, while cosmic rays (and/or X-rays and shocks) are the key players in shaping the molecular abundances and the initial conditions of star formation. Both our observed CO isotopologs line ratios and the derived extreme ISM conditions (high gas temperatures, densities, and cosmic-ray ionization rates) suggest the presence of a top-heavy stellar initial mass function. From the ∼330-550 GHz continuum, we also find evidence of nonthermal millimeter flux excess in APM 08279+5255 that might be related to the central supermassive black hole. Such deep spectral line surveys open a new window into the physics and chemistry of the ISM and the radiation field of galaxies in the early Universe.

The final data products of the tables derived from UVFIT are available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (ftp://130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/680/A95

We dedicate this paper to the memory of our coauthor and friend, Yu Gao, who passed away in May 2022.


RU-D
(1361)Dust Coagulation Reconciles Protoplanetary Disk Observations with the Vertical Shear Instability. I. Dust Coagulation and the VSI Dead Zone
  • Thomas Pfeil,
  • Tilman Birnstiel,
  • Hubert Klahr
The Astrophysical Journal (12/2023) doi:10.3847/1538-4357/ad00af
abstract + abstract -

Protoplanetary disks exhibit a vertical gradient in angular momentum, rendering them susceptible to the vertical shear instability (VSI). The most important condition for the onset of this mechanism is a short timescale of thermal relaxation (≲0.1 orbital timescales). Simulations of fully VSI active disks are characterized by turbulent, vertically extended dust layers. This is in contradiction with recent observations of the outer regions of some protoplanetary disks, which appear highly settled. In this work, we demonstrate that the process of dust coagulation can diminish the cooling rate of the gas in the outer disk and extinct the VSI activity. Our findings indicate that the turbulence strength is especially susceptible to variations in the fragmentation velocity of the grains. A small fragmentation velocity of ≈100 cm s-1 results in a fully turbulent simulation, whereas a value of ≈400 cm s-1 results in a laminar outer disk, being consistent with observations. We show that VSI turbulence remains relatively unaffected by variations in the maximum particle size in the inner disk regions. However, we find that dust coagulation can significantly suppress the occurrence of VSI turbulence at larger distances from the central star.


CN-2
RU-D
RU-E
(1360)Revised gas-phase formation network of methyl cyanide: the origin of methyl cyanide and methanol abundance correlation in hot corinos
  • Lisa Giani,
  • Cecilia Ceccarelli,
  • Luca Mancini,
  • Eleonora Bianchi,
  • Fernando Pirani
  • +2
Monthly Notices of the Royal Astronomical Society (12/2023) doi:10.1093/mnras/stad2892
abstract + abstract -

Methyl cyanide (CH3CN) is one of the most abundant and widely spread interstellar complex organic molecules (iCOMs). Several studies found that, in hot corinos, methyl cyanide and methanol abundances are correlated suggesting a chemical link, often interpreted as a synthesis of them on the interstellar grain surfaces. In this article, we present a revised network of the reactions forming methyl cyanide in the gas phase. We carried out an exhaustive review of the gas-phase CH3CN formation routes, propose two new reactions, and performed new quantum mechanics calculations of several reactions. We found that 13 of the 15 reactions reported in the databases KIDA and UDfA have incorrect products and/or rate constants. The new corrected reaction network contains 10 reactions leading to methyl cyanide. We tested the relative importance of those reactions in forming CH3CN using our astrochemical model. We confirm that the radiative association of CH3+ and HCN, forming CH3CNH+, followed by the electron recombination of CH3CNH+, is the most important CH3CN formation route in both cold and warm environments, notwithstanding that we significantly corrected the rate constants and products of both reactions. The two newly proposed reactions play an important role in warm environments. Finally, we found a very good agreement between the CH3CN predicted abundances with those measured in cold (~10 K) and warm (~90 K) objects. Unexpectedly, we also found a chemical link between methanol and methyl cyanide via the CH$_{3}^{+}$ ion, which can explain the observed correlation between the CH3OH and CH3CN abundances measured in hot corinos.


(1359)Coarsening and wavelength selection far from equilibrium: A unifying framework based on singular perturbation theory
  • Henrik Weyer,
  • Fridtjof Brauns,
  • Erwin Frey
Physical Review E (12/2023) doi:10.1103/PhysRevE.108.064202
abstract + abstract -

Intracellular protein patterns are described by (nearly) mass-conserving reaction-diffusion systems. While these patterns initially form out of a homogeneous steady state due to the well-understood Turing instability, no general theory exists for the dynamics of fully nonlinear patterns. We develop a unifying theory for nonlinear wavelength-selection dynamics in (nearly) mass-conserving two-component reaction-diffusion systems independent of the specific mathematical model chosen. Previous work has shown that these systems support an extremely broad band of stable wavelengths, but the mechanism by which a specific wavelength is selected has remained unclear. We show that an interrupted coarsening process selects the wavelength at the threshold to stability. Based on the physical intuition that coarsening is driven by competition for mass and interrupted by weak source terms that break strict mass conservation, we develop a singular perturbation theory for the stability of stationary patterns. The resulting closed-form analytical expressions enable us to quantitatively predict the coarsening dynamics and the final pattern wavelength. We find excellent agreement with numerical results throughout the diffusion- and reaction-limited regimes of the dynamics, including the crossover region. Further, we show how, in these limits, the two-component reaction-diffusion systems map to generalized Cahn-Hilliard and conserved Allen-Cahn dynamics, therefore providing a link to these two fundamental scalar field theories. The systematic understanding of the length-scale dynamics of fully nonlinear patterns in two-component systems provided here builds the basis to reveal the mechanisms underlying wavelength selection in multicomponent systems with potentially several conservation laws.


(1358)The BarYon Cycle project (ByCycle): identifying and localizing Mg II metal absorbers with machine learning
  • Roland Szakacs,
  • Céline Péroux,
  • Dylan Nelson,
  • Martin A. Zwaan,
  • Daniel Grün
  • +4
  • Simon Weng,
  • Alejandra Y. Fresco,
  • Victoria Bollo,
  • Benedetta Casavecchia
  • (less)
Monthly Notices of the Royal Astronomical Society (12/2023) doi:10.1093/mnras/stad2431
abstract + abstract -

The upcoming ByCycle project on the VISTA/4MOST multi-object spectrograph will offer new prospects of using a massive sample of ~1 million high spectral resolution (R = 20 000) background quasars to map the circumgalactic metal content of foreground galaxies (observed at R = 4000-7000), as traced by metal absorption. Such large surveys require specialized analysis methodologies. In the absence of early data, we instead produce synthetic 4MOST high-resolution fibre quasar spectra. To do so, we use the TNG50 cosmological magnetohydrodynamical simulation, combining photo-ionization post-processing and ray tracing, to capture Mg II (λ2796, λ2803) absorbers. We then use this sample to train a convolutional neural network (CNN) which searches for, and estimates the redshift of, Mg II absorbers within these spectra. For a test sample of quasar spectra with uniformly distributed properties ($\lambda _{\rm {Mg\, {\small II},2796}}$, $\rm {EW}_{\rm {Mg\, {\small II},2796}}^{\rm {rest}} = 0.05\!-\!5.15$ Å, $\rm {SNR} = 3\!-\!50$), the algorithm has a robust classification accuracy of 98.6 per cent and a mean wavelength accuracy of 6.9 Å. For high signal-to-noise (SNR) spectra ($\rm {SNR \gt 20}$), the algorithm robustly detects and localizes Mg II absorbers down to equivalent widths of $\rm {EW}_{\rm {Mg\, {\small II},2796}}^{\rm {rest}} = 0.05$ Å. For the lowest SNR spectra ($\rm {SNR=3}$), the CNN reliably recovers and localizes EW$_{\rm {Mg\, {\small II},2796}}^{\rm {rest}}$ ≥0.75 Å absorbers. This is more than sufficient for subsequent Voigt profile fitting to characterize the detected Mg II absorbers. We make the code publicly available through GitHub. Our work provides a proof-of-concept for future analyses of quasar spectra data sets numbering in the millions, soon to be delivered by the next generation of surveys.


(1357)Reviving stochasticity: uncertainty in SMBH binary eccentricity is unavoidable
  • Alexander Rawlings,
  • Matias Mannerkoski,
  • Peter H. Johansson,
  • Thorsten Naab
Monthly Notices of the Royal Astronomical Society (12/2023) doi:10.1093/mnras/stad2891
abstract + abstract -

We study supermassive black hole (SMBH) binary eccentricity of equal-mass galaxy mergers in N-body simulations with the KETJU code, which combines the GADGET-4 fast multipole gravity solver with accurate regularized integration and post-Newtonian corrections around SMBHs. In simulations with realistic, high-eccentricity galactic merger orbits, the hard binary eccentricity is found to be a non-linear function of the deflection angle in the SMBH orbit during the final, nearly radial close encounter between the SMBHs before they form a bound binary. This mapping between the deflection angle and the binary eccentricity has no apparent resolution dependence in our simulations spanning the resolution range of 1 × 105 to 8 × 106 particles per galaxy. The mapping is also captured using a simple model with an analytical potential, indicating that it is driven by the interplay between a smooth asymmetric stellar background potential and dynamical friction acting on the SMBHs. Due to the non-linearity of this mapping, in eccentric major merger configurations, small, parsec-scale variations in the merger orbit can result in binary eccentricities varying in nearly the full possible range between e = 0 and e = 1. In idealized simulations, such variations are caused by finite resolution effects, and convergence of the binary eccentricity can be achieved with increasing resolution. However, in real galaxies, other mechanisms such as nuclear gas and substructure that perturb the merger orbit are likely to be significant enough for the binary eccentricity to be effectively random. Our results indicate that the distribution of these effectively random eccentricities can be studied using even moderate resolution simulations.


(1356)RASS-MCMF: a full-sky X-ray selected galaxy cluster catalogue
  • Matthias Klein,
  • Daniel Hernández-Lang,
  • Joseph J. Mohr,
  • Sebastian Bocquet,
  • Aditya Singh
Monthly Notices of the Royal Astronomical Society (12/2023) doi:10.1093/mnras/stad2729
abstract + abstract -

We present the RASS-MCMF catalogue of 8449 X-ray selected galaxy clusters over 25 000 deg2 of extragalactic sky. The accumulation of deep multiband optical imaging data, the development of the Multi-Component Matched Filter (MCMF) cluster confirmation algorithm, and the release of the DESI Legacy Survey DR10 catalogue makes it possible - for the first time, more than 30 yr after the launch of the ROSAT X-ray satellite - to identify the majority of the galaxy clusters detected in the second ROSAT All-Sky-Survey (RASS) source catalogue (2RXS). The resulting 90 per cent pure RASS-MCMF catalogue is the largest intracluster medium (ICM)-selected cluster sample to date. RASS-MCMF probes a large dynamic range in cluster mass spanning from galaxy groups to the most massive clusters. The cluster redshift distribution peaks at $z$ ~ 0.1 and extends to redshifts $z$ ~ 1. Out to $z$ ~ 0.4, the RASS-MCMF sample contains more clusters per redshift interval (dN/dz) than any other ICM-selected sample. In addition to the main sample, we present two subsamples with 6912 and 5506 clusters, exhibiting 95 per cent and 99 per cent purity, respectively. We forecast the utility of the sample for a cluster cosmological study, using realistic mock catalogues that incorporate most observational effects, including the X-ray exposure time and background variations, the existence likelihood selection and the impact of the optical cleaning with the algorithm MCMF. Using realistic priors on the observable-mass relation parameters from a DES-based weak lensing analysis, we estimate the constraining power of the RASS-MCMF×DES sample to be of 0.026, 0.033, and 0.15 (1σ) on the parameters Ωm, σ8, and $w$, respectively.


CN-4
RU-D
(1355)The Metallicity and Distance of Leo A from Blue Supergiants
  • Miguel A. Urbaneja,
  • Fabio Bresolin,
  • Rolf-Peter Kudritzki
The Astrophysical Journal (12/2023) doi:10.3847/1538-4357/acfc3d
abstract + abstract -

We have obtained high-quality spectra of blue supergiant candidates in the dwarf irregular galaxy Leo A with the Low Resolution Imaging Spectrometer at the Keck I telescope. From the quantitative analysis of seven B8-A0 stars, we derive a mean metallicity [Z] = -1.35 ± 0.08, in excellent agreement with the gas-phase chemical abundance. From the stellar parameters and the flux-weighted gravity-luminosity relation (FGLR), we derive a spectroscopic distance modulus m - M = 24.77 ± 0.11 mag, significantly larger (~0.4 mag) than the value indicated by RR Lyrae and other stellar indicators. We explain the bulk of this discrepancy with blue loop stellar evolution at very low metallicity and show that the combination of metallicity effects and blue loop evolution amounts, in the case of Leo A, to an ~0.35 mag offset of the FGLR to fainter bolometric luminosities. We identify one outlier of low bolometric magnitude as a post-AGB star. Its metallicity is consistent with that of the young population, confirming the slow chemical enrichment of Leo A.


(1354)Set-conditional set generation for particle physics
  • Nathalie Soybelman,
  • Nilotpal Kakati,
  • Lukas Heinrich,
  • Francesco Armando Di Bello,
  • Etienne Dreyer
  • +4
  • Sanmay Ganguly,
  • Eilam Gross,
  • Marumi Kado,
  • Jonathan Shlomi
  • (less)
Machine Learning: Science and Technology (12/2023) doi:10.1088/2632-2153/ad035b
abstract + abstract -

The simulation of particle physics data is a fundamental but computationally intensive ingredient for physics analysis at the large Hadron collider, where observational set-valued data is generated conditional on a set of incoming particles. To accelerate this task, we present a novel generative model based on a graph neural network and slot-attention components, which exceeds the performance of pre-existing baselines.


(1353)Factorization of non-global LHC observables and resummation of super-leading logarithms
  • Thomas Becher,
  • Matthias Neubert,
  • Ding Yu Shao,
  • Michel Stillger
Journal of High Energy Physics (12/2023) doi:10.1007/JHEP12(2023)116
abstract + abstract -

We present a systematic formalism based on a factorization theorem in soft-collinear effective theory to describe non-global observables at hadron colliders, such as gap-between-jets cross sections. The cross sections are factorized into convolutions of hard functions, capturing the dependence on the partonic center-of-mass energy √{s ̂}, and low-energy matrix elements, which are sensitive to the low scale Q0 ≪ √{s ̂} characteristic of the veto imposed on energetic emissions into the gap between the jets. The scale evolution of both objects is governed by a renormalization-group equation, which we derive at one-loop order. By solving the evolution equation for the hard functions for arbitrary 2 → M jet processes in the leading logarithmic approximation, we accomplish for the first time the all-order resummation of the so-called "super-leading logarithms" discovered in 2006, thereby solving an old problem of quantum field theory. We study the numerical size of the corresponding effects for different partonic scattering processes and explain why they are sizable for pp → 2 jets processes, but suppressed in H/Z and H/Z + jet production. The super-leading logarithms are given by an alternating series, whose individual terms can be much larger than the resummed result, even in very high orders of the loop expansion. Resummation is therefore essential to control these effects. We find that the asymptotic fall-off of the resummed series is much weaker than for standard Sudakov form factors.


(1352)Multicomponent imaging of the Fermi gamma-ray sky in the spatio-spectral domain
  • L. I. Scheel-Platz,
  • J. Knollmüller,
  • P. Arras,
  • P. Frank,
  • M. Reinecke
  • +2
Astronomy and Astrophysics (12/2023) doi:10.1051/0004-6361/202243819
abstract + abstract -

The gamma-ray sky as seen by the Large Area Telescope (LAT) on board the Fermi satellite is a superposition of emissions from many processes. To study them, a rich toolkit of analysis methods for gamma-ray observations has been developed, most of which rely on emission templates to model foreground emissions. Here, we aim to complement these methods by presenting a template-free spatio-spectral imaging approach for the gamma-ray sky, based on a phenomenological modeling of its emission components. It is formulated in a Bayesian variational inference framework and allows a simultaneous reconstruction and decomposition of the sky into multiple emission components, enabled by a self-consistent inference of their spatial and spectral correlation structures. Additionally, we formulated the extension of our imaging approach to template-informed imaging, which includes adding emission templates to our component models while retaining the "data-drivenness" of the reconstruction. We demonstrate the performance of the presented approach on the ten-year Fermi LAT data set. With both template-free and template-informed imaging, we achieve a high quality of fit and show a good agreement of our diffuse emission reconstructions with the current diffuse emission model published by the Fermi Collaboration. We quantitatively analyze the obtained data-driven reconstructions and critically evaluate the performance of our models, highlighting strengths, weaknesses, and potential improvements. All reconstructions have been released as data products.


(1351)Inferring Evidence from Nested Sampling Data via Information Field Theory
  • Margret Westerkamp,
  • Jakob Roth,
  • Philipp Frank,
  • Will Handley,
  • Torsten Enßlin
abstract + abstract -

Nested sampling provides an estimate of the evidence of a Bayesian inference problem via probing the likelihood as a function of the enclosed prior volume. However, the lack of precise values of the enclosed prior mass of the samples introduces probing noise, which can hamper high-accuracy determinations of the evidence values as estimated from the likelihood-prior-volume function. We introduce an approach based on information field theory, a framework for non-parametric function reconstruction from data, that infers the likelihood-prior-volume function by exploiting its smoothness and thereby aims to improve the evidence calculation. Our method provides posterior samples of the likelihood-prior-volume function that translate into a quantification of the remaining sampling noise for the evidence estimate, or for any other quantity derived from the likelihood-prior-volume function.


(1350)XUE: Molecular Inventory in the Inner Region of an Extremely Irradiated Protoplanetary Disk
  • María Claudia Ramírez-Tannus,
  • Arjan Bik,
  • Lars Cuijpers,
  • Rens Waters,
  • Christiane Göppl
  • +22
  • Thomas Henning,
  • Inga Kamp,
  • Thomas Preibisch,
  • Konstantin V. Getman,
  • Germán Chaparro,
  • Pablo Cuartas-Restrepo,
  • Alex de Koter,
  • Eric D. Feigelson,
  • Sierra L. Grant,
  • Thomas J. Haworth,
  • Sebastián Hernández,
  • Michael A. Kuhn,
  • Giulia Perotti,
  • Matthew S. Povich,
  • Megan Reiter,
  • Veronica Roccatagliata,
  • Elena Sabbi,
  • Benoît Tabone,
  • Andrew J. Winter,
  • Anna F. McLeod,
  • Roy van Boekel,
  • Sierk E. van Terwisga
  • (less)
The Astrophysical Journal (12/2023) doi:10.3847/2041-8213/ad03f8
abstract + abstract -

We present the first results of the eXtreme UV Environments (XUE) James Webb Space Telescope (JWST) program, which focuses on the characterization of planet-forming disks in massive star-forming regions. These regions are likely representative of the environment in which most planetary systems formed. Understanding the impact of environment on planet formation is critical in order to gain insights into the diversity of the observed exoplanet populations. XUE targets 15 disks in three areas of NGC 6357, which hosts numerous massive OB stars, including some of the most massive stars in our Galaxy. Thanks to JWST, we can, for the first time, study the effect of external irradiation on the inner (<10 au), terrestrial-planet-forming regions of protoplanetary disks. In this study, we report on the detection of abundant water, CO, 12CO2, HCN, and C2H2 in the inner few au of XUE 1, a highly irradiated disk in NGC 6357. In addition, small, partially crystalline silicate dust is present at the disk surface. The derived column densities, the oxygen-dominated gas-phase chemistry, and the presence of silicate dust are surprisingly similar to those found in inner disks located in nearby, relatively isolated low-mass star-forming regions. Our findings imply that the inner regions of highly irradiated disks can retain similar physical and chemical conditions to disks in low-mass star-forming regions, thus broadening the range of environments with similar conditions for inner disk rocky planet formation to the most extreme star-forming regions in our Galaxy.


(1349)Evolution of compact states to molecular ones with coupled channels: The case of the X (3872 )
  • Jing Song,
  • L. R. Dai,
  • E. Oset
Physical Review D (12/2023) doi:10.1103/PhysRevD.108.114017
abstract + abstract -

We study the molecular probability of the X (3872 ) in the D0D¯*0 and D+D*- channels in several scenarios. One of them assumes that the state is purely due to a genuine nonmolecular component. However, it gets unavoidably dressed by the meson components to the point that in the limit of zero binding of the D0D¯*0 component becomes purely molecular. Yet, the small but finite binding allows for a nonmolecular state when the bare mass of the genuine state approaches the D0D¯*0 threshold, but, in this case the system develops a small scattering length and a huge effective range for this channel in flagrant disagreement with present values of these magnitudes. Next we discuss the possibility to have hybrid states stemming from the combined effect of a genuine state and a reasonable direct interaction between the meson components, where we find cases in which the scattering length and effective range are still compatible with data, but even then the molecular probability is as big as 95%. Finally, we perform the calculations when the binding stems purely from the direct interaction between the meson-meson components. In summary we conclude, that while present data definitely rule out the possibility of a dominant nonmolecular component, the precise value of the molecular probability requires a more precise determination of the scattering length and effective range of the D0D¯*0 channel, as well as the measurement of these magnitudes for the D+D*- channel which have not been determined experimentally so far.


(1348)A self-synthesized origin for heavy metals in hot subdwarf stars
  • T. Battich,
  • M. M. Miller Bertolami,
  • A. M. Serenelli,
  • S. Justham,
  • A. Weiss
Astronomy and Astrophysics (12/2023) doi:10.1051/0004-6361/202348157
abstract + abstract -

Context. A number of He-rich hot subdwarf stars present high abundances for trans-iron elements, such as Sr, Y, Zr, and Pb. Diffusion processes are important in hot subdwarf stars and it is generally believed that the high abundances of heavy elements in these peculiar stars are due to the action of radiative levitation. However, during the formation of He-rich hot subdwarf stars, hydrogen can be ingested into the convective zone driven by the He-core flash. It is known that episodes of protons being ingested into He-burning convective zones can lead to neutron-capture processes and the formation of heavy elements.
Aims: In this work, we aim to explore, for the first time, whether neutron-capture processes can occur in late He-core flashes taking place in the cores of the progenitors of He-rich hot subdwarfs. We aim to explore the possibility of a self-synthesized origin for the heavy elements observed in some He-rich hot subdwarf stars.
Methods: We computed a detailed evolutionary model for a stripped red-giant star using a stellar evolution code with a nuclear network comprising 32 isotopes. Then we post-processed the stellar models in the phase of helium and hydrogen burning using a post-processing nucleosynthesis code with a nuclear network of 1190 species, which allowed us to follow the neutron-capture processes in detail.
Results: We find the occurrence of neutron-capture processes in our model, with neutron densities reaching a value of ∼5 × 1012 cm−3. We determined that the trans-iron elements are enhanced in the surface by 1 to 2 dex, as compared to initial compositions. Moreover, the relative abundance pattern [Xi/Fe] produced by neutron-capture processes closely resembles those observed in some He-rich hot subdwarf stars, hinting at a possible self-synthesized origin for the heavy elements in these stars.
Conclusions: We conclude that intermediate neutron-capture processes can occur during a proton ingestion event in the He-core flash of stripped red-giant stars. This mechanism offers a natural channel for the production of the heavy elements observed in certain He-rich hot subdwarf stars.


CN-4
RU-C
(1347)Early-time Ultraviolet and Optical Hubble Space Telescope Spectroscopy of the Type II Supernova 2022wsp
  • Sergiy S. Vasylyev,
  • Christian Vogl,
  • Yi Yang,
  • Alexei V. Filippenko,
  • Thomas G. Brink
  • +8
  • Peter J. Brown,
  • Thomas Matheson,
  • Maryam Modjaz,
  • Avishay Gal-Yam,
  • Paolo A. Mazzali,
  • Thomas de Jaeger,
  • Kishore C. Patra,
  • Gabrielle E. Stewart
  • (less)
The Astrophysical Journal (12/2023) doi:10.3847/2041-8213/ad0e6b
abstract + abstract -

We report early-time ultraviolet (UV) and optical spectroscopy of the young, nearby Type II supernova (SN) 2022wsp obtained by the Hubble Space Telescope (HST)/STIS at about 10 and 20 days after the explosion. The SN 2022wsp UV spectra are compared to those of other well-observed Type II/IIP SNe, including the recently studied Type IIP SN 2021yja. Both SNe exhibit rapid cooling and similar evolution during early phases, indicating a common behavior among SNe II. Radiative-transfer modeling of the spectra of SN 2022wsp with the TARDIS code indicates a steep radial density profile in the outer layer of the ejecta, a solar metallicity, and a relatively high total extinction of E(B - V) = 0.35 mag. The early-time evolution of the photospheric velocity and temperature derived from the modeling agree with the behavior observed from other previously studied cases. The strong suppression of hydrogen Balmer lines in the spectra suggests interaction with a preexisting circumstellar environment could be occurring at early times. In the SN 2022wsp spectra, the absorption component of the Mg II P Cygni profile displays a double-trough feature on day +10 that disappears by day +20. The shape is well reproduced by the model without fine-tuning the parameters, suggesting that the secondary blueward dip is a metal transition that originates in the SN ejecta.


RU-A
(1346)50 Years of quantum chromodynamics
  • Franz Gross,
  • Eberhard Klempt,
  • Stanley J. Brodsky,
  • Andrzej J. Buras,
  • Volker D. Burkert
  • +90
  • Gudrun Heinrich,
  • Karl Jakobs,
  • Curtis A. Meyer,
  • Kostas Orginos,
  • Michael Strickland,
  • Johanna Stachel,
  • Giulia Zanderighi,
  • Nora Brambilla,
  • Peter Braun-Munzinger,
  • Daniel Britzger,
  • Simon Capstick,
  • Tom Cohen,
  • Volker Crede,
  • Martha Constantinou,
  • Christine Davies,
  • Luigi Del Debbio,
  • Achim Denig,
  • Carleton DeTar,
  • Alexandre Deur,
  • Yuri Dokshitzer,
  • Hans Günter Dosch,
  • Jozef Dudek,
  • Monica Dunford,
  • Evgeny Epelbaum,
  • Miguel A. Escobedo,
  • Harald Fritzsch,
  • Kenji Fukushima,
  • Paolo Gambino,
  • Dag Gillberg,
  • Steven Gottlieb,
  • Per Grafstrom,
  • Massimiliano Grazzini,
  • Boris Grube,
  • Alexey Guskov,
  • Toru Iijima,
  • Xiangdong Ji,
  • Frithjof Karsch,
  • Stefan Kluth,
  • John B. Kogut,
  • Frank Krauss,
  • Shunzo Kumano,
  • Derek Leinweber,
  • Heinrich Leutwyler,
  • Hai-Bo Li,
  • Yang Li,
  • Bogdan Malaescu,
  • Chiara Mariotti,
  • Pieter Maris,
  • Simone Marzani,
  • Wally Melnitchouk,
  • Johan Messchendorp,
  • Harvey Meyer,
  • Ryan Edward Mitchell,
  • Chandan Mondal,
  • Frank Nerling,
  • Sebastian Neubert,
  • Marco Pappagallo,
  • Saori Pastore,
  • José R. Peláez,
  • Andrew Puckett,
  • Jianwei Qiu,
  • Klaus Rabbertz,
  • Alberto Ramos,
  • Patrizia Rossi,
  • Anar Rustamov,
  • Andreas Schäfer,
  • Stefan Scherer,
  • Matthias Schindler,
  • Steven Schramm,
  • Mikhail Shifman,
  • Edward Shuryak,
  • Torbjörn Sjöstrand,
  • George Sterman,
  • Iain W. Stewart,
  • Joachim Stroth,
  • Eric Swanson,
  • Guy F. de Téramond,
  • Ulrike Thoma,
  • Antonio Vairo,
  • Danny van Dyk,
  • James Vary,
  • Javier Virto,
  • Marcel Vos,
  • Christian Weiss,
  • Markus Wobisch,
  • Sau Lan Wu,
  • Christopher Young,
  • Feng Yuan,
  • Xingbo Zhao,
  • Xiaorong Zhou
  • (less)
European Physical Journal C (12/2023) doi:10.1140/epjc/s10052-023-11949-2
abstract + abstract -

Quantum Chromodynamics, the theory of quarks and gluons, whose interactions can be described by a local SU(3) gauge symmetry with charges called "color quantum numbers", is reviewed; the goal of this review is to provide advanced Ph.D. students a comprehensive handbook, helpful for their research. When QCD was "discovered" 50 years ago, the idea that quarks could exist, but not be observed, left most physicists unconvinced. Then, with the discovery of charmonium in 1974 and the explanation of its excited states using the Cornell potential, consisting of the sum of a Coulomb-like attraction and a long range linear confining potential, the theory was suddenly widely accepted. This paradigm shift is now referred to as the November revolution. It had been anticipated by the observation of scaling in deep inelastic scattering, and was followed by the discovery of gluons in three-jet events. The parameters of QCD include the running coupling constant, αs(Q2) , that varies with the energy scale Q2 characterising the interaction, and six quark masses. QCD cannot be solved analytically, at least not yet, and the large value of αs at low momentum transfers limits perturbative calculations to the high-energy region where Q2≫ΛQCD2≃ (250 MeV)2. Lattice QCD (LQCD), numerical calculations on a discretized space-time lattice, is discussed in detail, the dynamics of the QCD vacuum is visualized, and the expected spectra of mesons and baryons are displayed. Progress in lattice calculations of the structure of nucleons and of quantities related to the phase diagram of dense and hot (or cold) hadronic matter are reviewed. Methods and examples of how to calculate hadronic corrections to weak matrix elements on a lattice are outlined. The wide variety of analytical approximations currently in use, and the accuracy of these approximations, are reviewed. These methods range from the Bethe-Salpeter, Dyson-Schwinger coupled relativistic equations, which are formulated in both Minkowski or Euclidean spaces, to expansions of multi-quark states in a set of basis functions using light-front coordinates, to the AdS/QCD method that imbeds 4-dimensional QCD in a 5-dimensional deSitter space, allowing confinement and spontaneous chiral symmetry breaking to be described in a novel way. Models that assume the number of colors is very large, i.e. make use of the large Nc-limit, give unique insights. Many other techniques that are tailored to specific problems, such as perturbative expansions for high energy scattering or approximate calculations using the operator product expansion are discussed. The very powerful effective field theory techniques that are successful for low energy nuclear systems (chiral effective theory), or for non-relativistic systems involving heavy quarks, or the treatment of gluon exchanges between energetic, collinear partons encountered in jets, are discussed. The spectroscopy of mesons and baryons has played an important historical role in the development of QCD. The famous X,Y,Z states - and the discovery of pentaquarks - have revolutionized hadron spectroscopy; their status and interpretation are reviewed as well as recent progress in the identification of glueballs and hybrids in light-meson spectroscopy. These exotic states add to the spectrum of expected q q ¯ mesons and qqq baryons. The progress in understanding excitations of light and heavy baryons is discussed. The nucleon as the lightest baryon is discussed extensively, its form factors, its partonic structure and the status of the attempt to determine a three-dimensional picture of the parton distribution. An experimental program to study the phase diagram of QCD at high temperature and density started with fixed target experiments in various laboratories in the second half of the 1980s, and then, in this century, with colliders. QCD thermodynamics at high temperature became accessible to LQCD, and numerical results on chiral and deconfinement transitions and properties of the deconfined and chirally restored form of strongly interacting matter, called the Quark-Gluon Plasma (QGP), have become very precise by now. These results can now be confronted with experimental data that are sensitive to the nature of the phase transition. There is clear evidence that the QGP phase is created. This phase of QCD matter can already be characterized by some properties that indicate, within a temperature range of a few times the pseudocritical temperature, the medium behaves like a near ideal liquid. Experimental observables are presented that demonstrate deconfinement. High and ultrahigh density QCD matter at moderate and low temperatures shows interesting features and new phases that are of astrophysical relevance. They are reviewed here and some of the astrophysical implications are discussed. Perturbative QCD and methods to describe the different aspects of scattering processes are discussed. The primary parton-parton scattering in a collision is calculated in perturbative QCD with increasing complexity. The radiation of soft gluons can spoil the perturbative convergence, this can be cured by resummation techniques, which are also described here. Realistic descriptions of QCD scattering events need to model the cascade of quark and gluon splittings until hadron formation sets in, which is done by parton showers. The full event simulation can be performed with Monte Carlo event generators, which simulate the full chain from the hard interaction to the hadronic final states, including the modelling of non-perturbative components. The contribution of the LEP experiments (and of earlier collider experiments) to the study of jets is reviewed. Correlations between jets and the shape of jets had allowed the collaborations to determine the "color factors" - invariants of the SU(3) color group governing the strength of quark-gluon and gluon-gluon interactions. The calculated jet production rates (using perturbative QCD) are shown to agree precisely with data, for jet energies spanning more than five orders of magnitude. The production of jets recoiling against a vector boson, W± or Z, is shown to be well understood. The discovery of the Higgs boson was certainly an important milestone in the development of high-energy physics. The couplings of the Higgs boson to massive vector bosons and fermions that have been measured so far support its interpretation as mass-generating boson as predicted by the Standard Model. The study of the Higgs boson recoiling against hadronic jets (without or with heavy flavors) or against vector bosons is also highlighted. Apart from the description of hard interactions taking place at high energies, the understanding of "soft QCD" is also very important. In this respect, Pomeron - and Odderon - exchange, soft and hard diffraction are discussed. Weak decays of quarks and leptons, the quark mixing matrix and the anomalous magnetic moment of the muon are processes which are governed by weak interactions. However, corrections by strong interactions are important, and these are reviewed. As the measured values are incompatible with (most of) the predictions, the question arises: are these discrepancies first hints for New Physics beyond the Standard Model? This volume concludes with a description of future facilities or important upgrades of existing facilities which improve their luminosity by orders of magnitude. The best is yet to come!


CN-7
RU-A
(1345)Conservation and breaking of pseudospin symmetry
  • Ting-Ting Sun,
  • Zhi Pan Li,
  • Peter Ring
Physics Letter B (12/2023) doi:10.1016/j.physletb.2023.138320
abstract + abstract -

Pseudospin symmetry (PSS) is a relativistic dynamical symmetry connected with the lower component of the Dirac spinor. Here, we investigate the conservation and breaking of PSS in the single-nucleon resonant states, as an example, using Green's function method that provides a novel way to precisely describe not only the resonant energies and widths but also the spacial density distributions for both narrow and wide resonances. The PSS conservation and breaking are perfectly displayed in the evolution of resonant parameters and density distributions with the potential depth: In the PSS limit, i.e., when the attractive scalar and repulsive vector potentials have the same magnitude but opposite sign, PSS is exactly conserved with strictly the same energy and width between the PS partners as well as identical density distributions of the lower components. As the potential depth increases, the PSS is broken gradually with energy and width splittings and a phase shift in the density distributions.


CN-6
(1344)Kinetic Simulations of Nonrelativistic High-mach-number Perpendicular Shocks Propagating in a Turbulent Medium
  • Karol Fulat,
  • Artem Bohdan,
  • Gabriel Torralba Paz,
  • Martin Pohl
The Astrophysical Journal (12/2023) doi:10.3847/1538-4357/ad04dc
abstract + abstract -

Strong nonrelativistic shocks are known to accelerate particles up to relativistic energies. However, for diffusive shock acceleration, electrons must have a highly suprathermal energy, implying the need for very efficient preacceleration. Most published studies consider shocks propagating through homogeneous plasma, which is an unrealistic assumption for astrophysical environments. Using 2D3V particle-in-cell simulations, we investigate electron acceleration and heating processes at nonrelativistic high-Mach-number shocks in electron-ion plasma with a turbulent upstream medium. For this purpose, slabs of plasma with compressive turbulence are simulated separately and then inserted into shock simulations, which require matching of the plasma slabs at the interface. Using a novel procedure of matching electromagnetic fields and currents, we perform simulations of perpendicular shocks setting different intensities of density fluctuations (≲10%) in the upstream region. The new simulation technique provides a framework for studying shocks propagating in turbulent media. We explore the impact of the fluctuations on electron heating, the dynamics of upstream electrons, and the driving of plasma instabilities. Our results indicate that while the presence of turbulence enhances variations in the upstream magnetic field, their levels remain too low to significantly influence the behavior of electrons at perpendicular shocks.


IDSL
RU-E
(1343)Replication elongates short DNA, reduces sequence bias and develops trimer structure
  • Adriana Calaça Serrão,
  • Felix T. Dänekamp,
  • Zsófia Meggyesi,
  • Dieter Braun
Nucleic Acids Research (12/2023) doi:https://doi.org/10.1093/nar/gkad1190
abstract + abstract -

The origin of molecular evolution required the replication of short oligonucleotides to form longer polymers. Prebiotically plausible oligonucleotide pools tend to contain more of some nucleobases than others. It has been unclear whether this initial bias persists and how it affects replication. To investigate this, we examined the evolution of 12-mer biased short DNA pools using an enzymatic model system. This allowed us to study the long timescales involved in evolution, since it is not yet possible with currently investigated prebiotic replication chemistries. Our analysis using next-generation sequencing from different time points revealed that the initial nucleotide bias of the pool disappeared in the elongated pool after isothermal replication. In contrast, the nucleotide composition at each position in the elongated sequences remained biased and varied with both position and initial bias. Furthermore, we observed the emergence of highly periodic dimer and trimer motifs in the rapidly elongated sequences. This shift in nucleotide composition and the emergence of structure through templated replication could help explain how biased prebiotic pools could undergo molecular evolution and lead to complex functional nucleic acids.


(1342)The Subtle Simplicity of Cosmological Correlators
  • Chandramouli Chowdhury,
  • Arthur Lipstein,
  • Jiajie Mei,
  • Ivo Sachs,
  • Pierre Vanhove
abstract + abstract -

We investigate cosmological correlators for conformally coupled $\phi^4$ theory in four-dimensional de Sitter space. These \textit{in-in} correlators differ from scattering amplitudes for massless particles in flat space due to the spacelike structure of future infinity in de Sitter. They also require a regularization which preserves de Sitter-invariance, which makes the flat space limit subtle to define at loop-level. Nevertheless we find that up to two loops, the \textit{in-in} correlators are structurally simpler than the wave function and have the same transcendentality as flat space amplitudes. Moreover, we show that their loop integrands can be recast in terms of flat space integrands and can be derived from a novel recursion relation.


CN-3
CN-4
RU-C
(1341)The Dark Energy Spectroscopic Instrument: one-dimensional power spectrum from first
  • Corentin Ravoux,
  • Marie Lynn Abdul Karim,
  • Eric Armengaud,
  • Michael Walther,
  • Naim Göksel Karaçaylı
  • +61
  • Paul Martini,
  • Julien Guy,
  • Jessica Nicole Aguilar,
  • Steven Ahlen,
  • Stephen Bailey,
  • Julian Bautista,
  • Sergio Felipe Beltran,
  • David Brooks,
  • Laura Cabayol-Garcia,
  • Solène Chabanier,
  • Edmond Chaussidon,
  • Jonás Chaves-Montero,
  • Kyle Dawson,
  • Rodrigo de la Cruz,
  • Axel de la Macorra,
  • Peter Doel,
  • Kevin Fanning,
  • Andreu Font-Ribera,
  • Jaime Forero-Romero,
  • Satya Gontcho A Gontcho,
  • Alma Gonzalez-Morales,
  • Calum Gordon,
  • Hiram Herrera-Alcantar,
  • Klaus Honscheid,
  • Vid Iršič,
  • Mustapha Ishak,
  • Robert Kehoe,
  • Theodore Kisner,
  • Anthony Kremin,
  • Martin Landriau,
  • Laurent Le Guillou,
  • Michael Levi,
  • Zarija Lukić,
  • Christophe Magneville,
  • Aaron Meisner,
  • Ramon Miquel,
  • John Moustakas,
  • Eva-Maria Mueller,
  • Andrea Muñoz-Gutiérrez,
  • Lucas Napolitano,
  • Jundan Nie,
  • Gustavo Niz,
  • Nathalie Palanque-Delabrouille,
  • Will Percival,
  • Ignasi Pérez-Ràfols,
  • Matthew Pieri,
  • Claire Poppett,
  • Francisco Prada,
  • César Ramírez Pérez,
  • Graziano Rossi,
  • Eusebio Sanchez,
  • David Schlegel,
  • Michael Schubnell,
  • Hee-Jong Seo,
  • Francesco Sinigaglia,
  • Ting Tan,
  • Gregory Tarlé,
  • Ben Wang,
  • Benjamin Weaver,
  • Christophe Yèche,
  • Zhimin Zhou
  • (less)
abstract + abstract -

We present the one-dimensional Ly α forest power spectrum measurement using the first data provided by the Dark Energy Spectroscopic Instrument (DESI). The data sample comprises 26 330 quasar spectra, at redshift z > 2.1, contained in the DESI Early Data Release and the first 2 months of the main survey. We employ a Fast Fourier Transform (FFT) estimator and compare the resulting power spectrum to an alternative likelihood-based method in a companion paper. We investigate methodological and instrumental contaminants associated with the new DESI instrument, applying techniques similar to previous Sloan Digital Sky Survey (SDSS) measurements. We use synthetic data based on lognormal approximation to validate and correct our measurement. We compare our resulting power spectrum with previous SDSS and high-resolution measurements. With relatively small number statistics, we successfully perform the FFT measurement, which is already competitive in terms of the scale range. At the end of the DESI survey, we expect a five times larger Ly α forest sample than SDSS, providing an unprecedented precise one-dimensional power spectrum measurement.


CN-2
RU-E
(1340)Formation mechanism of thermally controlled pH gradients
  • Thomas Matreux,
  • Bernhard Altaner,
  • Johannes Raith,
  • Dieter Braun,
  • Christof B. Mast
  • +1
Communications Physics (12/2023) doi:10.1038/s42005-023-01126-y
abstract + abstract -

Spatial proton gradients create energy in biological systems and are likely a driving force for prebiotic systems. Due to the fast diffusion of protons, they are however difficult to create as steady state, unless driven by other non-equilibria such as thermal gradients. Here, we quantitatively predict the heat-flux driven formation of pH gradients for the case of a simple acid-base reaction system. To this end, we (i) establish a theoretical framework that describes the spatial interplay of chemical reactions with thermal convection, thermophoresis, and electrostatic forces by a separation of timescales, and (ii) report quantitative measurements in a purpose-built microfluidic device. We show experimentally that the slope of such pH gradients undergoes pronounced amplitude changes in a concentration-dependent manner and can even be inverted. The predictions of the theoretical framework fully reflect these features and establish an understanding of how naturally occurring non-equilibrium environmental conditions can drive pH gradients.


(1339)Augmenting the power of time-delay cosmography in lens galaxy clusters by probing their member galaxies. I. Type Ia supernovae
  • A. Acebron,
  • S. Schuldt,
  • C. Grillo,
  • P. Bergamini,
  • G. Granata
  • +7
  • U. Meštrić,
  • G. B. Caminha,
  • M. Meneghetti,
  • A. Mercurio,
  • P. Rosati,
  • S. H. Suyu,
  • E. Vanzella
  • (less)
Astronomy and Astrophysics (12/2023) doi:10.1051/0004-6361/202348090
abstract + abstract -

We present a simple and promising new method to measure the expansion rate and the geometry of the universe that combines observations related to the time delays between the multiple images of time-varying sources, strongly lensed by galaxy clusters, and Type Ia supernovae, exploding in galaxies belonging to the same lens clusters. By means of two different statistical techniques that adopt realistic errors on the relevant quantities, we quantify the accuracy of the inferred cosmological parameter values. We show that the estimate of the Hubble constant is robust and competitive, and depends only mildly on the chosen cosmological model. Remarkably, the two probes separately produce confidence regions on the cosmological parameter planes that are oriented in complementary ways, thus providing in combination valuable information on the values of the other cosmological parameters. We conclude by illustrating the immediate observational feasibility of the proposed joint method in a well-studied lens galaxy cluster, with a relatively small investment of telescope time for monitoring from a 2 to 3 m class ground-based telescope.


(1338)Stability of coorbital planets around binaries
  • Stefan Adelbert,
  • Anna B. T. Penzlin,
  • Christoph M. Schäfer,
  • Wilhelm Kley,
  • Billy Quarles
  • +1
Astronomy and Astrophysics (12/2023) doi:10.1051/0004-6361/202244329
abstract + abstract -

In previous hydrodynamical simulations, we found a mechanism for nearly circular binary stars, such as Kepler-413, to trap two planets in a stable 1:1 resonance. Therefore, the stability of coorbital configurations becomes a relevant question for planet formation around binary stars. For this work, we investigated the coorbital planet stability using a Kepler-413 analogue as an example and then expanded the parameters to study a general n-body stability of planet pairs in eccentric horseshoe orbits around binaries. The stability was tested by evolving the planet orbits for 105 binary periods with varying initial semi-major axes and planet eccentricities. The unstable region of a single circumbinary planet is used as a comparison to the investigated coorbital configurations in this work. We confirm previous findings on the stability of single planets and find a first order linear relation between the orbit eccentricity ep and pericentre to identify stable orbits for various binary configurations. Such a linear relation is also found for the stability of 1:1 resonant planets around binaries. Stable orbits for eccentric horseshoe configurations exist with a pericentre closer than seven binary separations and, in the case of Kepler-413, the pericentre of the first stable orbit can be approximated by rc,peri = (2.90 ep + 2.46) abin.


(1337)Ultralight Dark Matter Search with Space-Time Separated Atomic Clocks and Cavities
  • Melina Filzinger,
  • Ashlee R. Caddell,
  • Dhruv Jani,
  • Martin Steinel,
  • Leonardo Giani
  • +2
  • Nils Huntemann,
  • Benjamin M. Roberts
  • (less)
abstract + abstract -

We devise and demonstrate a method to search for non-gravitational couplings of ultralight dark matter to standard model particles using space-time separated atomic clocks and cavity-stabilized lasers. By making use of space-time separated sensors, which probe different values of an oscillating dark matter field, we can search for couplings that cancel in typical local experiments. We demonstrate this method using existing data from a frequency comparison of lasers stabilized to two optical cavities connected via a 2220 km fiber link [Nat. Commun. 13, 212 (2022)]. The absence of significant oscillations in the data results in constraints on the coupling of scalar dark matter to electrons, d_me, for masses between 1e-19 eV and 2e-15 eV. These are the first constraints on d_me alone in this mass range, and improve the dark matter constraints on any scalar-Fermion coupling by up to two orders of magnitude.


CN-4
RU-C
RU-D
(1336)Exploring the low-mass regime of galaxy-scale strong lensing: Insights into the mass structure of cluster galaxies
  • Giovanni Granata,
  • Pietro Bergamini,
  • Claudio Grillo,
  • Massimo Meneghetti,
  • Amata Mercurio
  • +6
  • Uros Meštrić,
  • Antonio Ragagnin,
  • Piero Rosati,
  • Gabriel Bartosch Caminha,
  • Luca Tortorelli,
  • Eros Vanzella
  • (less)
Astronomy & Astrophysics (11/2023) e-Print:2310.02310 doi:10.1051/0004-6361/202347521
abstract + abstract -

We aim at a direct measurement of the compactness of three galaxy-scale lenses in massive clusters, testing the accuracy of the scaling laws that describe the members in strong lensing (SL) models of galaxy clusters. We selected the multiply imaged sources MACS J0416.1−2403 ID14 (z=3.221), MACS J0416.1−2403 ID16 (z=2.095), and MACS J1206.2−0847 ID14 (z=3.753). Eight images were observed for the first SL system, and six for the latter two. We focused on the main deflector of each galaxy-scale SL system (identified as members 8971, 8785, and 3910, respectively), and modelled its total mass distribution with a truncated isothermal sphere. We accounted for the lensing effects of the remaining cluster components, and included the uncertainty on the cluster-scale mass distribution through a bootstrapping procedure. We measured a truncation radius value of 6.1+2.3−1.1kpc, 4.0+0.6−0.4kpc, and 5.2+1.3−1.1kpc for members 8971, 8785, and 3910, respectively. Alternative non-truncated models with a higher number of free parameters do not lead to an improved description of the SL system. We measured the stellar-to-total mass fraction within the effective radius Re for the three members, finding 0.51±0.21, 1.0±0.4, and 0.39±0.16, respectively. We find that a parameterisation of the properties of cluster galaxies in SL models based on power-law scaling relations with respect to the total luminosity cannot accurately describe their compactness over their full total mass range. Our results agree with modelling of the cluster members based on the Fundamental Plane relation. Finally, we report good agreement between our values of the stellar-to-total mass fraction within Re and those of early-type galaxies from the SLACS Survey. Our work significantly extends the regime of the current samples of lens galaxies.


(1335)Progress in the partial-wave analysis methods at COMPASS
  • Julien Beckers,
  • Florian Kaspar,
  • Jakob Knollmüller
abstract + abstract -

We study the excitation spectrum of light and strange mesons in diffractive scattering. We identify different hadron resonances through partial wave analysis, which inherently relies on analysis models. Besides statistical uncertainties, the model dependence of the analysis introduces dominant systematic uncertainties. We discuss several of their sources for the $\pi^-\pi^-\pi^+$ and $K^0_S K^-$ final states and present methods to reduce them. We have developed a new approach exploiting a-priori knowledge of signal continuity over adjacent final-state-mass bins to stably fit a large pool of partial-waves to our data, allowing a clean identification of very small signals in our large data sets. For two-body final states of scalar particles, such as $K^0_S K^-$, mathematical ambiguities in the partial-wave decomposition lead to the same intensity distribution for different combinations of amplitude values. We will discuss these ambiguities and present solutions to resolve or at least reduce the number of possible solutions. Resolving these issues will allow for a complementary analysis of the $a_J$-like resonance sector in these two final states.


(1334)Flavored jets with exact anti-k<SUB>t</SUB> kinematics and tests of infrared and collinear safety
  • Fabrizio Caola,
  • Radosław Grabarczyk,
  • Maxwell L. Hutt,
  • Gavin P. Salam,
  • Ludovic Scyboz
  • +1
Physical Review D (11/2023) doi:10.1103/PhysRevD.108.094010
abstract + abstract -

We propose extensions of the anti-kt and Cambridge/Aachen hierarchical jet clustering algorithms that are designed to retain the exact jet kinematics of these algorithms, while providing an infrared-and-collinear-safe definition of jet flavor at any fixed order in perturbation theory. Central to our approach is a new technique called interleaved flavor neutralization (IFN), whereby the treatment of flavor is integrated with, but distinct from, the kinematic clustering. IFN allows flavor information to be meaningfully accessed at each stage of the clustering sequence, which enables a consistent assignment of flavor both to individual jets and to their substructure. We validate the IFN approach using a dedicated framework for fixed-order tests of infrared and collinear safety, which also reveals unanticipated issues in earlier approaches to flavored jet clustering. We briefly explore the phenomenological impact of IFN with anti-kt jets for benchmark tasks at the Large Hadron Collider.


CN-8
(1333)Emergence of homochirality via template-directed ligation in an RNA reactor
  • Gabin Laurent,
  • Tobias Göppel,
  • David Lacoste,
  • Ulrich Gerland
arXiv preprints (11/2023) e-Print:2311.04677
abstract + abstract -

RNA in extant biological systems is homochiral -- it consists exclusively of D-ribonucleotides rather than L-ribonucleotides. How the homochirality of RNA emerged is not known. Here, we use stochastic simulations to quantitatively explore the conditions for RNA homochirality to emerge in the prebiotic scenario of an `RNA reactor', in which RNA strands react in a non-equilibrium environment. These reactions include the hybridization, dehybridization, template-directed ligation, and cleavage of RNA strands. The RNA reactor is either closed, with a finite pool of ribonucleotide monomers of both chiralities (D and L), or the reactor is open, with a constant inflow of a racemic mixture of monomers. For the closed reactor, we also consider the interconversion between D- and L-monomers via a racemization reaction. We first show that template-free polymerization is unable to reach a high degree of homochirality, due to the lack of autocatalytic amplification. In contrast, in the presence of template-directed ligation, with base pairing and stacking between bases of the same chirality thermodynamically favored, a high degree of homochirality can arise and be maintained, provided that the non-equilibrium environment overcomes product inhibition, for instance via temperature cycling. Furthermore, if the experimentally observed kinetic stalling of ligation after chiral mismatches is also incorporated, the RNA reactor can evolve towards a fully homochiral state, in which one chirality is entirely lost. This is possible, because the kinetic stalling after chiral mismatches effectively implements a chiral cross-inhibition process. Taken together, our model supports a scenario, where the emergence of homochirality is assisted by template-directed ligation and polymerization in a non-equilibrium RNA reactor.


RU-D
(1332)The cosmic build-up of dust and metals. Accurate abundances from GRB-selected star-forming galaxies at 1.7<z<6.3
  • K. E. Heintz,
  • A. De Cia,
  • C. C. Thöne,
  • J.-K. Krogager,
  • R. M. Yates
  • +36
  • S. Vejlgaard,
  • C. Konstantopoulou,
  • J. P. U. Fynbo,
  • D. Watson,
  • D. Narayanan,
  • S. N. Wilson,
  • M. Arabsalmani,
  • S. Campana,
  • V. D'Elia,
  • M. De Pasquale,
  • D. H. Hartmann,
  • L. Izzo,
  • P. Jakobsson,
  • C. Kouveliotou,
  • A. Levan,
  • Q. Li,
  • D. B. Malesani,
  • A. Melandri,
  • B. Milvang-Jensen,
  • P. Møller,
  • E. Palazzi,
  • J. Palmerio,
  • P. Petitjean,
  • G. Pugliese,
  • A. Rossi,
  • A. Saccardi,
  • R. Salvaterra,
  • S. Savaglio,
  • P. Schady,
  • G. Stratta,
  • N. R. Tanvir,
  • A. de Ugarte Postigo,
  • S. D. Vergani,
  • K. Wiersema,
  • R. A. M. J. Wijers,
  • T. Zafar
  • (less)
abstract + abstract -

The chemical enrichment of dust and metals in the interstellar medium (ISM) of galaxies throughout cosmic time is one of the key driving processes of galaxy evolution. Here we study the evolution of the gas-phase metallicities, dust-to-gas (DTG), and dust-to-metal (DTM) ratios of 36 star-forming galaxies at 1.7<z<6.3 probed by gamma-ray bursts (GRBs). We compile all GRB-selected galaxies with intermediate (R=7000) to high (R>40,000) resolution spectroscopic data for which at least one refractory (e.g. Fe) and one volatile (e.g. S or Zn) element have been detected at S/N>3. This is to ensure that accurate abundances and dust depletion patterns can be obtained. We first derive the redshift evolution of the dust-corrected, absorption-line based gas-phase metallicity [M/H]tot in these galaxies, for which we determine a linear relation with redshift [M/H]tot(z)=(−0.21±0.04)z−(0.47±0.14). We then examine the DTG and DTM ratios as a function of redshift and through three orders of magnitude in metallicity, quantifying the relative dust abundance both through the direct line-of-sight visual extinction AV and the derived depletion level. We use a novel method to derive the DTG and DTM mass ratios for each GRB sightline, summing up the mass of all the depleted elements in the dust-phase. We find that the DTG and DTM mass ratios are both strongly correlated with the gas-phase metallicity and show a mild evolution with redshift as well. While these results are subject to a variety of caveats related to the physical environments and the narrow pencil-beam sightlines through the ISM probed by the GRBs, they provide strong implications for studies of dust masses to infer the gas and metal content of high-redshift galaxies, and particularly demonstrate the large offset from the average Galactic value in the low-metallicity, high-redshift regime.


CN-5
RU-D
(1331)Filament fragmentation: density gradients suppress end-dominated collapse
  • Elena Hoemann,
  • Stefan Heigl,
  • Andreas Burkert
Monthly Notices of the Royal Astronomical Society (11/2023) doi:10.1093/mnras/stad2517
abstract + abstract -

The onset of star formation is set by the collapse of filaments in the interstellar medium. From a theoretical point of view, an isolated cylindrical filament forms cores via the edge effect. Due to the self-gravity of a filament, the strong increase in acceleration at both ends leads to a pile-up of matter which collapses into cores. However, this effect is rarely observed. Most theoretical models consider a sharp density cut-off at the edge of the filament, whereas a smoother transition is more realistic and would also decrease the acceleration at the ends of the filament. We show that the edge effect can be significantly slowed down by a density gradient, although not completely avoided. However, this allows perturbations inside the filament to grow faster than the edge. We determine the critical density gradient for which the time-scales are equal and find it to be of the order of several times the filament radius. Hence, the density gradient at the ends of a filament is an essential parameter for fragmentation and the low rate of observed cases of the edge effect could be naturally explained by shallow gradients.


CN-2
RU-D
(1330)Beyond diffusion: a generalized mean-field theory of turbulent dust transport in protoplanetary discs
  • Fabian Binkert
Monthly Notices of the Royal Astronomical Society (11/2023) doi:10.1093/mnras/stad2471
abstract + abstract -

Turbulence in protoplanetary discs, when present, plays a critical role in transporting dust particles embedded in the gaseous disc component. When using a field description of dust dynamics, a diffusion approach is traditionally used to model this turbulent dust transport. However, it has been shown that classical turbulent diffusion models are not fully self-consistent. Several shortcomings exist, including the ambiguous nature of the diffused quantity and the non-conservation of angular momentum. Orbital effects are also neglected without an explicit prescription. In response to these inconsistencies, we present a novel Eulerian turbulent dust transport model for isotropic and homogeneous turbulence on the basis of a mean-field theory. Our model is based on density-weighted averaging applied to the pressureless fluid equations and uses appropriate turbulence closures. Our model yields novel dynamic equations for the turbulent dust mass flux and recovers existing turbulent transport models in special limiting cases, thus providing a more general and self-consistent description of turbulent particle transport. Importantly, our model ensures the conservation of global angular and linear momentum unconditionally and implicitly accounts for the effects of orbital dynamics in protoplanetary discs. Furthermore, our model correctly describes the vertical settling-diffusion equilibrium solutions for both small and large particles. Hence, this work presents a generalized Eulerian turbulent dust transport model, establishing a comprehensive framework for more detailed studies of turbulent dust transport in protoplanetary discs.