page 3 of 20
(1732)The LiteBIRD mission to explore cosmic inflation
  • T. Ghigna,
  • A. Adler,
  • K. Aizawa,
  • H. Akamatsu,
  • R. Akizawa
  • +153
  • E. Allys,
  • A. Anand,
  • J. Aumont,
  • J. Austermann,
  • S. Azzoni,
  • C. Baccigalupi,
  • M. Ballardini,
  • A. Banday,
  • R. Barreiro,
  • N. Bartolo,
  • S. Basak,
  • A. Basyrov,
  • S. Beckman,
  • M. Bersanelli,
  • M. Bortolami,
  • F. Bouchet,
  • T. Brinckmann,
  • P. Campeti,
  • E. Carinos,
  • A. Carones,
  • F. J. Casas,
  • K. Cheung,
  • Y. Chinone,
  • L. Clermont,
  • F. Columbro,
  • A. Coppolecchia,
  • D. Curtis,
  • P. de Bernardis,
  • T. de Haan,
  • E. de la Hoz,
  • M. De Petris,
  • S. Della Torre,
  • G. Delle Monache,
  • E. Di Giorgi,
  • C. Dickinson,
  • P. Diego-Palazuelos,
  • J. J. Díaz García,
  • M. Dobbs,
  • T. Dotani,
  • H. K. Eriksen,
  • J. Errard,
  • T. Essinger-Hileman,
  • N. Farias,
  • E. Ferreira,
  • C. Franceschet,
  • U. Fuskeland,
  • G. Galloni,
  • M. Galloway,
  • K. Ganga,
  • M. Gerbino,
  • M. Gervasi,
  • R. T. Génova-Santos,
  • S. Giardiello,
  • C. Gimeno-Amo,
  • E. Gjerløw,
  • R. González González,
  • L. Grandsire,
  • A. Gruppuso,
  • N. Halverson,
  • P. Hargrave,
  • S. E. Harper,
  • M. Hazumi,
  • S. Henrot-Versillé,
  • L. T. Hergt,
  • D. Herranz,
  • E. Hivon,
  • R. Hlozek,
  • T. D. Hoang,
  • J. Hubmayr,
  • K. Ichiki,
  • K. Ikuma,
  • H. Ishino,
  • G. Jaehnig,
  • B. Jost,
  • K. Kohri,
  • K. Konishi,
  • L. Lamagna,
  • M. Lattanzi,
  • C. Leloup,
  • F. Levrier,
  • A. Lanoppan,
  • G. Luzzi,
  • J. Macias-Perez,
  • B. Maffei,
  • E. Marchitelli,
  • E. Martínez-González,
  • S. Masi,
  • S. Matarrese,
  • T. Matsumura,
  • S. Micheli,
  • M. Migliaccio,
  • M. Monelli,
  • L. Montier,
  • G. Morgante,
  • L. Mousset,
  • Y. Nagano,
  • R. Nagata,
  • P. Natoli,
  • A. Novelli,
  • F. Noviello,
  • I. Obata,
  • A. Occhiuzzi,
  • K. Odagiri,
  • R. Omae,
  • L. Pagano,
  • A. Paiella,
  • D. Paoletti,
  • G. Pascual-Cisneros,
  • G. Patanchon,
  • V. Pavlidou,
  • F. Piacentini,
  • M. Piat,
  • G. Piccirilli,
  • M. Pinchera,
  • G. Pisano,
  • L. Porcelli,
  • N. Raffuzzi,
  • C. Raum,
  • M. Remazeilles,
  • A. Ritacco,
  • J. Rubino-Martin,
  • M. Ruiz-Granda,
  • Y. Sakurai,
  • G. Savini,
  • D. Scott,
  • Y. Sekimoto,
  • M. Shiraishi,
  • G. Signorelli,
  • S. L. Stever,
  • R. Sullivan,
  • A. Suzuki,
  • R. Takaku,
  • H. Takakura,
  • S. Takakura,
  • Y. Takase,
  • A. Tartari,
  • K. Tassis,
  • K. L. Thompson,
  • M. Tomasi,
  • M. Tristram,
  • C. Tucker,
  • L. Vacher,
  • B. van Tent,
  • P. Vielva,
  • K. Watanuki,
  • I. K. Wehus,
  • B. Westbrook,
  • G. Weymann-Despres,
  • B. Winter,
  • E. J. Wollack,
  • A. Zacchei,
  • M. Zannoni,
  • Y. Zhou
  • (less)
Space Telescopes and Instrumentation 2024: Optical, Infrared, and Millimeter Wave (08/2024) doi:10.1117/12.3021377
abstract + abstract -

LiteBIRD, the next-generation cosmic microwave background (CMB) experiment, aims for a launch in Japan's fiscal year 2032, marking a major advancement in the exploration of primordial cosmology and fundamental physics. Orbiting the Sun-Earth Lagrangian point L2, this JAXA-led strategic L-class mission will conduct a comprehensive mapping of the CMB polarization across the entire sky. During its 3-year mission, LiteBIRD will employ three telescopes within 15 unique frequency bands (ranging from 34 through 448 GHz), targeting a sensitivity of 2.2 μK-arcmin and a resolution of 0.5° at 100 GHz. Its primary goal is to measure the tensor-toscalar ratio r with an uncertainty δr = 0.001, including systematic errors and margin. If r ≥ 0.01, LiteBIRD expects to achieve a > 5σ detection in the l = 2-10 and l = 11-200 ranges separately, providing crucial insight into the early Universe. We describe LiteBIRD's scientific objectives, the application of systems engineering to mission requirements, the anticipated scientific impact, and the operations and scanning strategies vital to minimizing systematic effects. We will also highlight LiteBIRD's synergies with concurrent CMB projects.


(1731)Why cosmic voids matter: mitigation of baryonic physics
  • Nico Schuster,
  • Nico Hamaus,
  • Klaus Dolag,
  • Jochen Weller
Journal of Cosmology and Astroparticle Physics (08/2024) doi:10.1088/1475-7516/2024/08/065
abstract + abstract -

We utilize the Magneticum suite of state-of-the-art hydrodynamical, as well as dark-matter-only simulations to investigate the effects of baryonic physics on cosmic voids in the highest-resolution study of its kind. This includes the size, shape and inner density distributions of voids, as well as their radial density and velocity profiles traced by (sub-) halos, baryonic and cold dark matter particles. Our results reveal observationally insignificant effects that slightly increase with the inner densities of voids and are exclusively relevant on scales of only a few Mpc. Most notably, we identify deviations in the distributions of baryons and cold dark matter around halo-defined voids, relevant for weak lensing studies. In contrast, we find that voids identified in cold dark matter, as well as in halos of fixed tracer density exhibit nearly indistinguishable distributions and profiles between hydrodynamical and dark-matter-only simulations, consolidating the universality and robustness of the latter for comparisons of void statistics with observations in upcoming surveys. This corroborates that voids are the components of the cosmic web that are least affected by baryonic physics, further enhancing their use as cosmological probes.


(1730)Axially deformed relativistic quasiparticle random-phase approximation based on point-coupling interactions
  • A. Ravlić,
  • T. Nikšić,
  • Y. F. Niu,
  • P. Ring,
  • N. Paar
Physical Review C (08/2024) doi:10.1103/PhysRevC.110.024323
abstract + abstract -

Collective nuclear excitations, like giant resonances, are sensitive to nuclear deformation, as evidenced by alterations in their excitation energies and transition strength distributions. A common theoretical framework to study these collective modes, the random-phase approximation (RPA), has to deal with large dimensions spanned by all possible particle-hole configurations satisfying certain symmetries. It is the aim of this work to establish a new theoretical framework to study the impact of deformation on spin-isospin excitations, that is able to provide fast and reliable solutions of the RPA equations. The nuclear ground state is determined with the axially deformed relativistic Hartree-Bogoliubov (RHB) model based on relativistic point-coupling energy density functionals (EDFs). To study the excitations in the charge-exchange channel, an axially deformed proton-neutron relativistic quasiparticle RPA (pnRQRPA) is developed in the linear response approach. After benchmarking the axially deformed pnRQRPA in the spherical limit, a study of spin-isospin excitations including Fermi, Gamow-Teller (GT), and spin-dipole (SD) is performed for selected pf-shell nuclei. For GT transitions, it is demonstrated that deformation leads to a considerable fragmentation of the strength function. A mechanism inducing the fragmentation is studied by decomposing the total strength to different projections of total angular momentum K and constraining the nuclear shape to either spherical, prolate, or oblate. A similar fragmentation is also observed for SD transitions, although somewhat moderated by the complex structure of these transitions, while, as expected, the Fermi strength is almost shape independent. The axially deformed pnRQRPA introduced in this work open perspectives for the future studies of deformation effects on astrophysically relevant weak interaction processes, in particular beta decay and electron capture.


(1729)Constraints on exotic interactions from scalar spin-spin coupling in tritium deuteride (DT)
  • Lei Cong,
  • Derek F. Jackson Kimball,
  • Mikhail G. Kozlov,
  • Dmitry Budker
abstract + abstract -

A comparison of theoretical and experimental values of the scalar spin-spin interaction ($J$-coupling) in tritium deuteride molecules yield constraints for nucleon-nucleon exotic interactions of the dimensionless coupling strengths $g_Vg_V$, $g_Ag_A$ and $g_pg_p$, corresponding to the exchange of an vector, axial-vector, and pseudoscalar (axionlike) boson. The couplings between proton ($p$) and nucleon ($N$), denoted by $g_V^p g_V^N$, $g_p^p g_p^N$ are constrained to be less than $1.4 \times 10^{-6}$ and $2.7\times 10^{-6}$, respectively, for boson masses around 5 keV. The coupling constant $g_A^p g_A^N$ is constrained to be less than $1.0 \times 10^{-18}$ for boson masses $\leq 100$ eV. It is noteworthy that this study represents the first instance in which constraints on $g_V g_V$ have been established through the analysis of the potential term $V_2 + V_3$ for both tritium deuteride and hydrogen deuteride molecules.


(1728)An Exceptional Cluster Algebra for Higgs plus Jet Production
  • Rigers Aliaj,
  • Georgios Papathanasiou
abstract + abstract -

A recent evaluation of three-loop nonplanar Feynman integrals contributing to Higgs plus jet production has established their dependence on two novel symbol letters. We show that the resulting alphabet is described by a $G_2$ cluster algebra, enlarging the $C_2$ cluster algebra found to cover all previously known integrals relevant for this process. The cluster algebra connection we find reveals new adjacency relations, which significantly reduce the function space dimension of the non-planar triple ladder integral. These adjacencies may be understood in part by embedding $G_2$ inside higher-rank cluster algebras.


(1727)Spin-dependent exotic interactions
  • Lei Cong,
  • Wei Ji,
  • Pavel Fadeev,
  • Filip Ficek,
  • Min Jiang
  • +6
  • Victor V. Flambaum,
  • Haosen Guan,
  • Derek F. Jackson Kimball,
  • Mikhail G. Kozlov,
  • Yevgeny V. Stadnik,
  • Dmitry Budker
  • (less)
abstract + abstract -

Novel interactions beyond the four known fundamental forces in nature (electromagnetic, gravitational, strong and weak interactions), may arise due to "new physics" beyond the standard model, manifesting as a "fifth force". This review is focused on spin-dependent fifth forces mediated by exotic bosons such as spin-0 axions and axionlike particles and spin-1 Z' bosons, dark photons, or paraphotons. Many of these exotic bosons are candidates to explain the nature of dark matter and dark energy, and their interactions may violate fundamental symmetries. Spin-dependent interactions between fermions mediated by the exchange of exotic bosons have been investigated in a variety of experiments, particularly at the low-energy frontier. Experimental methods and tools used to search for exotic spin-dependent interactions, such as atomic comagnetometers, torsion balances, nitrogen-vacancy spin sensors, and precision atomic and molecular spectroscopy, are described. A complete set of interaction potentials, derived based on quantum field theory with minimal assumptions and characterized in terms of reduced coupling constants, are presented. A comprehensive summary of existing experimental and observational constraints on exotic spin-dependent interactions is given, illustrating the current research landscape and promising directions of further research.


(1726)Multi-dimensional optimisation of the scanning strategy for the LiteBIRD space mission
  • Y. Takase,
  • L. Vacher,
  • H. Ishino,
  • G. Patanchon,
  • L. Montier
  • +103
  • S. L. Stever,
  • K. Ishizaka,
  • Y. Nagano,
  • W. Wang,
  • J. Aumont,
  • K. Aizawa,
  • A. Anand,
  • C. Baccigalupi,
  • M. Ballardini,
  • A. J. Banday,
  • R. B. Barreiro,
  • N. Bartolo,
  • S. Basak,
  • M. Bersanelli,
  • M. Bortolami,
  • T. Brinckmann,
  • E. Calabrese,
  • P. Campeti,
  • E. Carinos,
  • A. Carones,
  • F. J. Casas,
  • K. Cheung,
  • L. Clermont,
  • F. Columbro,
  • A. Coppolecchia,
  • F. Cuttaia,
  • P. de Bernardis,
  • T. de Haan,
  • E. de la Hoz,
  • S. Della Torre,
  • P. Diego-Palazuelos,
  • G. D'Alessandro,
  • H. K. Eriksen,
  • J. Errard,
  • F. Finelli,
  • U. Fuskeland,
  • G. Galloni,
  • M. Galloway,
  • M. Gervasi,
  • T. Ghigna,
  • S. Giardiello,
  • C. Gimeno-Amo,
  • E. Gjerløw,
  • R. González González,
  • A. Gruppuso,
  • M. Hazumi,
  • S. Henrot-Versillé,
  • L. T. Hergt,
  • K. Ikuma,
  • K. Kohri,
  • L. Lamagna,
  • M. Lattanzi,
  • C. Leloup,
  • M. Lembo,
  • F. Levrier,
  • A. I. Lonappan,
  • M. López-Caniego,
  • G. Luzzi,
  • B. Maffei,
  • E. Martínez-González,
  • S. Masi,
  • S. Matarrese,
  • F. T. Matsuda,
  • T. Matsumura,
  • S. Micheli,
  • M. Migliaccio,
  • M. Monelli,
  • G. Morgante,
  • B. Mot,
  • R. Nagata,
  • T. Namikawa,
  • A. Novelli,
  • K. Odagiri,
  • S. Oguri,
  • R. Omae,
  • L. Pagano,
  • D. Paoletti,
  • F. Piacentini,
  • M. Pinchera,
  • G. Polenta,
  • L. Porcelli,
  • N. Raffuzzi,
  • M. Remazeilles,
  • A. Ritacco,
  • M. Ruiz-Granda,
  • Y. Sakurai,
  • D. Scott,
  • Y. Sekimoto,
  • M. Shiraishi,
  • G. Signorelli,
  • R. M. Sullivan,
  • H. Takakura,
  • L. Terenzi,
  • M. Tomasi,
  • M. Tristram,
  • B. van Tent,
  • P. Vielva,
  • I. K. Wehus,
  • B. Westbrook,
  • G. Weymann-Despres,
  • E. J. Wollack,
  • M. Zannoni,
  • Y. Zhou
  • (less)
abstract + abstract -

Large angular scale surveys in the absence of atmosphere are essential for measuring the primordial $B$-mode power spectrum of the Cosmic Microwave Background (CMB). Since this proposed measurement is about three to four orders of magnitude fainter than the temperature anisotropies of the CMB, in-flight calibration of the instruments and active suppression of systematic effects are crucial. We investigate the effect of changing the parameters of the scanning strategy on the in-flight calibration effectiveness, the suppression of the systematic effects themselves, and the ability to distinguish systematic effects by null-tests. Next-generation missions such as LiteBIRD, modulated by a Half-Wave Plate (HWP), will be able to observe polarisation using a single detector, eliminating the need to combine several detectors to measure polarisation, as done in many previous experiments and hence avoiding the consequent systematic effects. While the HWP is expected to suppress many systematic effects, some of them will remain. We use an analytical approach to comprehensively address the mitigation of these systematic effects and identify the characteristics of scanning strategies that are the most effective for implementing a variety of calibration strategies in the multi-dimensional space of common spacecraft scan parameters. We also present Falcons, a fast spacecraft scanning simulator that we developed to investigate this scanning parameter space.


(1725)On the electron self-energy to three loops in QED
  • Claude Duhr,
  • Federico Gasparotto,
  • Christoph Nega,
  • Lorenzo Tancredi,
  • Stefan Weinzierl
abstract + abstract -

We compute the electron self-energy in Quantum Electrodynamics to three loops in terms of iterated integrals over kernels of elliptic type. We make use of the differential equations method, augmented by an $\epsilon$-factorized basis, which allows us to gain full control over the differential forms appearing in the iterated integrals to all orders in the dimensional regulator. We obtain compact analytic expressions, for which we provide generalized series expansion representations that allow us to evaluate the result numerically for all values of the electron momentum squared. As a by product, we also obtain $\epsilon$-resummed results for the self-energy in the on-shell limit $p^2 = m^2$, which we use to recompute the known three-loop renormalization constants in the on-shell scheme.


(1724)Towards a Field Based Bayesian Evidence Inference from Nested Sampling Data
  • Margret Westerkamp,
  • Jakob Roth,
  • Philipp Frank,
  • Will Handley,
  • Torsten Enßlin
abstract + abstract -

Nested sampling (NS) is a stochastic method for computing the log-evidence of a Bayesian problem. It relies on stochastic estimates of prior volumes enclosed by likelihood contours, which limits the accuracy of the log-evidence calculation. We propose to transform the prior volume estimation into a Bayesian inference problem, which allows us to incorporate a smoothness assumption for likelihood-prior volume relations. As a result, we aim to increase the accuracy of the volume estimates and thus improve the overall log-evidence calculation using NS. The method presented works as a post-processing step for NS and provides posterior samples of the likelihood-prior-volume relation, from which the log-evidence can be calculated. We demonstrate an implementation of the algorithm and compare its results with plain NS on two synthetic datasets for which the underlying evidence is known. We find a significant improvement in accuracy for runs with less than one hundred active samples in NS, but are prone to numerical problems beyond this point.


(1723)Availability versus carrying capacity: Phases of asymmetric exclusion processes competing for finite pools of resources
  • Astik Haldar,
  • Parna Roy,
  • Erwin Frey,
  • Abhik Basu
abstract + abstract -

We address how the interplay between the finite availability and carrying capacity of particles at different parts of a spatially extended system can control the steady state currents and density profiles in the one-dimensional current-carrying lanes connecting the different parts of the system. To study this, we set up a minimal model consisting of two particle reservoirs of the same finite carrying capacity connected by two equally sized anti-parallel asymmetric exclusion processes (TASEP). We focus on the steady-state currents and particle density profiles in the two TASEP lanes. The ensuing phases and the phase diagrams, which can be remarkably complex, are parametrized by the model parameters defining particle exchange between the TASEP lanes and the reservoirs and the filling fraction of the particles that determine the total resources available. These parameters may be tuned to make the densities of the two TASEP lanes globally uniform or piece-wise continuous in the form of a combination of a single localized domain wall and a spatially constant density or a pair of delocalized domain walls. Our model reveals that the two reservoirs can be preferentially populated or depopulated in the steady states.


(1722)Supramolecular Assemblies in Active Motor-Filament Systems: Micelles, Bilayers, and Foams
  • Filippo De Luca,
  • Ivan Maryshev,
  • Erwin Frey
Physical Review X (08/2024) doi:10.1103/PhysRevX.14.031031
abstract + abstract -

Active matter systems evade the constraints of thermal equilibrium, leading to the emergence of intriguing collective behavior. A paradigmatic example is given by motor-filament mixtures, where the motion of motor proteins drives alignment and sliding interactions between filaments and their self-organization into macroscopic structures. After defining a microscopic model for these systems, we derive continuum equations, exhibiting the formation of active supramolecular assemblies such as micelles, bilayers, and foams. The transition between these structures is driven by a branching instability, which destabilizes the orientational order within the micelles, leading to the growth of bilayers at high microtubule densities. Additionally, we identify a fingering instability, modulating the shape of the micelle interface at high motor densities. We study the role of various mechanisms in these two instabilities, such as contractility, active splay, and anchoring, allowing for generalization beyond the system considered here.


(1721)Can Transformers Do Enumerative Geometry?
  • Baran Hashemi,
  • Roderic G. Corominas,
  • Alessandro Giacchetto
abstract + abstract -

How can Transformers model and learn enumerative geometry? What is a robust procedure for using Transformers in abductive knowledge discovery within a mathematician-machine collaboration? In this work, we introduce a new paradigm in computational enumerative geometry in analyzing the $\psi$-class intersection numbers on the moduli space of curves. By formulating the enumerative problem as a continuous optimization task, we develop a Transformer-based model for computing $\psi$-class intersection numbers based on the underlying quantum Airy structure. For a finite range of genera, our model is capable of regressing intersection numbers that span an extremely wide range of values, from $10^{-45}$ to $10^{45}$. To provide a proper inductive bias for capturing the recursive behavior of intersection numbers, we propose a new activation function, Dynamic Range Activator (DRA). Moreover, given the severe heteroscedasticity of $\psi$-class intersections and the required precision, we quantify the uncertainty of the predictions using Conformal Prediction with a dynamic sliding window that is aware of the number of marked points. Next, we go beyond merely computing intersection numbers and explore the enumerative "world-model" of the Transformers. Through a series of causal inference and correlational interpretability analyses, we demonstrate that Transformers are actually modeling Virasoro constraints in a purely data-driven manner. Additionally, we provide evidence for the comprehension of several values appearing in the large genus asymptotic of $\psi$-class intersection numbers through abductive hypothesis testing.


(1720)Torus reduction of maximal conformal supergravity
  • Franz Ciceri,
  • Axel Kleinschmidt,
  • Subrabalan Murugesan,
  • Bindusar Sahoo
abstract + abstract -

We consider the dimensional reduction of N=(2,0) conformal supergravity in six dimensions on a two-torus to N=4 conformal supergravity in four dimensions. At the level of kinematics, the six-dimensional Weyl multiplet is shown to reduce to a mixture of the N=4 Weyl and vector multiplets, which can be reinterpreted as a new off-shell multiplet of N=4 conformal supergravity. Similar multiplets have been constructed in other settings and are referred to as dilaton Weyl multiplets. We derive it here for the first time in a maximally supersymmetric context in four dimensions. Furthermore, we present the non-linear relations between all the six- and four-dimensional bosonic and fermionic fields, that are obtained by comparing the off-shell supersymmetry transformation rules.


(1719)Estimate for the Bulk Viscosity of Strongly Coupled Quark Matter Using Perturbative QCD and Holography
  • Jesús Cruz Rojas,
  • Tyler Gorda,
  • Carlos Hoyos,
  • Niko Jokela,
  • Matti Järvinen
  • +4
  • Aleksi Kurkela,
  • Risto Paatelainen,
  • Saga Säppi,
  • Aleksi Vuorinen
  • (less)
Physical Review Letters (08/2024) doi:10.1103/PhysRevLett.133.071901
abstract + abstract -

Modern hydrodynamic simulations of core-collapse supernovae and neutron-star mergers require knowledge not only of the equilibrium properties of strongly interacting matter, but also of the system's response to perturbations, encoded in various transport coefficients. Using perturbative and holographic tools, we derive here an improved weak-coupling and a new strong-coupling result for the most important transport coefficient of unpaired quark matter, its bulk viscosity. These results are combined in a simple analytic pocket formula for the quantity that is rooted in perturbative quantum chromodynamics at high densities but takes into account nonperturbative holographic input at neutron-star densities, where the system is strongly coupled. This expression can be used in the modeling of unpaired quark matter at astrophysically relevant temperatures and densities.


(1718)The $p\Lambda$ and $pp\Lambda$ correlation functions
  • E. Garrido,
  • A. Kievsky,
  • M. Gattobigio,
  • M. Viviani,
  • L. E. Marcucci
  • +3
  • R. Del Grande,
  • L. Fabbietti,
  • D. Melnichenko
  • (less)
abstract + abstract -

In this work we present the study of $p\Lambda$ and $pp\Lambda$ scattering processes using femtoscopic correlation functions. This observable has been recently used to access the low-energy interaction of hadrons emitted in the final state of high-energy collisions, delivering unprecedented precision information of the interaction among strange hadrons. The formalism for particle pairs is well established and it relates the measured correlation functions with the scattering wave function and the emission source. In the present work we analyze the $NN\Lambda$ scattering in free space and relate the corresponding wave function to the $pp\Lambda$ correlation measurement performed by the ALICE collaboration. The three-body problem is solved using the hyperspherical adiabatic basis. Regarding the $p\Lambda$ and $pp\Lambda$ interactions, different models are used and their impact on the correlation function is studied. The three body force considered in this work is anchored to describe the binding energy of the hypertriton and to give a good description of the two four-body hypernuclei. As a main result we have observed a huge, low-energy peak in the $pp\Lambda$ correlation function, mainly produced by the $J^\pi=1/2^+$ three-body state. The study of this peak from an experimental as well as a theoretical point of view will provide important constraints to the two- and three-body interactions.


(1717)Lattice holography on a quantum computer
  • Ying-Ying Li,
  • Muhammad Omer Sajid,
  • Judah Unmuth-Yockey
Physical Review D (08/2024) doi:10.1103/PhysRevD.110.034507
abstract + abstract -

We explore the potential application of quantum computers to the examination of lattice holography, which extends to the strongly coupled bulk theory regime. With adiabatic evolution, we compute the ground state of a spin system on a (2 +1 )-dimensional hyperbolic lattice, and measure the spin-spin correlation function on the boundary. Notably, we observe that with achievable resources for coming quantum devices, the correlation function demonstrates an approximate scale-invariant behavior, aligning with the pivotal theoretical predictions of the anti-de Sitter/conformal field theory correspondence.


(1716)Electroweak $\eta_w$ meson
  • Gia Dvali,
  • Archil Kobakhidze,
  • Otari Sakhelashvili
abstract + abstract -

We argue that the Standard Model is accompanied by a new pseudo-scalar degree of freedom, $\eta_w$-meson, which cancels the topological susceptibility of the electroweak vacuum and gets its mass from this effect. The prediction is based on the analyticity properties of the Chern-Simons correlator combined with the basic features of gravity. Depending on the quality-level of the $U(1)_{B+L}$-symmetry, $\eta_w$ emerges as a $B+L$ pseudo-Goldstone boson or as a Stückelberg $2$-form of the electroweak gauge redundancy. An intriguing scenario of the first category is the emergence of $\eta_w$ in the form of the phase of a $U(1)_{B+L}$-violating fermion condensate triggered by the instantons, somewhat similarly to $\eta'$-meson in QCD. Regardless of its particular origin, the presence of $\eta_w$-meson in the theory appears to be a matter of consistency.


(1715)Turbulent Pressure Support in Galaxy Clusters -- Impact of the Hydrodynamical Solver
  • Frederick Groth,
  • Milena Valentini,
  • Ulrich P. Steinwandel,
  • David Vallés-Pérez,
  • Klaus Dolag
abstract + abstract -

The amount of turbulent pressure in galaxy clusters is still debated, especially as for the impact of the dynamical state and the hydro-method used for simulations. We study the turbulent pressure fraction in the intra cluster medium of massive galaxy clusters. We aim to understand the impact of the hydrodynamical scheme, analysis method, and dynamical state on the final properties of galaxy clusters from cosmological simulations. We perform non-radiative simulations of a set of zoom-in regions of seven galaxy clusters with Meshless Finite Mass (MFM) and Smoothed Particle Hydrodynamics (SPH). We use three different analysis methods based on: $(i)$ the deviation from hydrostatic equilibrium, $(ii)$ the solenoidal velocity component obtained by a Helmholtz-Hodge decomposition, and $(iii)$ the small-scale velocity obtained through a multi-scale filtering approach. We split the sample of simulated clusters into active and relaxed clusters. Our simulations predict an increased turbulent pressure fraction for active compared to relaxed clusters. This is especially visible for the velocity-based methods. For these, we also find increased turbulence for the MFM simulations compared to SPH, consistent with findings from more idealized simulations. The predicted non-thermal pressure fraction varies between a few percent for relaxed clusters and $\approx13\%$ for active ones within the cluster center and increases towards the outskirts. No clear trend with redshift is visible. Our analysis quantitatively assesses the importance played by the hydrodynamical scheme and the analysis method to determine the non-thermal/turbulent pressure fraction. While our setup is relatively simple (non-radiative runs), our simulations show agreement with previous, more idealized simulations, and make a step further toward the understanding of turbulence.


(1714)Confronting sparse Gaia DR3 photometry with TESS for a sample of around 60 000 OBAF-type pulsators
  • Daniel Hey,
  • Conny Aerts
Astronomy and Astrophysics (08/2024) doi:10.1051/0004-6361/202450489
abstract + abstract -

Context. The Gaia mission has delivered hundreds of thousands of variable star light curves in multiple wavelengths. Recent work demonstrates that these light curves can be used to identify (non-)radial pulsations in OBAF-type stars, despite their irregular cadence and low light curve precision, of the order of a few millimagnitudes. With the considerably more precise TESS photometry, we revisited these candidate pulsators to conclusively ascertain the nature of their variability.
Aims: We seek to re-classify the Gaia light curves with the first two years of TESS photometry for a sample of 58 970 p- and g-mode pulsators, encompassing γ Dor, δ Scuti, slowly pulsating B, and β Cep variables. From the TESS data, we seek to assess the quality of Gaia's classification of non-radial pulsators, which is based on sparse, years-long light curves of millimagnitude precision. We also supply four new catalogues containing the confirmed pulsators, along with their dominant and secondary pulsation frequencies, the number of independent mode frequencies, and a ranking according to their usefulness for future asteroseismic ensemble analysis.
Methods: We first analysed the TESS light curves independent of their Gaia classification by pre-whitening all dominant pulsation modes down to a 1% false alarm probability. Using this, in combination with a feature-based random forest classifier, we identified different variability types across the sample.
Results: We find that the Gaia photometry is exceptionally accurate for detecting the dominant and secondary frequencies, reaching approximately 80% accuracy in frequency for p- and g-mode pulsators. The majority of Gaia classifications are consistent with the classifications from the TESS data, illustrating the power of the low-cadence Gaia photometry for pulsation studies. We find that the sample of g-mode pulsators forms a continuous group of variable stars along the main sequence across B, A, and F spectral types, implying that the mode excitation mechanisms for all these pulsators need to be updated with improved physics. Finally, we provide a rank-ordered table of pulsators according to their asteroseismic potential for follow-up studies, based on the number of sectors they have been observed in, their classification probability, and the number of independent modes found in the TESS light curves from the nominal mission.
Conclusions: Our catalogue offers a major increase in the number of confirmed g-mode pulsators with an identified dominant mode suitable for follow-up TESS ensemble asteroseismology of such stars.

Full Tables 1 and 3 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/688/A93.

The results of intermediate data products can be found at Zenodo https://doi.org/10.5281/zenodo.12578015.


(1713)A Dust-trapping Ring in the Planet-hosting Disk of Elias 2-24
  • Adolfo S. Carvalho,
  • Laura M. Pérez,
  • Anibal Sierra,
  • Maria Jesus Mellado,
  • Lynne A. Hillenbrand
  • +10
  • Sean Andrews,
  • Myriam Benisty,
  • Tilman Birnstiel,
  • John M. Carpenter,
  • Viviana V. Guzmán,
  • Jane Huang,
  • Andrea Isella,
  • Nicolas Kurtovic,
  • Luca Ricci,
  • David J. Wilner
  • (less)
The Astrophysical Journal (08/2024) doi:10.3847/1538-4357/ad5a07
abstract + abstract -

Rings and gaps are among the most widely observed forms of substructure in protoplanetary disks. A gap–ring pair may be formed when a planet carves a gap in the disk, which produces a local pressure maximum following the gap that traps inwardly drifting dust grains and appears as a bright ring owing to the enhanced dust density. A dust-trapping ring would provide a promising environment for solid growth and possibly planetesimal production via the streaming instability. We present evidence of dust trapping in the bright ring of the planet-hosting disk Elias 2-24, from the analysis of 1.3 and 3 mm Atacama Large Millimeter/submillimeter Array observations at high spatial resolution (0.″029, 4.0 au). We leverage the high spatial resolution to demonstrate that larger grains are more efficiently trapped and place constraints on the local turbulence (8 × 10‑4 < α turb < 0.03) and the gas-to-dust ratio (Σ g d < 30) in the ring. Using a scattering-included marginal probability analysis, we measure a total dust disk mass of <inline-formula> <mml:math overflow="scroll"><mml:msub><mml:mrow><mml:mi>M</mml:mi></mml:mrow><mml:mrow><mml:mi>dust</mml:mi></mml:mrow></mml:msub><mml:mo>=</mml:mo><mml:msubsup><mml:mrow><mml:mn>13.8</mml:mn></mml:mrow><mml:mrow><mml:mo>‑</mml:mo><mml:mn>0.5</mml:mn></mml:mrow><mml:mrow><mml:mo>+</mml:mo><mml:mn>0.7</mml:mn></mml:mrow></mml:msubsup><mml:mo>×</mml:mo><mml:msup><mml:mrow><mml:mn>10</mml:mn></mml:mrow><mml:mrow><mml:mo>‑</mml:mo><mml:mn>4</mml:mn></mml:mrow></mml:msup><mml:mspace width="0.33em"></mml:mspace><mml:msub><mml:mrow><mml:mi>M</mml:mi></mml:mrow><mml:mrow><mml:mo>&#8857;</mml:mo></mml:mrow></mml:msub></mml:math> </inline-formula>. We also show that at the orbital radius of the proposed perturber the gap is cleared of material down to a flux contrast of 10‑3 of the peak flux in the disk.


(1712)The Nature of X-Rays from Young Stellar Objects in the Orion Nebula Cluster—A Chandra HETGS Legacy Project
  • Norbert S. Schulz,
  • David P. Huenemoerder,
  • David A. Principe,
  • Marc Gagne,
  • Hans Moritz Günther
  • +8
  • Joel Kastner,
  • Joy Nichols,
  • Andrew Pollock,
  • Thomas Preibisch,
  • Paola Testa,
  • Fabio Reale,
  • Fabio Favata,
  • Claude R. Canizares
  • (less)
The Astrophysical Journal (08/2024) doi:10.3847/1538-4357/ad47c2
abstract + abstract -

The Orion Nebula Cluster (ONC) is the closest site of very young (∼1 Myr) massive star formation The ONC hosts more than 1600 young and X-ray bright stars with masses ranging from ∼0.1–35 M . The Chandra HETGS Orion Legacy Project observed the ONC with the Chandra High Energy Transmission Grating Spectrometer (HETGS) for 2.1 Ms. We describe the spectral extraction and cleaning processes necessary to separate overlapping spectra. We obtained 36 high-resolution spectra, which include a high-brilliance X-ray spectrum of θ 1 Ori C with over 100 highly significant X-ray lines. The lines show Doppler broadening between 300 and 400 km s‑1. Higher spectral diffraction orders allow us to resolve line components of high Z He-like triplets in θ 1 Ori C with unprecedented spectral resolution. Long-term light curves spanning ∼20 yr show all stars to be highly variable, including the massive stars. Spectral fitting with thermal coronal emission line models reveals that most sources show column densities of up to a few times 1022 cm‑2 and high coronal temperatures of 10–90 MK. We observe a bifurcation of the high-temperature component where some stars show a high component of 40 MK, while others show above 60 MK, indicating heavy flaring activity. Some lines are resolved with Doppler broadening above our threshold of ∼200 km s‑1, up to 500 km s‑1. This data set represents the largest collection of HETGS high-resolution X-ray spectra from young pre-main-sequence stars in a single star-forming region to date.


(1711)Sequential giant planet formation initiated by disc substructure
  • Tommy Chi Ho Lau,
  • Til Birnstiel,
  • Joanna Drążkowska,
  • Sebastian Markus Stammler
Astronomy and Astrophysics (08/2024) doi:10.1051/0004-6361/202450464
abstract + abstract -

Context. Planet formation models are necessary to understand the origins of diverse planetary systems. Circumstellar disc substructures have been proposed as preferred locations of planet formation, but a complete formation scenario has not been covered by a single model so far.
Aims: We aim to study the formation of giant planets facilitated by disc substructure and starting with sub-micron-sized dust.
Methods: We connect dust coagulation and drift, planetesimal formation, N-body gravity, pebble accretion, planet migration, planetary gas accretion, and gap opening in one consistent modelling framework.
Results: We find rapid formation of multiple gas giants from the initial disc substructure. The migration trap near the substructure allows for the formation of cold gas giants. A new pressure maximum is created at the outer edge of the planetary gap, which triggers the next generation of planet formation resulting in a compact chain of giant planets. A high planet formation efficiency is achieved, as the first gas giants are effective at preventing dust from drifting further inwards, which preserves material for planet formation.
Conclusions: Sequential planet formation is a promising framework to explain the formation of chains of gas and ice giants.


(1710)The SRG/eROSITA All-Sky Survey: Exploring halo assembly bias with X-ray-selected superclusters
  • A. Liu,
  • E. Bulbul,
  • T. Shin,
  • A. von der Linden,
  • V. Ghirardini
  • +13
  • M. Kluge,
  • J. S. Sanders,
  • S. Grandis,
  • X. Zhang,
  • E. Artis,
  • Y. E. Bahar,
  • F. Balzer,
  • N. Clerc,
  • N. Malavasi,
  • A. Merloni,
  • K. Nandra,
  • M. E. Ramos-Ceja,
  • S. Zelmer
  • (less)
Astronomy and Astrophysics (08/2024) doi:10.1051/0004-6361/202450519
abstract + abstract -

Numerical simulations indicate that the clustering of dark matter halos is not only dependent on the halo masses but has a secondary dependence on other properties, such as the assembly history of the halo. This phenomenon, known as the halo assembly bias (HAB), has been found mostly on galaxy scales; observational evidence on larger scales is scarce. In this work, we propose a novel method for exploring HAB on cluster scales using large samples of superclusters. Leveraging the largest-ever X-ray galaxy cluster and supercluster samples obtained from the first SRG/eROSITA all-sky survey, we constructed two subsamples of galaxy clusters that consist of supercluster members and isolated clusters, respectively. After correcting for the selection effects on redshift, mass, and survey depth, we computed the excess in the concentration of the intracluster gas of isolated clusters with respect to supercluster members, defined as δcgas ≡ cgas, ISO/cgas, SC − 1, to investigate the environmental effect on the concentration of clusters, a sign of HAB on cluster scales. We find that the average gas mass concentration of isolated clusters is a few percent higher than that of supercluster members, with a maximum significance of 2.8σ. The result for δcgas varies with the overdensity ratio, f, in supercluster identification, cluster mass proxies, and mass and redshift ranges but remains positive in almost all the measurements. We measure slightly larger δcgas when adopting a higher f for supercluster identification. The δcgas is also higher for low-mass and low-redshift clusters. We performed weak lensing analyses to compare the total mass concentration of the two classes and find a similar trend in total mass concentration as obtained from the gas mass concentration. Our results are consistent with the prediction of HAB on cluster scales, where halos located in denser environments are less concentrated; this trend is stronger for halos with lower masses and at lower redshifts. These phenomena can be explained by the fact that clusters in denser environments, such as superclusters, have experienced more mergers than isolated clusters in their assembling history. This work paves the way to explore HAB with X-ray superclusters and demonstrates that large samples of superclusters with X-ray and weak-lensing data can advance our understanding of the evolution of the large-scale structure.


(1709)The difficult path to coalescence: massive black hole dynamics in merging low-mass dark matter haloes and galaxies
  • Christian Partmann,
  • Thorsten Naab,
  • Antti Rantala,
  • Anna Genina,
  • Matias Mannerkoski
  • +1
Monthly Notices of the Royal Astronomical Society (08/2024) doi:10.1093/mnras/stae1712
abstract + abstract -

We present a high-resolution numerical study of the sinking and merging of massive black holes (MBHs) with masses in the range of $10^3 - 10^7 \, \mathrm{M}_\odot$ in multiple minor mergers of low-mass dark matter haloes without and with galaxies ($4\times 10^8 \, \mathrm{M}_\odot \lesssim {M}_{\mathrm{halo}} \lesssim 2\times 10^{10} \, \mathrm{M}_\odot)$. The KETJU simulation code, a combination of the GADGET tree solver with accurate regularized integration, uses unsoftened forces between the star/dark matter components and the MBHs for an accurate treatment of dynamical friction and scattering of dark matter/stars by MBH binaries or multiples. Post-Newtonian corrections up to order 3.5 for MBH interactions allow for coalescence by gravitational wave emission and gravitational recoil kicks. Low-mass MBHs ($\lesssim 10^5 \, \mathrm{M}_\odot$) hardly sink to the centre or merge. Sinking MBHs have various complex evolution paths - binaries, triplets, free-floating MBHs, and dynamically or recoil ejected MBHs. Collisional interactions with dark matter alone can drive MBHs to coalescence. The highest mass MBHs of $\gtrsim 10^6 \, \rm M_\odot$ mostly sink to the centre and trigger the scouring of dark matter and stellar cores. The scouring can transform a centrally baryon-dominated system into a dark-matter-dominated system. Our idealized high-resolution study highlights the difficulty to bring in and keep low-mass MBHs in the centres of low-mass haloes/galaxies - a remaining challenge for merger assisted MBH seed growth mechanisms.


(1708)Reality of Inverse Cascading in Neutron Star Crusts
  • Clara Dehman,
  • Axel Brandenburg
abstract + abstract -

The braking torque that dictates the timing properties of magnetars is closely tied to the large-scale dipolar magnetic field on their surface. The formation of this field has been a topic of ongoing debate. One proposed mechanism, based on macroscopic principles, involves an inverse cascade within the neutron star's crust. However, this phenomenon has not been observed in realistic simulations. In this study, we provide compelling evidence supporting the feasibility of the inverse cascading process in the presence of an initial helical magnetic field within realistic neutron star crusts and discuss its contribution to the amplification of the large-scale magnetic field. Our findings, derived from a systematic investigation that considers various coordinate systems, peak wavenumber positions, crustal thicknesses, magnetic boundary conditions, and magnetic Lundquist numbers, reveal that the specific geometry of the crustal domain - with its extreme aspect ratio - requires an initial peak wavenumber from small-scale structures for the inverse cascade to occur. However, this extreme aspect ratio limits the inverse cascade to magnetic field structures on scales comparable to the neutron star's crust, making the formation of a large-scale dipolar surface field unlikely. Despite this limitation, the inverse cascade can significantly impact the magnetic field evolution in the interior of the crust, potentially explaining the observed characteristics of highly magnetized objects with weak surface dipolar fields, such as low-field magnetars or central compact objects.


(1707)Population synthesis models indicate a need for early and ubiquitous disk substructures
  • Luca Delussu,
  • Tilman Birnstiel,
  • Anna Miotello,
  • Paola Pinilla,
  • Giovanni Rosotti
  • +1
Astronomy and Astrophysics (08/2024) doi:10.1051/0004-6361/202450328
abstract + abstract -

Context. Large millimeter surveys of star-forming regions enable the study of entire populations of planet-forming disks and reveal correlations between their observable properties. The ever-increasing number of these surveys has led to a flourishing of population study, a valuable tool and approach that is spreading in ever more fields. Population studies of disks have shown that the correlation between disk size and millimeter flux could be explained either through disks with strong substructure, or alternatively by the effects of radial inward drift of growing dust particles.
Aims: This study aims to constrain the parameters and initial conditions of planet-forming disks and address the question of the need for the presence of substructures in disks and, if needed, their predicted characteristics, based on the large samples of disk sizes, millimeter fluxes, and spectral indices available.
Methods: We performed a population synthesis of the continuum emission of disks, exploiting a two-population model (two-pop-py), considering the influence of viscous evolution, dust growth, fragmentation, and transport, varying the initial conditions of the disk and substructure to find the best match with the observed distributions. Disks both with and without substructure have been examined. We obtained the simulated population distribution for the disk sizes, millimeter fluxes, and spectral indices by post-processing the resulting disk profiles (surface density, maximum grain size, and disk temperature).
Results: We show that the observed distributions of spectral indices, sizes, and luminosities together can be best reproduced by disks with significant substructure; namely, a perturbation that is strong enough to be able to trap particles, that is formed early in the evolution of the disk, and that is within 0.4 Myr. Agreement is reached by relatively high initial disk masses (10−2.3 M ⩽ Mdisk ⩽ 10−0.5 M) and moderate levels of turbulence (10−3.5 ⩽ α ⩽ 10−2.5). Other disk parameters play a weaker role. Only opacities with a high absorption efficiency can reproduce the observed spectral indices.
Conclusions: Disk population synthesis is a precious tool for investigating and constraining the parameters and initial conditions of planet-forming disks. The generally low observed spectral indices call for significant substructure, like that which planets in the mass range of Saturn to a few Jupiters would induce, to already be present before 0.4 Myr. Our results indicate that substructure, which so far has only been assessed in individual disks, is likely ubiquitous and extends to the whole population, and imply that most "smooth" disks hide unresolved substructure.


(1706)Spatial segregation of massive clusters in a simulation of colliding dwarf galaxies
  • Bruce Elmegreen,
  • Natalia Lahen
The Open Journal of Astrophysics (08/2024) doi:10.33232/001c.122504
abstract + abstract -

The collective properties of star clusters are investigated using a simulation of the collision between two dwarf galaxies. The characteristic power law of the cluster mass function, N(M), with a logarithmic slope dN/dM ~ -1, is present from cluster birth and remains throughout the simulation. The maximum mass of a young cluster scales with the star formation rate (SFR). The relative average minimum separation, R(M)= N(M)^{1/p}D_min(M)/D(M_low), for average minimum distance D_min(M) between clusters of mass M, and for lowest mass, M_low, measured in projection (p=2) or three dimensions (p=3), has a negative slope, d log R/d log M ~ -0.2, for all masses and ages. This agrees with observations of R(M) in low-mass galaxies studied previously. Like the slope of N(M), R(M) is apparently a property of cluster birth for dwarf galaxies that does not depend on SFR or time. The negative slope for R(M) implies that massive clusters are more concentrated relative to lower mass clusters throughout the entire mass range. Cluster growth through coalescence is also investigated. The ratio of the kinetic to potential energy of all near-neighbor clusters is generally large, but a tail of low values in the distribution of this ratio suggests that a fraction of the clusters merge, ~8% by number throughout the ~300 Myr of the simulation and up to 60% by mass for young clusters in their first 10 Myr, scaling with the SFR above a certain threshold.


(1705)Diagnostics of 3D explosion asymmetries of stripped-envelope supernovae by nebular line profiles
  • Bart F. A. van Baal,
  • Anders Jerkstrand,
  • Annop Wongwathanarat,
  • Hans-Thomas Janka
Monthly Notices of the Royal Astronomical Society (08/2024) doi:10.1093/mnras/stae1603
abstract + abstract -

Understanding the explosion mechanism and hydrodynamic evolution of core-collapse supernovae (SNe) is a long-standing quest in astronomy. The asymmetries caused by the explosion are encoded into the line profiles which appear in the nebular phase of the SN evolution - with particularly clean imprints in He star explosions. Here, we carry out nine different supernova simulations of He-core progenitors, exploding them in 3D with parametrically varied neutrino luminosities using the PROMETHEUS-HOTB code, hydrodynamically evolving the models to the homologous phase. We then compute nebular phase spectra with the 3D Non-Local Thermodynamic Equilibrium spectral synthesis code EXTRASS (EXplosive TRAnsient Spectral Simulator). We study how line widths and shifts depend on progenitor mass, explosion energy, and viewing angle. We compare the predicted line profile properties against a large set of Type Ib observations, and discuss the degree to which current neutrino-driven explosions can match observationally inferred asymmetries. With self-consistent 3D modelling - circumventing the difficulties of representing $^{56}$Ni mixing and clumping accurately in 1D models - we find that neither low-mass He cores exploding with high energies nor high-mass cores exploding with low energies contribute to the Type Ib SN population. Models which have line profile widths in agreement with this population give sufficiently large centroid shifts for calcium emission lines. Calcium is more strongly affected by explosion asymmetries connected to the neutron star kicks than oxygen and magnesium. Lastly, we turn to the near-infrared spectra from our models to investigate the potential of using this regime to look for the presence of He in the nebular phase.


(1704)CSS161010: a luminous, fast blue optical transient with broad blueshifted hydrogen lines
  • Claudia P. Gutiérrez,
  • Seppo Mattila,
  • Peter Lundqvist,
  • Luc Dessart,
  • Santiago González-Gaitán
  • +34
  • Peter G. Jonker,
  • Subo Dong,
  • Deanne Coppejans,
  • Ping Chen,
  • Panos Charalampopoulos,
  • Nancy Elias-Rosa,
  • Thomas Reynolds,
  • Christopher Kochanek,
  • Morgan Fraser,
  • Andrea Pastorello,
  • Mariusz Gromadzki,
  • Jack Neustadt,
  • Stefano Benetti,
  • Erkki Kankare,
  • Tuomas Kangas,
  • Rubina Kotak,
  • Maximilian D. Stritzinger,
  • Thomas Wevers,
  • Bing Zhang,
  • David Bersier,
  • Subhash Bose,
  • David A. H. Buckley,
  • Raya Dastidar,
  • Anjasha Gangopadhyay,
  • Aleksandra Hamanowicz,
  • Juna Kollmeier,
  • Jirong Mao,
  • Stephen B. Potter,
  • Encarni Romero-Colmenero,
  • Mridweeka Singh,
  • Auni Somero,
  • Giacomo Terreran,
  • Petri Vaisanen,
  • Lukasz Wyrzykowski
  • (less)
abstract + abstract -

We present ultraviolet, optical and near-infrared photometric and optical spectroscopic observations of the luminous, fast blue optical transient (LFBOT), CSS161010:045834-081803 (CSS161010). The transient was found in a low-redshift (z=0.033) dwarf galaxy. The light curves of CSS161010 are characterized by an extremely fast evolution and blue colours. The V-band light curve shows that CSS161010 reaches an absolute peak of M$_{V}^{max}=-20.66\pm0.06$ mag in 3.8 days from the start of the outburst. After maximum, CSS161010 follows a power-law decline $\propto t^{-2.8\pm0.1}$ at all optical bands. These photometric properties are comparable to those of well-observed LFBOTs such as AT 2018cow, AT 2020mrf and AT 2020xnd. However, unlike these objects, the spectra of CSS161010 show a remarkable transformation from a blue and featureless continuum to spectra dominated by very broad, entirely blueshifted hydrogen emission lines of velocities of up to 10% of the speed of light. The persistent blueshifted emission and the lack of any emission at the rest wavelength of CSS161010 are unique features not seen in any transient before CSS161010. The combined observational properties of CSS161010 and its dwarf galaxy host favour the tidal disruption of a star by an intermediate-mass black hole as its origin.


(1703)HOLISMOKES -- XIV. Time-delay and differential dust extinction determination with lensed type II supernova color curves
  • J. Grupa,
  • S. Taubenberger,
  • S. H. Suyu,
  • S. Huber,
  • C. Vogl
  • +1
abstract + abstract -

The Hubble tension is one of the most relevant unsolved problems in cosmology today. Strongly gravitationally lensed transient objects, such as strongly lensed supernovae, are an independent and competitive probe that can be used to determine the Hubble constant. In this context, the time delay between different images of lensed supernovae is a key ingredient. We present a method, to retrieve time delays and the amount of differential dust extinction between multiple images of lensed type IIP supernovae through their color curves, which display a kink in the time evolution. With multiple realistic mock color curves based on an observed unlensed supernova from the Carnegie Supernova Project, we demonstrate that we can retrieve the time delay with uncertainties of $\pm$1.0 days for light curves with 2-day cadence and 35% missing data due to weather losses. The differential dust extinction is more susceptible to uncertainties, because it depends on imposing the correct extinction law. Further we also investigate the kink structure in the color curves for different rest-frame wavelength bands, particularly rest-frame UV light curves from SWIFT, finding sufficiently strong kinks for our method to work for typical lensed SN redshifts that would redshift the kink feature to optical wavelengths. With the upcoming Rubin Observatory Legacy Survey of Space and Time, hundreds of strongly lensed supernovae will be detected and our new method for lensed SN IIP is readily applicable to provide delays.


(1702)The Physalis system: discovery of ORC-like radio shells around a massive pair of interacting early-type galaxies with offset X-ray emission
  • Bärbel S. Koribalski,
  • Ildar Khabibullin,
  • Klaus Dolag,
  • Eugene Churazov,
  • Ray P. Norris
  • +5
  • Ettore Carretti,
  • Andrew M. Hopkins,
  • Tessa Vernstrom,
  • Stanislav S. Shabala,
  • Nikhel Gupta
  • (less)
Monthly Notices of the Royal Astronomical Society (08/2024) doi:10.1093/mnras/stae1669
abstract + abstract -

We present the discovery of large radio shells around a massive pair of interacting galaxies and extended diffuse X-ray emission within the shells. The radio data were obtained with the Australian Square Kilometre Array Pathfinder (ASKAP) in two frequency bands centred at 944 MHz and 1.4 GHz, respectively, while the X-ray data are from the XMM-Newton observatory. The host galaxy pair, which consists of the early-type galaxies ESO 184-G042 and LEDA 418116, is part of a loose group at a distance of only 75 Mpc (redshift $z = 0.017$). The observed outer radio shells (diameter ${\sim}$145 kpc) and ridge-like central emission of the system, ASKAP J1914-5433 (Physalis), are likely associated with merger shocks during the formation of the central galaxy (ESO 184-G042) and resemble the new class of odd radio circles (ORCs). This is supported by the brightest X-ray emission found offset from the centre of the Physalis system, instead centred at the less massive galaxy, LEDA 418116. The host galaxy pair is embedded in an irregular envelope of diffuse light, highlighting ongoing interactions. We complement our combined radio and X-ray study with high-resolution simulations of the circumgalactic medium (CGM) around galaxy mergers from the Magneticum project to analyse the evolutionary state of the Physalis system. We argue that ORCs/radio shells could be produced by a combination of energy release from the central active galactic nucleus and subsequent lightening up in radio emission by merger shocks travelling through the CGM of these systems.


(1701)Exploring the ultra-hot Jupiter WASP-178b. Constraints on atmospheric chemistry and dynamics from a joint retrieval of VLT/CRIRES<SUP>+</SUP> and space photometric data
  • D. Cont,
  • L. Nortmann,
  • F. Yan,
  • F. Lesjak,
  • S. Czesla
  • +12
  • A. Lavail,
  • A. Reiners,
  • N. Piskunov,
  • A. Hatzes,
  • L. Boldt-Christmas,
  • O. Kochukhov,
  • T. Marquart,
  • E. Nagel,
  • A. D. Rains,
  • M. Rengel,
  • U. Seemann,
  • D. Shulyak
  • (less)
Astronomy and Astrophysics (08/2024) doi:10.1051/0004-6361/202450064
abstract + abstract -

Despite recent progress in the spectroscopic characterization of individual exoplanets, the atmospheres of key ultra-hot Jupiters (UHJs) still lack comprehensive investigations. These include WASP-178b, one of the most irradiated UHJs known to date. We observed the dayside emission signal of this planet with CRIRES+ in the spectral K band. By applying the cross-correlation technique and a Bayesian retrieval framework to the high-resolution spectra, we identified the emission signature of 12CO (S/N = 8.9) and H2O (S/N = 4.9), and a strong atmospheric thermal inversion. A joint retrieval with space-based secondary eclipse measurements from TESS and CHEOPS allowed us to refine our results on the thermal profile and thus to constrain the atmospheric chemistry, yielding a solar to super-solar metallicity (1.4 ± 1.6 dex) and a solar C/O ratio (0.6 ± 0.2). We infer a significant excess of spectral line broadening and identify a slight Doppler-shift between the 12CO and H2O signals. These findings provide strong evidence for a super-rotating atmospheric flow pattern and suggest the possible existence of chemical inhomogeneities across the planetary dayside hemisphere. In addition, the inclusion of photometric data in our retrieval allows us to account for stellar light reflected by the planetary atmosphere, resulting in an upper limit on the geometric albedo (0.23). The successful characterization of WASP-178b's atmosphere through a joint analysis of CRIRES+, TESS, and CHEOPS observations highlights the potential of combined studies with space- and ground-based instruments and represents a promising avenue for advancing our understanding of exoplanet atmospheres.


(1700)Photoevaporation of protoplanetary discs with PLUTO+PRIZMO I. Lower X-ray-driven mass-loss rates due to enhanced cooling
  • Andrew D. Sellek,
  • Tommaso Grassi,
  • Giovanni Picogna,
  • Christian Rab,
  • Cathie J. Clarke
  • +1
abstract + abstract -

Context: Photoevaporation is an important process for protoplanetary disc dispersal but there has so far been a lack of consensus from simulations over the mass-loss rates and the most important part of the high-energy spectrum for driving the wind. Aims: We aim to isolate the origins of these discrepancies through carefully-benchmarked hydrodynamic simulations of X-ray photoevaporation with time-dependent thermochemistry calculated on the fly. Methods: We conduct hydrodynamic simulations with pluto where the thermochemistry is calculated using prizmo. We explore the contribution of certain key microphysical processes and the impact of using different spectra used previously in literature studies. Results: We find that additional cooling results from the excitation of O by neutral H, which leads to dramatically reduced mass-loss across the disc compared to previous X-ray photoevaporation models, with an integrated rate of 10^-9 Msun/yr. Such rates would allow for longer-lived discs than previously expected from population synthesis. An alternative spectrum with less soft X-ray produces mass-loss rates around a factor of 2-3 times lower. The chemistry is significantly out of equilibrium, with the survival of H2 into the wind aided by advection. This leads to its role as the dominant coolant at 10s au - thus stabilising a larger radial temperature gradient across the wind - as well as providing a possible wind tracer.


(1699)FAUST XIX. D<SUB>2</SUB>CO in the outflow cavities of NGC 1333 IRAS 4A: Recovering the physical structure of its original prestellar core
  • Layal Chahine,
  • Cecilia Ceccarelli,
  • Marta De Simone,
  • Claire J. Chandler,
  • Claudio Codella
  • +23
  • Linda Podio,
  • Ana López-Sepulcre,
  • Brian Svoboda,
  • Giovanni Sabatini,
  • Nami Sakai,
  • Laurent Loinard,
  • Charlotte Vastel,
  • Nadia Balucani,
  • Albert Rimola,
  • Piero Ugliengo,
  • Yuri Aikawa,
  • Eleonora Bianchi,
  • Mathilde Bouvier,
  • Paola Caselli,
  • Steven Charnley,
  • Nicolás Cuello,
  • Tomoyuki Hanawa,
  • Doug Johnstone,
  • Maria José Maureira,
  • Francois Ménard,
  • Yancy Shirley,
  • Leonardo Testi,
  • Satoshi Yamamoto
  • (less)
Monthly Notices of the Royal Astronomical Society (08/2024) doi:10.1093/mnrasl/slae080
abstract + abstract -

Molecular deuteration is a powerful diagnostic tool for probing the physical conditions and chemical processes in astrophysical environments. In this work, we focus on formaldehyde deuteration in the protobinary system NGC 1333 IRAS 4A, located in the Perseus molecular cloud. Using high-resolution (~ 100 au) ALMA observations, we investigate the [D2CO]/[HDCO] ratio along the cavity walls of the outflows emanating from IRAS 4A1. Our analysis reveals a consistent decrease in the deuteration ratio (from ~ 60-20% to ~ 10%) with increasing distance from the protostar (from ~ 2000 au to ~ 4000 au). Given the large measured [D2CO]/[HDCO], both HDCO and D2CO are likely injected by the shocks along the cavity walls into the gas-phase from the dust mantles, formed in the previous prestellar phase. We propose that the observed [D2CO]/[HDCO] decrease is due to the density profile of the prestellar core from which NGC 1333 IRAS 4A was born. When considering the chemical processes at the base of formaldehyde deuteration, the IRAS 4A's prestellar precursor had a predominantly flat density profile within 3000 au and a decrease of density beyond this radius.


(1698)Star Formation by Supernova Implosion
  • Leonard E. C. Romano,
  • Andreas Burkert,
  • Manuel Behrendt
The Astrophysical Journal (08/2024) doi:10.3847/2041-8213/ad6a57
abstract + abstract -

Recent hydrodynamical simulations of the late stages of supernova remnant (SNR) evolution have revealed that as they merge with the ambient medium, SNRs implode, leading to the formation of dense clouds in their center. While being highly chemically enriched by their host SNR, these clouds appear to have similar properties as giant molecular clouds, which are believed to be the main site of star formation. Here, we develop a simple model in order to estimate the efficiency of the star formation that might be triggered by the implosion of SNRs. We separately consider two cases: cyclic star formation, maintained by the episodic driving of feedback from new generations of stars, and a single burst of star formation, triggered by a single explosion. We find that in the cyclic case, star formation is inefficient, with implosion-triggered star formation contributing a few percent of the observed star formation efficiency per freefall timescale. In the single-burst case, higher star formation efficiencies can be obtained. However, while the implosion-triggered process might not contribute much to the overall star formation, due to the high chemical enrichment of the birth clouds, it can explain the formation of a significant fraction of metal-rich stars.


(1697)Final Moments. II. Observational Properties and Physical Modeling of Circumstellar-material-interacting Type II Supernovae
  • W. V. Jacobson-Galán,
  • L. Dessart,
  • K. W. Davis,
  • C. D. Kilpatrick,
  • R. Margutti
  • +50
  • R. J. Foley,
  • R. Chornock,
  • G. Terreran,
  • D. Hiramatsu,
  • M. Newsome,
  • E. Padilla Gonzalez,
  • C. Pellegrino,
  • D. A. Howell,
  • A. V. Filippenko,
  • J. P. Anderson,
  • C. R. Angus,
  • K. Auchettl,
  • K. A. Bostroem,
  • T. G. Brink,
  • R. Cartier,
  • D. A. Coulter,
  • T. de Boer,
  • M. R. Drout,
  • N. Earl,
  • K. Ertini,
  • J. R. Farah,
  • D. Farias,
  • C. Gall,
  • H. Gao,
  • M. A. Gerlach,
  • F. Guo,
  • A. Haynie,
  • G. Hosseinzadeh,
  • A. L. Ibik,
  • S. W. Jha,
  • D. O. Jones,
  • D. Langeroodi,
  • N. LeBaron,
  • E. A. Magnier,
  • A. L. Piro,
  • S. I. Raimundo,
  • A. Rest,
  • S. Rest,
  • R. Michael Rich,
  • C. Rojas-Bravo,
  • H. Sears,
  • K. Taggart,
  • V. A. Villar,
  • R. J. Wainscoat,
  • X. -F. Wang,
  • A. R. Wasserman,
  • S. Yan,
  • Y. Yang,
  • J. Zhang,
  • W. Zheng
  • (less)
The Astrophysical Journal (08/2024) doi:10.3847/1538-4357/ad4a2a
abstract + abstract -

We present ultraviolet/optical/near-infrared observations and modeling of Type II supernovae (SNe II) whose early time (δ t < 2 days) spectra show transient, narrow emission lines from shock ionization of confined (r < 1015 cm) circumstellar material (CSM). The observed electron-scattering broadened line profiles (i.e., IIn-like) of H I, He I/II, C IV, and N III/IV/V from the CSM persist on a characteristic timescale (t IIn) that marks a transition to a lower-density CSM and the emergence of Doppler-broadened features from the fast-moving SN ejecta. Our sample, the largest to date, consists of 39 SNe with early time IIn-like features in addition to 35 "comparison" SNe with no evidence of early time IIn-like features, all with ultraviolet observations. The total sample includes 50 unpublished objects with a total of 474 previously unpublished spectra and 50 multiband light curves, collected primarily through the Young Supernova Experiment and Global Supernova Project collaborations. For all sample objects, we find a significant correlation between peak ultraviolet brightness and both t IIn and the rise time, as well as evidence for enhanced peak luminosities in SNe II with IIn-like features. We quantify mass-loss rates and CSM density for the sample through the matching of peak multiband absolute magnitudes, rise times, t IIn, and optical SN spectra with a grid of radiation hydrodynamics and non-local thermodynamic equilibrium radiative-transfer simulations. For our grid of models, all with the same underlying explosion, there is a trend between the duration of the electron-scattering broadened line profiles and inferred mass-loss rate: <inline-formula> <mml:math overflow="scroll"><mml:msub><mml:mrow><mml:mi>t</mml:mi></mml:mrow><mml:mrow><mml:mi>IIn</mml:mi></mml:mrow></mml:msub><mml:mo>≈</mml:mo><mml:mn>3.8</mml:mn><mml:mo stretchy="false">[</mml:mo><mml:mover accent="true"><mml:mrow><mml:mi>M</mml:mi></mml:mrow><mml:mrow><mml:mo>&#775;</mml:mo></mml:mrow></mml:mover><mml:mrow><mml:mo stretchy="true">/</mml:mo></mml:mrow></mml:math> </inline-formula>(0.01 M &#8857; yr‑1)] days.


(1696)Foundations of ghost stability
  • Verónica Errasti Díez,
  • Jordi Gaset Rifà,
  • Georgina Staudt
abstract + abstract -

We present a new method to analytically prove global stability in ghost-ridden dynamical systems. Our proposal encompasses all prior results and consequentially extends them. In particular, we show that stability can follow from a conserved quantity that is unbounded from below, contrary to expectation. Novel examples illustrate all our results. Our findings take root on a careful examination of the literature, here comprehensively reviewed for the first time. This work lays the mathematical basis for ulterior extensions to field theory and quantization, and it constitutes a gateway for inter-disciplinary research in dynamics and integrability.


(1695)The UCHUU-GLAM BOSS and eBOSS LRG lightcones: exploring clustering and covariance errors
  • Julia Ereza,
  • Francisco Prada,
  • Anatoly Klypin,
  • Tomoaki Ishiyama,
  • Alex Smith
  • +4
  • Carlton M. Baugh,
  • Baojiu Li,
  • César Hernández-Aguayo,
  • José Ruedas
  • (less)
Monthly Notices of the Royal Astronomical Society (08/2024) doi:10.1093/mnras/stae1543
abstract + abstract -

This study investigates the clustering and bias of Luminous Red Galaxies (LRG) in the BOSS-LOWZ, -CMASS, -COMB, and eBOSS samples, using two types of simulated lightcones: (i) high-fidelity lightcones from UCHUUN-body simulation, employing SHAM technique to assign LRG to (sub)haloes, and (ii) 16 000 covariance lightcones from GLAM-UCHUUN-body simulations, including LRG using HOD data from UCHUU. Our results indicate that UCHUU and GLAM lightcones closely replicate BOSS/eBOSS data, reproducing correlation function and power spectrum across scales from redshifts 0.2 to 1.0, from 2 to $150 \,h^{-1}\,\mathrm{Mpc}$ in configuration space, from 0.005 to $0.7\, h\,\mathrm{Mpc}^{-1}$ in Fourier space, and across different LRG stellar masses. Furthermore, comparing with existing MD-PATCHY and EZMOCK BOSS/eBOSS lightcones based on approximate methods, our GLAM-UCHUU lightcones provide more precise clustering estimates. We identify significant deviations from observations within $20 \,h^{-1}\,\mathrm{Mpc}$ scales in MD-PATCHY and EZMOCK, with our covariance matrices indicating that these methods underestimate errors by between 10 per cent and 60 per cent. Lastly, we explore the impact of cosmology on galaxy clustering. Our findings suggest that, given the current level of uncertainties in BOSS/eBOSS data, distinguishing models with and without massive neutrino effects on large-scale structure (LSS) is challenging. This paper highlights the UCHUU and GLAM-UCHUU simulations' robustness in verifying the accuracy of Planck cosmological parameters, providing a strong foundation for enhancing lightcone construction in future LSS surveys. We also demonstrate that generating thousands of galaxy lightcones is feasible using N-body simulations with adequate mass and force resolution.


(1694)Metal accretion scars may be common on magnetic, polluted white dwarfs
  • S. Bagnulo,
  • J. D. Landstreet,
  • J. Farihi,
  • C. P. Folsom,
  • M. A. Hollands
  • +1
Astronomy and Astrophysics (08/2024) doi:10.1051/0004-6361/202451215
abstract + abstract -

More than 30% of white dwarfs exhibit atmospheric metals, which are understood to be from recent or ongoing accretion of circumstellar debris. In cool white dwarfs, surface motions should rapidly homogenise photospheric abundances, and the accreted heavy elements should diffuse inward on a timescale much longer than that for surface mixing. The recent discovery of a metal scar on WD 0816-310 implies its B ≈ 140 kG magnetic field has impeded surface mixing of metals near the visible magnetic pole. Here, we report the discovery of a second magnetic, metal-polluted white dwarf, WD 2138-332, which exhibits periodic variability in longitudinal field, metal line strength, and broadband photometry. All three variable quantities have the same period, and show remarkable correlations: the published light curves have a brightness minimum exactly when the longitudinal field and line strength have a maximum, and a maximum when the longitudinal field and line strength have a minimum. The simplest interpretation of the line strength variability is that there is an enhanced metal concentration around one pole of the magnetic field; however, the variable line-blanketing cannot account for the observed multi-band light curves. More theoretical work is required to understand the efficiency of horizontal mixing of the accreted metal atoms, and the origin of photometric variability. Because both magnetic, metal-polluted white dwarfs that have been monitored to date show that metal line strengths vary in phase with the longitudinal field, we suggest that metal scars around magnetic poles may be a common feature of metal-polluted white dwarfs.


(1693)Profile Likelihoods in Cosmology: When, Why and How illustrated with $\Lambda$CDM, Massive Neutrinos and Dark Energy
  • Laura Herold,
  • Elisa G. M. Ferreira,
  • Lukas Heinrich
abstract + abstract -

Frequentist parameter inference using profile likelihoods has received increased attention in the cosmology literature recently since it can give important complementary information to Bayesian credible intervals. Here, we give a pedagogical review to frequentist parameter inference in cosmology with particular focus on when the graphical profile likelihood construction gives meaningful constraints, i.e.\ confidence intervals with correct coverage. This construction rests on the assumption of the asymptotic limit of a large data set such as in \textit{Wilks' theorem}. We assess the validity of this assumption in the context of three cosmological models with \textit{Planck} 2018 \texttt{Plik\_lite} data: While our tests for the $\Lambda$CDM model indicate that the profile likelihood method gives correct coverage, $\Lambda$CDM with the sum of neutrino masses as a free parameter appears consistent with a Gaussian near a boundary motivating the use of the boundary-corrected or Feldman-Cousins graphical method; for $w_0$CDM with the equation of state of dark energy, $w_0$, as a free parameter, we find indication of a violation of the assumptions. Finally, we compare frequentist and Bayesian constraints of these models. Our results motivate care when using the graphical profile likelihood method in cosmology.


(1692)g$\delta N$ formalism
  • Takahiro Tanaka,
  • Yuko Urakawa
abstract + abstract -

The $\delta N$ formalism has been the major computational tool to study the superhorizon evolution of the scalar type perturbation sourced by scalar fields. Recently, this formalism was generalized to compute an arbitrary scalar, vector, and tensor type perturbations, including the gravitational waves (GWs), sourced by an arbitrary bosonic fields. In this paper, we explain how to use the generalized $\delta N$ formalism (the g$\delta N$ formalism), considering a model with U(1) gauge fields as a concrete example. Several new findings on this model and prospects on future gravitational wave experiments are also discussed, including the condition for the two linear polarizations of GWs to have different amplitudes. This paper provides a detailed explanation of our previous paper published in Physical Review Letters. We also discuss the Weinberg's adiabatic mode for an anisotropic background, showing a qualitative difference from the one for the FLRW background.


(1691)Unveiling galaxy chemical enrichment mechanisms out to cosmic dawn from direct determination of O &amp; Ar abundances from JWST/NIRSPEC spectroscopy
  • Souradeep Bhattacharya,
  • Magda Arnaboldi,
  • Ortwin Gerhard,
  • Chiaki Kobayashi,
  • Kanak Saha
abstract + abstract -

Galaxy chemical enrichment mechanisms have primarily been constrained by [$\alpha$/Fe] and [Fe/H] measurements of individual stars and integrated light from stellar populations. However such measurements are limited at higher redshifts (z>1). Recently, we proposed an analogous diagram of the oxygen-to-argon abundance ratio, log(O/Ar), vs Ar abundance, 12+log(Ar/H), as a new diagnostic window for emission nebulae. In this Letter, using robust line flux measurements including temperature sensitive auroral lines, we present direct determination of O and Ar abundances in nine SFGs from JWST/NIRSPEC spectra at z$\sim$1.3-7.7, and two more with Keck/MOSFIRE spectra at z$\sim$2.2. Utilising their positions on the log(O/Ar) vs 12+log(Ar/H) plane, we present the first inference of galaxy chemical enrichment mechanisms from an ensemble of galaxies. The SFGs at z$\sim$1.3-3.4 are consistent with the solar neighbourhood galactic chemical enrichment models of the Milky Way Galaxy that are driven by core-collapse and Type Ia supernovae. Such enrichment mechanisms thus occur at least out to z$\sim$3.4. However, the highest-redshift SFGs (z$\sim$3.6-7.7) have very low log(O/Ar) values, revealing a different enrichment process at z>3.6. Such low log(O/Ar) values may be caused by a rapid but intermittent star-formation and/or additional sources. The new diagnostic window for SFGs enables us to reveal the unique fingerprints of galaxy chemical enrichment out to cosmic dawn.


C2PAP
RU-D
(1690)C3NN: Cosmological Correlator Convolutional Neural Network an Interpretable Machine-learning Framework for Cosmological Analyses
  • Zhengyangguang Gong,
  • Anik Halder,
  • Annabelle Bohrdt,
  • Stella Seitz,
  • David Gebauer
The Astrophysical Journal (08/2024) doi:10.3847/1538-4357/ad582e
abstract + abstract -

Modern cosmological research in large-scale structure has witnessed an increasing number of machine-learning applications. Among them, convolutional neural networks (CNNs) have received substantial attention due to their outstanding performance in image classification, cosmological parameter inference, and various other tasks. However, many models based on CNNs are criticized as "black boxes" due to the difficulties in relating their outputs intuitively and quantitatively to the cosmological fields under investigation. To overcome this challenge, we present the Cosmological Correlator Convolutional Neural Network (C3NN)—a fusion of CNN architecture and cosmological N-point correlation functions (NPCFs). We demonstrate that its output can be expressed explicitly in terms of the analytically tractable NPCFs. Together with other auxiliary algorithms, we can open the "black box" by quantitatively ranking different orders of the interpretable outputs based on their contribution to classification tasks. As a proof of concept, we demonstrate this by applying our framework to a series of binary classification tasks using Gaussian and log-normal random fields and relating its outputs to the NPCFs describing the two fields. Furthermore, we exhibit the model's ability to distinguish different dark energy scenarios (w 0 = ‑0.95 and ‑1.05) using N-body simulated weak-lensing convergence maps and discuss the physical implications coming from their interpretability. With these tests, we show that C3NN combines advanced aspects of machine learning architectures with the framework of cosmological NPCFs, thereby making it an exciting tool to extract physical insights in a robust and explainable way from observational data.


(1689)The boundary of cosmic filaments
  • Wei Wang,
  • Peng Wang,
  • Hong Guo,
  • Xi Kang,
  • Noam I. Libeskind
  • +10
  • Daniela Galárraga-Espinosa,
  • Volker Springel,
  • Rahul Kannan,
  • Lars Hernquist,
  • Rüdiger Pakmor,
  • Hao-Ran Yu,
  • Sownak Bose,
  • Quan Guo,
  • Luo Yu,
  • César Hernández-Aguayo
  • (less)
Monthly Notices of the Royal Astronomical Society (08/2024) doi:10.1093/mnras/stae1801
abstract + abstract -

For decades, the boundary of cosmic filaments has been a subject of debate. In this work, we determine the physically motivated radii of filaments by constructing stacked galaxy number density profiles around the filament spines. We find that the slope of the profile changes with distance to the filament spine, reaching its minimum at approximately 1 Mpc at $z=0$ in both state-of-the-art hydrodynamical simulations and observational data. This can be taken as the average value of the filament radius. Furthermore, we note that the average filament radius rapidly decreases from $z=4$ to 1, and then slightly increases. Moreover, we find that the radius of the filament depends on the length of the filament, the distance from the connected clusters, and the masses of the clusters. These results suggest a two-phase formation scenario of cosmic filaments. The filaments experienced rapid contraction before $z=1$, but their density distribution has remained roughly stable since then. The subsequent mass transport along the filaments to the connected clusters is likely to have contributed to the formation of the clusters themselves.


(1688)FAUST. XVII. Super deuteration in the planet-forming system IRS 63 where the streamer strikes the disk
  • L. Podio,
  • C. Ceccarelli,
  • C. Codella,
  • G. Sabatini,
  • D. Segura-Cox
  • +53
  • N. Balucani,
  • A. Rimola,
  • P. Ugliengo,
  • C. J. Chandler,
  • N. Sakai,
  • B. Svoboda,
  • J. Pineda,
  • M. De Simone,
  • E. Bianchi,
  • P. Caselli,
  • A. Isella,
  • Y. Aikawa,
  • M. Bouvier,
  • E. Caux,
  • L. Chahine,
  • S. B. Charnley,
  • N. Cuello,
  • F. Dulieu,
  • L. Evans,
  • D. Fedele,
  • S. Feng,
  • F. Fontani,
  • T. Hama,
  • T. Hanawa,
  • E. Herbst,
  • T. Hirota,
  • I. Jiménez-Serra,
  • D. Johnstone,
  • B. Lefloch,
  • R. Le Gal,
  • L. Loinard,
  • H. Baobab Liu,
  • A. López-Sepulcre,
  • L. T. Maud,
  • M. J. Maureira,
  • F. Menard,
  • A. Miotello,
  • G. Moellenbrock,
  • H. Nomura,
  • Y. Oba,
  • S. Ohashi,
  • Y. Okoda,
  • Y. Oya,
  • T. Sakai,
  • Y. Shirley,
  • L. Testi,
  • C. Vastel,
  • S. Viti,
  • N. Watanabe,
  • Y. Watanabe,
  • Y. Zhang,
  • Z. E. Zhang,
  • S. Yamamoto
  • (less)
Astronomy and Astrophysics (08/2024) doi:10.1051/0004-6361/202450742
abstract + abstract -

Context. Recent observations suggest that planet formation starts early, in protostellar disks of ≤105 yr, which are characterized by strong interactions with the environment, such as through accretion streamers and molecular outflows.
Aims: To investigate the impact of such phenomena on the physical and chemical properties of a disk, it is key to understand what chemistry planets inherit from their natal environment.
Methods: In the context of the ALMA large program Fifty AU Study of the chemistry in the disk/envelope system of solar-like protostars (FAUST), we present observations on scales from ∼1500 au to ∼60 au of H2CO, HDCO, and D2CO toward the young planet-forming disk IRS 63.
Results: The H2CO probes the gas in the disk as well as in a large scale streamer (∼1500 au) impacting onto the southeast disk side. We detected for the first time deuterated formaldehyde, HDCO and D2CO, in a planet-forming disk and HDCO in the streamer that is feeding it. These detections allowed us to estimate the deuterium fractionation of H2CO in the disk: [HDCO]/[H2CO] ∼ 0.1 − 0.3 and [D2CO]/[H2CO] ∼ 0.1. Interestingly, while HDCO follows the H2CO distribution in the disk and in the streamer, the distribution of D2CO is highly asymmetric, with a peak of the emission (and [D]/[H] ratio) in the southeast disk side, where the streamer crashes onto the disk. In addition, D2CO was detected in two spots along the blue- and redshifted outflow. This suggests that (i) in the disk, HDCO formation is dominated by gas-phase reactions in a manner similar to H2CO, while (ii) D2CO is mainly formed on the grain mantles during the prestellar phase and/or in the disk itself and is at present released in the gas phase in the shocks driven by the streamer and the outflow.
Conclusions: These findings testify to the key role of streamers in the buildup of the disk concerning both the final mass available for planet formation and its chemical composition.


(1687)Speed of sound bounds and first-order phase transitions in compact stars
  • P. Laskos-Patkos,
  • G. A. Lalazissis,
  • Sibo Wang,
  • Jie Meng,
  • Peter Ring
  • +1
abstract + abstract -

In the present study we employ three distinct physically motivated speed of sound bounds in order to construct hybrid models where the high density phase is described by the maximally stiff equation of state. In particular, we consider the bounds related to special relativity, relativistic kinetic theory and conformality. The low density hadronic phase is described by a state-of-the-art microscopic relativistic Brueckner-Hartree-Fock theory. This work aims to access the effect of the different speed of sound constraints on the relevant parameter space of the key parameters of first-order phase transitions by utilising recent astronomical data. This involves a systematic analysis that also includes two distinct schemes for the construction of hybrid models, namely the Maxwell and Gibbs methods. Finally, a relevant discussion is conducted on the possible occurrence of a thermodynamic inconsistency that is related to the stability of the high density phase over hadronic matter at large densities.


CN-3
(1686)New mass window for primordial black holes as dark matter from the memory burden effect
  • Ana Alexandre,
  • Gia Dvali,
  • Emmanouil Koutsangelas
Physical Review D (08/2024) doi:10.1103/PhysRevD.110.036004
abstract + abstract -

The mass ranges allowed for primordial black holes (PBHs) to constitute all of dark matter (DM) are broadly constrained. However, these constraints rely on the standard semiclassical approximation which assumes that the evaporation process is self-similar. Quantum effects such as memory burden take the evaporation process out of the semiclassical regime latest by the time the black hole loses half of its mass. What happens beyond this time is currently not known. However, theoretical evidence based on prototype models indicates that the evaporation slows down, thereby extending the lifetime of a black hole. This modifies the mass ranges constrained, in particular, by big bang nucleosynthesis (BBN) and cosmic microwave background spectral distortions. We show that previous constraints are largely relaxed when the PBH lifetime is extended, making it possible for PBHs to constitute all of DM in previously excluded mass ranges. In particular, this is the case for PBHs lighter than 109 g that enter the memory burden stage before BBN and are still present today as DM.


(1685)Relevance of the coupled channels in the $\phi$p and $\rho^0$p Correlation Functions
  • A. Feijoo,
  • M. Korwieser,
  • L. Fabbietti
abstract + abstract -

The vector meson-baryon interaction in a coupled channel scheme is revisited within the correlation function framework. As illustrative cases to reveal the important role played by the coupled channels, we focus on the $\phi$p and $\rho^0$p systems given their complex dynamics and the presence of quasi-bound states or resonances in the vicinity of their thresholds. We show that the $\phi$p femtoscopic data provide novel information about a $N^*$ state present in the experimental region and anticipate the relevance of a future $\rho^0$p correlation function measurement in order to pin down the $S=0, Q=+1$ vector meson-baryon interaction as well as to disclose the characterizing features of the $N^*(1700)$ state.


(1684)Efficient Forward-Mode Algorithmic Derivatives of Geant4
  • Max Aehle,
  • Xuan Tung Nguyen,
  • Mihály Novák,
  • Tommaso Dorigo,
  • Nicolas R. Gauger
  • +3
  • Jan Kieseler,
  • Markus Klute,
  • Vassil Vassilev
  • (less)
abstract + abstract -

We have applied an operator-overloading forward-mode algorithmic differentiation tool to the Monte-Carlo particle simulation toolkit Geant4. Our differentiated version of Geant4 allows computing mean pathwise derivatives of user-defined outputs of Geant4 applications with respect to user-defined inputs. This constitutes a major step towards enabling gradient-based optimization techniques in high-energy physics, as well as other application domains of Geant4. This is a preliminary report on the technical aspects of applying operator-overloading AD to Geant4, as well as a first analysis of some results obtained by our differentiated Geant4 prototype. We plan to follow up with a more refined analysis.


(1683)Formation of long-period post-common-envelope binaries. II. Explaining the self-lensing binary KOI 3278
  • Diogo Belloni,
  • Matthias R. Schreiber,
  • Monica Zorotovic
Astronomy and Astrophysics (07/2024) doi:10.1051/0004-6361/202449320
abstract + abstract -

Context. The vast majority of close binaries containing a compact object, including the progenitors of supernovae Ia and at least a substantial fraction of all accreting black holes in the Galaxy, form through common-envelope (CE) evolution. Despite this importance, we struggle to even understand the energy budget of CE evolution. For decades, observed long-period post-CE binaries have been interpreted as evidence of additional energies contributing during CE evolution. We have recently shown that this argument is based on simplified assumptions for all long-period post-CE binaries containing massive white dwarfs (WDs). The only remaining post-CE binary star that has been claimed to require contributions from additional energy sources to understand its formation is KOI 3278.
Aims: Here, we address in detail the potential evolutionary history of KOI 3278. In particular, we investigate whether extra energy sources, such as recombination energy, are indeed required to explain its existence.
Methods: We used the 1D stellar evolution code MESA to carry out binary evolution simulations and searched for potential formation pathways for KOI 3278 that are able to explain its observed properties.
Results: We find that KOI 3278 can be explained if the WD progenitor filled its Roche lobe during a helium shell flash. In this case, the orbital period of KOI 3278 can be reproduced if the CE binding energy is calculated taking into account gravitational energy and thermodynamic internal energy. While the CE evolution that led to the formation of KOI 3278 must have been efficient - that is, most of the available orbital energy must have been used to unbind the CE - recombination energy is not required.
Conclusions: We conclude that currently not a single observed post-CE binary requires one to assume that energy sources other than gravitational and thermodynamic energy are contributing to CE evolution. KOI 3278, however, remains an intriguing post-CE binary as, unlike its siblings, understanding its existence requires highly efficient CE ejection.


(1682)Cosmology with galaxy cluster properties using machine learning
  • Lanlan Qiu,
  • Nicola R. Napolitano,
  • Stefano Borgani,
  • Fucheng Zhong,
  • Xiaodong Li
  • +8
  • Mario Radovich,
  • Weipeng Lin,
  • Klaus Dolag,
  • Crescenzo Tortora,
  • Yang Wang,
  • Rhea-Silvia Remus,
  • Sirui Wu,
  • Giuseppe Longo
  • (less)
Astronomy and Astrophysics (07/2024) doi:10.1051/0004-6361/202346683
abstract + abstract -

Context. Galaxy clusters are the largest gravitating structures in the universe, and their mass assembly is sensitive to the underlying cosmology. Their mass function, baryon fraction, and mass distribution have been used to infer cosmological parameters despite the presence of systematics. However, the complexity of the scaling relations among galaxy cluster properties has never been fully exploited, limiting their potential as a cosmological probe.
Aims: We propose the first machine learning (ML) method using galaxy cluster properties from hydrodynamical simulations in different cosmologies to predict cosmological parameters combining a series of canonical cluster observables, such as gas mass, gas bolometric luminosity, gas temperature, stellar mass, cluster radius, total mass, and velocity dispersion at different redshifts.
Methods: The ML model was trained on mock "measurements" of these observable quantities from Magneticum multi-cosmology simulations to derive unbiased constraints on a set of cosmological parameters. These include the mass density parameter, Ωm, the power spectrum normalization, σ8, the baryonic density parameter, Ωb, and the reduced Hubble constant, h0.
Results: We tested the ML model on catalogs of a few hundred clusters taken, in turn, from each simulation and found that the ML model can correctly predict the cosmology from where they have been picked. The cumulative accuracy depends on the cosmology, ranging from 21% to 75%. We demonstrate that this is sufficient to derive unbiased constraints on the main cosmological parameters with errors on the order of ~14% for Ωm, ~8% for σ8, ~6% for Ωb, and ~3% for h0.
Conclusions: This proof-of-concept analysis, though based on a limited variety of multi-cosmology simulations, shows that ML can efficiently map the correlations in the multidimensional space of the observed quantities to the cosmological parameter space and narrow down the probability that a given sample belongs to a given cosmological parameter combination. More large-volume, mid-resolution, multi-cosmology hydro-simulations need to be produced to expand the applicability to a wider cosmological parameter range. However, this first test is exceptionally promising, as it shows that these ML tools can be applied to cluster samples from multiwavelength observations from surveys such as Rubin/LSST, CSST, Euclid, and Roman in optical and near-infrared bands, and eROSITA in X-rays, to the constrain cosmology and effect of baryonic feedback.


(1681)Shockingly Bright Warm Carbon Monoxide Molecular Features in the Supernova Remnant Cassiopeia A Revealed by JWST
  • J. Rho,
  • S. -H. Park,
  • R. Arendt,
  • M. Matsuura,
  • D. Milisavljevic
  • +34
  • T. Temim,
  • I. De Looze,
  • W. P. Blair,
  • A. Rest,
  • O. Fox,
  • A. P. Ravi,
  • B. -C. Koo,
  • M. Barlow,
  • A. Burrows,
  • R. Chevalier,
  • G. Clayton,
  • R. Fesen,
  • C. Fransson,
  • C. Fryer,
  • H. L. Gomez,
  • H. -T. Janka,
  • F. Kirchschlager,
  • J. M. Laming,
  • S. Orlando,
  • D. Patnaude,
  • G. Pavlov,
  • P. Plucinsky,
  • B. Posselt,
  • F. Priestley,
  • J. Raymond,
  • N. Sartorio,
  • F. Schmidt,
  • P. Slane,
  • N. Smith,
  • N. Sravan,
  • J. Vink,
  • K. Weil,
  • J. Wheeler,
  • S. C. Yoon
  • (less)
The Astrophysical Journal (07/2024) doi:10.3847/2041-8213/ad5186
abstract + abstract -

We present JWST NIRCam (F356W and F444W filters) and MIRI (F770W) images and NIRSpec Integral Field Unit (IFU) spectroscopy of the young Galactic supernova remnant Cassiopeia A (Cas A) to probe the physical conditions for molecular CO formation and destruction in supernova ejecta. We obtained the data as part of a JWST survey of Cas A. The NIRCam and MIRI images map the spatial distributions of synchrotron radiation, Ar-rich ejecta, and CO on both large and small scales, revealing remarkably complex structures. The CO emission is stronger at the outer layers than the Ar ejecta, which indicates the re-formation of CO molecules behind the reverse shock. NIRSpec-IFU spectra (3–5.5 μm) were obtained toward two representative knots in the NE and S fields that show very different nucleosynthesis characteristics. Both regions are dominated by the bright fundamental rovibrational band of CO in the two R and P branches, with strong [Ar VI] and relatively weaker, variable strength ejecta lines of [Si IX], [Ca IV], [Ca V], and [Mg IV]. The NIRSpec-IFU data resolve individual ejecta knots and filaments spatially and in velocity space. The fundamental CO band in the JWST spectra reveals unique shapes of CO, showing a few tens of sinusoidal patterns of rovibrational lines with pseudocontinuum underneath, which is attributed to the high-velocity widths of CO lines. Our results with LTE modeling of CO emission indicate a temperature of ∼1080 K and provide unique insight into the correlations between dust, molecules, and highly ionized ejecta in supernovae and have strong ramifications for modeling dust formation that is led by CO cooling in the early Universe.


(1680)Simulating nearby disc galaxies on the main star formation sequence. I. Bar formation and the building of the central gas reservoir
  • Pierrick Verwilghen,
  • Eric Emsellem,
  • Florent Renaud,
  • Milena Valentini,
  • Jiayi Sun
  • +12
  • Sarah Jeffreson,
  • Ralf S. Klessen,
  • Mattia C. Sormani,
  • Ashley T. Barnes,
  • Klaus Dolag,
  • Kathryn Grasha,
  • Fu-Heng Liang,
  • Sharon Meidt,
  • Justus Neumann,
  • Miguel Querejeta,
  • Eva Schinnerer,
  • Thomas G. Williams
  • (less)
Astronomy and Astrophysics (07/2024) doi:10.1051/0004-6361/202348772
abstract + abstract -

Past studies have long emphasised the key role played by galactic stellar bars in the context of disc secular evolution, via the redistribution of gas and stars, the triggering of star formation, and the formation of prominent structures such as rings and central mass concentrations. However, the exact physical processes acting on those structures, as well as the timescales associated with the building and consumption of central gas reservoirs are still not well understood. We are building a suite of hydro-dynamical RAMSES simulations of isolated, low-redshift galaxies that mimic the properties of the PHANGS sample. The initial conditions of the models reproduce the observed stellar mass, disc scale length, or gas fraction, and this paper presents a first subset of these models. Most of our simulated galaxies develop a prominent bar structure, which itself triggers central gas fuelling and the building of an over-density with a typical scale of 100−1000 pc. We confirm that if the host galaxy features an ellipsoidal component, the formation of the bar and gas fuelling are delayed. We show that most of our simulations follow a common time evolution, when accounting for mass scaling and the bar formation time. In our simulations, the stellar mass of 1010 M seems to mark a change in the phases describing the time evolution of the bar and its impact on the interstellar medium. In massive discs (M ≥ 1010 M), we observe the formation of a central gas reservoir with star formation mostly occurring within a restricted starburst region, leading to a gas depletion phase. Lower-mass systems (M < 1010 M) do not exhibit such a depletion phase, and show a more homogeneous spread of star-forming regions along the bar structure, and do not appear to host inner bar-driven discs or rings. Our results seem to be supported by observations, and we briefly discuss how this new suite of simulations can help our understanding of the secular evolution of main sequence disc galaxies.


CN-5
RU-D
(1679)MeerKAT discovery of a double radio relic and odd radio circle: connecting cluster and galaxy merger shocks
  • Bärbel S. Koribalski,
  • Angie Veronica,
  • Klaus Dolag,
  • Thomas H. Reiprich,
  • Marcus Brüggen
  • +9
  • Ian Heywood,
  • Heinz Andernach,
  • Ralf-Jürgen Dettmar,
  • Matthias Hoeft,
  • Xiaoyuan Zhang,
  • Esra Bulbul,
  • Christian Garrel,
  • Gyula I. G. Józsa,
  • Jayanne English
  • (less)
Monthly Notices of the Royal Astronomical Society (07/2024) doi:10.1093/mnras/stae1254
abstract + abstract -

We present the serendipitous discovery of (1) a large double radio relic associated with the galaxy cluster PSZ2 G277.93 + 12.34 and (2) a new odd radio circle, ORC J1027-4422, both found in the same deep MeerKAT 1.3 GHz wide-band radio continuum image. The angular separation of the two arc-shaped cluster relics is ~16 arcmin or ~2.6 Mpc for a cluster redshift of z ≈ 0.158. The thin southern relic, which shows several ridges/shocks including one possibly moving inwards, has a linear extent of ~1.64 Mpc. In contrast, the northern relic is about twice as wide, twice as bright, but only has a largest linear size of ~0.66 Mpc. Complementary SRG/eROSITA X-ray images reveal extended emission from hot intracluster gas between the two relics and around the narrow-angle tail (NAT) radio galaxy PMN J1033-4335 (z ≈ 0.153) located just east of the northern relic. The radio morphologies of the NAT galaxy and the northern relic, which are also detected with the Australian Square Kilometer Array Pathfinder (ASKAP) at 888 MHz, suggest both are moving in the same outward direction. The discovery of ORC J1027-4422 in a different part of the same MeerKAT image makes it the fourth known single ORC. It has a diameter of ~90 arcsec corresponding to 400 kpc at a tentative redshift of z ≈ 0.3 and remains undetected in X-ray emission. Supported by simulations, we discuss similarities between outward moving galaxy and cluster merger shocks as the formation mechanisms for ORCs and radio relics, respectively.


(1678)Constraints on the formation history and composition of Kepler planets from their distribution of orbital period ratios
  • Di-Chang Chen,
  • Christoph Mordasini,
  • Ji-Wei Xie,
  • Ji-Lin Zhou,
  • Alexandre Emsenhuber
Astronomy and Astrophysics (07/2024) doi:10.1051/0004-6361/202449371
abstract + abstract -

Context. The Kepler high-precision planetary sample has revealed a `radius valley' separating compact super-Earths from sub-Neptunes with lower densities. Super-Earths are generally assumed to be rocky planets that were probably born in situ, while the composition and formation of sub-Neptunes remains debated. Numerous statistical studies have explored planetary and stellar properties and their correlations to provide observational clues. However, no conclusive result on the origin of the radius valley or the composition of sub-Neptunes has been derived to date.
Aims: To provide more constraints, our aim is to investigate the distributions of the orbital spacing of sub-Neptunes and super-Earth planets in Kepler systems and compare their distributions with theoretical predictions of planet pairs of different formation pathways and compositions in synthetic planetary systems.
Methods: Based on the Kepler planetary sample, we derived the distributions of period ratios of sub-Neptune and super-Earth planet pairs. Using synthetic planetary systems generated by the Generation III Bern Model, we also obtained theoretical predictions of period ratio distributions of planet pairs of different compositions and origins.
Results: We find that Kepler sub-Neptune pairs show a significant preference to be near first-order mean motion resonances by a factor of 1.7−0.3+0.3. This is smaller than the model predictions for `water-rich' pairs but larger than that of `water-poor' pairs by confidence levels of ~2σ. Kepler super-Earth pairs show no significant preference for mean motion resonances from a random distribution. The derived normalised fraction of near first-order resonances of actual Kepler super-Earth pairs is consistent with that of synthetic water-poor planet pairs but significantly (≳3σ) smaller than that of synthetic water-rich planet pairs.
Conclusions: The orbital migration has been more important for sub-Neptunes than for super-Earths, suggesting a partial ex situ formation of the former and an origin of the radius valley caused in part by distinct formation pathways. However, the model comparisons also show that sub-Neptunes in Kepler multiple systems are not likely (~2σ) to all be water-rich planets born ex situ but a mixture of the two (in situ and ex situ) pathways. Whereas, Kepler super-Earth planets are predominantly composed of water-poor planets that were born inside the ice line, likely through a series of giant impacts without large-scale migration.


(1677)Vertical shear instability with dust evolution and consistent cooling times. On the importance of the initial dust distribution
  • Thomas Pfeil,
  • Til Birnstiel,
  • Hubert Klahr
Astronomy and Astrophysics (07/2024) doi:10.1051/0004-6361/202449323
abstract + abstract -

Context. Gas in protoplanetary disks mostly cools via thermal accommodation with dust particles. Thermal relaxation is thus highly sensitive to the local dust size distributions and the spatial distribution of the grains. So far, the interplay between thermal relaxation and gas turbulence has not been dynamically modeled in hydrodynamic simulations of protoplanetary disks with dust.
Aims: We aim to study the effects of the vertical shear instability (VSI) on the thermal relaxation times, and vice versa. We are particularly interested in the influence of the initial dust grain size on the VSI and whether the emerging turbulence is sustained over long timescales.
Methods: We ran three axisymmetric hydrodynamic simulations of a protoplanetary disk including four dust fluids that initially resemble MRN size distributions of different initial grain sizes. From the local dust densities, we calculated the thermal accommodation timescale of dust and gas and used the result as the thermal relaxation time of the gas in our simulation. We included the effect of dust growth by applying the monodisperse dust growth rate and the typical growth limits.
Results: We find that the emergence of the VSI is strongly dependent on the initial dust grain size. Coagulation also counteracts the emergence of hydrodynamic turbulence in our simulations, as shown by others before. Starting a simulation with larger grains (100 μm) generally leads to a less turbulent outcome. While the inner disk regions (within ∼70 au) develop turbulence in all three simulations, we find that the simulations with larger particles do not develop VSI in the outer disk.
Conclusions: Our simulations with dynamically calculated thermal accommodation times based on the drifting and settling dust distribution show that the VSI, once developed in a disk, can be sustained over long timescales, even if grain growth is occurring. The VSI corrugates the dust layer and even diffuses the smaller grains into the upper atmosphere, where they can cool the gas. Whether the instability can emerge for a specific stratification depends on the initial dust grain sizes and the initial dust scale height. If the grains are initially ≳100 μm and if the level of turbulence is initially assumed to be low, we find no VSI turbulence in the outer disk regions.


(1676)A String Theoretic Derivation of Gibbons-Hawking Entropy
  • Gia Dvali
abstract + abstract -

We describe an attempt of string theoretic derivation of the Gibbons-Hawking entropy. Despite not admitting a de Sitter vacuum, the string theory, by the power of open-close correspondence, captures the Gibbons-Hawking entropy as the entropy of Chan-Paton species on a de Sitter-like state obtained via $D$-branes. Moreover, this derivation sheds a new light at the origin of the area-form, since the equality takes place for a critical 't Hooft coupling for which the species entropy of open strings saturates the area-law unitarity bound.


(1675)FROST-CLUSTERS - I. Hierarchical star cluster assembly boosts intermediate-mass black hole formation
  • Antti Rantala,
  • Thorsten Naab,
  • Natalia Lahén
Monthly Notices of the Royal Astronomical Society (07/2024) doi:10.1093/mnras/stae1413
abstract + abstract -

Observations and high-resolution hydrodynamical simulations indicate that massive star clusters assemble hierarchically from subclusters with a universal power-law cluster mass function. We study the consequences of such assembly for the formation of intermediate-mass black holes (IMBHs) at low metallicities (Z = 0.01 Z) with our updated N-body code BIFROST based on the hierarchical fourth-order forward integrator. BIFROST integrates few-body systems using secular and regularized techniques including post-Newtonian equations of motion up to order PN3.5 and gravitational-wave recoil kicks for BHs. Single stellar evolution is treated using the fast population synthesis code SEVN. We evolve three cluster assembly regions with Ntot = 1.70-2.35 × 106 stars following a realistic IMF in ~1000 subclusters for t = 50 Myr. IMBHs with masses up to m ~ 2200 M form rapidly mainly via the collapse of very massive stars (VMSs) assembled through repeated collisions of massive stars followed by growth through tidal disruption events and BH mergers. No IMBHs originate from the stars in the initially most massive clusters. We explain this by suppression of hard massive star binary formation at high velocity dispersions and the competition between core collapse and massive star lifetimes. Later the IMBHs form subsystems resulting in gravitational-wave BH-BH, IMBH-BH, and IMBH-IMBH mergers with a m ~ 1000 M gravitational-wave detection being the observable prediction. Our simulations indicate that the hierarchical formation of massive star clusters in metal poor environments naturally results in formation of potential seeds for supermassive black holes.


(1674)A deep-learning model for the density profiles of subhaloes in IllustrisTNG
  • Luisa Lucie-Smith,
  • Giulia Despali,
  • Volker Springel
Monthly Notices of the Royal Astronomical Society (07/2024) doi:10.1093/mnras/stae1487
abstract + abstract -

We present a machine-learning-based model for the total density profiles of subhaloes with masses $M \gtrsim 7\times 10^8\, h^{-1}{\rm M}_\odot$ in the IllustrisTNG100 simulation. The model is based on an interpretable variational encoder (IVE) which returns the independent factors of variation in the density profiles within a low-dimensional representation, as well as the predictions for the density profiles themselves. The IVE returns accurate and unbiased predictions on all radial ranges, including the outer region profile where the subhaloes experience tidal stripping; here its fit accuracy exceeds that of the commonly used Einasto profile. The IVE discovers three independent degrees of freedom in the profiles, which can be interpreted in terms of the formation history of the subhaloes. In addition to the two parameters controlling the normalization and inner shape of the profile, the IVE discovers a third parameter that accounts for the impact of tidal stripping on to the subhalo outer profile; this parameter is sensitive to the mass loss experienced by the subhalo after its infall on to its parent halo. Baryonic physics in the IllustrisTNG galaxy formation model does not impact the number of degrees of freedom identified in the profile compared to the pure dark matter expectations, nor their physical interpretation. Our newly proposed profile fit can be used in strong lensing analyses or other observational studies which aim to constrain cosmology from small-scale structures.


CN-3
RU-B
(1673)Constraints on self-interaction cross-sections of dark matter in universal bound states from direct detection
  • The CRESST Collaboration: G. Angloher,
  • S. Banik,
  • G. Benato,
  • A. Bento,
  • A. Bertolini
  • +54
  • R. Breier,
  • C. Bucci,
  • J. Burkhart,
  • E. Cipelli ,
  • L. Canonica,
  • A. D'addabbo ,
  • S. Di Lorenzo ,
  • L. Einfalt,
  • A. Erb ,
  • F.V. Feilitzsch,
  • S. Fichtinger ,
  • D. Fuchs,
  • A. Garai ,
  • V.M. Ghete,
  • P. Gorla ,
  • P.V. Guillaumon,
  • S. Gupta,
  • D. Hauff,
  • M. Ješkovský ,
  • J. Jochum,
  • M. Kaznacheeva,
  • A. Kinast ,
  • S. Kuckuk,
  • H. Kluck ,
  • H. Kraus ,
  • A. Langenkämper,
  • M. Mancuso,
  • L. Marini ,
  • B. Mauri ,
  • L. Meyer ,
  • V. Mokina,
  • M. Olmi,
  • T. Ortmann,
  • C. Pagliarone ,
  • L. Pattavina ,
  • F. Petricca ,
  • W. Potzel ,
  • P. Povinec,
  • F. Pröbst,
  • F. Pucci,
  • F. Reindl ,
  • J. Rothe,
  • K. Schäffner ,
  • J. Schieck,
  • S. Schönert,
  • C. Schwertner,
  • M. Stahlberg,
  • L. Stodolsky ,
  • C. Strandhagen ,
  • R. Strauss ,
  • I. Usherov,
  • F. Wagner,
  • V. Wagner,
  • V. Zema
  • (less)
arXiv e-prints (07/2024) e-Print:2407.04004
abstract + abstract -

Lambda- Cold Dark Matter (LambdaCDM) has been successful at explaining the large-scale structures in the universe but faces severe issues on smaller scales when compared to observations. Introducing self-interactions between dark matter particles claims to provide a solution to the small-scale issues in the LambdaCDM simulations while being consistent with the observations at large scales. The existence of the energy region in which these self-interactions between dark matter particles come close to saturating the S-wave unitarity bound can result in the formation of dark matter bound states called darkonium. In this scenario, all the low energy scattering properties are determined by a single parameter, the inverse scattering length gamma. In this work, we set bounds on gamma by studying the impact of darkonium on the observations at direct detection experiments using data from CRESST-III and XENON1T. The exclusion limits on gamma are then subsequently converted to exclusion limits on the self-interaction cross-section and compared with the constraints from astrophysics and N-body simulations.


(1672)The Galactic Bulge exploration III.: Calcium Triplet Metallicities for RR Lyrae Stars
  • Andrea Kunder,
  • Zdenek Prudil,
  • Claire Skaggs,
  • Henrique Reggiani,
  • David M. Nataf
  • +3
  • Joanne Hughes,
  • Kevin R. Covey,
  • Kathryn Devine
  • (less)
abstract + abstract -

RR Lyrae stars are excellent tracers of stellar populations for old, metal-poor components in the Milky Way Galaxy and the Local Group. Their luminosities have a metallicity-dependence, but determining spectroscopic [Fe/H] metallicities for RR Lyrae stars, especially at distances outside the solar neighbourhood, is challenging. Using 40 RRLs with metallicities derived from both Fe(II) and Fe(I) abundances, we verify the calibration between the [Fe/H] of RR Lyrae stars from the Calcium triplet. Our calibration is applied to all RR Lyrae stars with Gaia RVS spectra in Gaia DR3 as well as to 80 stars in the inner Galaxy from the BRAVA-RR survey. The co-added Gaia RVS RR Lyrae spectra provide RR Lyrae metallicities with an uncertainty of 0.25~dex, which is a factor of two improvement over the Gaia photometric RR Lyrae metallicities. Within our Galactic bulge RR Lyrae star sample, we find a dominant fraction with low energies without a prominent rotating component. Due to the large fraction of such stars, we interpret these stars as belonging to the $in-situ$ metal-poor Galactic bulge component, although we can not rule out that a fraction of these belong to an ancient accretion event such as Kraken/Heracles.


(1671)Resistively controlled primordial magnetic turbulence decay
  • A. Brandenburg,
  • A. Neronov,
  • F. Vazza
Astronomy and Astrophysics (07/2024) doi:10.1051/0004-6361/202449267
abstract + abstract -

Context. Magnetic fields generated in the early Universe undergo turbulent decay during the radiation-dominated era. The decay is governed by a decay exponent and a decay time. It has been argued that the latter is prolonged by magnetic reconnection, which depends on the microphysical resistivity and viscosity. Turbulence, on the other hand, is not usually expected to be sensitive to microphysical dissipation, which affects only very small scales.
Aims: We want to test and quantify the reconnection hypothesis in decaying hydromagnetic turbulence.
Methods: We performed high-resolution numerical simulations with zero net magnetic helicity using the PENCIL CODE with up to 20483 mesh points and relate the decay time to the Alfvén time for different resistivities and viscosities.
Results: The decay time is found to be longer than the Alfvén time by a factor that increases with increasing Lundquist number to the 1/4 power. The decay exponent is as expected from the conservation of the Hosking integral, but a timescale dependence on resistivity is unusual for developed turbulence and not found for hydrodynamic turbulence. In two dimensions, the Lundquist number dependence is shown to be leveling off above values of ≈25 000, independently of the value of the viscosity.
Conclusions: Our numerical results suggest that resistivity effects have been overestimated in earlier work. Instead of reconnection, it may be the magnetic helicity density in smaller patches that is responsible for the resistively slow decay. The leveling off at large Lundquist number cannot currently be confirmed in three dimensions.


(1670)Prospects of nuclear-coupled-dark-matter detection via correlation spectroscopy of I<SUB>2</SUB><SUP>+</SUP> and Ca<SUP>+</SUP>
  • Eric Madge,
  • Gilad Perez,
  • Ziv Meir
Physical Review D (07/2024) doi:10.1103/PhysRevD.110.015008
abstract + abstract -

The nature of dark matter (DM) and its interaction with the Standard Model (SM) is one of the biggest open questions in physics nowadays. The vast majority of theoretically motivated ultralight-DM (ULDM) models predict that ULDM couples dominantly to the SM strong/nuclear sector. This coupling leads to oscillations of nuclear parameters that are detectable by comparing clocks with different sensitivities to these nature's constants. Vibrational transitions of molecular clocks are more sensitive to a change in the nuclear parameters than the electronic transitions of atomic clocks. Here, we propose the iodine molecular ion, I2+, as a sensitive detector for such a class of ULDM models. The iodine's dense spectrum allows us to match its transition frequency to that of an optical atomic clock (Ca+) and perform correlation spectroscopy between the two clock species. With this technique, we project a few-orders-of-magnitude improvement over the most sensitive clock comparisons performed to date. We also briefly consider the robustness of the corresponding "Earth-bound" under modifications of the ZN -QCD axion model.


RU-B
(1669)Effective field theories for dark matter pairs in the early universe: center-of-mass recoil effects
  • S. Biondini,
  • N. Brambilla,
  • G. Qerimi,
  • A. Vairo
Journal of High Energy Physics (07/2024) doi:10.1007/JHEP07(2024)021
abstract + abstract -

For non-relativistic thermal dark matter, close-to-threshold effects largely dominate the evolution of the number density for most of the times after thermal freeze-out, and hence affect the cosmological relic density. A precise evaluation of the relevant interaction rates in a thermal medium representing the early universe includes accounting for the relative motion of the dark matter particles and the thermal medium. We consider a model of dark fermions interacting with a plasma of dark gauge bosons, which is equivalent to thermal QED. The temperature is taken to be smaller than the dark fermion mass and the inverse of the typical size of the dark fermion-antifermion bound states, which allows for the use of non-relativistic effective field theories. For the annihilation cross section, bound-state formation cross section, bound-state dissociation width and bound-state transition width of dark matter fermion-antifermion pairs, we compute the leading recoil effects in the reference frame of both the plasma and the center-of-mass of the fermion-antifermion pair. We explicitly verify the Lorentz transformations among these quantities. We evaluate the impact of the recoil corrections on the dark matter energy density. Our results can be directly applied to account for the relative motion of quarkonia in the quark-gluon plasma formed in heavy-ion collisions. They may be also used to precisely assess thermal effects in atomic clocks based on atomic transitions; the present work provides a first field theory derivation of time dilation for these processes in vacuum and in a medium.


(1668)Two-Higgs-doublet model matched to nonlinear effective theory
  • G. Buchalla,
  • F. König,
  • Ch. Müller-Salditt,
  • F. Pandler
Physical Review D (07/2024) doi:10.1103/PhysRevD.110.016015
abstract + abstract -

We use functional methods to match the two-Higgs-doublet model with heavy scalars in the nondecoupling regime to the appropriate nonlinear effective field theory, which takes the form of an electroweak chiral Lagrangian (HEFT). The effective Lagrangian is derived to leading order in the chiral counting. This includes the loop induced h →γ γ and h →Z γ local terms, which enter at the same chiral order as their counterparts in the Standard Model. An algorithm is presented that allows us to compute the coefficient functions to all orders in h . Some of the all-orders results are given in closed form. The parameter regimes for decoupling, nondecoupling, and alignment scenarios in the effective field theory context and some phenomenological implications are briefly discussed.


(1667)Cavity detection of gravitational waves: Where do we stand?
  • Claudio Gatti,
  • Luca Visinelli,
  • Michael Zantedeschi
Physical Review D (07/2024) doi:10.1103/PhysRevD.110.023018
abstract + abstract -

High-frequency gravitational waves (HFGWs) are predicted in various exotic scenarios involving both cosmological and astrophysical sources. These elusive signals have recently sparked the interest of a diverse community of researchers, due to the possibility of HFGW detection in the laboratory through graviton-photon conversion in strong magnetic fields. Notable examples include the redesign of the resonant cavities currently under development to detect the cosmic axion. In this work, we derive the sensitivities of some existing and planned resonant cavities to detect a HFGW background. As a concrete scenario, we consider the collective signals that originate from the merging of compact objects, such as two primordial black holes (PBHs) in the asteroid mass window. Our findings improve over existing work by explicitly discussing and quantifying the loss in the experimental reach due to the actual coherence of the source. We elucidate on the approach we adopt in relation with recent literature on the topic. Most notably, we give a recipe for the estimate of the stochastic background that focuses on the presence of the signal in the cavity at all times and showing that, in the relevant PBH mass region, the signal is dominated by coherent binary mergers.


CN-7
(1666)Inhomogeneous Kinetic Equation for Mixed Neutrinos: Tracing the Missing Energy
  • Damiano F. G. Fiorillo,
  • Georg G. Raffelt,
  • Günter Sigl
Physical Review Letters (07/2024) doi:10.1103/PhysRevLett.133.021002
abstract + abstract -

Flavor-dependent neutrino transport is described by a well-known kinetic equation for occupation-number matrices in flavor space. However, in the context of fast flavor conversion, we identify an unforeseen predicament: the pivotal self-induced exponential growth of small inhomogeneities strongly violates conservation of neutrino-neutrino refractive energy. We prove that it is traded with the huge reservoir of neutrino kinetic energy through gradients of neutrino flavor coherence (the off-diagonal piece of the flavor density matrix) and derive the missing gradient terms. The usual equations remain sufficient to describe flavor evolution, at the cost of renouncing energy conservation, which cannot play any role in explaining the numerically observed final state.


(1665)Hot new early dark energy bridging cosmic gaps: Supercooled phase transition reconciles stepped dark radiation solutions to the Hubble tension with BBN
  • Mathias Garny,
  • Florian Niedermann,
  • Henrique Rubira,
  • Martin S. Sloth
Physical Review D (07/2024) doi:10.1103/PhysRevD.110.023531
abstract + abstract -

We propose a simple model that can alleviate the H0 tension while remaining consistent with big bang nucleosynthesis (BBN). It is based on a dark sector described by a standard Lagrangian featuring a S U (N ) gauge symmetry with N ≥3 and a massive scalar field with a quartic coupling. The scalar acts as a dark Higgs leading to spontaneous symmetry breaking S U (N )→S U (N -1 ) via a first-order phase transition à la Coleman-Weinberg. This setup naturally realizes previously proposed scenarios featuring strongly interacting dark radiation (SIDR) with a mass threshold within hot new early dark energy. For a wide range of reasonable model parameters, the phase transition occurs between the BBN and recombination epochs and releases a sufficient amount of latent heat such that the model easily respects bounds on extra radiation during BBN while featuring a sufficient SIDR density around recombination for increasing the value of H0 inferred from the cosmic microwave background. Our model can be summarized as a natural mechanism providing two successive increases in the effective number of relativistic degrees of freedom after BBN but before recombination Δ NBBN→Δ NNEDE→Δ NIR alleviating the Hubble tension. The first step is related to the phase transition, and the second is related to the dark Higgs becoming nonrelativistic. This setup predicts further signatures, including a stochastic gravitational wave background and features in the matter power spectrum that can be searched for with future pulsar timing and Lyman-α forest measurements.


(1664)The stringy geometry of integral cohomology in mirror symmetry
  • Peng Cheng,
  • Ilarion V. Melnikov,
  • Ruben Minasian
abstract + abstract -

We examine the physical significance of torsion co-cycles in the cohomology of a projective Calabi-Yau three-fold for the (2,2) superconformal field theory (SCFT) associated to the non-linear sigma model with such a manifold as a target space. There are two independent torsion subgroups in the cohomology. While one is associated to an orbifold construction of the SCFT, the other encodes the possibility of turning on a topologically non-trivial flat gerbe for the NS-NS B-field. Inclusion of these data enriches mirror symmetry by providing a refinement of the familiar structures and points to a generalization of the duality symmetry, where the topology of the flat gerbe enters on the same footing as the topology of the underlying manifold.


(1663)Constraining the low-energy S =-2 meson-baryon interaction with two-particle correlations
  • V. Mantovani Sarti,
  • A. Feijoo,
  • I. Vidaña,
  • A. Ramos,
  • F. Giacosa
  • +2
Physical Review D (07/2024) doi:10.1103/PhysRevD.110.L011505
abstract + abstract -

In this paper we present a novel method to extract information on hadron-hadron interactions using for the first time femtoscopic data to constrain the low-energy constants of a QCD effective Lagrangian. This method offers a new way to investigate the nonperturbative regime of QCD in sectors where scattering experiments are not feasible, such as the multistrange and charm ones. As an example of its application, we use the very precise K-Λ correlation function data, recently measured in p p collisions at LHC, to constrain the strangeness S =-2 meson-baryon interaction. The model obtained delivers new insights on the molecular nature of the Ξ (1620 ) and Ξ (1690 ) states.


(1662)Fast identification of transients: applying expectation maximization to neutrino data
  • M. Karl,
  • P. Eller
Journal of Cosmology and Astroparticle Physics (07/2024) doi:10.1088/1475-7516/2024/07/057
abstract + abstract -

We present a novel method for identifying transients suitable for both strong signal-dominated and background-dominated objects. By employing the unsupervised machine learning algorithm known as expectation maximization, we achieve computing time reductions of over 104 on a single CPU compared to conventional brute-force methods. Furthermore, this approach can be readily extended to analyze multiple flares. We illustrate the algorithm's application by fitting the IceCube neutrino flare of TXS 0506+056.


(1661)Contrasting observables related to the <inline-formula id="IEq1"><mml:math><mml:mrow><mml:msup><mml:mi>N</mml:mi><mml:mo>∗</mml:mo></mml:msup><mml:mrow><mml:mo stretchy="false">(</mml:mo><mml:mn>1535</mml:mn><mml:mo stretchy="false">)</mml:mo></mml:mrow
  • Hai-Peng Li,
  • Jing Song,
  • Wei-Hong Liang,
  • R. Molina,
  • E. Oset
European Physical Journal C (07/2024) doi:10.1140/epjc/s10052-024-13015-x
abstract + abstract -

In this work we compare the predictions for the scattering length and effective range of the channels <inline-formula id="IEq3"><mml:math><mml:mrow><mml:msup><mml:mi>K</mml:mi><mml:mn>0</mml:mn></mml:msup><mml:msup><mml:mi mathvariant="normal">Σ</mml:mi><mml:mo>+</mml:mo></mml:msup><mml:mo>,</mml:mo><mml:msup><mml:mi>K</mml:mi><mml:mo>+</mml:mo></mml:msup><mml:msup><mml:mi mathvariant="normal">Σ</mml:mi><mml:mn>0</mml:mn></mml:msup><mml:mo>,</mml:mo><mml:msup><mml:mi>K</mml:mi><mml:mo>+</mml:mo></mml:msup><mml:mi mathvariant="normal">Λ</mml:mi></mml:mrow></mml:math></inline-formula> and <inline-formula id="IEq4"><mml:math><mml:mrow><mml:mi>η</mml:mi><mml:mi>p</mml:mi></mml:mrow></mml:math></inline-formula>, assuming the <inline-formula id="IEq5"><mml:math><mml:mrow><mml:msup><mml:mi>N</mml:mi><mml:mo>∗</mml:mo></mml:msup><mml:mrow><mml:mo stretchy="false">(</mml:mo><mml:mn>1535</mml:mn><mml:mo stretchy="false">)</mml:mo></mml:mrow></mml:mrow></mml:math></inline-formula> state as a molecular state of these channels, or an original genuine state, made for instance from three quarks. Looking at very different scenarios, what we conclude is that the predictions of these two pictures are drastically different, to the point that we advise the measurement of these magnitudes, accessible for instance by measuring correlation functions, in order to gain much valuable information concerning the nature of this state.


(1660)The chemistry of star and planet formation with SKA
  • C. Codella,
  • L. Testi,
  • G. Umana,
  • S. Molinari,
  • E. Bianchi
abstract + abstract -

In this contribution, we aim to summarise the efforts of the Italian SKA scientific community in conducting surveys of star-forming regions within our Galaxy, in the development of astrochemical research on protostellar envelopes and disks, and in studying the planet formation process itself. The objective is dual: Firstly, to investigate the accumulation and development of dust throughout the formation of planets, and secondly, to chemically examine protoplanetary disks and protostellar envelopes by studying heavy molecules, such as chains and rings containing over seven carbon atoms, which exhibit significantly reduced strength at millimeter wavelengths.


(1659)Emergence of High-Order Deformation in Rotating Transfermium Nuclei: A Microscopic Understanding
  • F. F. Xu,
  • Y. K. Wang,
  • Y. P. Wang,
  • P. Ring,
  • P. W. Zhao
Physical Review Letters (07/2024) doi:10.1103/PhysRevLett.133.022501
abstract + abstract -

The rotational properties of the transfermium nuclei are investigated in the full deformation space by implementing a shell-model-like approach in the cranking covariant density functional theory on a three-dimensional lattice, where the pairing correlations, deformations, and moments of inertia are treated in a microscopic and self-consistent way. The kinematic and dynamic moments of inertia of the rotational bands observed in the transfermium nuclei No 252 , No 254 , Rf 254 , and Rf 256 are well reproduced without any adjustable parameters using a well-determined universal density functional. It is found for the first time that the emergence of the octupole deformation should be responsible for the significantly different rotational behavior observed in No 252 and No 254 . The present results provide a microscopic solution to the long-standing puzzle on the rotational behavior in No isotopes, and highlight the risk of investigating only the hexacontetrapole (β60) deformation effects in rotating transfermium nuclei without considering the octupole deformation.


(1658)Interpretable correlator Transformer for image-like quantum matter data
  • Abhinav Suresh,
  • Henning Schlömer,
  • Baran Hashemi,
  • Annabelle Bohrdt
abstract + abstract -

Due to their inherent capabilities of capturing non-local dependencies, Transformer neural networks have quickly been established as the paradigmatic architecture for large language models and image processing. Next to these traditional applications, machine learning methods have also been demonstrated to be versatile tools in the analysis of image-like data of quantum phases of matter, e.g. given snapshots of many-body wave functions obtained in ultracold atom experiments. While local correlation structures in image-like data of physical systems can reliably be detected, identifying phases of matter characterized by global, non-local structures with interpretable machine learning methods remains a challenge. Here, we introduce the correlator Transformer (CoTra), which classifies different phases of matter while at the same time yielding full interpretability in terms of physical correlation functions. The network's underlying structure is a tailored attention mechanism, which learns efficient ways to weigh local and non-local correlations for a successful classification. We demonstrate the versatility of the CoTra by detecting local order in the Heisenberg antiferromagnet, and show that local gauge constraints in one- and two-dimensional lattice gauge theories can be identified. Furthermore, we establish that the CoTra reliably detects non-local structures in images of correlated fermions in momentum space (Cooper pairs) and that it can distinguish percolating from non-percolating images.


(1657)First Scan Search for Dark Photon Dark Matter with a Tunable Superconducting Radio-Frequency Cavity
  • Zhenxing Tang,
  • Bo Wang,
  • Yifan Chen,
  • Yanjie Zeng,
  • Chunlong Li
  • +14
  • Yuting Yang,
  • Liwen Feng,
  • Peng Sha,
  • Zhenghui Mi,
  • Weimin Pan,
  • Tianzong Zhang,
  • Yirong Jin,
  • Jiankui Hao,
  • Lin Lin,
  • Fang Wang,
  • Huamu Xie,
  • Senlin Huang,
  • Jing Shu,
  • Shanhe Collaboration
  • (less)
Physical Review Letters (07/2024) doi:10.1103/PhysRevLett.133.021005
abstract + abstract -

Dark photons have emerged as promising candidates for dark matter, and their search is a top priority in particle physics, astrophysics, and cosmology. We report the first use of a tunable niobium superconducting radio-frequency cavity for a scan search of dark photon dark matter with innovative data analysis techniques. We mechanically adjusted the resonant frequency of a cavity submerged in liquid helium at a temperature of 2 K, and scanned the dark photon mass over a frequency range of 1.37 MHz centered at 1.3 GHz. Our study leveraged the superconducting radio-frequency cavity's remarkably high quality factors of approximately 1010, resulting in the most stringent constraints to date on a substantial portion of the exclusion parameter space on the kinetic mixing coefficient ε between dark photons and electromagnetic photons, yielding a value of ε <2.2 ×10-16.


(1656)Soft-photon spectra and the Low-Burnett-Kroll theorem
  • R. Balsach,
  • D. Bonocore,
  • A. Kulesza
Physical Review D (07/2024) doi:10.1103/PhysRevD.110.016029
abstract + abstract -

The study of next-to-leading-power (NLP) corrections in soft emissions continues to attract interest both in quantum chromodynamics (QCD) and in quantum electrodynamics (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 nonradiative 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 nonradiative 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.


(1655)Self-consistent sharp interface theory of active condensate dynamics
  • Andriy Goychuk,
  • Leonardo Demarchi,
  • Ivan Maryshev,
  • Erwin Frey
Physical Review Research (07/2024) doi:10.1103/PhysRevResearch.6.033082
abstract + abstract -

Biomolecular condensates help organize the cell cytoplasm and nucleoplasm into spatial compartments with different chemical compositions. A key feature of such compositional patterning is the local enrichment of enzymatically active biomolecules which, after transient binding via molecular interactions, catalyze reactions among their substrates. Thereby, biomolecular condensates provide a spatial template for nonuniform concentration profiles of substrates. In turn, the concentration profiles of substrates, and their molecular interactions with enzymes, drive enzyme fluxes which can enable novel nonequilibrium dynamics. To analyze this generic class of systems, with a current focus on self-propelled droplet motion, we here develop a self-consistent sharp interface theory. In our theory, we diverge from the usual bottom-up approach, which involves calculating the dynamics of concentration profiles based on a given chemical potential gradient. Instead, reminiscent of control theory, we take the reverse approach by deriving the chemical potential profile and enzyme fluxes required to maintain a desired condensate form and dynamics. The chemical potential profile and currents of enzymes come with a corresponding power dissipation rate, which allows us to derive a thermodynamic consistency criterion for the passive part of the system (here, reciprocal enzyme-enzyme interactions). As a first-use case of our theory, we study the role of reciprocal interactions, where the transport of substrates due to reactions and diffusion is, in part, compensated by redistribution due to molecular interactions. More generally, our theory applies to mass-conserved active matter systems with moving phase boundaries.


(1654)Search for axion dark matter with the QUAX-LNF tunable haloscope
  • A. Rettaroli,
  • D. Alesini,
  • D. Babusci,
  • C. Braggio,
  • G. Carugno
  • +16
  • D. D'Agostino,
  • A. D'Elia,
  • D. Di Gioacchino,
  • R. Di Vora,
  • P. Falferi,
  • U. Gambardella,
  • A. Gardikiotis,
  • C. Gatti,
  • C. Ligi,
  • A. Lombardi,
  • G. Maccarrone,
  • A. Ortolan,
  • G. Ruoso,
  • S. Tocci,
  • G. Vidali,
  • QUAX Collaboration
  • (less)
Physical Review D (07/2024) doi:10.1103/PhysRevD.110.022008
abstract + abstract -

We report the first experimental results obtained with the new haloscope of the QUAX experiment located at Laboratori Nazionali di Frascati of INFN (LNF). The haloscope is composed of a OFHC Cu resonant cavity cooled down to about 30 mK and immersed in a magnetic field of 8 T. The cavity frequency was varied in a 6 MHz range between 8.831496 and 8.83803 GHz. This corresponds to a previously unprobed mass range between 36.52413 and 36.5511 μ eV . We don't observe any excess in the power spectrum and set limits on the axion-photon coupling in this mass range down to ga γ γ<0.882 ×10-13 GeV-1 with the confidence level set to 90%.


(1653)Novel parton density determination code
  • Francesca Capel,
  • Ritu Aggarwal,
  • Michiel Botje,
  • Allen Caldwell,
  • Oliver Schulz
  • +1
Physical Review D (07/2024) doi:10.1103/PhysRevD.110.014024
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 dataset.


(1652)Probing light dark matter through cosmic-ray cooling in active galactic nuclei
  • Gonzalo Herrera,
  • Kohta Murase
Physical Review D (07/2024) doi:10.1103/PhysRevD.110.L011701
abstract + abstract -

Recent observations of high-energy neutrinos from active galactic nuclei (AGN), NGC 1068 and TXS 0506 +056 , suggest that cosmic rays (CRs) are accelerated in the vicinity of the central supermassive black hole and high-energy protons and electrons can cool efficiently via interactions with ambient photons and gas. The dark matter density may be significantly enhanced near the black hole, and CRs could lose energies predominantly due to scatterings with the ambient dark matter particles. We propose CR cooling in AGN as a new probe of dark matter-proton and dark matter-electron scatterings. Under plausible astrophysical assumptions, our constraints on sub-GeV dark matter can be the strongest derived to date. Some of the parameter space favored by thermal light dark matter models might already be probed with current multimessenger observations of AGN.


(1651)Dianoga SIDM: Galaxy cluster self-interacting dark matter simulations
  • A. Ragagnin,
  • M. Meneghetti,
  • F. Calura,
  • G. Despali,
  • K. Dolag
  • +3
  • M. S. Fischer,
  • C. Giocoli,
  • L. Moscardini
  • (less)
Astronomy and Astrophysics (07/2024) doi:10.1051/0004-6361/202449872
abstract + abstract -

Context. Self-interacting dark matter (SIDM) can tackle or alleviate small-scale issues within the cosmological standard model ΛCDM, and diverse flavours of SIDM can produce unique astrophysical predictions, resulting in different possible signatures which can be used to test these models with dedicated observations of galaxy clusters.
Aims: This work aims to assess the impact of dark matter self-interactions on the properties of galaxy clusters. In particular, the goal is to study the angular dependence of the cross section by testing rare (large angle scattering) and frequent (small angle scattering) SIDM models with velocity-dependent cross sections.
Methods: We re-simulated six galaxy cluster zoom-in initial conditions with a dark matter-only run and with full-physics set-up simulations that include a self-consistent treatment of baryon physics. We tested the dark matter-only setup and the full physics setup with the collisionless cold dark matter, rare self-interacting dark matter, and frequent self-interacting dark matter models. We then studied their matter density profiles as well as their subhalo population.
Results: Our dark matter-only SIDM simulations agree with theoretical models, and when baryons are included in simulations, our SIDM models substantially increase the central density of galaxy cluster cores compared to full-physics simulations using collisionless dark matter. SIDM subhalo suppression in full-physics simulations is milder compared to the one found in the dark matter-only simulations because of the cuspier baryonic potential that prevents subhalo disruption. Moreover, SIDM with small-angle scattering significantly suppresses a larger number of subhaloes compared to large-angle scattering SIDM models. Additionally, SIDM models generate a broader range of subhalo concentration values, including a tail of more diffuse subhaloes in the outskirts of galaxy clusters and a population of more compact subhaloes in the cluster cores.


(1650)Emergence of R<SUP>4</SUP>-terms in M-theory
  • Ralph Blumenhagen,
  • Niccolò Cribiori,
  • Aleksandar Gligovic,
  • Antonia Paraskevopoulou
Journal of High Energy Physics (07/2024) doi:10.1007/JHEP07(2024)018
abstract + abstract -

It has been recently suggested that the strong Emergence Proposal is realized in M-theory limits by integrating out all light towers of states with a typical mass scale not larger than the species scale, i.e. the eleventh dimensional Planck mass. Within the BPS sector, these are transverse M2- and M5-branes, that can be wrapped and particle-like, carrying Kaluza-Klein momentum along the compact directions. We provide additional evidence for this picture by revisiting and investigating further the computation of R4-interactions in M-theory à la Green-Gutperle-Vanhove. A central aspect is a novel UV-regularization of Schwinger-like integrals, whose actual meaning and power we clarify by first applying it to string perturbation theory. We consider then toroidal compactifications of M-theory and provide evidence that integrating out all light towers of states via Schwinger-like integrals thus regularized yields the complete result for R4-interactions. In particular, this includes terms that are tree-level, one-loop and space-time instanton corrections from the weakly coupled point of view. Finally, we comment on the conceptual difference of our approach to earlier closely related work by Kiritsis-Pioline and Obers-Pioline, leading to a correspondence between two types of constrained Eisenstein series.


CN-4
RU-C
(1649)SPT-SZ MCMF: an extension of the SPT-SZ catalogue over the DES region
  • M. Klein,
  • J. J. Mohr,
  • S. Bocquet,
  • M. Aguena,
  • S. W. Allen
  • +102
  • O. Alves,
  • B. Ansarinejad,
  • M. L. N. Ashby,
  • D. Bacon,
  • M. Bayliss,
  • B. A. Benson,
  • L. E. Bleem,
  • M. Brodwin,
  • D. Brooks,
  • E. Bulbul,
  • D. L. Burke,
  • R. E. A. Canning,
  • J. E. Carlstrom,
  • A. Carnero Rosell,
  • J. Carretero,
  • C. L. Chang,
  • C. Conselice,
  • M. Costanzi,
  • A. T. Crites,
  • L. N. da Costa,
  • M. E. S. Pereira,
  • T. M. Davis,
  • J. De Vicente,
  • S. Desai,
  • T. de Haan,
  • M. A. Dobbs,
  • P. Doel,
  • I. Ferrero,
  • A. M. Flores,
  • J. Frieman,
  • E. M. George,
  • G. Giannini,
  • M. D. Gladders,
  • A. H. Gonzalez,
  • S. Grandis,
  • D. Gruen,
  • R. A. Gruendl,
  • G. Gutierrez,
  • N. W. Halverson,
  • S. R. Hinton,
  • G. P. Holder,
  • D. L. Hollowood,
  • W. L. Holzapfel,
  • K. Honscheid,
  • J. D. Hrubes,
  • N. Huang,
  • D. J. James,
  • G. Khullar,
  • K. Kim,
  • L. Knox,
  • R. Kraft,
  • F. Kéruzoré,
  • A. T. Lee,
  • D. Luong-Van,
  • G. Mahler,
  • A. Mantz,
  • D. P. Marrone,
  • J. L. Marshall,
  • M. McDonald,
  • J. J. McMahon,
  • J. Mena-Fernández,
  • F. Menanteau,
  • S. S. Meyer,
  • R. Miquel,
  • J. Myles,
  • S. Padin,
  • A. Pieres,
  • A. A. Plazas Malagón,
  • C. Pryke,
  • C. L. Reichardt,
  • K. Reil,
  • J. Roberson,
  • A. K. Romer,
  • C. Romero,
  • J. E. Ruhl,
  • B. R. Saliwanchik,
  • L. Salvati,
  • E. Sanchez,
  • A. Saro,
  • K. K. Schaffer,
  • T. Schrabback,
  • M. Schubnell,
  • I. Sevilla-Noarbe,
  • K. Sharon,
  • E. Shirokoff,
  • M. Smith,
  • T. Somboonpanyakul,
  • B. Stalder,
  • S. A. Stanford,
  • A. A. Stark,
  • V. Strazzullo,
  • E. Suchyta,
  • M. E. C. Swanson,
  • G. Tarle,
  • C. To,
  • K. Vanderlinde,
  • J. D. Vieira,
  • A. von der Linden,
  • N. Weaverdyck,
  • R. Williamson,
  • P. Wiseman,
  • M. Young
  • (less)
Monthly Notices of the Royal Astronomical Society (07/2024) doi:10.1093/mnras/stae1359
abstract + abstract -

We present an extension to a Sunyaev-Zel'dovich Effect (SZE) selected cluster catalogue based on observations from the South Pole Telescope (SPT); this catalogue extends to lower signal to noise than the previous SPT-SZ catalogue and therefore includes lower mass clusters. Optically derived redshifts, centres, richnesses, and morphological parameters together with catalogue contamination and completeness statistics are extracted using the multicomponent matched filter (MCMF) algorithm applied to the S/N > 4 SPT-SZ candidate list and the Dark Energy Survey (DES) photometric galaxy catalogue. The main catalogue contains 811 sources above S/N = 4, has 91 per cent purity, and is 95 per cent complete with respect to the original SZE selection. It contains in total 50 per cent more clusters and twice as many clusters above z = 0.8 in comparison to the original SPT-SZ sample. The MCMF algorithm allows us to define subsamples of the desired purity with traceable impact on catalogue completeness. As an example, we provide two subsamples with S/N > 4.25 and S/N > 4.5 for which the sample contamination and cleaning-induced incompleteness are both as low as the expected Poisson noise for samples of their size. The subsample with S/N > 4.5 has 98 per cent purity and 96 per cent completeness and is part of our new combined SPT cluster and DES weak-lensing cosmological analysis. We measure the number of false detections in the SPT-SZ candidate list as function of S/N, finding that it follows that expected from assuming Gaussian noise, but with a lower amplitude compared to previous estimates from simulations.


(1648)Euclid preparation. XLI. Galaxy power spectrum modelling in real space
  • Euclid Collaboration,
  • A. Pezzotta,
  • C. Moretti,
  • M. Zennaro,
  • A. Moradinezhad Dizgah
  • +244
  • M. Crocce,
  • E. Sefusatti,
  • I. Ferrero,
  • K. Pardede,
  • A. Eggemeier,
  • A. Barreira,
  • R. E. Angulo,
  • M. Marinucci,
  • B. Camacho Quevedo,
  • S. de la Torre,
  • D. Alkhanishvili,
  • M. Biagetti,
  • M. -A. Breton,
  • E. Castorina,
  • G. D'Amico,
  • V. Desjacques,
  • M. Guidi,
  • M. Kärcher,
  • A. Oddo,
  • M. Pellejero Ibanez,
  • C. Porciani,
  • A. Pugno,
  • J. Salvalaggio,
  • E. Sarpa,
  • A. Veropalumbo,
  • Z. Vlah,
  • A. Amara,
  • S. Andreon,
  • N. Auricchio,
  • M. Baldi,
  • S. Bardelli,
  • R. Bender,
  • C. Bodendorf,
  • D. Bonino,
  • E. Branchini,
  • M. Brescia,
  • J. Brinchmann,
  • S. Camera,
  • V. Capobianco,
  • C. Carbone,
  • V. F. Cardone,
  • J. Carretero,
  • S. Casas,
  • F. J. Castander,
  • M. Castellano,
  • S. Cavuoti,
  • A. Cimatti,
  • G. Congedo,
  • C. J. Conselice,
  • L. Conversi,
  • Y. Copin,
  • L. Corcione,
  • F. Courbin,
  • H. M. Courtois,
  • A. Da Silva,
  • H. Degaudenzi,
  • A. M. Di Giorgio,
  • J. Dinis,
  • X. Dupac,
  • S. Dusini,
  • A. Ealet,
  • M. Farina,
  • S. Farrens,
  • P. Fosalba,
  • M. Frailis,
  • E. Franceschi,
  • S. Galeotta,
  • B. Gillis,
  • C. Giocoli,
  • B. R. Granett,
  • A. Grazian,
  • F. Grupp,
  • L. Guzzo,
  • S. V. H. Haugan,
  • F. Hormuth,
  • A. Hornstrup,
  • K. Jahnke,
  • B. Joachimi,
  • E. Keihänen,
  • S. Kermiche,
  • A. Kiessling,
  • M. Kilbinger,
  • T. Kitching,
  • B. Kubik,
  • M. Kunz,
  • H. Kurki-Suonio,
  • S. Ligori,
  • P. B. Lilje,
  • V. Lindholm,
  • I. Lloro,
  • E. Maiorano,
  • O. Mansutti,
  • O. Marggraf,
  • K. Markovic,
  • N. Martinet,
  • F. Marulli,
  • R. Massey,
  • E. Medinaceli,
  • Y. Mellier,
  • M. Meneghetti,
  • E. Merlin,
  • G. Meylan,
  • M. Moresco,
  • L. Moscardini,
  • E. Munari,
  • S. -M. Niemi,
  • C. Padilla,
  • S. Paltani,
  • F. Pasian,
  • K. Pedersen,
  • W. J. Percival,
  • V. Pettorino,
  • S. Pires,
  • G. Polenta,
  • J. E. Pollack,
  • M. Poncet,
  • L. A. Popa,
  • L. Pozzetti,
  • F. Raison,
  • A. Renzi,
  • J. Rhodes,
  • G. Riccio,
  • E. Romelli,
  • M. Roncarelli,
  • E. Rossetti,
  • R. Saglia,
  • D. Sapone,
  • B. Sartoris,
  • P. Schneider,
  • T. Schrabback,
  • A. Secroun,
  • G. Seidel,
  • M. Seiffert,
  • S. Serrano,
  • C. Sirignano,
  • G. Sirri,
  • L. Stanco,
  • C. Surace,
  • P. Tallada-Crespí,
  • A. N. Taylor,
  • I. Tereno,
  • R. Toledo-Moreo,
  • F. Torradeflot,
  • I. Tutusaus,
  • E. A. Valentijn,
  • L. Valenziano,
  • T. Vassallo,
  • Y. Wang,
  • J. Weller,
  • G. Zamorani,
  • J. Zoubian,
  • E. Zucca,
  • A. Biviano,
  • E. Bozzo,
  • C. Burigana,
  • C. Colodro-Conde,
  • D. Di Ferdinando,
  • G. Mainetti,
  • M. Martinelli,
  • N. Mauri,
  • Z. Sakr,
  • V. Scottez,
  • M. Tenti,
  • M. Viel,
  • M. Wiesmann,
  • Y. Akrami,
  • V. Allevato,
  • S. Anselmi,
  • C. Baccigalupi,
  • M. Ballardini,
  • F. Bernardeau,
  • A. Blanchard,
  • S. Borgani,
  • S. Bruton,
  • R. Cabanac,
  • A. Cappi,
  • C. S. Carvalho,
  • G. Castignani,
  • T. Castro,
  • G. Cañas-Herrera,
  • K. C. Chambers,
  • S. Contarini,
  • A. R. Cooray,
  • J. Coupon,
  • S. Davini,
  • G. De Lucia,
  • G. Desprez,
  • S. Di Domizio,
  • H. Dole,
  • A. Díaz-Sánchez,
  • J. A. Escartin Vigo,
  • S. Escoffier,
  • P. G. Ferreira,
  • F. Finelli,
  • L. Gabarra,
  • K. Ganga,
  • J. García-Bellido,
  • F. Giacomini,
  • G. Gozaliasl,
  • A. Hall,
  • S. Ilić,
  • S. Joudaki,
  • J. J. E. Kajava,
  • V. Kansal,
  • C. C. Kirkpatrick,
  • L. Legrand,
  • A. Loureiro,
  • J. Macias-Perez,
  • M. Magliocchetti,
  • F. Mannucci,
  • R. Maoli,
  • C. J. A. P. Martins,
  • S. Matthew,
  • L. Maurin,
  • R. B. Metcalf,
  • M. Migliaccio,
  • P. Monaco,
  • G. Morgante,
  • S. Nadathur,
  • Nicholas A. Walton,
  • L. Patrizii,
  • V. Popa,
  • D. Potter,
  • A. Pourtsidou,
  • M. Pöntinen,
  • I. Risso,
  • P. -F. Rocci,
  • M. Sahlén,
  • A. G. Sánchez,
  • A. Schneider,
  • M. Sereno,
  • P. Simon,
  • A. Spurio Mancini,
  • J. Steinwagner,
  • G. Testera,
  • R. Teyssier,
  • S. Toft,
  • S. Tosi,
  • A. Troja,
  • M. Tucci,
  • J. Valiviita,
  • D. Vergani,
  • G. Verza,
  • P. Vielzeuf
  • (less)
Astronomy and Astrophysics (07/2024) doi:10.1051/0004-6361/202348939
abstract + abstract -

We investigate the accuracy of the perturbative galaxy bias expansion in view of the forthcoming analysis of the Euclid spectroscopic galaxy samples. We compare the performance of a Eulerian galaxy bias expansion using state-of-the-art prescriptions from the effective field theory of large-scale structure (EFTofLSS) with a hybrid approach based on Lagrangian perturbation theory and high-resolution simulations. These models are benchmarked against comoving snapshots of the flagship I N-body simulation at z = (0.9, 1.2, 1.5, 1.8), which have been populated with Hα galaxies leading to catalogues of millions of objects within a volume of about 58 h−3 Gpc3. Our analysis suggests that both models can be used to provide a robust inference of the parameters (h, ωc) in the redshift range under consideration, with comparable constraining power. We additionally determine the range of validity of the EFTofLSS model in terms of scale cuts and model degrees of freedom. From these tests, it emerges that the standard third-order Eulerian bias expansion - which includes local and non-local bias parameters, a matter counter term, and a correction to the shot-noise contribution - can accurately describe the full shape of the real-space galaxy power spectrum up to the maximum wavenumber of kmax = 0.45 h Mpc−1, and with a measurement precision of well below the percentage level. Fixing either of the tidal bias parameters to physically motivated relations still leads to unbiased cosmological constraints, and helps in reducing the severity of projection effects due to the large dimensionality of the model. We finally show how we repeated our analysis assuming a volume that matches the expected footprint of Euclid, but without considering observational effects, such as purity and completeness, showing that we can get constraints on the combination (h, ωc) that are consistent with the fiducial values to better than the 68% confidence interval over this range of scales and redshifts.


(1647)The impact of overshoot on the i-process in AGB stars
  • B. A. Remple,
  • T. Battich,
  • A. Weiss
Astronomy and Astrophysics (07/2024) doi:10.1051/0004-6361/202449821
abstract + abstract -

Context. The production of neutron-rich elements at neutron densities intermediate to those of the s- and r-processes, the so-called i-process, has been identified as possibly being responsible for the observed abundance pattern found in certain carbon-enhanced metal-poor (CEMP) stars. The production site may be low-metallicity stars on the asymptotic giant branch (AGB) where the physical processes during the thermal pulses are not well known.
Aims: We investigate the impact of overshoot from various convective boundaries during the AGB phase on proton ingestion events (PIEs) and the neutron densities as a necessary precondition for the i-process as well as on the structure and continued evolution of the models.
Methods: We therefore analyzed models of a 1.2 M, Z = 5 × 10−5 star. A fiducial model without overshoot on the AGB (overshoot was applied during the pre-AGB evolution) serves as a reference. The same model was then run with various overshoot values and the resulting models were compared to one another. Light element nucleosynthesis is also discussed. Additionally, we introduce a new timescale argument to predict PIE occurrence to discriminate between a physical and a numerical reason for a nonoccurrence. A comparison to observations as well as previous studies was conducted before finally presenting the most promising choice of overshoot parameters for the occurrence of the i-process in low-mass, low-metallicity models.
Results: The fiducial model reveals high neutron densities and a persistent split of the pulse-driven convection zone (PDCZ). Overshoot from the PDCZ results in either temporary or permanent remerging of the split PDCZ, influencing the star's structure and evolution. While both overshoot and non-overshoot models exhibit PIEs generating neutron densities suitable for the i-process, they lead to varied C/O and N/O ratios and notable Li enhancements. Comparison with previous studies and observations of CEMP-r/s stars suggests that while surface enhancements in our models may be exaggerated, abundance ratios align well. Though, for high values of overshoot from the PDCZ the agreement becomes worse.


(1646)Merge and strip: Dark matter-free dwarf galaxies in clusters can be formed by galaxy mergers
  • Anna Ivleva,
  • Rhea-Silvia Remus,
  • Lucas M. Valenzuela,
  • Klaus Dolag
Astronomy and Astrophysics (07/2024) doi:10.1051/0004-6361/202449605
abstract + abstract -

Context. Recent observations of galaxy mergers inside galaxy cluster environments, such as NGC 5291 in the vicinity of Abell 3574, report high star formation rates in the ejected tidal tails, which point towards currently developing tidal dwarf galaxies. This prompts the intriguing question whether these newly formed stellar structures could get stripped from the galaxy potential by the cluster and thus populate it with dwarf galaxies.
Aims: We verify whether environmental stripping of tidal dwarf galaxies from galaxy mergers inside galaxy cluster environments is a possible evolutionary channel to populate a galaxy cluster with low-mass and low surface brightness galaxies.
Methods: We performed three high-resolution hydrodynamical simulations of mergers between spiral galaxies in a cluster environment, implementing a stellar mass ratio of 2:1 with M200 = 9.5 × 1011 M for the more massive galaxy. Between the three different simulations, we varied the initial orbit of the infalling galaxies with respect to the cluster center.
Results: We demonstrate that cluster environments are capable of stripping tidal dwarf galaxies from the host potential independently of the infall orbit of the merging galaxy pair, without instantly destroying the tidal dwarfs. Starting to evolve separately from their progenitor, these newly formed dwarf galaxies reach total masses of Mtot ≈ 107 − 9 M within the limits of our resolution. In the three tested orbit scenarios, we find three, seven, and eight tidal dwarf galaxies per merger, respectively, which survive longer than 1 Gyr after the merger event. Exposed to ram pressure, these gas dominated dwarf galaxies exhibit high star formation rates while also losing gas to the environment. Experiencing a strong headwind due to their motion through the intracluster medium, they quickly lose momentum and start spiraling towards the cluster center, reaching distances on the order of 1 Mpc from their progenitor. About 4 Gyr after the merger event, we still find three and four intact dwarf galaxies in two of the tested scenarios, respectively. The other stripped tidal dwarf galaxies either evaporate in the hostile cluster environment due to their low initial mass, or are disrupted as soon as they reach the cluster center.
Conclusions: The dwarf production rate due to galaxy mergers is elevated when the interaction with a cluster environment is taken into account. Comparing their contribution to the observed galaxy mass function in clusters, our results indicate that ∼30% of dwarf galaxies in clusters could have been formed by stripping from galaxy mergers.

Movie associated to Fig. 3 is available at https://www.aanda.org.


(1645)LiteBIRD science goals and forecasts: primordial magnetic fields
  • D. Paoletti,
  • J. A. Rubino-Martin,
  • M. Shiraishi,
  • D. Molinari,
  • J. Chluba
  • +96
  • F. Finelli,
  • C. Baccigalupi,
  • J. Errard,
  • A. Gruppuso,
  • A. I. Lonappan,
  • A. Tartari,
  • E. Allys,
  • A. Anand,
  • J. Aumont,
  • M. Ballardini,
  • A. J. Banday,
  • R. B. Barreiro,
  • N. Bartolo,
  • M. Bersanelli,
  • M. Bortolami,
  • T. Brinckmann,
  • E. Calabrese,
  • P. Campeti,
  • A. Carones,
  • F. J. Casas,
  • K. Cheung,
  • L. Clermont,
  • F. Columbro,
  • G. Conenna,
  • A. Coppolecchia,
  • F. Cuttaia,
  • G. D'Alessandro,
  • P. de Bernardis,
  • S. Della Torre,
  • P. Diego-Palazuelos,
  • H. K. Eriksen,
  • U. Fuskeland,
  • G. Galloni,
  • M. Galloway,
  • M. Gerbino,
  • M. Gervasi,
  • T. Ghigna,
  • S. Giardiello,
  • C. Gimeno-Amo,
  • E. Gjerløw,
  • F. Grupp,
  • M. Hazumi,
  • S. Henrot-Versillé,
  • L. T. Hergt,
  • E. Hivon,
  • K. Ichiki,
  • H. Ishino,
  • K. Kohri,
  • E. Komatsu,
  • N. Krachmalnicoff,
  • L. Lamagna,
  • M. Lattanzi,
  • M. Lembo,
  • F. Levrier,
  • M. López-Caniego,
  • G. Luzzi,
  • E. Martínez-González,
  • S. Masi,
  • S. Matarrese,
  • S. Micheli,
  • M. Migliaccio,
  • M. Monelli,
  • L. Montier,
  • G. Morgante,
  • L. Mousset,
  • R. Nagata,
  • T. Namikawa,
  • P. Natoli,
  • A. Novelli,
  • I. Obata,
  • A. Occhiuzzi,
  • K. Odagiri,
  • L. Pagano,
  • A. Paiella,
  • G. Pascual-Cisneros,
  • F. Piacentini,
  • G. Piccirilli,
  • M. Remazeilles,
  • A. Ritacco,
  • M. Ruiz-Granda,
  • Y. Sakurai,
  • D. Scott,
  • S. L. Stever,
  • R. M. Sullivan,
  • Y. Takase,
  • K. Tassis,
  • L. Terenzi,
  • M. Tristram,
  • L. Vacher,
  • B. van Tent,
  • P. Vielva,
  • I. K. Wehus,
  • G. Weymann-Despres,
  • M. Zannoni,
  • Y. Zhou,
  • LiteBIRD Collaboration
  • (less)
Journal of Cosmology and Astroparticle Physics (07/2024) doi:10.1088/1475-7516/2024/07/086
abstract + abstract -

We present detailed forecasts for the constraints on the characteristics of primordial magnetic fields (PMFs) generated prior to recombination that will be obtained with the LiteBIRD satellite. The constraints are driven by some of the main physical effects of PMFs on the CMB anisotropies: the gravitational effects of magnetically-induced perturbations; the effects on the thermal and ionization history of the Universe; the Faraday rotation imprint on the CMB polarization spectra; and the non-Gaussianities induced in polarization anisotropies. LiteBIRD represents a sensitive probe for PMFs. We explore different levels of complexity, for LiteBIRD data and PMF configurations, accounting for possible degeneracies with primordial gravitational waves from inflation. By exploiting all the physical effects, LiteBIRD will be able to improve the current limit on PMFs at intermediate and large scales coming from Planck. In particular, thanks to its accurate B-mode polarization measurement, LiteBIRD will improve the constraints on infrared configurations for the gravitational effect, giving B n B=-2.9 1 Mpc< 0.8 nG at 95% C.L., potentially opening the possibility to detect nanogauss fields with high significance. We also observe a significant improvement in the limits when marginalized over the spectral index, B n Bmarg 1 Mpc< 2.2 nG at 95 % C.L. From the thermal history effect, which relies mainly on E-mode polarization data, we obtain a significant improvement for all PMF configurations, with the marginalized case, √⟨B 2marg<0.50 nG at 95 % C.L. Faraday rotation constraints will take advantage of the wide frequency coverage of LiteBIRD and the high sensitivity in B modes, improving the limits by orders of magnitude with respect to current results, B n B=-2.9 1 Mpc < 3.2 nG at 95 % C.L. Finally, non-Gaussianities of the B-mode polarization can probe PMFs at the level of 1 nG, again significantly improving the current bounds from Planck. Altogether our forecasts represent a broad collection of complementary probes based on widely tested methodologies, providing conservative limits on PMF characteristics that will be achieved with the LiteBIRD satellite.


(1644)Possible jet contribution to the γ-ray luminosity in NGC 1068
  • S. Salvatore,
  • B. Eichmann,
  • X. Rodrigues,
  • R. -J. Dettmar,
  • J. Becker Tjus
Astronomy and Astrophysics (07/2024) doi:10.1051/0004-6361/202348447
abstract + abstract -

NGC 1068 is a nearby, widely studied Seyfert II galaxy presenting radio, infrared, X-ray, and γ-ray emission, along with strong evidence for high-energy neutrino emission. Recently, the evidence for neutrino emission was explained in a multimessenger model, whereby the neutrinos originate from the corona of the active galactic nucleus. In this environment, γ-rays are strongly absorbed, so that an additional contribution is necessary, for instance, from the circumnuclear starburst ring. In this work, we discuss whether the radio jet can be an alternative source of the γ-rays between about 0.1 and 100 GeV, as observed by Fermi-LAT. In particular, we include both leptonic and hadronic processes, namely, accounting for inverse Compton emission and signatures from pp as well as pγ interactions. In order to constrain our calculations, we used VLBA and ALMA observations of the radio knot structures, which are spatially resolved at different distances from the supermassive black hole. Our results show that the best leptonic scenario for the prediction of the Fermi-LAT data is provided by the radio knot closest to the central engine. For that to be the case, a magnetic field strength of ∼1 mG is needed as well as a strong spectral softening of the relativistic electron distribution at (1 − 10) GeV. However, we show that neither such a weak magnetic field strength, nor such a strong softening is expected for that knot. A possible explanation for the ∼10 GeV γ-rays could potentially be provided by hadronic pion production in case of a gas density ≳104 cm−3. Nonetheless, this process is not found to contribute significantly to the low-energy end of the Fermi-LAT range. We conclude that the emission sites in the jet are not sufficient to explain the γ-rays across the whole Fermi-LAT energy band.


(1643)Mixing is easy: New insights for cosmochemical evolution from pre-stellar core collapse
  • Asmita Bhandare,
  • Benoît Commerçon,
  • Guillaume Laibe,
  • Mario Flock,
  • Rolf Kuiper
  • +3
  • Thomas Henning,
  • Andrea Mignone,
  • Gabriel-Dominique Marleau
  • (less)
Astronomy and Astrophysics (07/2024) doi:10.1051/0004-6361/202449594
abstract + abstract -

Context. Signposts of early planet formation are ubiquitous in substructured young discs. Dense, hot, and high-pressure regions that formed during the gravitational collapse process, integral to star formation, facilitate dynamical mixing of dust within the protostellar disc. This provides an incentive to constrain the role of gas and dust interaction and resolve potential zones of dust concentration during star and disc formation stages.
Aims: We explore whether the thermal and dynamical conditions that developed during protostellar disc formation can generate gas flows that efficiently mix and transport the well-coupled gas and dust components.
Methods: We simulated the collapse of dusty molecular cloud cores with the hydrodynamics code PLUTO augmented with radiation transport and self-gravity. We used a two-dimensional axisymmetric geometry and followed the azimuthal component of the velocity. The dust was treated as Lagrangian particles that are subject to drag from the gas, whose motion is computed on a Eulerian grid. We considered 1, 10, and 100 µm-sized neutral, spherical dust grains. Importantly, the equation of state accurately includes molecular hydrogen dissociation. We focus on molecular cloud core masses of 1 and 3 M and explore the effects of different initial rotation rates and cloud core sizes.
Results: Our study underlines mechanisms for the early transport of dust from the inner hot disc regions via the occurrence of two transient gas motions, namely meridional flow and outflow. The vortical flow fosters dynamical mixing and retention of dust, while the thermal pressure driven outflow replenishes dust in the outer disc. Notably, these phenomena occur regardless of the initial cloud core mass, size, and rotation rate.
Conclusions: Young dynamical precursors to planet-forming discs exhibit regions with complex hydrodynamical gas features and high-temperature structures. These can play a crucial role in concentrating dust for subsequent growth into protoplanets. Dust transport, especially, from sub-au scales surrounding the protostar to the outer relatively cooler parts, offers an efficient pathway for thermal reprocessing during pre-stellar core collapse.


(1642)Merging filaments II: The origin of the tuning fork
  • Elena Hoemann,
  • Andrea Socci,
  • Stefan Heigl,
  • Andreas Burkert,
  • Alvaro Hacar
Monthly Notices of the Royal Astronomical Society (07/2024) doi:10.1093/mnrasl/slae045
abstract + abstract -

We suggest that filaments in star-forming regions undergo frequent mergers. As stellar nurseries, filaments play a vital role in understanding star formation and mergers could pave the way for understanding the formation of more complex filamentary systems, such as networks and hubs. We compare the physical properties derived from hydrodynamic RAMSES simulations of merging filaments to those obtained from ALMA observations towards the LDN 1641-North region in Orion. We find similarities in the distributions of line-mass, column density, and velocity dispersion. Such common features support the hypothesis of filament mergers shaping the structure of the interstellar medium.


(1641)Detection of Fe and Ti on the dayside of the ultrahot Jupiter MASCARA-1b with CARMENES
  • B. Guo,
  • F. Yan,
  • L. Nortmann,
  • D. Cont,
  • A. Reiners
  • +18
  • E. Pallé,
  • D. Shulyak,
  • K. Molaverdikhani,
  • Th. Henning,
  • G. Chen,
  • M. Stangret,
  • S. Czesla,
  • F. Lesjak,
  • M. López-Puertas,
  • I. Ribas,
  • A. Quirrenbach,
  • J. A. Caballero,
  • P. J. Amado,
  • M. Blazek,
  • D. Montes,
  • J. C. Morales,
  • E. Nagel,
  • M. R. Zapatero Osorio
  • (less)
Astronomy and Astrophysics (07/2024) doi:10.1051/0004-6361/202449890
abstract + abstract -

Ultrahot Jupiters are a type of gaseous exoplanet that orbit extremely close to their host star, resulting in significantly high equilibrium temperatures. In recent years, high-resolution emission spectroscopy has been broadly employed in observing the atmospheres of ultrahot Jupiters. We used the CARMENES spectrograph to observe the high-resolution spectra of the dayside hemisphere of MASCARA-1b in both visible and near-infrared. Through cross-correlation analysis, we detected signals of Fe I and Ti I. Based on these detections, we conducted an atmospheric retrieval and discovered the presence of a strong inversion layer in the planet's atmosphere. The retrieved Ti and Fe abundances are broadly consistent with solar abundances. In particular, we obtained a relative abundance of [Ti/Fe] as −1.0 ± 0.8 under the free retrieval and −0.4−0.8+0.5 under the chemical equilibrium retrieval, suggesting the absence of significant titanium depletion on this planet. Furthermore, we considered the influence of planetary rotation on spectral line profiles. The resulting equatorial rotation speed was determined to be 4.4−2.0+1.6 km s−1, which agrees with the rotation speed induced by tidal locking.


(1640)Simulating the LOcal Web (SLOW). II. Properties of local galaxy clusters
  • Elena Hernández-Martínez,
  • Klaus Dolag,
  • Benjamin Seidel,
  • Jenny G. Sorce,
  • Nabila Aghanim
  • +4
  • Sergey Pilipenko,
  • Stefan Gottlöber,
  • Théo Lebeau,
  • Milena Valentini
  • (less)
Astronomy and Astrophysics (07/2024) doi:10.1051/0004-6361/202449460
abstract + abstract -

Context. This is the second paper in a series presenting the results from a 500 h−1Mpc large constrained simulation of the local Universe (SLOW). The initial conditions for this cosmological hydro-dynamical simulation are based on peculiar velocities derived from the CosmicFlows-2 catalog. The simulation follows cooling, star formation, and the evolution of super-massive black holes. This allows one to directly predict observable properties of the intracluster medium (ICM) within galaxy clusters, including X-ray luminosity, temperatures, and the Compton-y signal.
Aims: Comparing the properties of observed galaxy clusters within the local Universe with the properties of their simulated counterparts enables us to assess the effectiveness of the initial condition constraints in accurately replicating the mildly nonlinear properties of the largest, collapsed objects within the simulation.
Methods: Based on the combination of several, publicly available surveys we compiled a sample of galaxy clusters within the local Universe, of which we were able to cross-identify 46 of them with an associated counterpart within the SLOW simulation. We then derived the probability of the cross identification based on mass, X-ray luminosity, temperature, and Compton-y by comparing it to a random selection.
Results: Our set of 46 cross-identified local Universe clusters contains the 13 most massive clusters from the Planck SZ catalog as well as 70% of clusters with M500 larger than 2 × 1014 M. Compared to previous constrained simulations of the local volume, we found in SLOW a much larger amount of replicated galaxy clusters, where their simulation-based mass prediction falls within the uncertainties of the observational mass estimates. Comparing the median observed and simulated masses of our cross-identified sample allows us to independently deduce a hydrostatic mass bias of (1 − b)≈0.87.
Conclusions: The SLOW constrained simulation of the local Universe faithfully reproduces numerous fundamental characteristics of a sizable number of galaxy clusters within our local neighborhood, opening a new avenue for studying the formation and evolution of a large set of individual galaxy clusters as well as testing our understanding of physical processes governing the ICM.


(1639)Chemical evolution of the Galactic bulge with different stellar populations
  • M. Molero,
  • F. Matteucci,
  • E. Spitoni,
  • A. Rojas-Arriagada,
  • R. M. Rich
Astronomy and Astrophysics (07/2024) doi:10.1051/0004-6361/202450418
abstract + abstract -

Context. The metallicity distribution function (MDF) of the Galactic bulge is characterized by a multi-peak shape, with a metal-poor peak centered at [Fe/H] ∼ −0.3 dex and a metal-rich peak centered at [Fe/H] ∼ +0.3 dex. The bimodality of the MDF is also reflected in the [α/Fe] versus [Fe/H] abundance ratios, suggesting the presence of different stellar populations in the bulge.
Aims: In this work we aim to reproduce the observed MDF of the Galactic bulge by testing a scenario in which the metal-poor component of the bulge is formed by stars formed in situ, during a strong burst of star formation, while the metal-rich population is formed by stars created in situ during a second burst of star formation and/or stars accreted from the innermost part of the Galactic disk as an effect of a growing bar.
Methods: We adopted a chemical evolution model that is able to follow the evolution of several chemical species with detailed nucleosynthesis prescriptions. In particular, because of the importance of the production of Fe in constraining the MDF, close attention is paid to the production of this element in both Type Ia supernovae and massive stars. In particular, we included yields from rotating massive stars with different rotational velocity prescriptions. Our model also takes the infall and outflow of gas into account, as well as the effect of stellar migration. Results are compared to ∼13 000 stars from the SDSS/APOGEE survey that belong to the region located at a Galactocentric distance RGC ≤ 3.5 kpc.
Results: We successfully reproduce the observed double-peak shape of the bulge MDF as well as the abundance trends of the α elements relative to Fe by assuming both (i) a multi-burst star formation history with a quenching of the first burst of ∼102 Myr and (ii) migration of stars from the innermost part of the Milky Way disk, as an effect of a growing bar. According to our results, the fraction of the stellar mass of the bulge-bar that belongs to the inner disk is ∼40%. In terms of the nucleosynthesis, we conclude that models that assume either no rotation for massive stars or a distribution of rotational velocities that favors slow rotation at high metallicities best reproduce the observed MDF as well as the [α/Fe] and the [Ce/Fe] versus [Fe/H] abundance patterns.


(1638)Optimal Neural Summarisation for Full-Field Weak Lensing Cosmological Implicit Inference
  • Denise Lanzieri,
  • Justine Zeghal,
  • T. Lucas Makinen,
  • Alexandre Boucaud,
  • Jean-Luc Starck
  • +1
abstract + abstract -

Traditionally, weak lensing cosmological surveys have been analyzed using summary statistics motivated by their analytically tractable likelihoods, or by their ability to access higher-order information, at the cost of requiring Simulation-Based Inference (SBI) approaches. While informative, these statistics are neither designed nor guaranteed to be statistically sufficient. With the rise of deep learning, it becomes possible to create summary statistics optimized to extract the full data information. We compare different neural summarization strategies proposed in the weak lensing literature, to assess which loss functions lead to theoretically optimal summary statistics to perform full-field inference. In doing so, we aim to provide guidelines and insights to the community to help guide future neural-based inference analyses. We design an experimental setup to isolate the impact of the loss function used to train neural networks. We have developed the sbi_lens JAX package, which implements an automatically differentiable lognormal wCDM LSST-Y10 weak lensing simulator. The explicit full-field posterior obtained using the Hamilotnian-Monte-Carlo sampler gives us a ground truth to which to compare different compression strategies. We provide theoretical insight into the loss functions used in the literature and show that some do not necessarily lead to sufficient statistics (e.g. Mean Square Error (MSE)), while those motivated by information theory (e.g. Variational Mutual Information Maximization (VMIM)) can. Our numerical experiments confirm these insights and show, in our simulated wCDM scenario, that the Figure of Merit (FoM) of an analysis using neural summaries optimized under VMIM achieves 100% of the reference Omega_c - sigma_8 full-field FoM, while an analysis using neural summaries trained under MSE achieves only 81% of the same reference FoM.


(1637)Breakdown of hawking evaporation opens new mass window for primordial black holes as dark matter candidate
  • Valentin Thoss,
  • Andreas Burkert,
  • Kazunori Kohri
Monthly Notices of the Royal Astronomical Society (07/2024) doi:10.1093/mnras/stae1098
abstract + abstract -

The energy injection through Hawking evaporation has been used to put strong constraints on primordial black holes as a dark matter candidate at masses below 1017 g. However, Hawking's semiclassical approximation breaks down at latest after half-decay. Beyond this point, the evaporation could be significantly suppressed, as was shown in recent work. In this study we review existing cosmological and astrophysical bounds on primordial black holes, taking this effect into account. We show that the constraints disappear completely for a reasonable range of parameters, which opens a new window below 1010 g for light primordial black holes as a dark matter candidate.


(1636)Galaxy archaeology for wet mergers: Globular cluster age distributions in the Milky Way and nearby galaxies
  • Lucas M. Valenzuela,
  • Rhea-Silvia Remus,
  • Madeleine McKenzie,
  • Duncan A. Forbes
Astronomy and Astrophysics (07/2024) doi:10.1051/0004-6361/202348010
abstract + abstract -

Context. Identifying past wet merger activity in galaxies has been a longstanding issue in extragalactic formation history studies. Gaia's 6D kinematic measurements in our Milky Way (MW) have vastly extended the possibilities for Galactic archaeology, leading to the discovery of a multitude of early mergers in the MW's past. As recent work has established a link between younger globular clusters (GCs; less than about 10-11 Gyr old) and wet galaxy merger events, the MW provides an ideal laboratory for testing which GC properties can be used to trace extragalactic galaxy formation histories.
Aims: To test the hypothesis that GCs trace wet mergers, we relate the measured GC age distributions of the MW and three nearby galaxies, M 31, NGC 1407, and NGC 3115, to their merger histories and interpret the connection with wet mergers through an empirical model for GC formation.
Methods: The GC ages of observed galaxies are taken from a variety of studies to analyze their age distributions side-by-side with the model. For the MW, we additionally cross-match the GCs with their associated progenitor host galaxies to disentangle the connection to the GC age distribution. For the modeled GCs, we take galaxies with similar GC age distributions as observed to compare their accretion histories with those inferred through observations.
Results: We find that the MW GC age distribution is bimodal, mainly caused by younger GCs (10-11 Gyr old associated with Gaia-Sausage/Enceladus (GSE) and in part by unassociated high-energy GCs. The GSE GC age distribution also appears to be bimodal. We propose that the older GSE GCs (12-13 Gyr old) were accreted together with GSE, while the younger ones formed as a result of the merger. For the nearby galaxies, we find that clear peaks in the GC age distributions coincide with active early gas-rich merger phases. Even small signatures in the GC age distributions agree well with the expected wet formation histories of the galaxies inferred through other observed tracers. From the models, we predict that the involved cold gas mass can be estimated from the number of GCs found in the formation burst.
Conclusions: Multimodal GC age distributions can trace massive wet mergers as a result of GCs being formed through them. From the laboratory of our own MW and nearby galaxies we conclude that the ages of younger GC populations of galaxies can be used to infer the wet merger history of a galaxy.


(1635)Tracing the Milky Way spiral arms with 26Al -- The role of nova systems in the 2D distribution of 26Al
  • Arianna Vasini,
  • Emanuele Spitoni,
  • Francesca Matteucci,
  • Gabriele Cescutti,
  • Massimo della Valle
abstract + abstract -

Massive stars are one of the most important and investigated astrophysical production sites of $^{26}$Al, a short-lived radioisotope with $\sim$ 1 Myr half-life. Its short lifetime prevents us from observing its complete chemical history, and only the $^{26}$Al that was recently produced by massive stars can be observed. Hence, it is considered a tracer of star formation rate (SFR). However, important contributions to $^{26}$Al comes from nova systems that pollute the interstellar medium with a large delay, thus partly erasing the correlation between $^{26}$Al and SFR. In this work we describe the 2D distribution of the mass of $^{26}$Al as well as that of massive stars and nova systems in the Milky Way, to investigate their relative contributions to the production of $^{26}$Al. We use a detailed 2D chemical evolution model where the SFR is azimuthally dependent and is required to reproduce the spiral arm pattern observed in the Milky Way. We test two different models, one where the $^{26}$Al comes from massive stars and novae, and one with massive stars only. We then compare the predictions to the $\sim$ 2 M$_{\odot}$ of $^{26}$Al mass observed by the surveys COMPTEL and INTEGRAL. The results show that novae do not trace SFR and, in the solar vicinity, they concentrate in its minima. The effect of novae on the map of the $^{26}$Al mass consists in damping the spiral pattern by a factor of five. Regarding the nucleosynthesis, we find that $\sim$75% of the $^{26}$Al is produced by novae and the $\sim$25% by massive stars. We conclude that novae cannot be neglected as $^{26}$Al producers since the observations can only be reproduced by including their contribution. Moreover, we suggest that bulge novae should eject around six times more material than the disc ones to well reproduce the observed mass of $^{26}$Al.


(1634)Molecular complexity of young solar analogues
  • E. Bianchi,
  • M. De Simone,
  • G. Sabatini,
  • J. Frediani,
  • L. Podio
  • +1
abstract + abstract -

How does molecular complexity emerge and evolve during the process leading to the formation of a planetary system? Astrochemistry is experiencing a golden age, marked by significant advancements in the observation and understanding of the chemical processes occurring in the inner regions of protostellar systems. However, many questions remain open, such as the origin of the chemical diversity observed in the early evolutionary stages, which may influence the chemical composition of the forming planets. Additionally, astrochemistry provides us with powerful tools to investigate the accretion/ejection processes occurring in the inner regions of young embedded objects, such as jets, winds, accretion streamers, and shocks. In this chapter, we review the observational efforts carried out in recent years to chemically characterize the inner regions of Solar-System analogs. We summarize our current understanding of molecular complexity in planet-forming disks and shed light on the existing limitations and unanswered questions. Finally, we highlight the important role of future radio facilities, like SKAO and ngVLA, in exploring the chemical complexity of the regions where planetary systems are emerging.


(1633)The MillenniumTNG Project: Impact of massive neutrinos on the cosmic large-scale structure and the distribution of galaxies
  • César Hernández-Aguayo,
  • Volker Springel,
  • Sownak Bose,
  • Carlos Frenk,
  • Adrian Jenkins
  • +8
  • Monica Barrera,
  • Fulvio Ferlito,
  • Rüdiger Pakmor,
  • Simon D. M. White,
  • Lars Hernquist,
  • Ana Maria Delgado,
  • Rahul Kannan,
  • Boryana Hadzhiyska
  • (less)
abstract + abstract -

We discuss the cold dark matter plus massive neutrinos simulations of the MillenniumTNG (MTNG) project, which aim to improve understanding of how well ongoing and future large-scale galaxy surveys will measure neutrino masses. Our largest simulations, $3000\,{\rm Mpc}$ on a side, use $10240^3$ particles of mass $m_{p} = 6.66\times 10^{8}\,h^{-1}{\rm M}_\odot$ to represent cold dark matter, and $2560^3$ to represent a population of neutrinos with summed mass $M_\nu = 100\,{\rm meV}$. Smaller volume runs with $\sim 630\,{\rm Mpc}$ also include cases with $M_\nu = 0\,\textrm{and}\, 300\,{\rm meV}$. All simulations are carried out twice using the paired-and-fixed technique for cosmic variance reduction. We evolve the neutrino component using the particle-based $\delta f$ importance sampling method, which greatly reduces shot noise in the neutrino density field. In addition, we modify the GADGET-4 code to account both for the influence of relativistic and mildly relativistic components on the expansion rate and for non-Newtonian effects on the largest represented simulation scales. This allows us to quantify accurately the impact of neutrinos on basic statistical measures of nonlinear structure formation, such as the matter power spectrum and the halo mass function. We use semi-analytic models of galaxy formation to predict the galaxy population and its clustering properties as a function of summed neutrino mass, finding significant ($\sim 10\%$) impacts on the cosmic star formation rate history, the galaxy mass function, and the clustering strength. This offers the prospect of identifying combinations of summary statistics that are optimally sensitive to the neutrino mass.