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Physics Astrophysics

astro-ph Watch Astrophysics

Monday 8 December

High Energy Astrophysical Phenomena

A unified model of active repeating fast radio bursts associated with persistent radio sources

F. Y. Wang, H. T. Lan, Z. Y. Zhao et al. (+5 more)

Fast radio bursts (FRBs) are intense pulses with unknown origins. A subclass of repeating FRBs show some common features, such as associated compact persistent radio sources (PRSs), high burst rates, and large host-galaxy dispersion measures (DMs). Meanwhile, they show diverse DM and rotation measure (RM) variations, which cannot be explained by current models. A unified model urgently needs to be established. Here we show the first evidence for a supernova remnant surrounding the FRB 20190520B source. We then demonstrate that the five active repeating FRB sources associated with PRSs can be understood within a single model in which central objects are young magnetars in massive binary systems embedded in supernova remnants. This model naturally predicts distinct variations of DM and RM for repeating FRBs. Crucially, young magnetar wind nebulae can generate bright PRSs. As a magnetar becomes older, the luminosity of a PRS will fade, which can naturally explain less-luminous PRSs for some active FRBs. Our results support a unified population of active FRBs in dynamic magnetized environments.
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All authors F. Y. Wang, H. T. Lan, Z. Y. Zhao, Q. Wu, Y. Feng, S. X. Yi, Z. G. Dai, K. S. Cheng

Astrophysics of Galaxies

Statistics of the projected angles between the black-hole spin and the host-galaxy rotation axes from NewHorizon

Sebastien Peirani, Yasushi Suto, Clotilde Laigle et al. (+3 more)

Understanding the alignment between AGN jets and their host galaxies is crucial for interpreting AGN unification models, jet feedback processes, and the co-evolution of galaxies and their central black holes (BH). In this study, we use the high-resolution cosmological zoom-in simulation NewHorizon, which self-consistently evolves BH mass and spin, to statistically examine the relationship between AGN jet orientation and host galaxy structure. Building upon our previous work, we extend the analysis of projected (2-d) alignment angles to facilitate more direct comparisons with recent observational studies. In our methodology, galaxy orientations are estimated using optical position angles derived from synthetic DESI-LS and Euclid images, while BH spin vectors serve as proxies for AGN jet directions. From a carefully selected sample of 100 BH-galaxy systems at low redshift, we generate a catalog of 5,000 mock optical images using a Monte Carlo approach that samples random viewing angles and redshifts. Our results reveal a statistically significant tendency for AGN jets to align with the orientation of their host galaxies, consistent with recent observations combining Very Long Baseline Interferometry (VLBI) and optical imaging of nearby AGNs. Furthermore, we find a slightly stronger alignment when using kinematic position angles derived from synthetic MaNGA-like stellar velocity fields. These findings underscore the importance of combining morphological, kinematic, and polarimetric information to disentangle the complex interplay between black hole spin evolution, accretion mode, and the galactic environment in shaping the direction of relativistic jets.
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All authors Sebastien Peirani, Yasushi Suto, Clotilde Laigle, Yen-Ting Lin, Yohan Dubois, Sukyoung K. Yi

Cosmology and Nongalactic Astrophysics

Vision Transformers for Cosmological Fields: Application to Weak Lensing Mass Maps

Jash Kakadia, Shubh Agrawal, Kunhao Zhong et al. (+1 more)

Weak gravitational lensing is a powerful probe of the universe's growth history. While traditional two-point statistics capture only the Gaussian features of the convergence field, deep learning methods such as convolutional neural networks (CNNs) have shown promise in extracting non-Gaussian information from small-scale, nonlinear structures. In this work, we evaluate the effectiveness of attention-based architectures, including variants of vision transformers (ViTs) and shifted window (Swin) transformers, in constraining the cosmological parameters $\Omega_m$ and $S_8$ from weak lensing mass maps. Using a simulation-based inference (SBI) framework, we compare transformer-based methods to CNNs. We also examine performance scaling with the number of available $N$-body simulations, highlighting the importance of pre-training for transformer architectures. We find that the Swin transformer performs significantly better than vanilla ViTs, especially with limited training data. Despite their higher representational capacity, the Figure of Merit for cosmology achieved by transformers is comparable to that of CNNs under realistic noise conditions.
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All authors Jash Kakadia, Shubh Agrawal, Kunhao Zhong, Bhuvnesh Jain

High Energy Astrophysical Phenomena

Universal relation involving fundamental modes in two-fluid dark matter admixed neutron stars

Hajime Sotani and Ankit Kumar

We systematically investigate the fundamental oscillation frequencies of dark matter admixed neutron stars, focusing on models with self-interacting fermionic dark matter that couples to normal matter solely through gravity. The analysis is carried out within a two-fluid formalism under the relativistic Cowling approximation, where the perturbation equations follow from the linearized energy-momentum conservation laws of both components. We find that the mass-scaled fundamental frequencies of the nuclear (dark) fluid in dark core (halo) configurations exhibit a remarkably tight correlation with the total stellar compactness. This universality persists across the dark matter parameter space explored in this study and is largely insensitive to the choice of nuclear equation of state. In contrast, we also find the breakdown of such universality with the tidal deformability, i.e, the same frequencies show substantial deviations from universality when expressed in terms of the tidal deformability. These contrasting behaviors highlight possible observational imprints of dark matter in neutron star interiors.
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Cosmology and Nongalactic Astrophysics

Dynamical Dark Energy in light of DESI BAO and Full-Shape Data

Quan Zhou and Sibo Zheng

Recently, the DESI BAO data has reported a preference of dynamical dark energy (DDE) over the \LambdaCDM cosmology. Apart from the BAO data, the DDE model should be also sensitive to low-redshift measurements of the matter power spectrum data. In this study, we address this point by combining the DESI Y1 data about the matter power spectrum, extracted from the DESI Full-Shape data, with the DESI DR2 BAO data among other probes. After building the DESI Y1 likelihood, we carry out a Markov Chain Monte Carlo analysis, showing that the constraints on $w_0$ and $w_a$ with DESI Y1 data included are improved over those without it for three different datasets widely considered, especially in the case of the DESY5 sample.
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High Energy Astrophysical Phenomena

Trends in gravitational wave emission in axisymmetric simulations of rotating core-collapse supernovae

Bailey Sykes and Bernhard Müller

The quantitative impact of strong rotation on the amplitudes and frequencies of the post-bounce gravitational wave (GW) signal from core-collapse supernovae (CCSNe) is still not fully understood. To study trends in frequencies and amplitudes, and possibly spectacular phenomena like resonant amplification, we perform a series of axisymmetric long-duration magnetohydrodynamic CCSN simulations of a 17 $M_\odot$ progenitor using a finely spaced grid in initial rotation rate from 0.29 rad/s to 3.48 rad/s. We find that these rotating models produce GWs at frequencies of up to 3 kHz, higher than in typical non-rotating models in the literature. The high frequencies arise due to small polar radii of rapidly rotating proto-neutron stars and stabilization by angular momentum gradients at lower latitude. GW frequencies and amplitudes tend to decrease with faster rotation. Different from two complementary simulations without magnetic fields, the magnetohydrodynamic models are characterized by an absence of p-modes above the dominant high-frequency emission band. We find no indication of resonant mode amplification for any rotation rate, although a temporo-spatial and space-frequency analysis reveals some interesting couplings of quadrupolar motions across the proto-neutron star and the gain region. Generalized, multi-dimensional perturbative techniques need to be developed to study the mode structure and mode interaction in the collapse of rapidly rotating massive stars.
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Cosmology and Nongalactic Astrophysics

A Multi-Probe ISW Study of Dark Energy Models with Negative Energy Density: Galaxy Correlations, Lensing Bispectrum, and Planck ISW-Lensing Likelihood

Payam Ghafari, Mahdi Najafi, Mina Ghodsi Yengejeh et al. (+3 more)

We investigate the late-time imprints of three dark energy (DE) models, namely, the Chevallier-Polarski-Linder (CPL) parametrization, $\Lambda_{\rm s}$CDM, and an Omnipotent DE model, on cosmological observables sensitive to the time evolution of gravitational potentials. While CPL serves as a reference parameterization, the Omnipotent and $\Lambda_{\rm s}$CDM scenarios were originally proposed as possible solutions to the $H_0$ tension and are selected here because they can yield negative dark energy. These models are examined within a multi-probe framework based on the Integrated Sachs-Wolfe (ISW) effect and the lensing-ISW bispectrum. By analyzing both two- and three-point Cosmic Microwave Background (CMB) correlations, we assess how their late-time dynamics modify the growth and decay of large-scale gravitational potentials compared to the standard $\Lambda$CDM cosmology. Despite producing nearly indistinguishable CMB angular spectra at high multipoles, these models yield distinctive signatures in the low-$\ell$ ISW plateau as well as in higher-order statistics related to ISW, highlighting the power of both large-scale CMB anisotropies and higher-order CMB statistics in testing dark energy physics. Our results demonstrate that combining complementary ISW probes provides an effective way to discriminate between dark energy scenarios and will be crucial to determine whether negative or sign-switching dark energy is ultimately favored or disfavored by forthcoming data.
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All authors Payam Ghafari, Mahdi Najafi, Mina Ghodsi Yengejeh, Emre Özülker, Eleonora Di Valentino, Javad T. Firouzjaee

Sunday 7 December

Astrophysics of Galaxies

JWST reveals extended stellar disks for ALMA-bright dusty star-forming galaxies in the Spiderweb protocluster

Y. H. Zhang, H. Dannerbauer, J. M. Pérez-Martínez et al. (+14 more)

We present JWST/NIRCam imaging of dusty star-forming galaxies (DSFGs) detected by Atacama Large Millimeter/submillimeter Array (ALMA) in the Spiderweb protocluster at $z=2.16$. We identify 22 DSFGs detected by both ALMA and JWST, 10 of which are spectroscopically confirmed as protocluster members. This is the first systematic analysis of a statistical DSFG sample in $z\sim2$ protocluster environments using JWST/NIRCam data. Most of the DSFG members exhibit very red colors and reside in the dusty star-forming region of the rest-frame UVJ diagram, indicating strong dust obscuration. The Gini-M20 diagram suggests that most DSFGs in this protocluster are late-type disks, with a significant fraction displaying clumpy and disturbed rest-frame UV/optical morphologies, but few showing clear merger signatures. The DSFG members exhibit relatively large stellar disks and effective radii with a median stellar mass of log(M/Msun) = 10.8 +/- 0.3, placing them above coeval field DSFGs and typical protocluster galaxies in the size-mass relation at both rest-frame optical and near-infrared wavelengths. These sizes are comparable to those of more evolved field DSFGs at z~1-2, indicating accelerated structural growth in dense environments. Moreover, these DSFG members show a decreasing trend in stellar size from shorter to longer wavelengths, with a moderately steep slope comparable to coeval field DSFGs. These results may support an inside-out growth scenario for protocluster evolution, in which massive galaxies near the center are more evolved and more strongly affected by AGN feedback and environmental effects, e.g., ram-pressure stripping. We propose that the cold gas accretion at the protocluster outskirts drives intense star formation and stellar disk growth in ALMA-detected DSFGs, which are expected to evolve into massive elliptical galaxies at later stages.
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All authors Y. H. Zhang, H. Dannerbauer, J. M. Pérez-Martínez, Y. Koyama, X. Z. Zheng, R. Calvi, Z. Chen, K. Daikuhara, C. De Breuck, C. D'Eugenio, B. H. C. Emonts, S. Jin, T. Kodama, M. D. Lehnert, J. Nadolny, A. Naufal, P. G. Pérez-González

Solar and Stellar Astrophysics

Giant outbursts of clumpy material preceding Type II supernova 2024qiw

T. Nagao, H. Kuncarayakti, K. Maeda et al. (+6 more)

Observations of core-collapse supernovae suggest that some massive stars undergo intense mass loss shortly before explosion, but the underlying mechanisms remain unknown. Here we report evidence of giant outbursts of clumpy material from a massive star in the final decades before explosion. Photometric, spectroscopic, and polarimetric data of SN~2024qiw reveal a bumpy light curve, a broad H$\alpha$ profile, and variable polarization, all consistent with interaction between SN ejecta and clumpy circumstellar material, implying a mass-loss rate of $\gtrsim 10^{-2}$ M$_\odot$ yr$^{-1}$. Taken together, the most likely explanation is multiple major eruptions, similar to those of Luminous Blue Variables (LBVs), but occurring shortly before explosion. This challenges standard stellar evolution theory by requiring either that LBVs explode terminally, or that other evolutionary phases produce eruptive episodes. In spite of very high pre-SN mass loss, the resulting SN is of Type~II, rather than Type IIn, highlighting diverse and previously unrecognized late-stage mass-loss processes.
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All authors T. Nagao, H. Kuncarayakti, K. Maeda, S. Mattila, R. Kotak, T. Killestein, C. Humina, D. Steeghs, D. Jarvis

High Energy Astrophysical Phenomena

Paucity of downward UHE neutrino tracks in IceCube versus unexpected huge KM3-230213A event: solving the puzzles?

D. Fargion

Recently the ARCA array detector published the down-ward-horizontal event: the KM3-230213A. It appeared as the most energetic neutrino ever observed: about 200 PeV (2 10^17 eV) up to EeV (10^18 eV) energy. This huge value, is puzzling. It is not statistically consistent with several upper bound derived by two greater and longer life detectors: by IceCube and in particular by AUGER array. Asymmetry in recent IceCube neutrino alert tracks upward and downward at same horizontal angles as ARCA one, suggest that they are mostly polluted atmospheric muon bundles. This paucity also disfavor the skimming neutrino interpretation by ARCA. We suggest that the array floating and bending in the deep sea may lead, sometime, to a misleading geometry that is pointing to a wrong arrival angle direction: a much less horizontal muon (neutrino) track respect to a much real one, more inclined and vertical, due to atmospheric muon bundle or charmed single event. Contrary to present argument, if such a rare event would be soon rediscovered in data or re-observed, it would open the road to a new guaranteed Tau neutrino Astronomy. At EeV energy such upward tau air-showers should shine AUGER telescopes or blaze future satellite in Space. A previous model in astrophysics considered energetic neutrino E>>100 EeV, neutrino scattering, onto cosmic, relic, light mass ones. Their ultra-relativistic Z boson resonance formation and its decay in flight would produce hadron UHECR relics around tens-hundred EeV energy. Explaining how sources located at far distances, above the usual GZK hundred Mpc, cut off ones, may shine and cluster in AUGER or TA data.
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Earth and Planetary Astrophysics

Understanding the Planetary Formation and Evolution in Star Clusters(UPiC)-II: Catalog of planets/candidates in Open Clusters and Moving Groups

Yuan-Zhe Dai, Hui-Gen Liu, Xiaoying Pang et al. (+4 more)

Detecting planets in open clusters offers a unique opportunity to test planet formation theories in clustered environments. The precisely determined ages of young open clusters make their planets particularly valuable for tracing the early evolution of planetary systems. As the second paper of the UPiC project, this study focuses on stars in stellar groups that host transiting planets or planetary candidates. We categorize these stellar groups into Open Clusters (OCs) and Moving Groups (MGs) based on the Jacobi radius to investigate potential differences in their planetary systems. By cross-matching the latest star cluster catalogs with catalogs of transiting planets and candidates, we have compiled the most extensive catalog to date, containing 106 confirmed planets and 168 candidates within OCs and MGs. We refitted the structural parameters of these stellar groups and identified substructures using the HDBSCAN and Gaussian Mixture Model (GMM) algorithms. Our analysis reveals the density evolution of both MGs and OCs during their first Gyr. We find that MGs consistently exhibit a significantly higher planet fraction than OCs, regardless of sample selection, particularly for Hot Jupiters. Furthermore, exoplanet radii show a clear dichotomy at early stages: most sub-Jupiters evolve into Neptune-sized planets within 100 Myr, while super-Jupiters undergo only minimal contraction. These results suggest that young sub-Jupiters (\textless 100 Myr) represent puffy, Neptune-mass planets undergoing vigorous photoevaporation, whereas Jupiter-mass planets can maintain their atmospheres. We also report evidence for the early emergence of the hot-Neptune desert at 100 Myr in both OCs and MGs.
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All authors Yuan-Zhe Dai, Hui-Gen Liu, Xiaoying Pang, Yueyue Jiang, Jerome P. de Leon, Jing Zhong, Ji-Lin Zhou

Cosmology and Nongalactic Astrophysics

Core-halo scaling relations in self-interacting scalar field dark matter

Jessica N. López-Sánchez, Erick Munive-Villa and Tanja Rindler-Daller

We study the impact of self-interactions on the structure and evolution of scalar field dark matter (SFDM) halos. Using three-dimensional Gross-Pitaevskii-Poisson simulations of multiple soliton mergers, we explore both repulsive and attractive regimes across a wide range of scattering lengths. Our results show that repulsive self-interactions lead to more massive and extended cores with lower central densities compared to the free (non-interacting) fuzzy dark matter case, while attractive interactions enhance central densities and can drive cores toward collapse, once a critical mass is exceeded. We confirm that the mass-radius relation of solitonic cores is well described by analytical predictions, even in the presence of self-interactions, and we extend the core-halo mass relation to scenarios beyond fuzzy dark matter. We find that the scaling relations between core mass, size, and total energy are not universal but depend sensitively on the strength and sign of the self-interaction, as well as on the evolutionary stage of the halo. These results demonstrate that self-interactions provide a natural mechanism to regulate core properties, with important implications for the formation of supermassive black holes and for potential astrophysical signatures in galactic cores.
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High Energy Astrophysical Phenomena

SS433 PeV neutron jet feeding the far TeV gamma beam

Daniele Fargion, Pier Giorgio De Sanctis Lucentini, Sara Turriziani et al. (+2 more)

The SS433 is a well-known binary system with an internal black hole, which is stripping mass from an orbiting companion of ten solar masses, at a hundred of light-seconds away. The black hole and its accretion disk fuel a thin precessing jet, whose spirals are well-observed. Surprisingly, disconnected gamma-ray tails have recently been discovered by H.E.S.S., HAWC and LHAASO, hundreds of light-years away and with energies of tens of TeV. We suggest that tens PeV neutron burst jets were ejected from the SS433 system over the past century. These beams of ultra high-energy PeVatron neutrons, by their in-flight beta decay and Inverse Compton scattering, could be the source of the enigmatic, distant and disconnected tens of TeV gamma-ray beams. These ultra-relativistic PeV neutron jets could have been formed during one of the system's rare and intense tidal eruptions, when tens of PeV protons collide CV October 2025 with thermal ultraviolet photons, creating delta resonances. Their decay into secondary neutron beams of tens of PeV is well consistent with observations. Alternative models appear uncompetitive.
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All authors Daniele Fargion, Pier Giorgio De Sanctis Lucentini, Sara Turriziani, Danila Sopin, Maxim Yu. Khlopov

High Energy Astrophysical Phenomena

Over-abundant gamma-like signals around Solar disk shadows by twin bent and smeared muon and electron pairs secondaries, versus rare local TeV gamma

Daniele Fargion, Omar Tibolla, Pier Giorgio De Sanctis Lucentini et al. (+4 more)

Cosmic rays with energies of tens of TeV and above, skimming the Sun, could fragment into pions. The resulting gamma photons and muons, as well as subsequent electron pairs, will reach us in the form of gamma or electromagnetic air-showers , gamma-like air-showers on Earth. Their multiple presence may soon be observed and disentangled by the LHAASO telescope array.
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All authors Daniele Fargion, Omar Tibolla, Pier Giorgio De Sanctis Lucentini, Sara Turriziani, Sarah Kaufmann, Danila Sopin, Maxim Yu. Khlopov

High Energy Astrophysical Phenomena

Anisotropic diffusion modeling of cosmic-ray lepton propagation

V.D. Borisov and I.A. Kudryashov

We analyze DAMPE and H.E.S.S. measurements of the total cosmic-ray electron-positron spectrum, together with the AMS-02 positron fraction, using an anisotropic, spatially varying diffusion framework. The diffusion-tensor components are computed via numerical integration of test-particle trajectories in a prescribed Galactic magnetic-field model. We show that simultaneously accounting for the spatial dependence and anisotropy of the diffusion tensor yields an accurate description of the local electron and positron data up to TeV energies. The inferred injection spectral index, $\gamma=2.169$, is fully consistent with expectations from diffusive shock-acceleration theory. In this approach, the observed spectral softening arises naturally from enhanced energy losses experienced by leptons propagating over larger effective distances along the large-scale magnetic field.
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Astrophysics of Galaxies

The GLEAM 4-Jy (G4Jy) Sample: III. Further host-galaxy identification, and redshift assessment

Sarah V. White, Precious K. Sejake, Kshitij Thorat et al. (+17 more)

In this paper we present 127 new host-galaxy identifications for G4Jy sources (S_151MHz > 4 Jy), based on radio images from MeerKAT, the Very Large Array Sky Survey (VLASS), and the Rapid ASKAP (Australian Square Kilometre Array Pathfinder) Continuum Survey (RACS). This includes identifications that result from visual inspection of radio contours on K_s-band images, as opposed to the AllWISE-W1 images that were used for the original set of overlays when defining the G4Jy Sample (Papers I and II). Our aim is to achieve 100 per cent spectroscopic completeness for the sample, where all of the spectroscopy is available in digital form online. For now, we have gathered (i) digital optical spectroscopy for 34 per cent of the sample, (ii) photometric redshifts for an additional 21 per cent of the sample, and (iii) further redshifts found through the NASA/IPAC Extragalactic Database (but not recently verified). Our assessment of the redshifts includes visual inspection of all of the digital spectroscopy, and re-fitting redshift templates where necessary. The resulting redshift range is (currently) 0.0 < z < 3.6. We also present 151-MHz luminosities and linear sizes for the G4Jy Sample, based on initial analysis.
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All authors Sarah V. White, Precious K. Sejake, Kshitij Thorat, Heinz Andernach, Thomas M.O. Franzen, O. Ivy Wong, Anna D. Kapinska, Joseph R. Callingham, Christopher J. Riseley, Nick Seymour, Randall Wayth, Lister Staveley-Smith, Rajan Chhetri, Natasha Hurley-Walker, John Morgan, Paul Hancock, Francesco Massaro, Abigail Garcia-Perez, Ana Jimenez-Gallardo, Harold A. Pena-Herazo

Cosmology and Nongalactic Astrophysics

Probing memory-burdened Primordial Black Holes with global 21 cm signal

Priyanka Sarmah and Kingman Cheung

We investigate the imprints of memory-burdened primordial black holes (PBH) on the global 21 cm signal during the cosmic dawn. Recent studies reopened the possibility of a mass window of PBHs as a compelling candidate for dark matter, particularly in low-mass regimes ($M_{\text {PBH}}< 10^{15}$ g) where conventional constraints from evaporation are being revisited in light of quantum gravitational effects. One such effect, the memory burden effect, slows down black hole evaporation by incorporating the backreaction of radiation on the black hole microstates, substantially extending the lifetime of light PBHs and thus modifying their late-time emission spectra. This prolonged emission can dramatically alter the energy injection history in the early universe. By computing the modified energy injection rates into the intergalactic medium and incorporating them into the thermal and ionization evolution of neutral hydrogen, we obtain projected constraints on the fraction of dark matter. The bounds are obtained from the fact that these low mass PBHs, which were thought otherwise evaporated, can modify the absorption amplitude in the global 21-cm signal at redshift $z\approx17$. Considering the two viable scenarios of transition to the memory-burden phase: fast (or instantaneous) and slow (transition with a finite width), we show how the 21 cm bounds are sensitive to different mass ranges. For a broad transition with $\delta=10^{-2}$ we find that PBHs in the mass range $M_{\rm PBH}\simeq10^{8}$-$10^{13}$g are excluded at the level of $f_{\rm PBH}\gtrsim10^{-8}$. In contrast, for a fast-transition case with the lowest suppression exponent $k=1$, the evaporation is suppressed so efficiently that no meaningful 21\,cm constraint remains for $M_{\rm PBH}\gtrsim10^{7}$g.
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Solar and Stellar Astrophysics

Precise determination of circumstellar disk lifetimes: Disk evolution in a single star-forming region

Fabian A. Polnitzky, Sebastian Ratzenböck, Josefa E. Großschedl et al. (+1 more)

Determining how long circumstellar disks last is key to understanding the timescale of planet formation. Typically, this is done by measuring the fraction of young stars with infrared-excess, a sign of circumstellar material, in stellar clusters of different ages. However, comparing data from different star-forming regions at different distances introduces uncertainties and biases because of the different sample completeness and environment. This study addresses these challenges by analyzing 33 clusters, aged 3 to 21 million years (PARSEC isochrones), within the Scorpius-Centaurus OB association, sampling the stellar IMF from the hydrogen burning limit to about 8 M$_\odot$. By using $\mathit{Gaia}$, 2MASS, and WISE data, we identified stars with infrared-excess through color-color diagrams and spectral energy distributions, ensuring a consistent selection of disk-bearing sources. Our results indicate a disk lifetime of $5.8 \pm 0.3$ Myr, about a factor of two longer than most previous estimates, suggesting that planet formation may have more time than previously thought. We also find that an exponential decay model best describes disk dispersal. These findings emphasize the importance of studying disk evolution in a single star-forming region to reduce uncertainties and refine our understanding of planet formation timelines.
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All authors Fabian A. Polnitzky, Sebastian Ratzenböck, Josefa E. Großschedl, João Alves

Earth and Planetary Astrophysics

TOI-7166 b: A Habitable Zone mini-Neptune planet around a nearby low-mass star

Khalid Barkaoui, Francisco J. Pozuelos, Benjamin V. Rackham et al. (+41 more)

We present the discovery and validation of TOI-7166b, a 2.01+/-0.05R_Earth planet orbiting a nearby low-mass star. We validated the planet by combining TESS and multi-color high-precision photometric observations from ground-based telescopes, together with spectroscopic data, high-contrast imaging, archival images, and statistical arguments. The host star is an M4-type dwarf at a distance of ~35 pc from the Sun. It has a mass and a radius of Ms=0.190+/-0.004M_Sun and Rs=0.222+/-0.005R_Sun, respectively. TOI-7166b has an orbital period of 12.9 days, which places it close to the inner edge of the Habitable Zone of its host star, receiving an insolation flux of Sp=1.07+/-0.08S_Earth and an equilibrium temperature of Teq=249+/-5K (assuming a null Bond albedo). The brightness of the host star makes TOI-7166 a suitable target for radial velocity follow-up to measure the planetary mass and bulk density. Moreover, the physical parameters of the system including the infrared brightness (Kmag = 10.6) of the star and the planet-to-star radius ratio (0.0823+/-0.0012) make TOI-7166b an exquisite target for transmission spectroscopic observations with the JWST, to constrain the exoplanet atmospheric compositions.
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All authors Khalid Barkaoui, Francisco J. Pozuelos, Benjamin V. Rackham, Adam J. Burgasser, Amaury H.M.J. Triaud, Miquel Serra-Ricart, Mathilde Timmermans, Selçuk. Yalç{\i}nkaya, Abderahmane Soubkiou, Keivan G. Stassun, Karen A. Collins, Pedro J. Amado, Özgur Baştürk, Artem Burdanov, Yasmin T. Davis, Julien de Wit, Brice-Olivier Demory, Sarah Deveny, Georgina Dransfield, Elsa Ducrot, Michaël Gillon, Yilen Gómez Maqueo Chew, Matthew J. Hooton, Keith Horne, Steve B. Howell, Clàudia Janó Muñoz, Emmanuel Jehin, John M. Jenkins, Colin Littlefield, Eduardo L. Martín, Prajwal Niraula, Peter P. Pedersen, Dedier Queloz, Madison G. Scott, Ramotholo Sefako, Avi Shporer, Christopher Stockdale, Emma Softich, Alfredo Sota, Benjamin Tofflemire, Özlem Şimşir, Roberto Varas, Francis Zong Lang, Sebastián S. Zúñiga-Fernández

Earth and Planetary Astrophysics

Multicolour Validation of Two Temperate Mini-Neptunes Around M-dwarf Habitable Zones

Chengzi Jiang, Aleksandra Selezneva, Hannu Parviainen et al. (+17 more)

For small planets orbiting within the habitable zones of their host stars, multicolour validation via photometric transit observations offers an efficient alternative to prioritize targets before intensive radial-velocity follow-up, thereby expanding the sample of habitable-zone exoplanets amenable for atmospheric characterisation. In this study, we validate two exceptional habitable-zone TESS candidates, orbiting around M-dwarfs, as genuine planets, precisely determining their transit and physical parameters. We perform Bayesian model comparison by jointly fitting multicolour light curves from TESS and ground-based follow-up, including observations with HiPERCAM at the 10.4-m GTC. Our approach uses wavelength-dependent transit depth variations and precise transit geometry to reject false positives. We validate TOI-2094 b and TOI-7166 b as two new benchmark temperate mini-Neptunes. TOI-2094 b (1.90 $R_{\oplus}$) orbits its M3V star with a period of $\sim$18.79 days, well within the habitable zone ($\sim$0.98 Earth insolation). TOI-7166 b (2.39 $R_{\oplus}$) orbits its M4.5V host star with a period of $\sim$12.92 days, placing it near the inner edge of the habitable zone ($\sim$1.93 Earth insolation). Statistical mass and density estimates suggest that TOI-2094 b may be a volatile-rich planet, such as a water world or a gaseous planet, and is less likely to be rocky, while TOI-7166 b is likely to be volatile-rich. Both planets are of great interest for detailed atmospheric characterisation with the JWST and future ELTs, which requires further precise mass measurements.
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All authors Chengzi Jiang, Aleksandra Selezneva, Hannu Parviainen, Felipe Murgas, Enric Pallé, Gareb Fernández-Rodríguez, Samuel Geraldía-González, Jaume Orell-Miquel, Norio Narita, Akihiko Fukui, Jerome de Leon, Izuru Fukuda, Kai Ikuta, Kiyoe Kawauchi, Steve B. Howell, Colin Littlefield, Sarah J. Deveny, Joseph D. Twicken, Richard P. Schwarz, Avi Shporer

Cosmology and Nongalactic Astrophysics · Cross-listed from gr-qc

Extreme mass ratio inspirals in the cold vector dark matter environment

Rajesh Karmakar, Debaprasad Maity and Kaustubh Mukund Vispute

With regard to the observed dark matter density profile in galaxies and clusters, the scalar dark matter scenario has been previously studied for potential detectability through gravitational wave observations at measurable signal-to-noise ratios. In the present study, we consider the case of dark matter described by a massive vector field, also referred to as the Proca field. The density profile in the vicinity of the black hole is explicitly constructed for a broad range of dark matter mass, $\mu\sim 10^{-10}-10^{-15}{\mathrm eV}$, which allows it to exhibit both particle and wave-like characteristics. While in the particle regime, the computation of the DM density distribution is analytically tractable, we find it convenient to compute the same numerically in the wave regime. Nevertheless, in the outer region, the surrounding dark matter is assumed to follow a broken power-law distribution, represented by a Navarro-Frenk-White (NFW) profile with a central spike. For the purpose of investigating the detectability of the vector dark matter in the gravitational wave spectrum, we have modelled a stellar-mass black hole ($1M_{\odot}$) inspiralling into a Schwarzschild black hole of mass $10^4M_{\odot}$ within such a vector dark matter environment. With this setup, we analyzed the dephasing in the gravitational wave strain induced by vector dark matter and performed a Fisher forecast for upcoming LISA observations, with particular emphasis on the distinctive features in both the particle and wave regimes of the dark matter. Additionally, most of the important results have been compared with the scalar dark matter case.
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High Energy Astrophysical Phenomena

Non-thermal Synchrotron Emission and Polarization Signatures during Black Hole Flux Eruptions

Fan Zhou, Jiewei Huang, Yuehang Li et al. (+4 more)

In this work, we investigate synchrotron emission and the observational signatures of anisotropic non-thermal electrons during magnetic-flux eruptions in a magnetically arrested disk, using 3D GRMHD simulations. Non-thermal electrons are assumed to be accelerated from the thermal background through magnetic reconnection, with pitch-angle distributions modeled as beamed or loss-cone types, alongside an isotropic case for comparison. The results show that non-thermal emission can produce pronounced flux outbursts and localized brightening during eruptions, while the associated increase in optical depth can suppress the linear polarization fraction. Introducing pitch-angle anisotropy further reshapes the angular distribution of the intrinsic emissivity and modulates its contribution to various observable signatures. Strong field-aligned beaming in the electron distribution suppresses non-thermal emission for near-axis observers, effectively driving the image morphology toward a purely thermal limit. In contrast, moderately anisotropic models remain effective at imprinting non-thermal electron signatures on both the total intensity and polarization structure. We further quantify how eruption-driven increases in absorption depth and enhanced Faraday effects reduce the linear polarization fraction and modify the azimuthal coherence of the polarization field. Overall, our results demonstrate that incorporating anisotropic non-thermal electrons is essential for a physically self-consistent interpretation of time-variable EHT polarimetric observations.
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All authors Fan Zhou, Jiewei Huang, Yuehang Li, Zhenyu Zhang, Yehui Hou, Minyong Guo, Bin Chen

Astrophysics of Galaxies

The influence of external environment at cosmic noon on the subsequent evolution of galaxy stellar mass

Tianmu Gao, J. Trevor Mendel, Lucas C. Kimmig et al. (+4 more)

Connecting high-redshift galaxies to their low-redshift descendants is one of the most important and challenging tasks of galaxy evolution studies. In this work, we investigate whether incorporating high-redshift environmental factors improves the accuracy of matching high-redshift galaxies to their $z\sim0$ descendants, using data from the EAGLE and MAGNETICUM simulations. Using random forest regression, we evaluate the relative importance of a set of environmental metrics at $z\sim3$ in determining the stellar mass of descendant galaxies at $z\sim0$. We identify the spherical overdensity within 1 cMpc ($\delta_{1,\mathrm{sp}}$) as the most important environmental predictor. Tracking galaxies at $z\sim3$ with similar initial stellar masses but different $\delta_{1,\mathrm{sp}}$ values, we find that, across all mass bins in both simulations, high-density environments produce $z\sim0$ descendants with median stellar masses up to eight times higher than the descendants of galaxies in low-density environments. For galaxies with $M_{*}\lesssim10^{10}M_{\odot}$, the difference is attributable to more merger-induced mass growth in high-density environments, whereas for higher-mass galaxies, it results from a combination of enhanced in-situ star formation and greater external mass accretion. By assessing the importance of overdensity across multiple scales and redshifts, we find that at $z\gtrsim2$, environmental factors become as important as stellar mass in predicting the stellar mass of $z\sim0$ descendants. Compared to using stellar mass at $z\sim3$ alone, incorporating $\delta_{1,\mathrm{sp}}$ reduces the scatter in the residuals between the predicted and actual stellar masses by approximately 20% in EAGLE and 35% in MAGNETICUM.
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All authors Tianmu Gao, J. Trevor Mendel, Lucas C. Kimmig, Claudia del P. Lagos, Rhea-Silvia Remus, Emily Wisnioski, Kathryn Grasha

Earth and Planetary Astrophysics

Revisiting the atmosphere of HAT-P-70b with CARMENES high-resolution transmission spectroscopy

Tianjun Gan, Jaume Orell-Miquel, Fei Yan et al. (+19 more)

Owing to hot and inflated envelopes that facilitate atmospheric studies, ultra-hot Jupiters (UHJs) have attracted much attention. Significant progress has been achieved, from enlarging the sample size to broadening the studies to encompass diverse stellar types and ages. Here, we present a transmission spectroscopy study of HAT-P-70b, an UHJ orbiting a young A-type star, through high-resolution observations with CARMENES at the 3.5m Calar Alto telescope. By using the line-by-line technique, we confirm the previous detections of Ha, Na I, and Ca II, report a new tentative detection of K I, and impose an upper limit on the He triplet absorption. Through cross-correlation analysis, we identify the Ca II and Fe I absorptions, both blue-shifted by approximately 5 km/s, indicating a day-to-night side atmospheric wind. Additionally, we find a new tentative detection of K I. We do not see any significant atmospheric molecular signal in the near-infrared data. Putting HAT-P-70b in the context of UHJs from the literature, it turns out that (1) Ha absorption is more common on gas giants orbiting stars younger than 1 Gyr, with a relative detection probability of $P_{\rm Age<1\,Gyr}({\rm Ha})/P_{\rm Age\geq1\,Gyr}({\rm Ha})\sim 3$; (2) any UHJ is likely to exhibit Fe I absorption if it has Ca II.
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All authors Tianjun Gan, Jaume Orell-Miquel, Fei Yan, Lisa Nortmann, Jorge Sanz-Forcada, Enric Pallé, Shude Mao, Pedro J. Amado, José A. Caballero, Stefan Cikota, David Cont, Artie P. Hatzes, Thomas Henning, Fabio Lesjak, Manuel López-Puertas, David Montes, Juan Carlos Morales, Alberto Peláez-Torres, Andreas Quirrenbach, Ansgar Reiners, Ignasi Ribas, Andreas Schweitzer

Earth and Planetary Astrophysics

A Fast, Parallelized, GPU-Accelerated Photochemical Model, XODIAC, with Built-in Equilibrium Chemistry and Multiple Chemical Networks for Exoplanetary Atmospheres

Priyankush Ghosh, Sambit Mishra, Shubham Dey et al. (+3 more)

The launch of the James Webb Space Telescope (JWST) has delivered high-quality atmospheric observations and expanded the known chemical inventory of exoplanetary atmospheres, opening new avenues for atmospheric chemistry modeling to interpret these data. Here, we present XODIAC, a fast, GPU-accelerated, one-dimensional photochemical model with a built-in equilibrium chemistry solver, an updated thermochemical database, and three chemical reaction networks. This framework enables comparative atmospheric chemistry studies, including the newly developed XODIAC-2025 network, a state-of-the-art C-H-O-N-P-S-Metals network, linking 594 species through 7,720 reactions. The other two are existing, publicly available C-H-O-N-S and C-H-O-N-S-Metals networks, from the established photochemical models VULCAN and ARGO, respectively, which are commonly used in the community. The XODIAC model has been rigorously benchmarked on the well-studied hot Jupiter HD 189733 b, with results compared against these two models. Benchmarking shows excellent agreement and demonstrates that, when the same chemical network and initial conditions are used, the numerical scheme for solving atmospheric chemistry does not significantly affect the results. We also revisited the atmospheric chemistry of HD 189733 b and performed a comparative analysis across the three networks. Sulfur chemistry shows the least variation across networks, carbon chemistry shows slightly more, and phosphorus chemistry varies the most, primarily due to the introduction of unique PHO and PN pathways comprising 390 reactions in the XODIAC-2025 network. These findings highlight XODIAC's capability to advance exoplanetary atmospheric chemistry and provide a robust framework for comparative exoplanetology.
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All authors Priyankush Ghosh, Sambit Mishra, Shubham Dey, Debayan Das, Paul B. Rimmer, Liton Majumdar

Cosmology and Nongalactic Astrophysics

Interacting scalar field dark matter and stepped dark radiation in an extended Wess-Zumino dark radiation model

Gang Liu

We extend the Wess-Zumino dark radiation (WZDR) model by replacing cold dark matter with scalar field dark matter and introducing a pure momentum coupling between the scalar field and stepped dark radiation. This coupling avoids excessive early-universe damping, thereby preserving the predictive power of the WZDR framework while offering a potential mechanism for exploring the Hubble and $S_8$ tensions.Using a combination of cosmic microwave background, baryon acoustic oscillations, Type Ia supernovae, the SH0ES $H_0$ measurement, Dark Energy Survey Year 3 (DES) $S_8$ data, and Atacama Cosmology Telescope data, we constrain the model. When only one of the SH0ES and DES priors is included, the new model outperforms WZDR in $\chi^2$ and $Q_{\rm DMAP}$; with both priors, it is disfavored. Using the latest cosmological data, we find that at 68% C.L. the coupled model gives $H_0 = 71.08^{+0.73}_{-0.66}$ km/s/Mpc and $S_8 = 0.8162\pm0.0073$, close to the WZDR values of $71.20^{+0.73}_{-0.61}$ and $0.8165^{+0.0078}_{-0.0066}$. Both models raise $H_0$ effectively, but the new model only marginally reduces $S_8$, which remains above the $\Lambda$CDM prediction. The coupling is weak, with $\log_{10}(\xi) < -3.36$ (95% C.L.), and performs worse than WZDR in both $\chi^2$ and AIC. Hence, although it does not fully resolve the tensions, this work provides a useful reference for studies of interacting dark sectors.
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Cosmology and Nongalactic Astrophysics

What Galaxy Clusters Have to Say About Dynamical Dark Energy and $H_0$

Andrés N. Salcedo, Eduardo Rozo, Hao-Yi Wu et al. (+4 more)

We show that, in flat $\Lambda$CDM, low-redshift structure probes – cluster abundances, 3$\times$2-point analyses, and full-shape clustering – are mutually consistent, jointly delivering precise constraints on $\sigma_8$ and $\Omega_{\rm m}$ that agree with geometrical datasets (CMB+BAO+SN). In $w_0w_a$CDM, adding clusters to the geometry dataset reduces the evidence for evolving dark energy while relaxing the $H_0$ tension, suggesting a $\Lambda$CDM evolution of the late-time Universe and a sound horizon that differs from its standard value.
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All authors Andrés N. Salcedo, Eduardo Rozo, Hao-Yi Wu, Shulei Cao, Enrique Paillas, Hanyu Zhang, Eli S. Rykoff

Cosmology and Nongalactic Astrophysics · Cross-listed from cs.CV

Masked Autoencoder Pretraining on Strong-Lensing Images for Joint Dark-Matter Model Classification and Super-Resolution

Achmad Ardani Prasha, Clavino Ourizqi Rachmadi, Muhamad Fauzan Ibnu Syahlan et al. (+5 more)

Strong gravitational lensing can reveal the influence of dark-matter substructure in galaxies, but analyzing these effects from noisy, low-resolution images poses a significant challenge. In this work, we propose a masked autoencoder (MAE) pretraining strategy on simulated strong-lensing images from the DeepLense ML4SCI benchmark to learn generalizable representations for two downstream tasks: (i) classifying the underlying dark matter model (cold dark matter, axion-like, or no substructure) and (ii) enhancing low-resolution lensed images via super-resolution. We pretrain a Vision Transformer encoder using a masked image modeling objective, then fine-tune the encoder separately for each task. Our results show that MAE pretraining, when combined with appropriate mask ratio tuning, yields a shared encoder that matches or exceeds a ViT trained from scratch. Specifically, at a 90% mask ratio, the fine-tuned classifier achieves macro AUC of 0.968 and accuracy of 88.65%, compared to the scratch baseline (AUC 0.957, accuracy 82.46%). For super-resolution (16x16 to 64x64), the MAE-pretrained model reconstructs images with PSNR ~33 dB and SSIM 0.961, modestly improving over scratch training. We ablate the MAE mask ratio, revealing a consistent trade-off: higher mask ratios improve classification but slightly degrade reconstruction fidelity. Our findings demonstrate that MAE pretraining on physics-rich simulations provides a flexible, reusable encoder for multiple strong-lensing analysis tasks.
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All authors Achmad Ardani Prasha, Clavino Ourizqi Rachmadi, Muhamad Fauzan Ibnu Syahlan, Naufal Rahfi Anugerah, Nanda Garin Raditya, Putri Amelia, Sabrina Laila Mutiara, Hilman Syachr Ramadhan

High Energy Astrophysical Phenomena

Fast X-ray Variability from the Coronae of Supermassive Black Holes

Xiurui Zhao, Luca Comisso, Stefano Marchesi et al. (+4 more)

We present the first systematic study of short-timescale X-ray variability in radio-quiet active galactic nuclei (AGN), utilizing archival Chandra observations of approximately 3,000 broad-line AGN selected from the SDSS and DESI spectroscopic surveys. We identify 14 AGN exhibiting rapid (on timescales of tens of kiloseconds) X-ray flux variations by factors of two or more that are statistically significant ($p\le6\times10^{-4}$), indicative of fast coronal variability. By converting minimum variability timescales to light-crossing times, we place upper limits on the sizes of the variable coronal regions, finding typical scales of $\lesssim10^{-4}$~pc. The coronal variable region size upper limits of an AGN in our sample are found to be much smaller than the typical coronal sizes inferred from microlensing, suggesting that its corona is composed of localized, transient structures rather than smooth, homogeneous plasmas. Such efficient magnetic energy dissipation in compact volumes is consistent with expectations for magnetically dominated coronae and is supported by recent general relativistic magnetohydrodynamic simulations. Future high-throughput X-ray observatories will enable the detection of even faster coronal variability, providing direct constraints on the physical mechanisms driving plasma energization and flux fluctuation near supermassive black holes. Our results suggest that luminous AGN hosting massive black holes are prime targets for probing the small-scale structure and dynamics of AGN coronae.
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All authors Xiurui Zhao, Luca Comisso, Stefano Marchesi, Marco Ajello, Elias Kammoun, Yue Shen, Qiaoya Wu

Saturday 6 December

Astrophysics of Galaxies

A XRISM/Resolve view of the dynamics in the hot gaseous atmosphere of M87

XRISM Collaboration: M. Audard, H. Awaki, R. Ballhausen et al. (+138 more)

The XRISM/Resolve microcalorimeter directly measured the gas velocities in the core of the Virgo Cluster, the closest example of AGN feedback in a cluster. This proximity allows us to resolve the kinematic impact of feedback on scales down to 5 kpc. Our spectral analysis reveals a high velocity dispersion of $\sigma_v$=262 (+45 / -38) km/s near the AGN, which steeply declines to ~60 km/s between 5 and 25 kpc in the northwest direction. The observed line-of-sight bulk velocity in all regions is broadly consistent with the central galaxy, M87, with a mild trend toward blueshifted motions at larger radii. Systematic uncertainties have been carefully assessed and do not affect the measurements. The central velocities, if attributed entirely to isotropic turbulence, correspond to a transonic ICM at sub-6 kpc scales with three-dimensional Mach number 0.69 (+0.14 / -0.11) and a non-thermal pressure fraction of 21 (+7 / -5)%. Simple models of weak shocks and sound waves and calculations assuming isotropic turbulence both support the hypothesis that the velocity field reflects a mix of shock-driven expansion and turbulence. Compared to other clusters observed by XRISM to date, M87's central region stands out as the most kinematically disturbed, exhibiting both the highest velocity dispersion and the largest 3D Mach number, concentrated at the smallest physical scales.
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All authors XRISM Collaboration: M. Audard, H. Awaki, R. Ballhausen, A. Bamba, E. Behar, R. Boissay-Malaquin, L. Brenneman, G. V. Brown, L. Corrales, E. Costantini, R. Cumbee, M. Diaz Trigo, C. Done, T. Dotani, K. Ebisawa, M. E. Eckart, D. Eckert, S. Eguchi, T. Enoto, Y. Ezoe, A. Foster, R. Fujimoto, Y. Fujita, Y. Fukazawa, K. Fukushima, A. Furuzawa, L. Gallo, J. A. García, L. Gu, M. Guainazzi, K. Hagino, K. Hamaguchi, I. Hatsukade, K. Hayashi, T. Hayashi, N. Hell, E. Hodges-Kluck, A. Hornschemeier, Y. Ichinohe, D. Ishi, M. Ishida, K. Ishikawa, Y. Ishisaki, J. Kaastra, T. Kallman, E. Kara, S. Katsuda, Y. Kanemaru, R. Kelley, C. Kilbourne, S. Kitamoto, S. Kobayashi, T. Kohmura, A. Kubota, M. Leutenegger, M. Loewenstein, Y. Maeda, M. Markevitch, H. Matsumoto, K. Matsushita, D. McCammon, B. McNamara, F. Mernier, E. D. Miller, J. M. Miller, I. Mitsuishi, M. Mizumoto, T. Mizuno, K. Mori, K. Mukai, H. Murakami, R. Mushotzky, H. Nakajima, K. Nakazawa, J.-U. Ness, K. Nobukawa, M. Nobukawa, H. Noda, H. Odaka, S. Ogawa, A. Ogorzałek, T. Okajima, N. Ota, S. Paltani, R. Petre, P. Plucinsky, F. S. Porter, K. Pottschmidt, K. Sato, T. Sato, M. Sawada, H. Seta, M. Shidatsu, A. Simionescu, R. Smith, H. Suzuki, A. Szymkowiak, H. Takahashi, M. Takeo, T. Tamagawa, K. Tamura, T. Tanaka, A. Tanimoto, M. Tashiro, Y. Terada, Y. Terashima, Y. Tsuboi, M. Tsujimoto, H. Tsunemi, T. Tsuru, A. Tümer, H. Uchida, N. Uchida, Y. Uchida, H. Uchiyama, S. Ueda, Y. Ueda, S. Uno, J. Vink, S. Watanabe, B. J. Williams, S. Yamada, S. Yamada, H. Yamaguchi, K. Yamaoka, N. Yamasaki, M. Yamauchi, S. Yamauchi, T. Yaqoob, T. Yoneyama, T. Yoshida, M. Yukita, I. Zhuravleva, M. Charbonneau, N. Dizdar, M. Fujita, D. Ito, J. Martin, H. McCall, H. Russell, J. ZuHone