High Energy Astrophysical Phenomena
A mysterious feature in the NICER spectrum of 4U 1820-30: A gravitationally redshifted absorption line?
R. Iaria, T. Di Salvo, A. Anitra et al. (+6 more)
A mysterious absorption feature at approximately 3.8 keV has been identified in the NICER spectrum of the low-mass X-ray binary system 4U 1820-30. We interpret this feature as a gravitationally redshifted iron absorption line. This interpretation is supported by the temporal proximity of the NICER observation to the detection of a carbon superburst by the X-ray monitor MAXI, suggesting that the presence of the line is associated with this rare and extreme event. From the inferred
redshift of the absorption line, the compactness of the
neutron star can be derived. Using a photoionization absorption model, we measure a gravitational
redshift of about 1.72, which corresponds to a compactness R/M of 4.46 \pm 0.13 km per
solar mass, or 3.02 \pm 0.09 in dimensionless units. This unique feature highlights the importance of further observations and detailed modelling, offering promising insights into the equation of state of matter under extreme density conditions.
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All authors R. Iaria, T. Di Salvo, A. Anitra, F. Barra, A. Sanna, C. Maraventano, C. Miceli, W. Leone, L. Burderi
Cosmology and Nongalactic Astrophysics · Cross-listed from gr-qc
Anisotropic Bianchi-I cosmological model in non-conservative unimodular gravity
Marcelo H. Alvarenga and Júlio C. Fabris
In this article, we propose an anisotropic Bianchi-I type cosmological model in non-conservative Unimodular
Gravity ($\mathrm{NUG}$). We show that simply using the Bianchi-I type metric does not resolve a striking characteristic of the field equations in $\mathrm{NUG}$: their underdetermination. This fact led us to implement extra conditions on the combination $\left(\rho+p\right)$ and, consequently, obtain a consistent background cosmological analysis. In the
vacuum case, we obtain an analogy between the Kasner solutions and the equations in $\mathrm{NUG}$. We also propose a new analysis of a non-homogeneous equation of state, the combination $\left(\rho+p\right)=l$. We identify that the cosmological dynamics are strictly dependent on the value of the constant $l$. The physically interesting case is at the value $l<0$, which seems to indicate a super-accelerated, ghost-like universe. This case still requires a more detailed analysis, for example, from a thermodynamic point of view, keeping in mind that $\left(\rho+p\right)$ may be interpreted as enthalpy of the system. For the cases $\left(\rho+p\right)\propto a^{-3}$ and $\left(\rho+p\right) \propto a^{-4}$, we obtain a description consistent with the anisotropic cosmological model described by $\mathrm{GR}$. In all cases analyzed, a small value for the anisotropic parameter $\Omega_{A}$ (on the order of $10^{-2}$) is required in order to have agreement, for example, with the age of the universe to be approximately $12-14\, \mathrm{Gyr}$, agreeing with the age of globular clusters. As the universe expands an isotropization is verified, with the anistropies going to zero asymptotically, similarly with what happens in an anistropic cosmological model based on $\mathrm{GR}$.
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Astrophysics of Galaxies
Discovery of new N-emitters over a wide redshift range
I. Morel, D. Schaerer, R. Marques-Chaves et al. (+5 more)
JWST observations have revealed rare
galaxies with UV spectra exhibiting intense lines of nitrogen, indicative of super-
solar N/O abundances at low
metallicity. To better understand these enigmatic objects and provide new constraints on proposed scenarios, we have undertaken a systematic search for
galaxies with UV emission lines of nitrogen. Using public JWST NIRSpec data, we have identified 45 N-emitters with robust NIII] or NIV] detections, including 4 previously known objects. We find N-emitters from
redshift $z\sim 3-11$ among a broad diversity of
galaxies, in terms of morphology, UV magnitude,
stellar mass, SFR,
metallicity, and rest-optical line strengths. The UV nitrogen lines show typical equivalent widths between $\sim 5-50$ Å. Carbon lines are generally fainter than the N lines. Using strong line calibrations established at high-
redshift, we find
metallicities $12+log(O/H)\sim 7.15-8.5$, including thus also high
metallicities. The H$\beta$ equivalent width of N-emitters varies strongly, and sources with low EWs show clear signs of a Balmer break, indicative of composite
stellar populations combining both young (< 10 Myr)
stars responsible of the UV emission lines and an older population contributing to the rest-optical spectrum. Supersolar N/O ratios are found in all N-emitters. C/O abundances are comparable to those of
galaxies at the same
metallicity, and all N-emitters show high N/C ratios or lower limits ($\log(N/C) > 0.5$), independently of
metallicity. The observed abundance ratios are compatible with ejecta from H-burning and do not show signs of Carbon enhancements, even at higher
metallicities. Finally, we find that the fraction of N-emitters increases with
redshift, and we quantify this
evolution. Our study increases the sample of known N-emitters by a factor $\sim 3$, reveals a diversity of properties among N-emitters, and provides new constraints on their nature.
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All authors I. Morel, D. Schaerer, R. Marques-Chaves, N. Prantzos, C. Charbonnel, G. Brammer, M. Xiao, M. Dessauges-Zavadsky
Astrophysics of Galaxies
Molecular hydrogen in filaments at high Galactic latitudes
P. M. W. Kalberla
Context. Neutral atomic hydrogen (HI) absorption lines can be used to probe the cold neutral medium (CNM) at high
Galactic latitudes. Cold HI with a significant optical depth from the GASKAP-HI survey is found to be located predominantly if not exclusively within filamentary structures that can be identified as caustics with the Hessian operator. Most of these HI filaments (57%) are also observable in the far-infrared (FIR) and trace the orientation of
magnetic field lines. Aims. We considered whether molecular hydrogen (H2) might also be preferentially associated with CNM filaments. Methods. We analyzed 241 H2 absorption lines against
stars and determined whether the lines of sight intersected HI or FIR filaments. Using Far Ultraviolet Spectroscopic Explorer (FUSE) H2 data in the velocity range -50 < vLSR < 50 km/s, we traced 65 additional H2 lines for filamentary HI and FIR structures in velocity and probed the H2 absorption for coincidences in position and velocity. Results. For 305 out of 306 positions, the lines of sight with H2 absorption intersect HI filaments. In 120 cases, there is also evidence for a correlation with dusty FIR filaments. All of the 65 available sight lines with known velocities intersect HI filaments. In 64 cases, the H2 velocities are consistent with HI filament velocities. For FIR filaments, an agreement is found for only 13 out of 14 H2 absorption lines. Conclusions. For the majority of H2 absorption lines, there is evidence that H2 is associated with cold HI filaments. Evidence of an association with FIR filaments is less compelling. Confusion along the line of sight limits the detectability of FIR filaments. For a comparable degree of UV excitation in the disk and lower
Galactic halo, the formation rate of H2 appears to be enhanced in HI filaments with increased CNM densities.
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High Energy Astrophysical Phenomena
Rotational effects in quark stars: comparing different models
Adamu Issifu, Andreas Konstantinou, Franciele M. da Silva et al. (+1 more)
We investigate the rotational properties of self-bound strange
quark stars using two representative
quark matter equations of state (EOS): the vector MIT bag model and the density-dependent
quark mass (DDQM) model. Through general-relativistic calculations of uniformly rotating sequences, we analyze their mass–radius relations, moments of inertia, quadrupole moments, surface
redshifts, Keplerian frequencies, and energy components. A central result of this work is the full decomposition of the
stellar energy budget in rotating strange
stars, separating gravitational, internal, rotational, and binding energy contributions. Rotation amplifies the intrinsic EOS differences: the MIT model supports more massive ($M_{\max} \gtrsim 3.3\,M_\odot$) compact
stars with larger moments of inertia and greater resistance to deformation, while the DDQM model produces larger radii, less massive
stars limited by mass-shedding at lower frequencies. Combined measurements of mass, radius, and frequency can thus break the EOS degeneracy; massive, rapidly rotating
pulsars favors MIT-like EOS, whereas larger radii in canonical
stars point to a DDQM-like model. These rotational observables, soon to be tightly constrained by NICER and next-generation gravitational-wave detectors, offer a means to test the existence and composition of self-bound
quark matter in compact
stars.
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All authors Adamu Issifu, Andreas Konstantinou, Franciele M. da Silva, Tobias Frederico
Solar and Stellar Astrophysics
Advances and Challenges in Solar Flare Prediction: A Review
Mingfu Shao, Suo Liu, Haiqing Xu et al. (+8 more)
Solar flares, as one of the most prominent manifestations of
solar activity, have a profound impact on both the Earth's space environment and human activities. As a result, accurate
solar flare prediction has emerged as a central topic in space weather research. In recent years, substantial progress has been made in the field of
solar flare forecasting, driven by the rapid advancements in space observation technology and the continuous improvement of data processing capabilities. This paper presents a comprehensive review of the current state of research in this area, with a particular focus on tracing the
evolution of data-driven approaches – which have progressed from early statistical learning techniques to more sophisticated machine learning and deep learning paradigms, and most recently, to the emergence of
Multimodal Large Models (MLMs). Furthermore, this study examines the realistic performance of existing
flare forecasting platforms, elucidating their limitations in operational space weather applications and thereby offering a practical reference for future advancements in technological optimization and system design.
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All authors Mingfu Shao, Suo Liu, Haiqing Xu, Peng Jia, Hui Wang, Liyue Tong, Yang Bai, Chen Yang, Yuyang Li, Nan Li, Jiaben Lin
Cosmology and Nongalactic Astrophysics · Cross-listed from hep-ph
Chiral phonons in metal-organic frameworks as quantum sensors for the direct detection of dark matter
Marek Matas, Filip Krizek and Carl P. Romao
We investigate a new
quantum sensor for dark matter direct detection with sub-eV sensitivity, focusing on several candidate materials that potentially host
chiral phonons with large
magnetic moments that can be directly read out with an external magnetometer. We focus on metal-organic frameworks (MOFs) as possible candidate materials for single
chiral phonon detection due to their noncentrosymmetric structure, tunability, and the ability to host these excitations in stable acoustic bands. We identify several promising candidates and compare their projected dark matter detection sensitivity for all possible interactions identified within effective field theory. We establish that the expected sensitivity does not depend heavily on the specific choice of the MOF, enabling us to tailor the final material composition to facilitate the
magnetic readout. We then propose a prototype setup able to test the direct readout of a
chiral phonon sensor with a surface-integrated magnetometer.
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High Energy Astrophysical Phenomena
A Self-Consistent Model of the Ultra High-Energy Gamma-Ray Emission of Pulsar Wind Nebulae: Insights from LHAASO and ATNF Catalogs
Samy Kaci, Gwenael Giacinti and Dmitri Semikoz
Pulsar wind nebulae (PWNe) are the dominant Ultra-high-energy (UHE) gamma-ray sources in the LHAASO catalog suggesting that they are the dominant leptonic PeVatrons in our
Galaxy. Despite this, still very little is known about their UHE gamma-ray emission, their number in the
Galaxy, or their contribution to the gamma-ray emission of our
Galaxy. In this work, we propose a self-consistent data-driven model of the UHE gamma-ray emission of PWNe based on the ATNF and LHAASO catalogs. More specifically, we build a model of the UHE gamma-ray emission of PWNe that preserves the statistical relationships in the ATNF catalog and reproduces the number of PWNe detected in the LHAASO catalog. To cope with the limited data available in the LHAASO catalog when performing fits on gamma-ray data, we introduce the concept of censored regression that allows to also use the information provided by unresolved sources. Using our model, we find that reproducing the number of PWNe detected by LHAASO requires either fractions of misaligned
pulsars smaller ($\lesssim60\%$) than usually found in the literature, or that some of the associations of PWNe to ATNF
pulsars made by LHAASO may not be true. In both cases, we find that in order to reach self-consistency between
radio and gamma-ray data, it is necessary that the majority of the unidentified sources in the LHAASO catalog are PWNe associated to an unseen
pulsar. Moreover, using our model we also find that the contribution of unresolved PWNe to the total (diffuse) gamma-ray background measured by LHAASO in the $1-1000\,\rm{TeV}$ range is always smaller than $\lesssim10\%$ ($\lesssim30\%$). We conclude that PWNe mostly contribute to the source component of the UHE gamma-ray sky, while having almost no imprint on its diffuse component.
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Cosmology and Nongalactic Astrophysics
The effect of sound speed on the gravitational wave spectrum of first order phase transitions in the early universe
Mika Mäki
Gravitational waves from first-order phase transitions are a promising probe of physics beyond the Standard Model, as many extensions of the standard model result in first-order phase transitions in the early universe, from which the resulting gravitational waves could be detectable with the upcoming
Laser Interferometer Space
Antenna (LISA). The properties of the phase transition and the resulting gravitational wave spectrum are determined by five key parameters: the nucleation temperature $T_n$, phase transition strength at the nucleation temperature $\alpha_n$, bubble wall speed $v_\text{wall}$, transition rate $\beta$ and the sound speed $c_s$. Of these, the sound speed $c_s$ is determined by the equation of state $p(T,\phi)$. In most studies, the
plasma of the early universe has been assumed to be ultrarelativistic and therefore following the bag equation of state with $c_s = \frac{1}{\sqrt{3}}$. In this thesis, the PTtools simulation framework for first-order phase transitions, based on the Sound Shell Model, has been extended to include support for arbitrary equations of state and therefore for a temperature- and phase-dependent sound speed $c_s(T,\phi)$. The thesis also functions as a reference manual for PTtools. The framework has been tested with the constant sound speed model, in which the sound speed is a different constant in each phase. The sound speed has been shown to have a significant effect on the resulting gravitational wave spectrum, especially when changing the sound speed results in a change in the type of the solution. This has laid the groundwork for simulating cosmological phase transitions with realistic equations of state. This will result in in gravitational wave spectra that can be used in the LISA data analysis pipeline to search for the existence and parameters of a first-order phase transition in the early universe.
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Astrophysics of Galaxies · Cross-listed from gr-qc
Resolving white dwarf binaries within globular clusters with LISA
Wouter G. J. van Zeist, Gijs Nelemans, Shu-Xu Yi et al. (+1 more)
Context: Globular clusters (GCs) around the Milky Way (MW) are expected to host white
dwarf (WD) binaries emitting gravitational waves that could be detectable by LISA. Aims: Our aim is to investigate whether LISA can resolve WD binaries in GCs well enough in terms of sky location and distance that they can be distinguished from binaries in the MW disc. Methods: We used a sample of 20 of the most massive GCs around the MW and simulated LISA's sky location and distance measurement errors for WD binaries in these GCs using the software package GWToolbox. We did this in the context of a model of the LISA-detectable binaries in the MW from the population synthesis code SeBa. Results: We find that for five of the GCs in our sample, binaries in the GC could be easily distinguished from MW disc binaries using the sky location alone; for another five, binaries in the GCs could be distinguished using a combination of LISA's sky location and distance measurements; and for the final ten, binaries in the GCs could not be distinguished from overlapping MW disc binaries. The results depend strongly on the sky locations of the GCs, with GCs far away from the
Galactic plane being easy to resolve, while GCs close to the
Galactic centre overlap with many MW disc binaries. The most promising GC for finding a WD binary that could be resolved to that GC, based on sky location and GC mass, is 47 Tucanae.
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All authors Wouter G. J. van Zeist, Gijs Nelemans, Shu-Xu Yi, Simon F. Portegies Zwart
High Energy Astrophysical Phenomena
Jet reorientation revealed by intermittent jet activity in radio galaxy 0954+556
Ai-Ling Zeng, Wei Zhao, Jun Yang et al. (+9 more)
Intermittent jet activity of AGNs is a common phenomenon, whereas significant jet reorientation during episodic jet activity in relatively young
radio galaxies are rarely reported. The
quasar 0954+556 at
redshift of 0.903 is an intriguing source exhibiting an unusual
radio jet structure with significantly different jet directions at kpc and pc scales. At kpc scales, images from the VLA exhibit a bright core, a linear jet extending 24 kpc to the northwest, and a discrete jet component 16 kpc to the northeast. At pc scales, images from the VLBA show a two-component structure with a projected separation of 360 pc in the north-south direction. The peculiar structure of 0954+556 might result from jet reorientation. Here, our aim was to investigate the possible mechanism via multiscale and multifrequency deep
radio images. We performed VLA and VLBA observations of 0954+556. Together with some existing data in the NRAO data archive, we made multiple VLA images at 1.4-22 GHz and VLBA images at 1.7-43 GHz for various image analyses of the jet structure. We identified the location of the
radio core at pc scales, detected the faint counter-jets at both pc and kpc scales for the first time, and revealed a diffuse emission region connecting pc and kpc scale forward jets. Our spectral index distribution and spectral aging analysis indicate that 0954+556 might undergo at least two episodes of jet activity during the current AGN phase. Moreover, pc scale polarization maps display a well-resolved spine-sheath polarization structure. It seems that the jet direction of 0954+556 changed significantly during intermittent jet activity. This may explain the different jet orientations and spectral ages observed from kpc to pc scales. The research provides a strong case that AGN jet direction might change rapidly on timescales of one million years.
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All authors Ai-Ling Zeng, Wei Zhao, Jun Yang, Xu-Zhi Hu, Furen Deng, Yu Lei, Xiaoyu Hong, Xiang Liu, Liang Chen, Mai Liao, Xiaolong Yang, Hai-Tian Shang
Cosmology and Nongalactic Astrophysics
Estimating the triaxiality of massive clusters from 2D observables in MillenniumTNG with machine learning
Ana Maria Delgado, Michelle Ntampaka, Sownak Bose et al. (+7 more)
Properties of massive
galaxy clusters, such as mass abundance and concentration, are sensitive to cosmology, making cluster statistics a powerful tool for cosmological studies. However, favoring a more simplified, spherically symmetric model for
galaxy clusters can lead to biases in the estimates of cluster properties. In this work, we present a deep-learning approach for estimating the triaxiality and orientations of massive
galaxy clusters (those with masses $\gtrsim 10^{14}\,M_\odot h^{-1}$) from 2D observables. We utilize the flagship hydrodynamical volume of the suite of cosmological-hydrodynamical MillenniumTNG (MTNG) simulations as our ground truth. Our model combines the feature extracting power of a convolutional neural network (CNN) and the message passing power of a graph neural network (GNN) in a multi-modal, fusion network. Our model is able to extract 3D geometry information from 2D idealized cluster multi-wavelength images (soft X-ray, medium X-ray, hard X-ray and tSZ effect) and mathematical graph representations of 2D cluster member observables (line-of-sight radial velocities, 2D projected positions and V-band luminosities). Our network improves cluster geometry estimation in MTNG by $30\%$ compared to assuming spherical
symmetry. We report an $R^2 = 0.85$ regression score for estimating the major axis length of triaxial clusters and correctly classifying $71\%$ of prolate clusters with elongated orientations along our line-of-sight.
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All authors Ana Maria Delgado, Michelle Ntampaka, Sownak Bose, Fulvio Ferlito, Boryana Hadzhiyska, Lars Hernquist, John Soltis, John F. Wu, Mikaeel Yunus, John ZuHone
Cosmology and Nongalactic Astrophysics
Impact of Simulation Box Size for Weak Lensing: Replication and Super-Sample Effects
Akira Tokiwa, Adrian E. Bayer, Joaquin Armijo et al. (+6 more)
We quantify the bias caused by small simulation box size on weak
lensing observables and covariances, considering both replication and super-sample effects for a range of higher-order statistics. Using two simulation suites – one comprising large boxes ($3750\,h^{-1}{\rm Mpc}$) and another constructed by tiling small boxes ($625\,h^{-1}{\rm Mpc}$) – we generate full-sky convergence maps and extract $10^\circ \times 10^\circ$ patches via a Fibonacci grid. We consider biases in the mean and covariance of the angular power spectrum, bispectrum (up to $\ell=3000$), PDF, peak/minima counts, and Minkowski functionals. By first identifying lines of sight that are impacted by replications, we find that replication causes a O$(10\%)$ bias in the PDF and Minkowski functionals, and a O$(1\%)$ bias in other summary statistics. Replication also causes a O$(10\%)$ bias in the covariances, increasing with source
redshift and $\ell$, reaching $\sim25\%$ for $z_s=2.5$. We additionally show that replication leads to heavy biases (up to O$(100\%)$ at high
redshift) when performing gnomonic projection on a patch that is centered along a direction of replication. We then identify the lines of sight that are minimally affected by replication, and use the corresponding patches to isolate and study super-sample effects, finding that, while the mean values agree to within $1\%$, the variances differ by O$(10\%)$ for $z_s\leq2.5$. We show that these effects remain in the presence of noise and smoothing scales typical of the DES, KiDS, HSC, LSST, Euclid, and Roman surveys. We also discuss how these effects scale as a function of box size. Our results highlight the importance of large simulation volumes for accurate
lensing statistics and covariance estimation.
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All authors Akira Tokiwa, Adrian E. Bayer, Joaquin Armijo, Jia Liu, Ryo Terasawa, Leander Thiele, Marcelo Alvarez, Linda Blot, Masahiro Takada
Astrophysics of Galaxies
Black Hole merger rates in the first billion years in light of JWST data
P. F. V. Cáceres-Burgos, P. Dayal, P. Lira et al. (+3 more)
Context. Recent James Webb Space
Telescope (JWST) discoveries have unveiled an abundance of faint and massive Active
Galactic Nuclei (AGNs) at high
redshifts (z=4-9), that surpass by 10 to 100 times the extrapolated bolometric (Bol) and ultraviolet (UV) luminosity functions (LF) from previous AGN campaigns. The two main models that are put forward to explain these observations correspond to light seeds (150 Msol) accreting in episodes of super Eddington, and heavy seeds ($10^3$ - $10^5$ Msol) growing at the Eddington limit. Future gravitational observatories like the
Laser Interferometer Satellite
Antenna (LISA) will help disentangle these models by reporting the BH-BH merger events from mid to high
redshifts. Aims. This work aims to report the predicted merger rates in the heavy seed scenario in light of recent JWST data. In our models we explore (i) instantaneous merging between BHs, (ii) delayed merging after a dynamical timescale, as well as extreme
spin configurations (a=0.99, a=-0.99) to bracket BH mass growth. Methods. We use Delphi, a semi-analytical model that tracks baryonic physics over a hierarchical
evolution of dark matter
halos through
cosmic time within the first billion years of the Universe. We calibrate this model for it to simultaneously reproduce
galaxy and JWST-AGNs observables. Results. We show reasonable agreement with the Bolometric Luminosity function at z=6, where BHs must accrete 10-100 times more gas than in previous works calibrated to pre-JWST data. However, we underpredict (overpredict) the bright end $10^45.5$ erg s$^-1$ (all luminosity range) at z=7 (z=5) by 1-3.2 dex (0.22-1.6 dex). Regarding BH-BH merger events, the instantaneous (delayed) models predict a total of 28.06 (19.61) yr$^-1$ for BHs at z>=5, which is within the range of merger rates reported in previous literature.
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All authors P. F. V. Cáceres-Burgos, P. Dayal, P. Lira, V. Mauerhofer, F. P. Pratama, M. Trebitsch
Solar and Stellar Astrophysics
Radio Burst Phenomenology of AD Leonis and Associated Signatures of Propagation Effects
Jiale Zhang, Harish K. Vedantham, Joseph R. Callingham et al. (+1 more)
We present the high-resolution
radio dynamic spectra of AD Leonis (AD Leo) between 1.0 and 1.5 GHz taken by the Five-hundred-meter Aperture Spherical
radio Telescope (FAST) on Dec. 1st, 2023. Over a 15-minute period, we identify complex, superimposed spectro-temporal structures, including: (1) broadband, second-long modulation lanes with downward frequency drifts, (2) narrowband ($\approx$ 50 MHz), short-duration S-burst envelopes with upward drifts, and (3) even narrower ($\approx$ 10 MHz), millisecond-scale S-burst striae within these envelopes. Using the discrete
Fourier transform and auto-correlation function, we identify two dominant periodic emission patterns, corresponding to the periodicities of the S-bursts ($\approx0.1$ s) and the striae ($\approx0.01$ s). The complex superposition of diverse time-frequency structures poses a challenge to interpreting all the emission variability as intrinsic to the source. We propose that the modulation lanes could be a propagation effect as the
radio waves traverse an inhomogeneous, regularly structured
plasma region in the AD Leo's magnetosphere. By modelling a
plasma screen with sinusoidal phase variation in one dimension, we show that we could qualitatively reconstruct the observed modulation lanes. The origin of the finest structures, the striae, remains unclear. Our work highlights that propagation effects in the
stellar magnetosphere can potentially probe kilometre-scale structures in the emission regions and provide novel constraints on density inhomogeneities caused by magnetohydrodynamic waves that are difficult to access by other means.
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All authors Jiale Zhang, Harish K. Vedantham, Joseph R. Callingham, Hui Tian
High Energy Astrophysical Phenomena · Cross-listed from nucl-th
Anisotropic flows in Au+Au collisions at $\sqrt{s_{\rm{NN}}} = 2.4\,\text{GeV}$ with a Skyrme pseudopotential
Xin Li, Si-Pei Wang, Rui Wang et al. (+4 more)
Within the framework of the
lattice Boltzmann-Uehling-Uhlenbeck transport model, we present a systematic study of
proton anisotropic flow observables measured by the HADES collaboration, by utilizing the recently developed density-, momentum- and isospin-dependent N$5$LO Skyrme pseudopotential. In particular, we investigate the impacts of the momentum dependence of nucleon mean-field potentials, the stiffness of symmetric
nuclear matter (SNM) EOS, the high-density behaviors of the
symmetry energy and the in-medium modification of nucleon-nucleon elastic cross sections on
proton $v_{1}$, $v_{2}$, $v_{3}$, and $v_{4}$ in Au+Au collisions at $\sqrt{s_{\rm{NN}}} = 2.4\,\text{GeV}$. Our results show that the
proton anisotropic flows are strongly sensitive to the momentum dependence of nucleon mean-field potential as well as the incompressibility coefficient $K_0$ of SNM. In addition, the transverse momentum dependence of the
proton $v_2$ exhibits a modest sensitivity to the higher-order skewness coefficient $J_0$ and kurtosis coefficient $I_0$ of SNM as well as the momentum dependence of the
symmetry potential, while the transverse momentum dependence of the
proton $v_1$ is shown to modestly depend on the in-medium modification of nucleon-nucleon elastic cross sections. Moreover, the high-density
symmetry energy seems to have limited effects on the
proton anisotropic flows. These findings highlight the necessity of considering the momentum dependence of nucleon mean-field potentials including the
symmetry potential, the higher-order characteristic parameters of SNM EOS beyond $K_0$, and the in-medium modification of nucleon-nucleon elastic cross sections, in future
Bayesian transport model analyses on
proton anisotropic flows in heavy-ion collisions at HADES energies, thereby to extract information on
nuclear matter EOS as well as the associated underlying
nuclear effective interactions.
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All authors Xin Li, Si-Pei Wang, Rui Wang, Zhen Zhang, Jie Pu, Chun-Wang Ma, Lie-Wen Chen
Instrumentation and Methods for Astrophysics
Performance Calibration of the Wavefront Sensor's EMCCD Detector for the Cool Planets Imaging Coronagraph Aboard CSST
Jiangpei Dou, Bingli Niu, Gang Zhao et al. (+5 more)
The wavefront sensor (WFS), equipped with an electron-multiplying charge-coupled device (EMCCD) detector, is a critical component of the Cool
Planets Imaging Coronagraph (CPI-C) on the Chinese Space Station
Telescope (CSST). Precise calibration of the WFS's EMCCD detector is essential to meet the stringent requirements for high-contrast
exoplanet imaging. This study comprehensively characterizes key performance parameters of the detector to ensure its suitability for astronomical observations. Through a multi-stage screening protocol, we identified an EMCCD chip exhibiting high resolution and low noise. The electron-multiplying gain (EM Gain) of the EMCCD was analyzed to determine its impact on signal amplification and noise characteristics, identifying the optimal operational range. Additionally, noise properties such as readout noise were investigated. Experimental results demonstrate that the optimized detector meets CPI-C's initial application requirements, achieving high resolution and low noise. This study provides theoretical and experimental foundations for the use of EMCCD-based WFS in adaptive optics and astronomical observations, ensuring their reliability for advanced space-based imaging applications
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All authors Jiangpei Dou, Bingli Niu, Gang Zhao, Xi Zhang, Gang Wang, Baoning Yuan, Di Wang, Xingguang Qian
High Energy Astrophysical Phenomena · Cross-listed from nucl-th
Toward a Unified Understanding of the Dense Matter Equation of State
Kshitij Agarwal, Johannes Jahan, Behruz Kardan et al. (+3 more)
Efforts to understand the equation of state (EOS) of dense
nuclear matter at supra-saturation densities have grown more sophisticated over the past decade, driven by a surge in high-precision data from both terrestrial experiments and astrophysical observations. While for the former, heavy-ion collisions (HIC) represent a unique opportunity to constrain the EOS in a controlled laboratory setting, the latter can be precisely probed thanks to the advent of multi-messenger astronomy (MMA). However, as we move away from understanding drawn from individual sources and limited statistics to the era of precision physics with improved
datasets, the need for a systematic way to combine them becomes clear. In this article, we trace the individual methods for extracting the EOS both for HIC and MMA. We then review the current state-of-the-art collaborative efforts to combine these individual sources of information, focusing on: the
Nuclear Physics and Multi-Messenger Astrophysics (NMMA) framework, which relies on
Bayesian inference methods; the Modular Unified Solver for the Equation of State (MUSES) calculation engine, which integrates EOS priors with HIC data and produces predictions for key
neutron star properties; and the
Bayesian Analysis of
Nuclear Dynamics (BAND) framework, which uses cutting-edge
Bayesian methods to produce reliable and trustworthy predictions for
nuclear and astrophysical problems. We highlight the scientific advances with respect to the EOS and
neutron star properties made possible by each framework and outline the remaining challenges that must be addressed to build a coherent, predictive picture of dense
nuclear matter across all relevant regimes. We conclude with a detailed discussion of how these frameworks might be integrated with each other to form a unified workflow for future EOS predictions.
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All authors Kshitij Agarwal, Johannes Jahan, Behruz Kardan, Peter T. H. Pang, Tom Reichert, Alexandra C. Semposki
High Energy Astrophysical Phenomena · Cross-listed from physics.plasm-ph
The PLUTO Code on GPUs: A First Look at Eulerian MHD Methods
Marco Rossazza, Andrea Mignone, Matteo Bugli et al. (+7 more)
We present preliminary performance results of gPLUTO, the new GPU-optimized implementation of the PLUTO code for computational
plasma astrophysics. Like its predecessor, gPLUTO employs a finite-volume formulation to numerically solve the equations of magnetohydrodynamics (MHD) in multiple spatial dimensions. Still, this new implementation is a complete rewrite in C++ and leverages the OpenACC programming model to achieve acceleration on NVIDIA GPUs. While a more comprehensive description of the code and its several other modules will be presented in a future paper, here we focus on some preparatory results that demonstrate the code potential and performance on pre exa-scale parallel architectures.
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All authors Marco Rossazza, Andrea Mignone, Matteo Bugli, Stefano Truzzi, Lubomir Riha, Tomas Panoc, Ondrej Vysocky, Nitin Shukla, Alessandro Romeo, Vittoria Berta
High Energy Astrophysical Phenomena
Impact of Spectral Coverage on Parameter recovery in Blazar Modeling
N. Sahakyan, D. Bégué, P. Giommi et al. (+2 more)
Understanding the impact of spectral coverage on parameter recovery is critical for accurate interpretation of blazar spectra. In this study, we examine how the data coverage influences the reliability of parameter estimation within the one-zone synchrotron self-Compton (SSC) framework. Using OJ 287, TXS 0506+056, and Mrk 421 as representative of the low-, intermediate- and high synchrotron peak classes (LSP, ISP and HSP), respectively, we generate synthetic SEDs based on their best-fit models and perform 1,000 fits for each of the 21 observational configurations per source type. Our analysis quantifies the coverage probability for all model parameters, such has the
magnetic field strength and the electron luminosity, and reveals that different blazar subclasses exhibit distinct sensitivities to spectral gaps. For LSPs, a minimal
dataset comprising optical/UV, X-ray, and GeV $\gamma$-ray bands is sufficient for robust parameter inference. In contrast, ISPs and HSPs require broader spectral coverage to constrain the physical parameters. For ISP, we find that reliable parameter recovery can be achieved with two different minimal band combinations: (i) X-ray, high energy $\gamma$-ray, and very high energy $\gamma$-ray data, or (ii) optical/UV, X-ray, and high energy $\gamma$-ray data. For HSPs, the minimal configuration enabling reliable parameter recovery includes the optical/UV, X-ray, and very high energy $\gamma$-ray bands. We discuss the role of very high energy $\gamma$-ray observations, showing that they significantly enhance parameter recovery for HSPs. Our results provide practical guidelines for designing optimized multi-wavelength observation campaigns and for assessing the robustness of SSC model inferences under incomplete spectral coverage.
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All authors N. Sahakyan, D. Bégué, P. Giommi, H. Dereli-Bégué, Asaf Pe'er
Earth and Planetary Astrophysics
Projections of Earth's Technosphere: Strategies for Observing Technosignatures on Terrestrial Exoplanets
Jacob Haqq-Misra, Ravi Kopparapu and George Profitiliotis
The search for technosignatures–remotely detectable evidence of extraterrestrial technology–draws upon examples from the recent history of Earth as well as projections of Earth's technosphere. Facilities like the Habitable Worlds Observatory (HWO) will significantly advance the feasibility of characterizing the atmospheres of habitable
exoplanets at visible and near-infrared wavelengths, while other future mission concepts could extend this search to mid-infrared wavelengths. We draw upon a recently developed set of 10 self-consistent scenarios for future Earth technospheres as analogs for extraterrestrial technospheres, which we use to outline a stepwise technosignature search strategy, beginning with HWO and followed by other missions. We find that HWO could reveal elevated abundances of a CO$_2$ + NO$_2$ pair on
planets with combustion and other large-scale industry, which could be observable in up to eight of the 10 scenarios. Follow-up
radio observations could reveal narrowband directed transmissions, as occur in two of the scenarios. Further study involving direct detections at mid-infrared wavelengths with the Large Interferometer for
Exoplanets could reveal spectral features from industry, such as the combinations of CO$_2$ + CFC-11/12 in four scenarios and CO$_2$ + CFC-11/12 + CF$_4$ in one scenario; two of these also include the N$_2$O + CH$_4$ + NH$_3$ triple from large-scale agriculture. Other mission concepts, such as a
solar-gravitational-lens mission, could reveal large-scale surface features in two scenarios that would otherwise show no detectable technosignatures, while an interplanetary flyby or probe mission would be the most conclusive way to reveal the presence of technology on terrestrial
exoplanets.
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High Energy Astrophysical Phenomena
From Empirical to Physical Model: Direct Fits of Optically Thin Inverse Compton Scattering to Prompt GRB Spectra
Pragyan Pratim Bordoloi, Shubh Mittal and Shabnam Iyyani
Gamma-ray burst (GRB)
prompt emission is commonly attributed to non-thermal radiation processes operating in the optically thin regions of a relativistic
outflow. Among these, optically thin inverse-Compton (IC) scattering remains an important yet under-tested mechanism. From an initial set of 41 bursts selected using empirical Band-function criteria that highlight quasi-thermal low-energy slopes ($\alpha > -0.5$) and constrained high-energy indices ($-1.7 > \beta > -3.3$), only four events satisfy these conditions consistently in both time-integrated and time-resolved spectra. The IC fits yield self-consistent constraints on the seed-
photon field and the electron population at the dissipation site. For bulk Lorentz factors $\Gamma \sim 170$-$550$, we infer seed thermal peaks of $\sim 0.05$-$0.2$ keV and electron thermal energies of $\sim 20$-$300$ keV in the co-moving frame. A fraction of only $0.1\%$-$20\%$ of electrons are accelerated into a non-thermal tail with an average index value of $\delta \sim 1.8$. The derived Comptonisation parameters indicate moderate $y$ values ($\sim 1$-$3$), optical depths $\tau \sim 0.2$-$0.6$, and dissipation radii just above the photosphere, consistent with mildly relativistic ($\gamma_{\min} \sim 1.2$-$2.6$),
photon-dominated, low-
magnetic-field dissipation environments. Furthermore, the framework allows us to constrain even sub-dominant thermal components that lie below the detector's low-energy threshold. Taken together, our results show that optically thin IC scattering offers a physically consistent and observationally viable explanation for the
prompt emission in a subset of bright GRBs, motivating the application of IC models in future GRB studies.
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Astrophysics of Galaxies
Tails of Gravity: Persistence of Star Formation in the CMZ Environment
Linjing Feng, Sihan Jiao, Fengwei Xu et al. (+16 more)
We characterize
star-forming gas in six molecular clouds (Sgr B1-off, Sgr B2, Sgr C, the 20 km s$^{-1}$ and 50 km s$^{-1}$ molecular clouds, and the Brick) in the
Galactic central molecular zone (CMZ), and compare their
star-forming activities with those in molecular clouds outside the CMZ. Using multi-band continuum observations taken from ${\it Planck}$, ${\it Herschel}$, JCMT/SCUBA-2, and CSO/SHARC2, we derived 8.5" resolution column density maps for the CMZ clouds and evaluated the column density probability distribution functions (N-PDFs). With the archival Atacama Large Millimeter/submillimeter Array (ALMA) 1.3 mm
dust continuum data, we further evaluated the mass of the most massive cores ($M_{\rm core}^{\rm ma x}$). We find that the N-PDFs of four of the selected CMZ clouds are well described by a piecewise log-normal + power-law function, while the N-PDFs of the remaining two can be approximated by log-normal functions. In the first four targets, the masses in the power-law component ($M_{\rm gas}^{\rm bound}$), $M_{\rm core}^{\rm max}$, and
star formation rate (SFR) are correlated. These correlations are very similar to those derived from low-mass clouds in the
Solar neighborhood and massive
star-forming regions on the
Galactic disk. These findings lead to our key hypotheses: (1) In the extreme environment of the CMZ, the power-law component in the N-PDF also represents self-gravitationally bound gas structures, and (2)
evolution and
star-forming activities of self-gravitationally bound gas structures may be self-regulated, insensitive to the exterior environment on $\gtrsim$5-10 pc scales.
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All authors Linjing Feng, Sihan Jiao, Fengwei Xu, Hauyu Baobab Liu, Xing Lu, Neal J. Evans II, Elisabeth A.C. Mills, Attila Kovács, Qizhou Zhang, Yuxin Lin, Jingwen Wu, Chao-Wei Tsai, Di Li, Zhi-Yu Zhang, Zhiqiang Yan, Hao Ruan, Fangyuan Deng, Yuanzhen Xiong, Ruofei Zhang
Astrophysics of Galaxies
Projection Effects in Barred Galaxies Causing Wrong Interpretation of Radial Flows
E. Salibur, A. Hallé and F. Combes
Galaxy disks in rotation are sometimes the site of radial flows, especially in their gas component. It is important to estimate the
outflows, due to AGN or
supernovae feedback, or inflows due to bar
gravity torques. However, these radial flows may be confused with non-circular motions, which are quite frequent in the center of
galaxy disks. We use a simulated
giant, barred spiral
galaxy from the GalMer database to study the non-circular motions induced by the bar. Our goal is to identify the spurious radial flows that kinematics modeling
algorithms can detect, assuming circular orbits for the gas. Using mock data of a strongly barred
galaxy, we quantify the radial velocities computed by the 3D-Barolo
algorithm for different disk inclinations and several bar orientations in the plane of the sky: along the major and minor kinematic axes and at 45{\deg} from them. Our results show that projection effects cause kinematics modeling
algorithms to confuse the radial component of velocity due to elliptical orbits with significant radial flows with mean values up to 92 km.s$^{-1}$, within the bar region. The computed rotation curve is also wrongly estimated inside the bar region, by as much as 150 km.s$^{-1}$ for the highest inclination.
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High Energy Astrophysical Phenomena
Search for Radio Pulsations from Neutron Star Candidates in Detached Binaries
Shi-Jie Gao, Xiang-Dong Li, Song Wang et al. (+7 more)
Recent optical astrometric and spectroscopic surveys have identified numerous
neutron star (NS) candidates in non-accreting detached binary systems, but their compact-object nature remains unconfirmed. In this work, we present targeted
radio observations of 31 such candidates using the Five-hundred-meter Aperture Spherical
radio Telescope (FAST), the Robert C. Byrd Green Bank
Telescope, and the Shanghai TianMa
Radio Telescope. Over a total of 46.65 hours of observing time, we detected neither periodic nor single-pulse
radio emissions. These nondetections place stringent upper limits on the flux densities of any potential
radio signals, reaching ~4 $\mu$Jy for periodic emission and ~10 mJy for single pulses with FAST. Since our observations are highly sensitive and the flux density upper limits are well below the median fluxes of known
Galactic pulsars, this suggests that
geometric beaming is the most likely explanation for the non-detections if these objects are indeed
pulsars. Alternatively, the NSs may be sufficiently old ($\gtrsim$ 10 Gyr) and have become intrinsically
radio-quiet. In this case, our findings highlight the inherent difficulty of confirming NSs in such old detached binary systems through
radio pulsation searches.
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All authors Shi-Jie Gao, Xiang-Dong Li, Song Wang, Kareem El-Badry, De-Jiang Zhou, Yi-Xuan Shao, Zhen Yan, Pei Wang, Ping Zhou, Jin-Lin Han
Instrumentation and Methods for Astrophysics
Simulating the Stellar Bycatch: Constraining the Prevalence of Extraterrestrial Transmitters within Radio SETI Surveys
Louisa A. Mason, Michael A. Garrett and Andrew P. V. Siemion
Searches for
radio technosignatures place constraints on the prevalence of extraterrestrial transmitters in our
Galaxy and beyond. It is important to account for the complete
stellar population captured within a
radio telescope's field of view, or
stellar 'bycatch'. In recent years, catalogues from ESA's
Gaia mission have enabled SETI surveys to place tighter limits on extraterrestrial transmitter statistics. However,
Gaia remains restricted by magnitude limits, astrometric uncertainty at large distances, and confusion in crowded regions. To address these limitations, we investigate the use of the Besançon
Galactic Model to simulate the statistical underlying
stellar population to derive more realistic constraints on the occurrence of extraterrestrial transmitters. We apply this method to Breakthrough Listen's Enriquez/Price survey, modelling 6,182,364
stellar objects within 1229 individual pointings and extending the search out to distances $\leq 25$kpc. We place limits on the prevalence of high duty cycle transmitters within 2.5kpc, suggesting $\leq (0.000995 \pm 0.000002)\%$ of
stellar systems contain such a transmitter (for near-zero drift rates and EIRP$_{\mathrm{min}} \gtrsim 5 \times 10^{16}$W). In support of broader adoption, we provide a simple calculator tool that enables other researchers to incorporate this approach into their own SETI analyses. Our results enable a more complete statistical estimation of the number and
stellar type of systems probed, thereby strengthening constraints on technosignature prevalence and guiding the analysis of future SETI efforts. We also conclude that SETI surveys are, in fact, much less biased by anthropocentric assumptions than is often suggested.
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Solar and Stellar Astrophysics
Rotation of flux ropes in the low corona
Brigitte Schmieder, Anwesha Maharana, Jin Han Guo et al. (+2 more)
Eruptions of filaments are defined by different parameters, specially, sigmoid handedness and direction of the eruption, which are important parameters for
forecasting the geoeffectiveness of consequent interplanetary coronal mass ejection (ICME) or
magnetic cloud.
Solar filaments often exhibit rotation and deflection during eruptions, which would significantly affect the geoeffectiveness of the coronal mass ejections (CMEs). Therefore, understanding the mechanisms that lead to such lateral displacement of filaments is a great concern to space weather
forecasting. Two case studies are discussed. Firstly, the events of September 8 and September 10 2014, were analyzed from the Sun to the Earth. The numerical heliospheric simulation EUHFORIA shows that the handedness of the EUV sigmoid deduced from coronagraph observations was different from the tilt of the ICME at 1~au, suggesting a rotation of the CME in the low corona. A potential undetected low coronal rotation led to erroneous space weather prediction. The second event concerns a filament observed on August 20 2021, which underwent a rotation of 73 degrees during its eruption, implying a significant lateral drifting of the filament material. A data-constrained magnetohydrodynamic (MHD) simulation confirms such a rotation. These two studies reinforce the idea that CMEs are subjected to more significant rotation and deflection in the low corona than during their journey in the heliosphere.
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All authors Brigitte Schmieder, Anwesha Maharana, Jin Han Guo, Luis Linan, Stefaan Poedts
Cosmology and Nongalactic Astrophysics
The Evolving Baryonic Tully Fisher Relation: A Universal Law from Galaxies to Galactic Clusters
Stuart Marongwe and Stuart Kauffman
The Baryonic Tully-Fisher relation (BTFR) links the baryonic mass of
galaxies to their characteristic rotational velocity and has been shown to hold with remarkable precision across a wide mass range. Recent studies, however, indicate that
galaxy clusters occupy a parallel but offset relation, raising questions about the universality of the BTFR. Here, we demonstrate that the offset between
galaxies and clusters arises naturally from
cosmic time
evolution. Using the evolving BTFR derived from the Nexus Paradigm of
quantum gravity, we show that the normalization of the relation evolves as an exponential function of
cosmic time., while the slope remains fixed at $\sim 4$. This provides a simple and predictive framework in which both
galaxies and clusters obey the same universal scaling law, with their apparent offset reflecting their different formation epochs. Our results unify mass-velocity scaling across five orders of magnitude in baryonic mass, offering new insights into
cosmic structure formation.
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Astrophysics of Galaxies
Search for the potential electromagnetic counterparts of neutrino events in SDSS galaxies at z<0.1
O. Sergijenko., I.B. Vavilova, I.O. Izviekova et al. (+1 more)
Identification of electromagnetic emission in coincidence with high-energy
neutrinos is fundamentally important for multimessenger astronomy. Such observations are essential for constraining source localization, determining the source type, and understanding emission mechanisms. Typically, they require following up a
neutrino alert (IceCube issues two alert streams: Gold, with at least 50 percent probability of astrophysical origin, and Bronze, with at least 30 percent probability) with an electromagnetic facility, primarily in X-ray and gamma-ray bands. Another approach involves electromagnetic monitoring of hot spots in the IceCube skymap, i.e., positions exceeding the instrument sensitivity. An alternative method consists in performing correlation analysis across available
neutrino events and source catalogs. We searched for spatial coincidence between
galaxies from SDSS and high-energy
neutrino events. The analysis includes IceCube Gold alerts and
neutrino-electromagnetic coincidence events from AMON (Astrophysical Multimessenger Observatory Network), identified through the end of September 2025. We examined
galaxies from the morphological catalog at
redshifts 0.02 to 0.1, which contains 315,776 SDSS DR9 objects with absolute
stellar magnitudes in the range from -24 to -13 in the r band. Among 59 IceCube Gold alerts, we found three with only one
galaxy (SDSS J231231.52+033415.1) within the 50 percent containment radius. Among 24
neutrino-electromagnetic coincidence events, three more contain only one
galaxy (SDSS J220711.14+122535.9) within the same radius. These six
galaxies represent the most promising candidates for potential host
galaxies of
neutrino sources. We summarize their available multiwavelength data and the ZTF light curves obtained from 2018 to 2025.
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All authors O. Sergijenko., I.B. Vavilova, I.O. Izviekova, D.R. Karakuts
Astrophysics of Galaxies
Gravitational potential drives the concentration dependence of the stellar mass-halo mass relation
Kai Wang, Joop Schaye, Alejandro Benítez-Llambay et al. (+8 more)
We investigate the origin of the scatter in the
stellar mass-
halo mass (SMHM) relation using the \colibre cosmological hydrodynamical simulations. At fixed
halo mass, we find a clear positive correlation between
stellar mass and
halo concentration, particularly in low-mass
haloes between $10^{11}$ and $10^{12}\,\rm M_\odot$, where all
halo properties are computed from the corresponding dark-matter-only simulation. Two scenarios have been proposed to explain this trend: the earlier formation of higher-concentration
haloes allows more time for
star formation, or the deeper gravitational potential wells of higher-concentration
haloes enhance
baryon retention. To distinguish between them, we examine correlations between
halo concentration,
stellar mass,
stellar age, and
stellar metallicity. While, at fixed
halo mass,
halo concentration correlates with
stellar age,
stellar age itself shows only a weak correlation with
stellar mass, indicating that early formation alone cannot account for the concentration-dependence in the scatter of the SMHM relation. In contrast, both
stellar metallicity and
halo concentration exhibit correlations with
stellar mass. The connection between
halo concentration and
stellar metallicity persists even when simultaneously controlling for both
halo mass and
stellar mass. These results support the scenario in which the deeper gravitational potentials in higher-concentration
haloes suppress feedback-driven
outflows, thereby enhancing both
baryon and metal retention.
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All authors Kai Wang, Joop Schaye, Alejandro Benítez-Llambay, Evgenii Chaikin, Carlos S. Frenk, Filip Huško, Robert J. McGibbon, Sylvia Ploeckinger, Alexander J. Richings, Matthieu Schaller, James W. Trayford