Current date: 2025-11-25
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Datestamp limit: 2025-11-25 (0 days ago)
Created/updated limit: 2025-11-18 (7 days ago)
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Number of records retrieved: 1016
Keyword score statistics
score 12 -- 1 abstracts
score 11 -- 1 abstracts
score 10 -- 1 abstracts
score 7 -- 2 abstracts
score 6 -- 2 abstracts
score 5 -- 6 abstracts
score 4 -- 5 abstracts
score 3 -- 15 abstracts
score 2 -- 19 abstracts
in total -- 52 abstracts
Articles that appeared on 2025-11-25
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[abstract 1 / 52] Wow! (score: 12)
- Title: Kinematics show consistency between stellar mass and supermassive BLACK HOLE parent population JET speedsAuthors: Clara Lilje, Rob Fender, James H. Matthews,Comments: Accepted for publication in MNRASSubjects: astro-ph.HECreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
Jets from stellar-mass and supermassive BLACK HOLEs provide the unique opportunity to study similar processes in two very different mass regimes. Historically, the apparent speeds of BLACK HOLE x-ray binary (BHXRBs) JETs have been observed to be lower than JET speeds from ACTIVE GALACTIC NUCLEi (AGN) and specifically BLAZARs. In this work, we show that selection effects could be the primary cause of the observed population differences. For the first time, it is possible to perform a statistical analysis of the underlying BHXRB JET Lorentz factor distribution. We use both the Anderson-Darling test and apply nested sampling to this problem. With Bayes factors, we confirm that the Lorentz factor distribution of BHXRBs is best described with a power law, the same model that has been applied to AGN JETs. For a Lorentz factor distribution following $\rm N(Γ) \propto Γ^b$ we find a value for the exponent of $b=-2.64_{-0.55}^{+0.46}$. This exponent is consistent with values found in AGN population studies, within $1σ$ for \textit{SWIFT}-BAT and \textit{FERMI}-LAT selected AGN. The best-fit exponent for the radio selected MOJAVE sample is just above our $2 σ$ limit. This is a remarkable agreement given the different scales at which the JETs are observed. The observed slower apparent speeds in BHXRBs are largely due to the much larger inclinations in this sample. Furthermore, nested sampling confirms that $Γ_{\rm max}$ is completely unconstrained using this method. Therefore, based on kinematics alone, BHXRB JETs are broadly consistent with being just as RELATIVISTIC as those from supermassive BLACK HOLEs.
[abstract 2 / 52] Wow! (score: 11) - Title: The variability of BLAZARs throughout the electroMAGNETic spectrumAuthors: Claudia M. Raiteri,Comments: Review article published by The Astronomy and Astrophysics ReviewSubjects: astro-ph.HE astro-ph.GACreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
With their JET pointing towards us, BLAZARs are ideal tools to study the physics and structure of extragalactic JETs. Their powerful JETs are cosmic particle accelerators and are alleged to be one of the production sites of the high-energy neutrinos detected by the IceCube Observatory. Doppler beaming of the JET nonthermal radiation increases BLAZAR brightness, blue-shifts their emission, and shortens their variability time scales, which are observed to range from years down to minutes. This review will focus on BLAZAR flux, spectral, and POLARIZATION variability across the electroMAGNETic spectrum. Interpretation of BLAZAR variability calls into question both intrinsic and extrinsic mechanisms. Shock waves, MAGNETic RECONNECTion, and turbulence can accelerate particles inside the JET, while JET precession, rotation, and twisting can produce variations in Doppler beaming. Microvariability puts strong constraints on the size of the emitting regions, suggesting a multizone emitting JET. Twisting JETs have been proposed to explain the long-term multiwavelength variability. They are supported by radio observations of bent or helical JETs, and by results of RELATIVISTIC MAGNETohydrodynamics simulations of plasma JETs. Detection of (quasi)periodic behaviour has been ascribed to orbital motion in BLACK HOLE binary systems, JET precession, kink instabilities developing inside the JET, or perturbations in the accretion disc. Gravitational microlensing has been suggested to explain BLAZAR behaviour in some cases. Polarization provides information on the structure and behaviour of the MAGNETic field in the emission zones. Both the degree and angle of POLARIZATION can show strong and fast variability, which is sometimes correlated with flux. The interpretation of flux, spectral, and POLARIZATION variability within a consistent picture challenges current models of BLAZAR variability.
[abstract 3 / 52] Wow! (score: 10) - Title: TXS 0506+056-like BLAZAR sources and their role as possible neutrino emittersAuthors: Ilaria Viale, Giacomo Principe, Chiara Righi, Matteo Cerruti, Fabrizio Tavecchio, Elisa Bernardini,Comments: Accepted for publication in Astroparticle PhysicsSubjects: astro-ph.HECreated: 2025-11-23; Updated: 2025-11-25; Datestamp: 2025-11-25
The interest in BLAZARs as candidate neutrino emitters grew after the 3$σ$ evidence for a contemporaneous joint photon and neutrino emission from the flaring BLAZAR TXS 0506+056 in 2017. Blazars, a class of extragalactic sources with RELATIVISTIC JETs pointing toward Earth, present a broadband emission interpretable via leptonic and hadronic processes, the latter relevant for proton acceleration and neutrino production. Several emission models have been developed to explain this multi-messenger observation, but the details of the neutrino production and the nature of TXS 0506+056 are not yet fully understood. In this work we investigate the properties of sources similar to TXS 0506+056. We select a sample of BLAZARs from the FERMI 4LAC-DR2 catalog by constraining a number of key parameters in ranges centered on TXS 0506+056 values. We estimate their disk accretion efficiency and model their spectral energy distribution (SED) in terms of lepto-hadronic emission, gaining information respectively on the potential similarity of their environment with that of TXS 0506+056 and on their neutrino flux and detectability prospects at TeV energies. Our study shows the candidates' high energy emission to be dominated by leptonic processes. Part of them also show a high accretion rate, characteristic of FSRQs. For these sources, the very high energy (VHE) and neutrino fluxes appear undetectable by current and future instruments in an average emission state.
[abstract 4 / 52] Wow! (score: 7) - Title: Transition to Petschek Reconnection in SubRELATIVISTIC Pair Plasmas: Implications for Particle AccelerationAuthors: Adam Robbins, Anatoly Spitkovsky,Comments: 13 pages, 9 figures, accepted to ApJ. Comments welcomeSubjects: physics.plasm-ph astro-ph.HECreated: 2025-11-22; Updated: 2025-11-25; Datestamp: 2025-11-25
While RELATIVISTIC MAGNETic RECONNECTion in pair plasmas has emerged in recent years as a candidate for the origin of radiation from extreme astrophysical environments, the corresponding subRELATIVISTIC pair plasma regime has remained less explored, leaving open the question of how RELATIVISTIC physics affects RECONNECTion. In this paper, we investigate the differences between these regimes by contrasting 2D particle-in-cell simulations of RECONNECTion in pair plasmas with RELATIVISTIC MAGNETization ($σ\gg 1$) and subRELATIVISTIC MAGNETization ($σ< 1$). By utilizing unprecedentedly large domain sizes and outflow boundary conditions, we demonstrate that lowering the MAGNETization results in a change in the RECONNECTion geometry from a plasmoid chain to a Petschek geometry, where laminar exhausts bounded by slow-mode shocks emanate from a single diffusion region. We attribute this change to the reduced plasmoid production rate in the low-$σ$ case: when the secondary tearing rate is sufficiently low, plasmoids are too few in number to prevent the system from relaxing into a stable Petschek configuration. This geometric change also affects particle energization: we show that while high-$σ$ plasmoid chains generate power-law energy spectra, low-$σ$ Petschek exhausts merely heat incoming plasma and yield negligible nonthermal acceleration. These results have implications for predicting the global current sheet geometry and the resulting energy spectrum in a variety of systems.
[abstract 5 / 52] Wow! (score: 7) - Title: $\mathtt{Entity}$ -- Hardware-agnostic Particle-in-Cell Code for Plasma Astrophysics. II: General Relativistic ModuleAuthors: Alisa Galishnikova, Hayk Hakobyan, Alexander Philippov, Benjamin Crinquand,Comments: 22 pages, 5 figures, 1 tableSubjects: astro-ph.HECreated: 2025-11-21; Updated: 2025-11-25; Datestamp: 2025-11-25
Black hole environments often host plasmas that are fully collisionless or contain intrinsically collisionless regions, including RELATIVISTIC JETs and coronae where particle energization is ubiquitous. Capturing the physics of these systems requires numerical methods capable of modeling RELATIVISTIC, MAGNETized, collisionless plasmas in strong gravitational fields. In this work, we introduce the general-RELATIVISTIC module for the Entity -- the first open-source, coordinate-agnostic performance-portable particle-in-cell code. The code enables fast axisymmetric simulations of collisionless plasmas around BLACK HOLEs on any modern high-performance computing architecture (both GPUs and CPUs).
[abstract 6 / 52] Yes (score: 6) - Title: GRB 240715A: Revealing Novel Intrinsic Mechanism by Different Individual PulseAuthors: Wen-Jun Tan, Chen-Wei Wang, Shao-Lin Xiong, Shi-Jie Zheng, Jiang He, Xiao-Yun Zhao, Yue Huang, Shu-Xu Yi, Bing Li, He Gao, Bo-bing Wu, Bing Zhang, Frederic Daigne, Maria-Grazia Bernardini, Bin-Bin Zhang, Stephane Basa, Bertrand Cordier, Jin-Song Deng, Yong-Wei Dong, Damien Dornic, Olivier Godet, Xu-Hui Han, Mao-Hai Huang, Cyril Lachaud, Hua-Li Li, Pierre Maggi, Frederic Piron, Yu-Lei Qiu, Stephane Schanne, Li-Ming Song, Damien Turpin, Susanna Vergani, Jing Wang, Ping Wang, Jian-Yan Wei, Chao Wu, Li-Ping Xin, Yang Xu, Li Zhang, Shuang-Nan Zhang,Comments: 21 pages, 4 figures, accepted by The Astrophysical Journal LettersSubjects: astro-ph.HECreated: 2025-11-23; Updated: 2025-11-25; Datestamp: 2025-11-25
The Space-based multiband astronomical Variable Objects Monitor (SVOM), detected its first short GAMMA-RAY BURST, GRB 240715A, in-flight, which was jointly observed by FERMI. Based on observational data of SVOM/GRM and FERMI/GBM, we perform a comprehensive temporal and spectral analysis for individual pulse in the prompt emission of this burst, and novel characteristics are revealed. Firstly, opposite evolutions of spectral lag are found in the first and third pulse of this burst. Second, the large negative lag of the first pulse is an outlier in short GRB sample, especially when the pulse duration is considered. Spectral analysis shows that the negative lag of the first pulse is caused by the evolution of spectrum index, and is irrelevant to Epeak, which is inconsistent with the previous study. The intrinsic mechanism is probably attributed to electron cooling in the decaying MAGNETic field, which leads to the continuous hardening of the spectrum index and results in negative lag. Furthermore, spectral analysis also shows that the third pulse is more likely to be described by a quasi-thermal spectrum, indicating the existence of photospheric emission. It is difficult to explain how the SYNCHROTRON radiation appears before photospheric emission in a single GRB and some assumptions are discussed.
[abstract 7 / 52] Yes (score: 6) - Title: Gamma-ray Time Delay and Magnification Ratio in the Gravitationally-Lensed Blazar PKS 1830-211Authors: S. Buson, M. De Toma, S. Larsson, C. C. Cheung, P. Cristarella Orestano, S. Ciprini, C. Spingola, M. Razzano, A. Dominguez, M. Ajello, S. Cutini,Comments: Under review; feedback welcomeSubjects: astro-ph.HECreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
We present the characterization of macrolensing properties of the gravitationally lensed system PKS 1830-211, utilizing data from the FERMI Large Area Telescope. While at gamma-rays we can not spatially resolve the lensed images, a macrolensing-induced time pattern is expected in the BLAZAR's lightcurve, resulting from the delay between variable gamma-ray components originating from its two brightest lensed images. Compared to our previous study, here we employ high-quality lightcurves coupled with prolonged outburst activity, and improved time-series techniques. Analyzing six independent data segments, we identified a delay of 20.26 +/- 0.62 days (statistical and stochastic uncertainty), with a chance detection probability at the 2.5 x $10^{-5}$ level (post-trial). We also present a novel approach to the magnification ratio estimate based on a comparison with simulated data. Our work suggests that the gamma-ray flux ratio between the two main lens components is $μ_γ \lesssim$ 1.8. We do not observe convincing evidence of microlensing effects, as previously claimed. The measured gamma-ray time delay is in 2-sigma tension with radio-based estimates, suggesting either distinct emission sites, underestimated radio uncertainties, or gamma-ray production in a region opaque to radio. Our study highlights the potential of well sampled lightcurves and advanced time-series techniques to distinguish true lensing-induced delays from stochastic variability. When combined with improved radio constraints and refined lens models, PKS 1830-211 and similar sources constitute promising systems for time-delay cosmography, offering new insights into both JET structure and cosmological parameters.
[abstract 8 / 52] Yes (score: 5) - Title: The Compton-Getting origin of the large-scale anisotropy of Galactic COSMIC RAYsAuthors: Bing-qiang Qiao, Wei Liu, Huirong Yan, Yi-qing Guo,Comments: 11 pages, 6 figures, accepted by APJSubjects: astro-ph.HECreated: 2025-11-22; Updated: 2025-11-25; Datestamp: 2025-11-25
Recent studies suggest that the anisotropy in cosmic-ray arrival directions can provide insight into local acceleration sites and propagation conditions. We developed a unified framework to interpret both the observed energy spectra and the large-scale anisotropy. In this work, we explore the influence of the Sun's motion relative to the local plasma frame - the Compton-Getting (CG) effect - on the anisotropy. We find that incorporating the CG effect could slightly reduce the dipole amplitude and shift the phase away from the direction of the local regular MAGNETic field at tens of TeV. At lower energies, where the anisotropy from the cosmic-ray density gradient is weak, the Sun's relative motion becomes more prominent. Below $\sim 200$ GeV, the dipole amplitude increases again, approaching the value expected from the CG effect. Additionally, a phase flip is observed at a few hundred GeV, aligning with the CG direction. Future anisotropy measurements from $100$ GeV to TeV energies could serve as a critical test of this effect.
[abstract 9 / 52] Yes (score: 5) - Title: Anisotropic Cosmic Ray Transport in strong MHD Turbulence due to Magnetic Mirroring and Resonant Curvature ScatteringAuthors: Jeremiah Lübke, Frederic Effenberger, Mike Wilbert, Horst Fichtner, Rainer Grauer,Comments: 9 pages, 6 figures. Comments welcome!Subjects: astro-ph.HE physics.plasm-phCreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
The transport of COSMIC RAYs through turbulent astrophysical plasmas still constitutes an open problem. Building on recent progress, we study the combined effect of MAGNETic mirroring and resonant curvature scattering on parallel and perpendicular transport. We conduct test-particle simulations in snapshots of an anisotropic MAGNETohydrodynamics simulation with $δB/B_0\sim 1$ and record MAGNETic moment variation and field line curvature around pitch-angle reversals. We find for strongly MAGNETized particles that (i) pitch-angle reversals may occur either in coherent regions of the field with small variation of the MAGNETic moment via MAGNETic mirroring or in chaotic regions of the field with strong variation of the MAGNETic moment via resonant curvature scattering; (ii) parallel transport can be modeled as a Lévy walk with a truncated power-law distribution based on pitch-angle reversal times; and (iii) perpendicular transport is enhanced by resonant curvature scattering in synergy with chaotic field line separation and diminished by MAGNETic mirroring due to confinement in locally ordered field line bundles. While MAGNETic mirroring constitutes the bulk of reversal events, resonant curvature scattering additionally acts on trajectories that fall in the loss cones of typical mirroring structures and thus provides the cut-off for the reversal time distribution. Our results, which highlight the role of the MAGNETic field line geometry in cosmic-ray transport processes, are consistent with energy-independent diffusion coefficients. We conclude by considering how energy-dependent observations could arise from an intermittently inhomogeneous interstellar medium.
[abstract 10 / 52] Yes (score: 5) - Title: HST Confirms Sub-5 kpc Dual Quasar Pairs at Cosmic NoonAuthors: Qian Wang, Xuheng Ding, John Silverman, J. Xavier Prochaska, Tommaso Treu, Hassen M. Yesuf, Andrew D. Goulding, Masatoshi Imanishi, Nobunari Kashikawa, Issha Kayo, Kotaro Kohno, Kai Liao, Yoshiki Matsuoka, Michael A. Strauss, Shenli Tang,Comments: 11 pages, 6 figures, 1 table. revised version after resubmissionSubjects: astro-ph.GACreated: 2025-11-23; Updated: 2025-11-25; Datestamp: 2025-11-25
During cosmic noon ($z\sim1-3$), when both STAR FORMATION and BLACK HOLE growth peaked, galaxy mergers are predicted to trigger dual ACTIVE GALACTIC NUCLEi (AGN) that eventually coalesce as supermassive BLACK HOLE (SMBH) binaries. However, observations of dual QUASARs with sub-5 kpc separations-the critical phase preceding final coalescence-have remained challenging due to angular resolution limitations. We present the discovery and confirmation of two sub-arcsecond dual QUASARs at $z>1$, selected from 59,025 SDSS QUASARs, which fall within the footprint of the Hyper Suprime-Cam Survey. Using high-resolution Hubble Space Telescope (HST) imaging and slitless spectroscopy, we confirmed SDSS J1625+4309 ($z=1.647$, separation 0.55"/4.7 kpc) and SDSS J0229$-$0514 ($z=3.174$, separation 0.42"/3.2 kpc), probing the sub-5 kpc separation regime. Through novel combination of WFC3/IR direct imaging (F140W) and grism spectroscopy (G141), we resolve both components morphologically and spectroscopically confirm their dual nature via detection of H$β$+[OIII] and MgII emission lines in each nucleus. Two-dimensional image decomposition reveals distinct host galaxy morphologies: J1625+4309 shows an extended, disturbed structure ($R_e$=4.7 kpc) indicative of an ongoing major merger, while J0229$-$0514 exhibits a compact host ($R_e$=1.4 kpc) suggesting an advanced coalescence stage. Black hole mass estimates based on virial relations yield M$_{\mathrm{BH}} \sim 10^{8.1}-10^{8.7} M_\odot$ with line-of-sight velocity offsets of $(0.7\pm0.1)\times10^{3}$ km s$^{-1}$ and $(1.0\pm0.2)\times10^{3}$ km s$^{-1}$, respectively. These confirmations directly constrain the frequency and properties of close dual QUASARs, opening new avenues for studying SMBH mergers at cosmic noon.
[abstract 11 / 52] Yes (score: 5) - Title: Entity -- Hardware-agnostic Particle-in-Cell Code for Plasma Astrophysics. I: Curvilinear Special Relativistic ModuleAuthors: Hayk Hakobyan, Ludwig M. Böss, Yangyang Cai, Alexander Chernoglazov, Alisa Galishnikova, Evgeny A. Gorbunov, Jens F. Mahlmann, Alexander Philippov, Siddhant Solanki, Arno Vanthieghem, Muni Zhou,Comments: 30 pages, 12 figuresSubjects: astro-ph.HE physics.plasm-phCreated: 2025-11-21; Updated: 2025-11-25; Datestamp: 2025-11-25
Entity is a new-generation, fully open-source particle-in-cell (PIC) code developed to overcome key limitations in astrophysical plasma modeling, particularly the extreme separation of scales and the performance challenges associated with evolving, GPU-centric computing infrastructures. It achieves hardware-agnostic performance portability across various GPU and CPU architectures using the Kokkos library. Crucially, Entity maintains a high standard for usability, clarity, and customizability, offering a robust and easy-to-use framework for developing new algorithms and grid geometries, which allows extensive control without requiring edits to the core source code. This paper details the core general-coordinate special-RELATIVISTIC module. Entity is the first PIC code designed to solve the Vlasov-Maxwell system in general coordinates, enabling a coordinate-agnostic framework that provides the foundational structure for straightforward extension to arbitrary coordinate geometries. The core methodology achieves numerical stability by solving particle equations of motion in the global orthonormal Cartesian basis, despite using generalized coordinates like Cartesian, axisymmetric spherical, and quasi-spherical grids. Charge conservation is ensured via a specialized current deposition technique using conformal currents. The code exhibits robust scalability and performance portability on major GPU platforms (AMD MI250X, NVIDIA A100, and Intel Max Series), with the 3D particle pusher and the current deposition operating efficiently at about 2 nanoseconds per particle per timestep. Functionality is validated through a comprehensive suite of standard Cartesian plasma tests and the accurate modeling of RELATIVISTIC MAGNETospheres in curvilinear axisymmetric geometries.
[abstract 12 / 52] Yes (score: 5) - Title: Cosmogenic Origin of KM3-230213A: Delayed Gamma-Ray Emission from A Cosmic-Ray TransientAuthors: Sovan Boxi, Saikat Das, Nayantara Gupta,Comments: 8 pages, 7 figuresSubjects: astro-ph.HECreated: 2025-11-22; Updated: 2025-11-25; Datestamp: 2025-11-25
The highest-energy cosmic neutrino detected by the ARCA detector of KM3NeT has reignited the quest to pinpoint the sources of ultrahigh-energy COSMIC RAYs (UHECRs; $E\gtrsim 0.1$ EeV). By uncovering the associated multimessenger signals, we investigate the origin of the 220 PeV $ν_μ$ event KM3-230213A from a transient source that accelerated COSMIC RAYs to $\sim 10$ EeV. UHECR protons that escape the source interact with the cosmic background radiation, producing a PeV-EeV cosmogenic neutrino spectrum. The secondary $e^\pm$ and $γ$-rays initiate an electroMAGNETic cascade, resulting in a cosmogenic $γ$-ray spectrum that peaks at a delayed time due to deflection of charged particles in the extragalactic MAGNETic field (EGMF). Our results shed light on the nature of the UHECR source for the $ν_μ$ event and provide crucial insights into the detection of multi-TeV $γ$-rays of cosmogenic origin from similar past cosmological transients. Using the $γ$-ray sensitivity of currently operating and next-generation imaging atmospheric Cherenkov telescopes, the flux and time-delay distribution can constrain the source distance. We further show that the detection of such a $γ$-ray signal above the background depends on the EGMF strength. Together with the non-detection of coincident spatial or temporal photon counterparts at the current epoch, this detection is the first compelling candidate for a sub-EeV cosmogenic neutrino.
[abstract 13 / 52] Yes (score: 5) - Title: Insights into JET-NLR energetics in PMN J0948+0022Authors: B. Dalla Barba, L. Foschini, M. Berton, A. Lähteenmäki, M. Tornikoski, E. Sani, L. Crepaldi, E. Congiu, G. Venturi, W. J. Hon, A. Vietri,Comments: 7 pages, proceeding of the 15SCSLSASubjects: astro-ph.HE astro-ph.GACreated: 2025-11-23; Updated: 2025-11-25; Datestamp: 2025-11-25
The analysis of the optical spectra of PMN J0948+0022 showed significant variations in the spectral lines that, when combined with the FERMI $γ$-ray light curve and radio observations reported by other authors, were interpreted as the result of interactions between the RELATIVISTIC JET and the narrow-line region (NLR). In this work, we present order-of-magnitude calculations of the energetics associated with this proposed JET-NLR interaction. We demonstrate that the observed outflows are capable of absorbing a fraction of the JET energy and converting it into kinetic energy. This mechanism provides a natural explanation for the optical spectral variability recorded with the X-shooter and Multi-Unit Spectroscopic Explorer (MUSE) instruments. Our results support the scenario in which feedback from the RELATIVISTIC JET can dynamically influence the circumnuclear gas, offering new insights into the coupling between JETs and the NLR in $γ$-ray-emitting narrow-line Seyfert 1 galaxies.
[abstract 14 / 52] Yes (score: 4) - Title: A Targeted Gamma-Ray Search of Five Prominent Galaxy Merger Systems with 17 years of FERMI-LAT DataAuthors: Siddhant Manna, Shantanu Desai,Comments: 16 pages, 16 figures. Published in the Open Journal of AstrophysicsSubjects: astro-ph.HE astro-ph.CO astro-ph.GACreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
Galaxy mergers are among the most energetic astrophysical phenomena, driving intense STAR FORMATION and potentially fueling COSMIC RAY acceleration, which can produce high energy $γ$-ray emission through hadronic processes. We present a targeted search for $γ$-ray emission from five prominent galaxy merger systems, NGC~3256, NGC~660, UGC~813/816, UGC~12914/12915, and VV~114 using 16.9 years of FERMI-LAT data in the 1--300~GeV energy range. Employing a binned maximum likelihood analysis, we model the emission with power-law spectra and derive spectral energy distributions (SEDs) to constrain $γ$-ray fluxes and spectral indices. Marginal detections are found for NGC~3256 (TS = 15.4, $\sim$3.51$σ$) and NGC~660 (TS = 8.16, $\sim$2.39$σ$), with photon fluxes of $(7.21 \pm 3.17) \times 10^{-11}$ and $(8.28 \pm 3.56) \times 10^{-11}$ ph cm$^{-2}$ s$^{-1}$, respectively, suggesting merger driven STAR FORMATION contributes to $γ$-ray emission. The remaining systems yield non-detections (TS $< 5$). This is the first targeted study of $γ$-ray emission from these aforementioned galaxy merger systems.
[abstract 15 / 52] Yes (score: 4) - Title: Revisiting Very High Energy Gamma-Ray Absorption in Cosmic Propagation under the Combined Effects of Axion-Like Particles and Lorentz ViolationAuthors: Longhua Qin, Jiancheng Wang, Chuyuan Yang, Huaizhen Li, Quangui Gao, Ju Ma, Ao Wang, Weiwei Na, Ming Zhou, Zunli Yuan, Chunxia Gu, Guangbo Long,Comments: The paper has been submitted, Discussions are welcomeSubjects: astro-ph.HE hep-phCreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
Very high energy (VHE) gamma rays with energies above 100 GeV are expected to experience strong attenuation during cosmic propagation due to pair production with the extragalactic background light (EBL). However, recent observations-particularly the detection of GRB 221009A with photons up to 18 TeV by LHAASO and a 300 TeV photon by Carpet-3,pose a significant challenge to conventional EBL absorption models. These extraordinarily high-energy photons suggest the presence of new physics influencing photon propagation over cosmological distances. The gamma-ray spectrum in the tens-to-hundreds of TeV range provides a powerful probe of possible Lorentz invariance violation (LIV) or photon-axion-like particle (ALP) mixing in cosmic MAGNETic fields. Yet, when treated independently, neither LIV nor ALPs can fully explain the observed transparency of the Universe to VHE gamma rays. In this work, we propose a unified framework that combines both effects-ALPs and LIV-to account for the unexpectedly high survival probability of VHE photons. We analyze the multi-wavelength spectrum of GRB 221009A under this hybrid model and demonstrate that the combined influence of ALPs, characterized by a coupling constant $g_{aγ} = 1.685 \times 10^{-10},\mathrm{GeV}^{-1}$ and mass ($m_a = 9.545 \times 10^{-8},\mathrm{eV}$) alongside second-order LIV characterized by an energy scale $E_{\rm LIV,2} = (1.30_{-0.35}^{+0.56}) \times 10^{-7} E_{\rm Pl}$ adopted from the literature, significantly enhances the photon survival probability across the 10-300 TeV range. This synergistic ALP-LIV model provides a coherent explanation for the observed extreme-energy transparency of the Universe and the delayed arrival of ultra-high-energy photons, offering valuable insights into physics beyond the Standard Model.
[abstract 16 / 52] Yes (score: 4) - Title: Broadband X-ray observations of the periodic optical source ZTF J185139.81+171430.3 and its identification as a massive intermediate polarAuthors: Ren Deng, Kaya Mori, Eric Miao, Gabriel Bridges, Charles J. Hailey, David A. H. Buckley, Gavin Ramsay, Dan Jarvis,Comments: 13 pages, 9 figures, submitted to ApJSubjects: astro-ph.HECreated: 2025-11-21; Updated: 2025-11-25; Datestamp: 2025-11-25
We present X-ray observations of the periodic optical source ZTF J185139.81+171430.3 (hereafter ZTF J1851) by the XMM, NICER and NUSTAR telescopes. The source was initially speculated to be a white dwarf (WD) pulsar system due to its short period ($P\sim12$ min) and highly-modulated optical lightcurves. Our observations revealed a variable X-ray counterpart extending up to 40 keV with an X-ray luminosity of $L_X \sim 3\times10^{33}$ erg s$^{-1}$ (0.3--40 keV). Utilizing timing data from XMM and NICER, we detected a periodic signal at $P_{\rm spin}=12.2640(7)\pm0.0583$ min with $>6σ$ significance. The pulsed profile displays $\sim 25\%$ and $\sim10\%$ modulation in the 0.3--2 and 2--10 keV bands, respectively. Broadband X-ray spectra are best characterized by an absorbed optically-thin thermal plasma model with $kT \approx 25$ keV and a Fe K-$α$ fluorescent line at 6.4 keV. The bright and hard X-ray emission rules out the possibility of a WD pulsar or ultra-compact X-ray binary. The high plasma temperature and Fe emission lines suggest that ZTF J1851 is an intermediate polar spinning at 12.264 min. We employed an X-ray spectral model composed of the accretion column emission and X-ray reflection to fit the broadband X-ray spectra. Assuming spin equilibrium between the WD and the inner accretion disk, we derived a WD mass range of $M_{\rm WD}=(1.07\rm{-}1.32)M_{\odot}$ exceeding the mean WD mass of IPs ($\langle M_{\rm WD} \rangle = 0.8 M_\odot)$. Our findings illustrate that follow-up broadband X-ray observations could provide unique diagnostics to elucidate the nature of periodic optical sources anticipated to be detected in the upcoming Rubin all-sky optical surveys.
[abstract 17 / 52] Yes (score: 4) - Title: General RELATIVISTIC Lagrangian continuum theories -- Part II: electroMAGNETic fluids and solids with junction conditionsAuthors: Francçois Gay-Balmaz,Comments: 58 pages; 2 figuresSubjects: math-ph gr-qc math.MPCreated: 2025-11-23; Updated: 2025-11-25; Datestamp: 2025-11-25
We develop a covariant variational framework for RELATIVISTIC electroMAGNETic continua (fluids and solid) based on Hamilton's principle formulated directly in the material description. The approach extends the geometric theory of RELATIVISTIC continua introduced in Part I to include POLARIZATION, MAGNETization, and general elastic-electroMAGNETic coupling through a unified energy functional. By exploiting spacetime and material covariance, the framework yields the corresponding spacetime and convective variational principles, together with transparent expressions for the stress-energy-momentum tensor and the covariant Euler-type balance equations governing nonlinear electroMAGNETic continua. Coupling to general relativity is naturally incorporated, and when the action is augmented with Gibbons-Hawking-York boundary terms, the gravitational and electroMAGNETic junction conditions follow directly from the variational formulation. The results provide a coherent foundation for modeling nonlinear electroMAGNETic continua in RELATIVISTIC regimes, with relevance to astrophysical systems where RELATIVISTIC continuum dynamics and electroMAGNETic fields are known to be strongly coupled, such as neutron-star crusts, MAGNETar flares, RELATIVISTIC JETs, and accretion disks. We also offer systematic connections with several formulations appearing in the existing literature.
[abstract 18 / 52] Yes (score: 4) - Title: Measurement of Milli-Charged Particles with a running electroMAGNETic coupling constant at IceCubeAuthors: Ye Xu,Comments: 15 pages, 9 figuresSubjects: astro-ph.HECreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
It is assumed that heavy DARK MATTER $ϕ$ with O(TeV) mass captured by the Earth may decay to RELATIVISTIC light milli-charged particles (MCPs). These MCPs could be measured by the IceCube neutrino telescope. The massless hidden photon model was taken for MCPs to interact with nuclei with a running electroMAGNETic coupling constant, so that the numbers and fluxes of expected MCPs may be evaluated at IceCube. Meanwhile, the numbers of expected neutrino background events were also evaluated at IceCube. Based on the assumption that no events are observed at IceCube in 10 years, the corresponding upper limits on MCP fluxes were calculated at 90\% C. L.. These results indicated that the MCPs from the Earth's core could be directly detected at O(1TeV) energies at IceCube when $5.65\times10^{-5}\lesssimε^2\lesssim1.295\times10^{-3}$. And a new region of 4 GeV < $m_{MCP}$ < 100 GeV and $5.51\times10^{-2}$ < $ε$ < 0.612 is ruled out in the $m_{MCP}$-$ε$ plane with 10 years of IceCube data.
[abstract 19 / 52] (score: 3) - Title: Formulation and verification of multiscale gyrokinetic simulation of kinetic-MHD processes in toroidal plasmasAuthors: Xishuo Wei, Pengfei Liu, Gyungjin Choi, Guillaume Brochard, Jian Bao, Javier H Nicolau, Yuehao Ma, Haotian Chen, Handi Huang, Shuying Sun, Yangyang Yu, Ethan Green, Fernando Eizaguirre, Zhihong Lin,Comments:Subjects: physics.plasm-phCreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
A comprehensive gyrokinetic simulation model has been implemented in the global toroidal gyrokinetic code (GTC) and verified for studying low-frequency waves and turbulence in MAGNETic fusion plasmas by treating all kinetic-MHD processes on an equal footing. A theoretical framework has been formulated to unify various methods for efficiently solving the electron drift kinetic equation in multiscale simulations by separating electron responses into analytic and non-analytic parts based on the smallness parameter of electron-to-ion mass ratio. The model can be reduced to the ideal MHD model with both the linear dispersion relation and the nonlinear ponderomotive force in theory and simulation. The model is used for the verification and validation of simulating internal kink modes in the DIII-D tokamak with accurate calculations of equilibrium parallel current and compressible MAGNETic perturbation. A large simulation database has been generated to train a surrogate model to predict the kink instability. Statistical analysis shows that the radial location of safety factor q=1 flux-surface and the plasma beta inside the q=1 surface are the most important parameters for predicting the kink instability.
[abstract 20 / 52] (score: 3) - Title: A BLACK HOLE in a near-pristine galaxy 700 million years after the Big BangAuthors: Roberto Maiolino, Hannah Uebler, Francesco D'Eugenio, Jan Scholtz, Ignas Juodzbalis, Xihan Ji, Michele Perna, Volker Bromm, Pratika Dayal, Sophie Koudmani, Boyuan Liu, Raffaella Schneider, Debora Sijacki, Rosa Valiante, Alessandro Trinca, Saiyang Zhang, Marta Volonteri, Kohei Inayoshi, Stefano Carniani, Kimihiko Nakajima, Yuki Isobe, Joris Witstok, Gareth C. Jones, Sandro Tacchella, Santiago Arribas, Andrew Bunker, Elisa Cataldi, Stephane Charlot, Giovanni Cresci, Mirko Curti, Andrew C. Fabian, Harley Katz, Nimisha Kumari, Nicolas Laporte, Giovanni Mazzolari, Brant Robertson, Fengwu Sun, Bruno Rodriguez Del Pino, Giacomo Venturi,Comments: Replaced with accepted version, 19 pages, 11 figures, 2 tablesSubjects: astro-ph.GA astro-ph.COCreated: 2025-11-22; Updated: 2025-11-25; Datestamp: 2025-11-25
The recent discovery of a large number of massive BLACK HOLEs within the first two billion years after the Big Bang, as well as their peculiar properties, have been largely unexpected based on the extrapolation of the properties of luminous QUASARs. These findings have prompted the development of several theoretical models for the early formation and growth of BLACK HOLEs, which are, however, difficult to differentiate. We report the metallicity measurement around a gravitationally lensed massive BLACK HOLE at redshift 7.04 (classified as a Little Red Dot), hosted in a galaxy with very low dynamical mass. The weakness of the [OIII]5007 emission line relative to the narrow H$β$ emission indicates extremely low metallicity, about $4\times 10^{-2}$ solar, and even more metal poor in the surrounding few 100 pc. We argue that such properties cannot be uncommon among accreting BLACK HOLEs around this early cosmic epoch. Explaining such a low chemical enrichment in a system that has developed a massive BLACK HOLE is challenging for most theories. Models assuming heavy BLACK HOLE seeds (such as Direct Collapse Black Holes) or super-Eddington accretion scenarios struggle to explain the observations, although they can potentially reproduce the observed properties in some cases. Models invoking "primordial BLACK HOLEs" (i.e. putative BLACK HOLEs formed shortly after the Big Bang) may potentially explain the low chemical enrichment associated with this BLACK HOLE, although this class of models also requires further developments for proper testing.
[abstract 21 / 52] (score: 3) - Title: JADES and BlackTHUNDER: rest-frame Balmer-line absorption and the local environment in a Little Red Dot at z = 5Authors: Francesco D'Eugenio, Ignas Juodžbalis, Xihan Ji, Jan Scholtz, Roberto Maiolino, Stefano Carniani, Michele Perna, Giovanni Mazzolari, Hannah Übler, Santiago Arribas, Rachana Bhatawdekar, Andrew J. Bunker, Giovanni Cresci, Emma Curtis-Lake, Kevin Hainline, Kohei Inayoshi, Yuki Isobe, Benjamin D. Johnson, Gareth C. Jones, Tobias J. Looser, Erica J. Nelson, Eleonora Parlanti, Dávid Puskás, Pierluigi Rinaldi, Brant Robertson, Bruno Rodríguez Del Pino, Irene Shivaei, Fengwu Sun, Sandro Tacchella, Giacomo Venturi, Marta Volonteri, Christina C. Williams, Christopher N. A. Willmer, Chris Willott, Joris Witstok,Comments: 29 pages, 22 figures, 2 tables. Published in MNRASSubjects: astro-ph.GACreated: 2025-11-22; Updated: 2025-11-25; Datestamp: 2025-11-25
We present a broad-line AGN at z=5.077, observed with both NIRSpec/MSA and NIRSpec/IFU by the JADES and BlackTHUNDER surveys. The target exhibits all the hallmark features of a 'Little Red Dot' (LRD) AGN. The combination of spatially resolved and high-resolution spectroscopy offers deeper insight into its nature. The H$α$ line has multiple components, including two broad Gaussians, yielding a black-hole mass of $\log(M_{\rm BH}/M_\odot)=7.65$, while the narrow [O III]$λ$5007 gives a galaxy dynamical mass of $\log(M_{\rm dyn}/M_\odot)=9.1$ suggesting a dynamically overmassive BLACK HOLE relative to the host galaxy. The target is immersed in a 7-kpc wide pool of ionized gas and has three neighbours: a satellite galaxy, a possible satellite/gas cloud and a tentatively detected spatially detached outflow. H$α$ shows strong absorption, deeper than the continuum, thus ruling out a stellar origin, and with velocity and velocity dispersion of v=-13 km s$^{-1}$ and $σ$=120 km s$^{-1}$. There is tentative evidence (2.6 $σ$) of temporal variability in the EW of the H$α$ absorber over two rest-frame months. If confirmed, this would suggest a highly dynamic environment. Notably, while the H$α$ absorber is clearly visible and even dominant in the high-resolution G395H observations, it is not detected in the medium-resolution G395M data of the same epoch. This implies that the current incidence rate of absorbers in LRDs - and especially of rest-frame absorbers - may be severely underestimated, because most LRDs rely on lower-resolution spectroscopy. In this context, the high incidence rate of rest-frame absorbers in LRDs may indicate a configuration that is either intrinsically stationary, such as a rotating disc, or that exhibits time-averaged stability, such as an oscillatory 'breathing mode' accretion of cyclic expansion and contraction of the gas around the SMBH.
[abstract 22 / 52] (score: 3) - Title: 20 GeV halo-like excess of the Galactic diffuse emission and implications for DARK MATTER annihilationAuthors: Tomonori Totani,Comments: 32 pages, 16 figures. Minor revision to Fig. 15, to match the published version in JCAPSubjects: astro-ph.HE astro-ph.CO hep-phCreated: 2025-11-23; Updated: 2025-11-25; Datestamp: 2025-11-25
Fifteen years of the FERMI Large Area Telescope (LAT) data in the halo region of the Milky Way (MW) are analyzed to search for gamma rays from DARK MATTER annihilation. Gamma-ray maps within the region of interest ($|l| \le 60^\circ$, $10^\circ \le |b| \le 60^\circ$) are modeled using point sources, the GALPROP models of cosmic-ray interactions, isotropic background, and templates of Loop I and the FERMI bubbles, and then the presence of a halo-like component is further examined. A statistically significant halo-like excess is found with a spectral peak around 20 GeV, while its flux is consistent with zero below 2 GeV and above 200 GeV. Examination of the fit residual maps indicates that a spherically symmetric halo component fits the map data well. The radial profile agrees with annihilation by the smooth NFW density profile, and may be slightly shallower than this, especially in the central region. Various systematic uncertainties are investigated, but the 20 GeV peak remains significant. In particular, the halo excess with a similar spectrum is detected even relative to the LAT standard background model, which contains non-template patches adjusted to match the observed map. The halo excess spectrum can be fitted by annihilation with a particle mass $m_χ\sim$ 0.5-0.8 TeV and cross section $\langle σ\upsilon \rangle \sim$ (5-8)$\times 10^{-25} \ \rm cm^3 \, s^{-1}$ for the $b\bar{b}$ channel. This cross section is larger than the upper limits from dwarf galaxies and the canonical thermal relic value, but considering various uncertainties, especially the density profile of the MW halo, the DARK MATTER interpretation of the 20 GeV ``FERMI halo'' remains feasible. The prospects for verification through future observations are briefly discussed.
[abstract 23 / 52] (score: 3) - Title: Machine learning classification of BLACK HOLEs in the mass--spin diagramAuthors: Nathan Steinle, Samar Safi-Harb,Comments: submitted to PRDSubjects: astro-ph.HE astro-ph.CO gr-qcCreated: 2025-11-22; Updated: 2025-11-25; Datestamp: 2025-11-25
We present the mass--spin diagram for classifying BLACK HOLEs and studying their formation pathways providing an analogue to the Hertzsprung-Russell diagram. This allows for BLACK HOLE evolutionary tracks as a function of redshift, combining formation, accretion, and merger histories for the variety of BLACK HOLE populations. A realistic BLACK HOLE continuum constructed from initial mass and spin functions and approximate redshift evolution reveals possible BLACK HOLE main sequences, such as sustained coherent accretion through cosmic time or hierarchical merger trees. In the stellar-mass regime, we use a binary population synthesis software to compare three spin prescriptions for tidal evolution of Wolf-Rayet progenitors, showing how the mass--spin diagram exposes interesting modeling differences. We then classify BLACK HOLE populations by applying supervised and unsupervised machine learning clustering methods to mass--spin datasets. While bare unsupervised clustering can nearly recover canonical population boundaries (stellar-mass, intermediate-mass, and supermassive), a more sophisticated approach utilizing deep learning via variational autoencoders for latent space representation learning aids in clustering of realistic datasets with subclasses that highly overlap in mass--spin space. We find that a supervised random forest can accurately recover the correct clusters from the learned latent space representation depending on the complexity of the underlying dataset, semi-supervised methods show potential for further development, and the performance of unsupervised classifiers is a great challenge. Our findings motivate future machine learning applications and demonstrate that the mass--spin diagram can be used to connect gravitational-wave and electroMAGNETic observations with theoretical models.
[abstract 24 / 52] (score: 3) - Title: The Type Ia Supernova 2021hem: A 2003fg-like Event in an Apparently Hostless EnvironmentAuthors: Subhash Bose, M. D. Stritzinger, A. Malmgaard, C. J. Miller, N. Elias-Rosa, J. P. U. Fynbo, C. Ashall, C. R. Burns, J. M. DerKacy, L. Galbany, C. P. Gutiérrez, W. B. Hoogendam, E. Y. Hsiao, E. A. M. Jensen, K. Medler, Alaa Alburai, J. Anderson, E. Baron, J. Duarte, M. Gromadzki, C. Inserra, P. A. Mazzali, T. E. Müller-Bravo, P. Lundqvist, A. Reguitti, I. Salmaso, D. J. Sand, G. Valerin,Comments: 22pages, 15 figures, accepted for publication in Astronomy & AstrophysicsSubjects: astro-ph.HECreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
We report observations of Type Ia SN 2021hem, located in an apparently hostless environment. With a peak absolute B-band magnitude of -19.96 mag, and a lack of secondary maximum in near-infrared and i-band light curves make it resemble 2003fg-like events. The slowly evolving light curves, and the earliest spectrum showing CII absorption lines, further support this classification. Fireball model fit to early light curves yields a time of first light of -16.43 days relative to B-band maximum. The first detection occurs 1.51 days before the onset of the fireball-like flux rise. This early emission, and $(g - r)_0$ color, is inconsistent with circumstellar or companion interaction. Instead, shallow $^{56}$Ni mixing or an asymmetric $^{56}$Ni distribution offers a plausible explanation. SN2021hem is the fifth known 2003fg-like SN with early-time excess flux emission. The estimated mass of radioactive $^{56}$Ni in SN2021hem is $1.00\pm0.09 M_\odot$. Deep GTC imaging obtained 2.5 yr after the explosion (with $m_{lim,r}=24.4$ mag and $μ_{lim,r} = 26.3\rm~mag~arsec^{-2}$), reveals no coincident host, thereby ruling out most faint dwarf and UDGs. Alternatively, assuming the nearest plausible AGN host galaxy, at a distance of 104 kpc, implies a hyper-velocity progenitor ejected at $\sim$2200 km/s by AGN interaction. A faint diffuse feature ~6 kpc from the SN site has also been detected in the image, with its surface brightness of a UDGs. However, it is unclear whether it is a galaxy and is associated with SN2021hem. Considering its large normalized directional light distance ($d_{DLR}\sim3-4$) from SN, and its unusual elongation, it is a candidate of low probability to be the host galaxy of SN2021hem. These results identify SN2021hem as one of the strongest candidates for a hostless SN Ia, underscoring the diversity of luminous, slowly evolving, 2003fg-like explosions.
[abstract 25 / 52] (score: 3) - Title: Hierarchical Interferometric Bayesian ImagingAuthors: Paul Tiede, William Moses, Valentin Churavy, Michael D. Johnson, Dominic Pesce, Lindy Blackburn, Peter Galison,Comments: submitted to ApJSubjects: astro-ph.IM astro-ph.HECreated: 2025-11-21; Updated: 2025-11-25; Datestamp: 2025-11-25
Very long baseline interferometry (VLBI) achieves the highest angular resolution in astronomy. VLBI measures corrupted Fourier components, known as visibilities. Reconstructing on-sky images from these visibilities is a challenging inverse problem, particularly for sparse arrays such as the Event Horizon Telescope (EHT) and the Very Long Baseline Array (VLBA), where incomplete sampling and severe calibration errors introduce significant uncertainty in the image. To help guide convergence and control the uncertainty in image reconstructions, regularization on the space of images is utilized, such as enforcing smoothness or similarity to a fiducial image. Coupled with this regularization is the introduction of a new set of parameters that modulate its strength. We present a hierarchical Bayesian imaging approach (Hierarchical Interferometric Bayesian Imaging, HIBI) that enables the quantification of uncertainty for al parameters. Incorporating instrumental effects within HIBI is straightforward, allowing for simultaneous imaging and calibration of data. To showcase HIBI's effectiveness and flexibility, we build a simple imaging model based on Markov random fields and demonstrate how different physical components can be included, e.g., BLACK HOLE shadow size, and their uncertainties can be inferred. For example, while the original EHT publications were unable to constrain the ring width of M87*, HIBI measures a width of $9.3\pm 1.3\,μ{\rm as}$. We apply HIBI to image and calibrate EHT synthetic data, real EHT observations of M87*, and multifrequency observations of \oj287. Across these tests, HIBI accurately recovers a wide variety of image structures and quantifies their uncertainties. HIBI is publicly available in the Comrade.jl VLBI software repository.
[abstract 26 / 52] (score: 3) - Title: PROJECT-J: the shocking H2 outflow from HH46Authors: Maria Gabriela Navarro, Brunella Nisini, Teresa Giannini, Patrick J. Kavanagh, Alessio Caratti o Garatti, Simone Antoniucci, Hector G. Arce, Francesca Bacciotti, Sylvie Cabrit, Deirdre Coffey, Catherine Dougados, JJochen Eislöffel, Patrick Hartigan, Alberto Noriega-Crespo, Linda Podio, Ewine F. van Dishoeck, Emma T. Whelan,Comments: 37 pages, 21 figures, 6 tables, accepted for publication in ApJ on November 12, 2025Subjects: astro-ph.GA astro-ph.SRCreated: 2025-11-21; Updated: 2025-11-25; Datestamp: 2025-11-25
We analyze the H2 emission observed in the HH46 Class I system as part of PROJECT-J (Protostellar Jets Cradle Tested with JWST), to investigate the origin and excitation of the warm molecular outflow. We used NIRSpec and MIRI spectral maps (1.6-27.9 microns) to trace the structure and physical conditions of the outflow. By fitting the H2 rotational diagrams with a multi-temperature gas model, we derived key physical parameters including temperature, extinction, column densities, and the ortho-to-para ratio. This information is combined with a detailed kinematical analysis and comparison with irradiated shock models. We find no evidence of H2 temperature or velocity stratification from the axis to the edge of the outflow, as would be expected in MHD disk-wind models and as observed in other outflows. Instead, the observations suggest that the H2 emission arises from shock interactions between JET bow shocks and/or wide-angle winds with the ambient medium and cavity walls. NIRSpec emission and velocity maps reveal expanding molecular shells, likely driven by the less luminous source in the binary system. We infer an accretion rate of less than 10^-9 solar masses per year for the secondary source, approximately one order of magnitude lower than that of the primary. The H2 emission is consistent with excitation by low-velocity (approximately 10 km/s) J-type shocks, irradiated by an external UV field that may originate from strong dissociative shocks driven by the atomic JET. Future JWST observations will further constrain the evolution of the expanding shell and the mechanisms driving the outflow.
[abstract 27 / 52] (score: 3) - Title: Revisiting $γ$-Ray Orbital Modulation in the Redback Millisecond Pulsar PSR J2039-5617Authors: Mengqing Zhang, Shengbin Pei, Shan Chang, Pengfei Zhang,Comments: 9 pages, 6 figures, accepted by ApJSubjects: astro-ph.HECreated: 2025-11-22; Updated: 2025-11-25; Datestamp: 2025-11-25
PSR J2039-5617 is a redback millisecond pulsar binary system consisting of a compact star with a mass of 1.1-1.6 $M_\odot$ and a low-mass companion of 0.15-0.22 $M_\odot$. For this binary, we performed a timing analysis using 16 years of data from the FERMI Large Area Telescope, covering the period from 2008 August to 2024 October. Our analysis detected an orbital modulation with a period of 0.2279781 days at a significance level of $\sim4σ$, which is in good agreement with previous findings. However, unlike previous reports, we identified a transition in the orbital modulation around 2021 August, after which the orbital signal disappeared. We speculate that the system may be undergoing a transition from a rotation-powered to an accretion-powered state at this epoch. Additionally, we conducted the phase-resolved and spectral analyses, and in the phase-resolved results, we observed an anti-correlation between its $γ$-ray and X-ray emissions, which consistent with the predictions of high-energy radiation models for such systems. We provide some predictive discussions based on the results of $γ$-ray data analysis, and future FERMI-LAT observations will determine whether these predictions hold true.
[abstract 28 / 52] (score: 3) - Title: Probing Loop Quantum Gravity BLACK HOLEs through gravitational lensingAuthors: Arun Kumar, Qiang Wu, Tao Zhu, Sushant G. Ghosh,Comments: 13 pages, 6 figures, 2 tablesSubjects: gr-qcCreated: 2025-11-22; Updated: 2025-11-25; Datestamp: 2025-11-25
We investigate strong gravitational lensing by a charged loop quantum gravity (LQG) BLACK HOLE obtained through the polymerisation scheme of Borges \textit{et al.} \cite{Borges:2023fog}. These effective geometries replace the Reissner--Nordström singularity with a symmetric transition surface and admit an extremal, cold remnant determined by the minimal area gap in LQG. In turn, we derive the null geodesic equations, investigate the photon effective potential, and obtain expressions for the photon-sphere radius and critical impact parameter. We compute the weak-field deflection angle and Einstein ring size, highlighting the deviations induced by the polymerisation parameter and the Barbero--Immirzi parameter. In the strong-field regime, we compute the strong deflection coefficients $(\bar{a},\bar{b})$ and evaluate the lensing observables $θ_\infty$, $s$, and $r_{\rm mag}$. Unlike the Reissner--Nordström case, the LQG corrections enhance the deflection angle and increase the angular separation of RELATIVISTIC images, with deviations growing as the geometry approaches the LQG remnant limit. We further compute the corresponding observables for Sgr~A* and M87*, finding that the quantum-gravity modifications lie within the potential sensitivity of next-generation VLBI facilities. For M87*, the angular separation $s\in(0.05712,0.19123)\,μ\text{as}$, while it is $s\in(0.07595,0.25426)\,μ\text{as}$ for Sgr A*. The relative flux ratio is found to lie in the range, $r_{\rm mag}\in(4.49272,5.96397)$. Our analysis demonstrates that LQG-induced corrections leave characteristic strong and weak-lensing imprints, offering a promising observational pathway to probe quantum gravity using near-future high-resolution observations.
[abstract 29 / 52] (score: 3) - Title: Deep X-ray observation of NGC 3221: everything everywhere all at onceAuthors: Sanskriti Das, Smita Mathur, Bret D. Lehmer, Steven W. Allen, Yair Krongold, Anjali Gupta,Comments: 16 pages, 6 figures, 2 tables; accepted for publication in ApJSubjects: astro-ph.GA astro-ph.HECreated: 2025-11-23; Updated: 2025-11-25; Datestamp: 2025-11-25
We present a comprehensive analysis of 475 ks (438 ks unpublished & 37 ks archival) XMM-Newton/EPIC-pn observation of a nearby, highly inclined, star-forming, luminous infrared galaxy NGC 3221 through spatial, temporal, and spectral information. We confirm the presence of a low-luminosity (presumably Compton-thick) AGN. The 0.4$-$12 keV luminosity and the hardness ratio of the six ultra-luminous X-ray sources (ULX) previously identified in Chandra data exhibit diverse variability on day-scale. The collective emission from unresolved sources exhibits a different day-scale variability. We have also discovered two new predominantly soft ($<1$ keV) sources. One of these has an enigmatic spectral shape featuring a soft component, which we interpret as a superbubble in NGC 3221, and a variable hard component from a compact object, which is unresolved from the superbubble. We do not confidently detect any X-ray emission from SN 1961L. The hot gas in the ISM (out to $\pm$6 kpc from the disk plane) and the extraplanar region (6$-$12 kpc) both require two thermal phases at $\sim 0.15$ keV and $\sim 0.55$ keV. The $\sim 0.55$ keV component is fainter in the ISM than the $\sim 0.15$ keV component, but the emission from the latter falls off more steeply with disk height than the former. This makes the extraplanar region hotter and less dense than the ISM. The proximity of NGC 3221 and the occurrence of the underluminous AGN offer a unique observing opportunity to study the hot diffuse medium in conjunction with nuclear and disk-wide point sources.
[abstract 30 / 52] (score: 3) - Title: Black Hole Spin Estimation with Time-variable Image of M87 During the Flaring StateAuthors: Mikiya M. Takahashi, Tomohisa Kawashima, Ken Ohsuga,Comments: 12 pages, 12 figures, accepted by PASJSubjects: astro-ph.HE astro-ph.GA gr-qcCreated: 2025-11-23; Updated: 2025-11-25; Datestamp: 2025-11-25
By investigating the time-variable 230 GHz images using ray-tracing general RELATIVISTIC radiative transfer calculation, we propose a novel method for estimating the spin parameter of the supermassive BLACK HOLE at the M87 center by utilizing the sudden and short-term increase in emissivity in the innermost region of the accretion disk. It is found that the flux of the photon ring increases simultaneously as the flux of the direct ring, which brightens first, decreases, and then gradually diminishes, when the increase in emissivity persists for $15 t_{\rm g}$ with $t_{\rm g}$ being the light crossing time of the gravitational radius. The direct ring is formed by photons emitted from the vicinity of the innermost region of the disk and traveling directly to the observer without orbiting around the BLACK HOLE, while the photon ring is formed by photons passing near the spherical photon orbit. The time-averaged width of the dark region between the direct ring and the photon ring (dark crescent) becomes thinner when the spin parameter is higher and the increase in the emissivity of the accretion disk is greater. The time variation of two rings also causes the intensity-weighted center to oscillate both in the direction of the BLACK HOLE's angular momentum vector projected onto the screen ($Y$-direction) and in the perpendicular direction ($X$-direction). The amplitude of oscillatory time variation in the $X$-direction becomes large when the spin parameter is higher, and that in the $Y$-direction becomes large when the increase in the emissivity of the disk is large. The spin parameter can be estimated by combining the time-averaged dark crescent width and the ratio of the amplitudes in the $X$- and $Y$-directions. This method is applicable when the duration of the increase in emissivity of the accretion disk ranges at least from approximately 10-20 $t_{\rm g}$.
[abstract 31 / 52] (score: 3) - Title: Off-Equatorial Orbits around Magnetically Charged Black HolesAuthors: Xilai Li, David E. Kaplan, Loris Del Grosso,Comments:Subjects: gr-qcCreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
We present a complete characterization of stable, off-equatorial circular orbits around MAGNETically charged BLACK HOLEs (MBHs). For a static, spherically symmetric MBH, we derive an exact analytic expression for the orbital latitude theta as a function of radius r. We establish a direct connection between these orbits and the spacetime fundamental structure, and demonstrate their stability against SYNCHROTRON radiation. We show that charged particles such as electrons and protons can exhibit O(1) latitude deviations at the ISCO radius and remain stable under SYNCHROTRON emission even for extremely small values of the BLACK HOLE MAGNETic charge. We then extend the analysis to rotating MBHs, numerically computing the prograde and retrograde orbital branches and demonstrating how frame-dragging modifies their structure and stability regions. We show that these off-equatorial orbits are a unique feature of the MAGNETic charge, being forbidden in the analogous electrically charged Kerr-Newman spacetime. Our results suggest that environments surrounding MAGNETically charged BLACK HOLEs can exhibit distinctive phenomenological signatures, with potential implications for BLACK HOLE imaging and polarimetric observations.
[abstract 32 / 52] (score: 3) - Title: Time-dependent Turbulent Electron Acceleration and Transport in Solar FlaresAuthors: Luiz A. C. A. Schiavo, Natasha L. S. Jeffrey, Gert J. J. Botha, James A. McLaughlin,Comments:Subjects: astro-ph.SRCreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
Solar flares are explosive releases of MAGNETic energy stored in the solar corona, driven by MAGNETic RECONNECTion. These events accelerate electrons, generating hard X-ray emissions and often display Quasi Periodic Pulsations (QPPs) across the energy spectra. However, the energy transfer process remains poorly constrained, with competing theories proposing different acceleration mechanisms. We investigate electron acceleration and transport in a flaring coronal loop by solving a time-dependent Fokker-Planck equation. Our model incorporates transient turbulent acceleration, simulating the effects of impulsive energy input to emulate the dynamics of time-dependent RECONNECTion processes. We compute the density-weighted electron flux, a diagnostic directly comparable to observed X-ray emissions, across the energy and spatial domains from the corona to the chromosphere. We investigate different time-dependent functional forms of the turbulent acceleration, finding that the functional form of the acceleration source maintains its signature across energy bands (1 to 100 keV) with a response time that is energy dependent (with higher energy bands displaying a longer response time). In addition, we find that (a) for a square pulse the switch on and off response time is different; (b) for a sinusoidal input the periodicity is preserved; and (c) for a damped sinusoidal the decay rate increases with density and higher energy bands lose energy faster. This work presents a novel methodology for analyzing electron acceleration and transport in flares driven by time-dependent sources.
[abstract 33 / 52] (score: 3) - Title: Probing the Formation Environment of Strongly Lensed Black Hole Mergers: Implications for the AGN-disk ChannelAuthors: Johan Samsing, Lorenz Zwick, Pankaj Saini, János Takátsy,Comments: comments welcomeSubjects: astro-ph.HE astro-ph.COCreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
The observation of multiple images from a strongly lensed gravitational wave (GW) source provides the observer with a stereoscopic view of the source. This allows for a measure of its relative proper motion by comparing the induced GW Doppler shifts between the different images. In addition, if the GW source is in a dynamical environment it will be subject to an acceleration, which will show up as a time dependent Doppler shift in each individual image. In this work we quantify for the first time how a joint detection of these effects can be used to constrain the underlying dynamics and environment of the lensed GW source. We consider a range of different astrophysical environments, from massive clusters to stellar triples, and find that binary BLACK HOLE (BBH) mergers in Active Galactic Nuclei disks (AGN-disks) are particularly likely to have orbital parameters that can be constrained through our considered lensing setup. Applying these methods to the upcoming catalog of cosmologically strongly lensed GW sources will open up new possibilities for probing their origin and underlying formation mechanisms.
[abstract 34 / 52] (score: 2) - Title: DESI 2024 V: Full-Shape Galaxy Clustering from Galaxies and QuasarsAuthors: A. G. Adame, J. Aguilar, S. Ahlen, S. Alam, D. M. Alexander, M. Alvarez, O. Alves, A. Anand, U. Andrade, E. Armengaud, S. Avila, A. Aviles, H. Awan, S. Bailey, C. Baltay, A. Bault, J. Behera, S. BenZvi, F. Beutler, D. Bianchi, C. Blake, R. Blum, S. Brieden, A. Brodzeller, D. Brooks, E. Buckley-Geer, E. Burtin, R. Calderon, R. Canning, A. Carnero Rosell, R. Cereskaite, J. L. Cervantes-Cota, S. Chabanier, E. Chaussidon, J. Chaves-Montero, S. Chen, X. Chen, T. Claybaugh, S. Cole, A. Cuceu, T. M. Davis, K. Dawson, A. de la Macorra, A. de Mattia, N. Deiosso, A. Dey, B. Dey, Z. Ding, P. Doel, J. Edelstein, S. Eftekharzadeh, D. J. Eisenstein, A. Elliott, P. Fagrelius, K. Fanning, S. Ferraro, J. Ereza, N. Findlay, B. Flaugher, A. Font-Ribera, D. Forero-Sánchez, J. E. Forero-Romero, C. Garcia-Quintero, L. H. Garrison, E. Gaztañaga, H. Gil-Marín, S. Gontcho A Gontcho, A. X. Gonzalez-Morales, V. Gonzalez-Perez, C. Gordon, D. Green, D. Gruen, R. Gsponer, G. Gutierrez, J. Guy, B. Hadzhiyska, C. Hahn, M. M. S Hanif, H. K. Herrera-Alcantar, K. Honscheid, C. Howlett, D. Huterer, V. Iršič, M. Ishak, S. Juneau, N. G. Karaçaylı, R. Kehoe, S. Kent, D. Kirkby, H. Kong, S. E. Koposov, A. Kremin, A. Krolewski, Y. Lai, T. -W. Lan, M. Landriau, D. Lang, J. Lasker, J. M. Le Goff, L. Le Guillou, A. Leauthaud, M. E. Levi, T. S. Li, K. Lodha, C. Magneville, M. Manera, D. Margala, P. Martini, M. Maus, P. McDonald, L. Medina-Varela, A. Meisner, J. Mena-Fernández, R. Miquel, J. Moon, S. Moore, J. Moustakas, E. Mueller, A. Muñoz-Gutiérrez, A. D. Myers, S. Nadathur, L. Napolitano, R. Neveux, J. A. Newman, N. M. Nguyen, J. Nie, G. Niz, H. E. Noriega, N. Padmanabhan, E. Paillas, N. Palanque-Delabrouille, J. Pan, S. Penmetsa, W. J. Percival, M. M. Pieri, M. Pinon, C. Poppett, A. Porredon, F. Prada, A. Pérez-Fernández, I. Pérez-Ràfols, D. Rabinowitz, A. Raichoor, C. Ramírez-Pérez, S. Ramirez-Solano, M. Rashkovetskyi, C. Ravoux, M. Rezaie, J. Rich, A. Rocher, C. Rockosi, F. Rodríguez-Martínez, N. A. Roe, A. Rosado-Marin, A. J. Ross, G. Rossi, R. Ruggeri, V. Ruhlmann-Kleider, L. Samushia, E. Sanchez, C. Saulder, E. F. Schlafly, D. Schlegel, M. Schubnell, H. Seo, R. Sharples, J. Silber, A. Slosar, A. Smith, D. Sprayberry, T. Tan, G. Tarlé, S. Trusov, R. Vaisakh, D. Valcin, F. Valdes, M. Vargas-Magaña, L. Verde, M. Walther, B. Wang, M. S. Wang, B. A. Weaver, N. Weaverdyck, R. H. Wechsler, D. H. Weinberg, M. White, M. J. Wilson, J. Yu, Y. Yu, S. Yuan, C. Yèche, E. A. Zaborowski, P. Zarrouk, H. Zhang, C. Zhao, R. Zhao, R. Zhou, H. Zou,Comments: This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers/). 90 pages, 26 figures. This version updates the published version in JCAP, correcting a typo when reporting the datavectors and matrices of Appendix A. Material for reproducing all figures available at https://zenodo.org/records/16992652Subjects: astro-ph.COCreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
We present the measurements and cosmological implications of the galaxy two-point clustering using over 4.7 million unique galaxy and QUASAR redshifts in the range $0.1
[abstract 35 / 52] (score: 2) - Title: Relativistic excitation of compact starsAuthors: Zhiqiang Miao, Xuefeng Feng, Zhen Pan, Huan Yang,Comments: 23 pages, 9 figures, updated to publishing versionSubjects: gr-qcCreated: 2025-11-23; Updated: 2025-11-25; Datestamp: 2025-11-25
In this work, we study the excitation of a compact star under the influence of external gravitational driving in the RELATIVISTIC regime. Using a model setup in which a wave with constant frequency is injected from past null infinity and scattered by the star to future null infinity, we show that the scattering coefficient encodes rich information of the star. For example, the analytical structure of the scattering coefficient implies that the decay rate of a mode generally plays the role of ``star excitation factor'', similar to the ``BLACK HOLE excitation factor'' previously defined for describing BLACK HOLE mode excitations. With this star excitation factor we derive the transient mode excitation as a binary system crosses a generic mode resonance of a companion star during the inspiral stage. This application is useful because previous description of resonant mode excitation of stars still relies on the mode and driving force decomposition based on the Newtonian formalism. In addition, we show that the scattering phase is intimately related to the total energy of spacetime and matter under the driving of a steady input wave from infinity. We also derive the relevant tidal energy of a star under steady driving and compare that with the dynamic tide formula. We estimate that the difference may lead to $\mathcal{O}(0.5)$ radian phase modulation in the late stage of the binary neutron star inspiral waveform.
[abstract 36 / 52] (score: 2) - Title: On energy consistency of intermediate states in HLL-type MHD Riemann solversAuthors: Fan Zhang, Andrea Lani, Stefaan Poedts,Comments: Submitted to JCPSubjects: physics.flu-dynCreated: 2025-11-22; Updated: 2025-11-25; Datestamp: 2025-11-25
Approximate Riemann solvers are widely used for solving hyperbolic conservation laws, including those of MAGNETohydrodynamics (MHD). However, due to the nonlinearity and complexity of MHD, obtaining accurate and robust numerical solutions to MHD equations is non-trivial, and it may be challenging for an approximate MHD Riemann solver to preserve the positivity of scalar variables, particularly when the plasma \b{eta} is low. As we have identified that the inconsistency between the numerically calculated MAGNETic field and MAGNETic energy may be at least partly responsible for the loss of positivity of scalar variables, we propose a consistency condition for calculating the intermediate energies within the Riemann fan and implement it in HLL-type MHD Riemann solvers, thereby alleviating erroneous MAGNETic field solutions that break scalar positivity. In addition, (I) for the HLLC-type scheme, we have designed a revised two-state approximation, specifically reducing numerical error in MAGNETic field solutions, although sacrificing the contact-resolving capability, and (II) for the HLLD-type scheme, we replace the constant total pressure assumption by a three-state assumption for the intermediate thermal energy, which is more consistent with our other assumptions. The proposed schemes perform better in numerical examples with low plasma \b{eta}. Moreover, we explained the energy error introduced during time integration.
[abstract 37 / 52] (score: 2) - Title: MUSE IFU observations of galaxies hosting of Tidal Disruption EventsAuthors: M. Pursiainen, G. Leloudas, J. Lyman, C. M. Byrne, P. Charalampopoulos, P. Ramsden, S. Kim, S. Schulze, J. P. Anderson, F. E. Bauer, L. Dai, L. Galbany, H. Kuncarayakti, M. Nicholl, T. Pessi, J. L. Prieto, S. F. Sanchez,Comments: Accepted for publication in MNRAS on 2025-11-21Subjects: astro-ph.HE astro-ph.GACreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
We present an analysis of twenty tidal disruption event (TDE) host galaxies observed with the MUSE integral-field spectrograph on ESO VLT. We investigate the presence of extended emission line regions (EELRs) and study stellar populations mostly at sub-kpc scale around the host nuclei. EELRs are detected in 5/20 hosts, including two unreported systems. All EELRs are found at z<0.045, suggesting a distance bias and faint EELRs may be missed at higher redshift. EELRs only appear in post-merger systems and all such hosts at z<0.045 show them. Thus, we conclude that TDEs and galaxy mergers have a strong relation, and >45% of post-merger hosts in the sample exhibit EELRs. Furthermore, we constrained the distributions of stellar masses near the central BLACK HOLEs (BHs), using the spectral synthesis code Starlight and BPASS stellar evolution models. The youngest nuclear populations have typical ages of 1 Gyr and stellar masses below 2.5MSun. The populations that can produce observable TDEs around non-rotating BHs are dominated by subsolar-mass stars. 3/4 TDEs requiring larger stellar masses exhibit multi-peaked light curves, possibly implying relation to repeated partial disruptions of high-mass stars. The found distributions are in tension with the masses of the stars derived using light curve models. Mass segregation of the disrupted stars can enhance the rate of TDEs from supersolar-mass stars but our study implies that low-mass TDEs should still be abundant and even dominate the distribution, unless there is a mechanism that prohibits low-mass TDEs or their detection.
[abstract 38 / 52] (score: 2) - Title: Harnessing data-driven methods for precise model independent event shape estimation in RELATIVISTIC heavy-ion collisionsAuthors: Dipankar Basak, H. Hushnud, Kalyan Dey,Comments: 10 pages, 7 figuresSubjects: hep-phCreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
This study demonstrates the application of supervised machine learning (ML) techniques to distinguish between isotropic and JET-like event topologies in heavy-ion collisions via the spherocity observable. State-of-the-art ML algorithms, optimized through systematic hyperparameter tuning, are employed to predict both traditional transverse spherocity $S_{0}$ and unweighted transverse spherocity $S_{0}^{p_{\rm T}=1}$ directly from raw event data. Moreover, the results from this study demonstrated that our approach remains largely model-independent, underscoring its potential applicability in future experimental heavy-ion physics analyses.
[abstract 39 / 52] (score: 2) - Title: Long-wave instability of stratified two-phase MHD flowAuthors: Arseniy Parfenov, Alexander Gelfgat, Neima Brauner,Comments:Subjects: physics.flu-dynCreated: 2025-11-23; Updated: 2025-11-25; Datestamp: 2025-11-25
Instability of a stratified two-phase MHD parallel flow between two infinite plates is addressed. We examine the effect of the transverse MAGNETic field on the base flow and long wave instability of a two-layer system consisting of conductive liquid and non-conductive gas. Both perfectly insulating and perfectly conducting boundaries are considered. To capture the behavior at small but finite wavenumbers, the conventional first-order long-wave stability analysis is extended to higher order terms. Using mercury-air system as a representative test case, the results demonstrate distinct and non-similar base flow and disturbance profiles, as well as different stability maps for insulating versus conducting boundaries. The stability diagrams reveal a non-monotonic influence of the MAGNETic field on flow stability, showing that, in addition to its expected stabilizing effect, the field can also induce destabilization under certain conditions. Inspection of the disturbance profiles indicates that despite the strong damping of mercury flow by the MAGNETic field, interaction of the two fluids at the interface and the shear-induced instabilities in the gas layer dominate and can lead to flow destabilization as the MAGNETic field strength increases.
[abstract 40 / 52] (score: 2) - Title: High-Throughput Quantification of AlterMAGNETic Band SplittingAuthors: Ali Sufyan, Brahim Marfoua, J. Andreas Larsson, Erik van Loon, Rickard Armiento,Comments:Subjects: cond-mat.mtrl-sciCreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
AlterMAGNETism represents a recently established class of collinear MAGNETism that combines zero net MAGNETization with momentum-dependent spin POLARIZATION, enabled by symmetry constraints rather than spin-orbit coupling. This distinctive behavior gives rise to sizable spin splitting even in materials composed of light, earth-abundant elements, offering promising prospects for next-generation spintronics applications. Despite growing theoretical and experimental interest, the discovery of alterMAGNETic materials remains limited due to the complexity of MAGNETic symmetry and the inefficiency of conventional approaches. Here, we present a comprehensive high-throughput screening of the entire MAGNDATA database, integrating symmetry analysis with spin-polarized density functional theory (DFT) calculations to identify and characterize alterMAGNETic candidates. Our workflow uncovers 173 materials exhibiting significant spin splitting ($\geq 50$ meV within $\pm 3$ eV of the FERMI level), spanning both metallic and semiconducting systems. Crucially, our momentum-resolved analysis reveals that the spin splitting varies strongly across the Brillouin zone, and that the maximal splitting tends to occur away from the high-symmetry paths, a result that directly informs and guides future photoemission experiments. By expanding the catalog of known alterMAGNETs and elucidating the symmetry-protected origins of spin splitting, this work lays a robust foundation for future experimental and theoretical advances in spintronics and quantum materials discovery.
[abstract 41 / 52] (score: 2) - Title: An Overabundance of Radio-AGN in the SPT2349-56 Protocluster: Preheating the Intra-Cluster MediumAuthors: Scott C. Chapman, Roger P. Deane, Dazhi Zhou, Manuel Aravena, William Rasakanya, Melanie Archipley, James Burgoyne, Jared Cathey, Anthony H. Gonzalez, Ryley Hill, Chayce Hughes, Monica Natalia Isla Llave, Matt Malkan, Kedar A. Phadke, Vismaya Pillai, Ana Posses, Bonnie Slocombe, Manuel Solimano, Justin Spilker, Nikolaus Sulzenauer, Fabio Vito, Joaquin D. Vieira, David Vizgan, George Wang, Axel Weiss,Comments: 15 pages, submitted to ApJSubjects: astro-ph.GACreated: 2025-11-21; Updated: 2025-11-25; Datestamp: 2025-11-25
Following the detection of a radio-loud Active Galactic Nucleus (AGN) in the z=4.3 protocluster SPT2349-56, we have obtained additional observations with MeerKAT in S-band (2.4 GHz) with the aim of further characterizing radio emission from amongst the ~30 submillimeter (submm) galaxies (SMGs) identified in the structure. We newly identify three of the protocluster SMGs individually at 2.4GHz as having a radio-excess, two of which are now known to be X-ray luminous AGN. Two additional members are also detected with radio emission consistent with their STAR FORMATION rate (SFR). Archival MeerKAT UHF (816 MHz) observations further constrain luminosities and radio spectral indices of these five galaxies. The Australia Telescope Compact Array (ATCA) is used to detect and resolve the central two sources at 5.5 and 9.0 GHz finding elongated, JET-like morphologies. The excess radio luminosities range from L1.4,rest = (1-20)x10^25 W/Hz, ~10-100x higher than expected from the SFRs, assuming the usual far-infrared-radio correlation. Of the known cluster members, only the SMG `N1' shows signs of AGN in any other diagnostics, namely a large and compact excess in CO(11-10) line emission. We compare these results to field samples of radio sources and SMGs. The overdensity of radio-loud AGN in the compact core region of the cluster may be providing significant heating to the recently discovered nascent intra-cluster medium (ICM) in SPT2349-56.
[abstract 42 / 52] (score: 2) - Title: ACES: The Magnetic Field in Large Filaments in the Galactic CenterAuthors: Dylan M. Paré, Zi-Xuan Feng, Yue Hu, Maya A. Petkova, Jack Sullivan, Robin G. Tress, Cara Battersby, Janik Karoly, Alex Lazarian, Dani Lipman, Xing Pan, Marco Donati, Mattia C. Sormani, John Bally, Ashley T. Barnes, Natalie O. Butterfield, Laura Colzi, Christoph Federrath, Pablo Garcia, Adam Ginsburg, Savannah R. Gramze, Anika Schmiedeke, Christian Henkel, Jonathan D. Henshaw, Paul T. Ho, Pei-Ying Hsieh, Izaskun Jimenez-Serra, Ralf S. Klessen, J. M. Diederik Kruijssen, Steven N. Longmore, Xing Lu, Elisabeth A. C. Mills, Álvaro Sánchez-Monge, Daniel L. Walker, Jennifer Wallace, Qizhou Zhang,Comments: Accepted for publication in ApJSubjects: astro-ph.GACreated: 2025-11-22; Updated: 2025-11-25; Datestamp: 2025-11-25
The Galactic Center (GC) is an extreme region of the Milky Way that is host to a complex set of thermal and non-thermal structures. In particular, the GC contains high-density gas and dust that is collectively referred to as the Central Molecular Zone (CMZ). In this work, we study a subset of HNCO filaments identified in band 3 ALMA observations of the GC obtained by the ALMA CMZ Exploration Survey (ACES) that are comparable to high density filaments identified in the Galactic Disk. We compare the orientation of the MAGNETic field derived from 214 um SOFIA and 850 um JCMT observations with the filament orientation to determine which mechanisms dominate the formation of these filaments. We observe a large range of MAGNETic orientations in our observed filaments indicating the complex environments the filaments are located in. We also compare the observational results to synthetic data sets created using an MHD model of the GC. Our analysis reveals that the dominant mechanisms local to the HNCO filaments vary throughout the GC with some filaments being dominated by supersonic turbulence and others by subsonic turbulence. The comparison to synthetic observations indicates that the observed filaments are in MAGNETically dominated environments that could be supporting these filaments against collapse. Our results on the CMZ filaments are also compared to results obtained on similar filaments located in the Galactic Disk, and we find that the filaments studied here are possible CMZ analogs to the dense filamentary "bones" observed previously in the Galactic Disk.
[abstract 43 / 52] (score: 2) - Title: Full calibration of the tomographic redshift distribution from the HSC PDR3 Shape Catalog with DESIAuthors: J. Choppin de Janvry, S. Gontcho A Gontcho, U. Seljak, A. Baleato Lizancos, E. Chaussidon, W. d'Assignies, J. DeRose, S. Heydenreich, E. Paillas, D. Valcin, T. Zhang, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, G. Gutierrez, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, R. Joyce, S. Juneau, R. Kehoe, D. Kirkby, T. Kisner, A. Kremin, O. Lahav, C. Lamman, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, S. Nadathur, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, I. Pérez-Ràfols, G. Rossi, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou,Comments: 39 pages, 9 figures, 5 tablesSubjects: astro-ph.COCreated: 2025-11-22; Updated: 2025-11-25; Datestamp: 2025-11-25
The calibration of tomographic redshift distributions is essential for cosmological analysis of weak lensing data. In this work, we calibrate all four tomographic bins of the Hyper Suprime Camera (HSC) weak lensing catalog with the Dark Energy Spectroscopic Instrument (DESI) Data Release 1 and 2 using the clustering redshifts technique. We include $z>1.2$ redshift sources such as emission line galaxies (ELG) and QUASARs (QSO) sources in our calibration, which were not available in the previous HSC calibration (Rau et al. 2022, arXiv:2211.16516), allowing a complete calibration of all the redshift bins. We find the first tomographic bin exhibits a small shift towards low redshifts. The second bin is in good agreement with the photometric calibration, while third and fourth bin exhibit a shift towards higher redshifts. However, these shifts are considerably smaller than the shifts obtained in the HSC Year 3 cosmic shear analyses. We evaluate the impact of galaxy bias and magnification effects from all the samples on the measurements, finding them to be small, and we propose corrections to reduce them further. We model the redshift distributions with splines and compare our results to previous analyses as well as to other parameterizations found in literature. For the two high-redshift tomographic bins, we find the shifts to higher redshifts with respect to the measurements performed in Rau+2022 to be $Δz_3=-0.039^{+0.020}_{-0.021}$ and $Δz_4=-0.048^{+0.012}_{-0.012}$.
[abstract 44 / 52] (score: 2) - Title: Hybrid RANS-LES simulation of transverse fuel injection in a Mach-10 scramJET engineAuthors: Nick Plewacki, Benjamin Kale, Manu Kamin, Luis Bravo,Comments:Subjects: physics.flu-dynCreated: 2025-11-22; Updated: 2025-11-25; Datestamp: 2025-11-25
Hypersonic flight poses unique propulsion challenges, requiring engines that maintain thrust, efficiency, and stability across a wide range of operating conditions. These engines must transition smoothly between flight regimes and altitudes. ScramJETs (supersonic combustion ramJETs) play a key role in addressing these challenges. Recent advancements in high-fidelity computational fluid dynamics (CFD) tools allow researchers to explore novel designs and improve the feasibility of hypersonic travel. In this work, we analyze a radical-farming type scramJET engine mounted at the University of Queensland's T4 Wind Tunnel at Mach 10. We use the Improved Delayed Detached Eddy Simulation (IDDES) model, which combines Reynolds-Averaged Navier-Stokes (RANS) and Large Eddy Simulation (LES) in different flow regions. A novel integrated modeling strategy is introduced, coupling the inlet, fuel injectors, combustor, and nozzle for full-scale engine analysis. Hydrogen combustion is modeled using a Finite Rate Chemistry (FRC) approach with a 12-species, 27-reaction mechanism to capture shock-induced chemical kinetics across equivalence ratios of $ϕ= 0.5$ to $0.9$. The Takeno flame index analysis reveals multiple combustion regimes, with ignition occurring in the partially premixed regime. This is supported by Chemical Explosive Mode Analysis (CEMA), which identifies regions of high chemical sensitivity, correlating with observed hot pockets and providing insights into autoignition and flame stabilization mechanisms. The combination of IDDES and FRC improves the transport of hydrogen to hot pockets, producing combustion patterns that match experimental results. This work establishes a framework to address critical challenges in future air-breathing propulsion systems.
[abstract 45 / 52] (score: 2) - Title: Constraint on massive vector field with extreme-mass-ratio inspirals around a slowly rotating BLACK HOLEAuthors: Tieguang Zi, Peng-Cheng Li, Bao-Min Gu, Fu-Wen Shu,Comments: 20 pages, 7 figures, 2 tablesSubjects: gr-qc astro-ph.HECreated: 2025-11-23; Updated: 2025-11-25; Datestamp: 2025-11-25
We study the influence of a massive vector (Proca) field on the energy fluxes from extreme-mass-ratio inspirals (EMRIs) around a slowly rotating Kerr BLACK HOLE. The secondary compact object, carrying a Proca hair, emits additional dipolar radiation that alters total energy flux relative to general relativity (GR). These modifications induce a secular drift in the orbital evolution of circular geodesic orbits, leading to measurable dephasing in the resulting EMRIs waveforms. By evaluating waveform mismatches between the Einstein-Proca framework and its GR counterpart, we show that the Laser Interferometer Space Antenna (LISA) can distinguish the signatures of a light Proca field when BLACK HOLE rotation is included. Furthermore, using a Fisher information matrix analysis, we forecast LISA's capability to place stringent constraints on the Proca mass with EMRIs signal from slowly rotating Kerr BLACK HOLEs. For representative EMRIs configurations, we find that LISA can detect or constrain Proca masses down to $μ_v\sim 10^{-20}$eV, with typical fractional uncertainties at the level of tens percent, depending on the black-hole spin.
[abstract 46 / 52] (score: 2) - Title: Approximate analytic model of the boundary layer around a low MAGNETic field neutron star at the disk accretionAuthors: G. S. Bisnovatyi-Kogan,Comments: 11 pages, 1 figureSubjects: astro-ph.HECreated: 2025-11-23; Updated: 2025-11-25; Datestamp: 2025-11-25
An approximate analytic one-dimensional model is constructed, for the accretion disk boundary layer surrounding a neutron star whose low MAGNETic field does not affect the process of accretion. A high luminosity model is considered, with radiation pressure dominant in the interior part of the disk.
[abstract 47 / 52] (score: 2) - Title: r-Process nucleosynthesis from hyperaccreting neutron stars in common envelopesAuthors: Peter Anninos, Matthew Portman, Scott Carmichael, Robert Hoffman, Andre Sieverding,Comments:Subjects: astro-ph.HECreated: 2025-11-23; Updated: 2025-11-25; Datestamp: 2025-11-25
We investigate nuclear reactions and feedback in hyperaccreting neutron star environments, considering accretion rates in the range 0.3 - $3\times10^4$ $M_\odot$ yr$^{-1}$, typical of short-period compact object binaries in common envelopes. Our mode ls account for weak reactions, neutrino energy loss, nuclear energy release, pair production, degenerate equations of state, and general RELATIVISTIC hydrodynamics. Depending on accretion rates, these systems can develop both proton and neutron-rich atmospheres with strong convective instabilities linking the neutrino sphere to the outgoing accretion shock inside the radia tion trapping zone. Convection drives nucleons through multiple heating and cooling cycles, with photodisintegration dominat ing during the heating phase and heavy element synthesis during the cooling phase, ejecting material with abundances that dep end on the accretion rate and depth of the final decompression trajectory. The turbulent nature of convective currents is con ducive to creating a wide range of nuclear products through a variety of effects, including NSE freezeout and $r$, $p$ and $\ gamma$ processes. We also observe a novel multi-step process in reheated trajectories, consisting of proton-capture and photo-dissociation reactions operating on $r$-process seeds, producing overall neutron-deficient isotopes. A significant amount of infalling gas experiences high entropy and short (millisecond) freezeout timescales capable of making $r$-process elements w ith high over-abundances through a disequilibrium effect between neutrons and $α$-particles that does not require an excess of neutrons.
[abstract 48 / 52] (score: 2) - Title: Fast Radio Bursts from White Dwarf Binary Mergers: Isolated and Triple-Induced ChannelsAuthors: Cheyanne Shariat, Claire S. Ye, Smadar Naoz, Sanaea Rose,Comments: 11 pages, 3 figures; Submitted to ApJL, all comments are welcome!Subjects: astro-ph.HE astro-ph.GA astro-ph.SRCreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
The detection of fast radio bursts (FRBs) in both young and old stellar populations suggests multiple formation pathways, beyond just young MAGNETars from core-collapse SUPERNOVAe. A promising delayed channel involves the formation of FRB-emitting neutron stars through merger- or accretion-induced collapse of a massive white dwarf (WD). By simulating a realistic stellar population with both binaries and triples, we identify pathways to WD collapse that could produce FRB candidates. We find that (i) triple dynamics open new merger channels inaccessible to isolated binaries, significantly enhancing the overall merger rate; (ii) triple-induced mergers broaden the delay-time distribution, producing long-delay ($\gtrsim1$-8~Gyr) events largely independent of metallicity, alongside a shorter-delay population ($\lesssim100$~Myr) of rapid mergers; (iii) these long delays naturally yield FRBs in older environments such as quiescent host galaxies and galactic halos; (iv) when convolved with the cosmic star-formation history, binary channels track the star-formation rate ($z_{\rm peak} \sim 2$), while triple channels peak later ($z_{\rm peak} \sim 1$), giving a combined local source rate of $R_0 \approx 2\times10^4~{\rm Gpc^{-3}~yr^{-1}}$, consistent with observations; and (v) applying the same framework to Type~Ia SUPERNOVAe, we find that triples extend the delay-time tail and roughly double the Ia efficiency relative to binaries, yielding rates and redshift evolution in good agreement with observations. If FRBs originate from the collapse of WDs, our results establish triples, alongside binaries, as a crucial and previously overlooked formation pathway whose predicted rates, host demographics, and redshift evolution offer clear tests for upcoming surveys.
[abstract 49 / 52] (score: 2) - Title: Ion Temperature Anisotropy Limits from Magnetic Curvature Scattering in Magnetotail Reconnection JetsAuthors: Louis Richard, Anton V. Artemyev, Cecilia Norgren, Xin An, Sergey R. Kamaletdinov, Yuri V. Khotyaintsev,Comments: 12 pages, 5 figuresSubjects: physics.plasm-phCreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
In collisionless plasmas, relaxation of the deviations of ion velocity distribution functions (VDFs) from local thermodynamic equilibrium (LTE) occurs through particle interactions with electroMAGNETic fields. In particular, in the Earth's MAGNETotail, the deviations of the ion VDFs, typically consisting of multiple components, from the equilibrium must be limited to maintain stability of the current sheet. Curvature scattering is a leading candidate mechanism to limit such deviations, but its role remains insufficiently understood. We investigate the limits of ion temperature anisotropy in a MAGNETotail-like configuration by modeling a quasi-1D current sheet with a finite MAGNETic field curvature and three ion populations. We derive analytical thresholds for anisotropy based on current sheet stability and validate against spacecraft observations and numerical results. Our findings demonstrate that curvature scattering imposes limits on ion anisotropies, thereby maintaining the stability of the current sheet.
[abstract 50 / 52] (score: 2) - Title: Physics-informed Neural Operator Learning for Nonlinear Grad-Shafranov EquationAuthors: Siqi Ding, Zitong Zhang, Guoyang Shi, Xingyu Li, Xiang Gu, Yanan Xu, Huasheng Xie, Hanyue Zhao, Yuejiang Shi, Tianyuan Liu,Comments: 42 pages, 17 figures, 8 tables,Subjects: physics.plasm-ph cs.AICreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
As artificial intelligence emerges as a transformative enabler for fusion energy commercialization, fast and accurate solvers become increasingly critical. In MAGNETic confinement nuclear fusion, rapid and accurate solution of the Grad-Shafranov equation (GSE) is essential for real-time plasma control and analysis. Traditional numerical solvers achieve high precision but are computationally prohibitive, while data-driven surrogates infer quickly but fail to enforce physical laws and generalize poorly beyond training distributions. To address this challenge, we present a Physics-Informed Neural Operator (PINO) that directly learns the GSE solution operator, mapping shape parameters of last closed flux surface to equilibrium solutions for realistic nonlinear current profiles. Comprehensive benchmarking of five neural architectures identifies the novel Transformer-KAN (Kolmogorov-Arnold Network) Neural Operator (TKNO) as achieving highest accuracy (0.25% mean L2 relative error) under supervised training (only data-driven). However, all data-driven models exhibit large physics residuals, indicating poor physical consistency. Our unsupervised training can reduce the residuals by nearly four orders of magnitude through embedding physics-based loss terms without labeled data. Critically, semi-supervised learning--integrating sparse labeled data (100 interior points) with physics constraints--achieves optimal balance: 0.48% interpolation error and the most robust extrapolation performance (4.76% error, 8.9x degradation factor vs 39.8x for supervised models). Accelerated by TensorRT optimization, our models enable millisecond-level inference, establishing PINO as a promising pathway for next-generation fusion control systems.
[abstract 51 / 52] (score: 2) - Title: FPGA-Based Spill Regulation System for the Muon Delivery Ring at FERMIlabAuthors: J. R. Berlioz, D. Bracey, B. Fellenz, M. A. Ibrahim, V. Nagaslaev, A. Narayanan, P. Prieto, K. Danison-Fieldhouse, W. Sullivan,Comments: North American Particle Accelerator Conference (NAPAC2025)Subjects: physics.acc-phCreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
The Muon to Electron Experiment (Mu2e) requires a uniform beam profile from the Muon Delivery Ring to meet their experimental needs. A specialized Spill Regulation System (SRS) has been developed to help achieve consistent spill uniformity. The system is based on a custom-designed carrier board featuring an Arria 10 SoC, capable of executing real-time feedback control. The FPGA processes beam pulses of approximately 200 ns every 1.695 $μ$s, allowing for continuous monitoring of the extracted spill intensity through fast bunch integration. The system directly controls three quadrupole MAGNETs, which work in conjunction with sextupole MAGNETs to achieve third-order resonant extraction. Furthermore, the board interfaces with FERMIlab's Accelerator Control Network (ACNET), enabling operators to modify spill regulation settings in real-time via the control network while providing diagnostic waveforms. These waveforms help operators monitor the process and fine-tune the feedback mechanisms. This paper presents an overview of the board's architecture and its initial progress toward regulating beam extraction. This initial version of the regulation system aims to evaluate baseline performance to inform future system improvements.
[abstract 52 / 52] (score: 2) - Title: Guesswork in the gap: the impact of uncertainty in the compact binary population on source classificationAuthors: Utkarsh Mali, Reed Essick,Comments: 26 pages, 12 figures, 5 tablesSubjects: astro-ph.HE gr-qc physics.comp-ph physics.data-an physics.space-phCreated: 2025-11-24; Updated: 2025-11-25; Datestamp: 2025-11-25
The nature of the compact objects within the supposed "lower mass gap" remains uncertain. Observations of GW190814 and GW230529 highlight the challenges gravitational waves face in distinguishing neutron stars from BLACK HOLEs. Interpreting these systems is especially difficult because classifications depend simultaneously on measurement noise, compact binary population models, and equation of state (EOS) constraints on the maximum neutron star mass. We analyze 66 confident events from GWTC-3 to quantify how the probability of a component being a neutron star, P(NS), varies across the population. The effects are substantial, the dominant drivers of classification are the pairing preferences of neutron stars with other compact objects, and the neutron star spin distributions. The data reveals that P(NS) varies between 1% - 67% for GW230529's primary and between 51% - 100% for GW190425's primary. By contrast, P(NS) for GW190814's secondary varies by <10%, demonstrating robustness from its high signal-to-noise ratio and small mass ratio. Analysis using EOS information tends to affect P(NS) through the inferred maximum neutron star mass rather than the maximum spin. As it stands, P(NS) remains sensitive to numerous population parameters, limiting its reliability and potentially leading to ambiguous classifications of future GW events.
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