Current date: 2026-04-29
Setting default datestamp limit: 0
Datestamp limit: 2026-04-29 (0 days ago)
Created/updated limit: 2026-04-22 (7 days ago)
Found keywords_cs.datFound keywords_cis.dat
Suggested sets: physics, physics:astro-ph, physics:gr-qc, physics:physics
Setting default set: physics
OAI-PMH request: http://export.arxiv.org/oai2?verb=ListRecords&from=2026-04-29&until=2026-04-29&set=physics&metadataPrefix=arXiv
Scoring abstracts
Number of records retrieved: 777
Keyword score statistics
score 11 -- 1 abstracts
score 9 -- 2 abstracts
score 6 -- 2 abstracts
score 5 -- 5 abstracts
score 4 -- 3 abstracts
score 3 -- 12 abstracts
score 2 -- 16 abstracts
in total -- 41 abstracts
Articles that appeared on 2026-04-29
-
[abstract 1 / 41] Wow! (score: 11)
- Title: CAZ catalog and optical light curves of 7918 BLAZAR-selected ACTIVE GALACTIC NUCLEiAuthors: Pouya M. Kouch, Elina Lindfors, Talvikki Hovatta, Ioannis Liodakis, Karri I. I. Koljonen, Alessandro Paggi, Kari Nilsson, Jenni Jormanainen, Vandad Fallah Ramazani, Sofia Kankkunen, Folkert Wierda, Sarah M. Wagner, Matthew J. Graham,Comments: 22 Pages, 23 Figures, Published in A&A, Catalog is public at CDS: https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/708/A382Subjects: astro-ph.HECreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
Active galactic nuclei (AGN) are some of the brightest and most variable objects in the Universe. Those with RELATIVISTIC JETs observed at small viewing angles are BLAZARs. Due to Doppler boosting, BLAZARs exhibit extreme stochastic variability. While the origin of this variability is thought to be changes in the accretion flow and JET dynamics, much about BLAZAR variability remains unknown. In this paper we use several BLAZAR-dominated AGN samples to form a catalog of 7918 BLAZARs and candidates -- the largest to date. We also collected source types, redshifts, peak frequencies of the spectral energy distribution, radio variability Doppler factors, and X-ray flux densities for as many sources as possible. We used all-sky surveys (CRTS, ATLAS, and ZTF, abbreviated as ``CAZ'') to extract their optical multiband flux density on a nightly basis between 2007 and 2023, and we constructed as long and as high cadence light curves as possible for as many sources as attainable. We quantified the variability of the light curves and applied the Bayesian blocks algorithm to determine their flaring periods. The CAZ catalog and light curves as well as the corresponding Bayesian blocks and flaring periods are all provided in the accompanying electronic tables, with the goal of enabling analyses involving JETted AGN variability with unprecedented sample sizes. Overall, we find (1) optical flares generally have a faster rise than decay; (2) optical brightness and variability are strongly dependent on the SYNCHROTRON peak frequency; (3) flat spectrum radio QUASARs and BL Lac objects have comparable optical variability and flare characteristics at the same SYNCHROTRON peak frequency; and (4) optical flare times tend to decrease while amplitudes increase with an increasing radio variability Doppler factor.
[abstract 2 / 41] Wow! (score: 9) - Title: Association of the IceCube neutrinos with CAZ BLAZAR light curvesAuthors: Pouya M. Kouch, Talvikki Hovatta, Elina Lindfors, Ioannis Liodakis, Karri I. I. Koljonen, Alessandro Paggi,Comments: 18 Pages, 10 Figures, Published in A&A, Data tables at CDS: https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/708/A383Subjects: astro-ph.HECreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
The IceCube Neutrino Observatory has detected several hundred high-energy neutrinos from cosmic sources. Despite numerous studies searching for their origin, it is still not known which sources emit them. A few likely individual associations exist with ACTIVE GALACTIC NUCLEi (AGNs), mostly comprising BLAZARs (AGNs with JETs pointed toward Earth). Nonetheless, on a population level, BLAZAR-neutrino correlation strengths are rather weak. This could mean that BLAZARs as a population do not emit high-energy neutrinos or that the detection power of the tests is insufficient due to the strong atmospheric neutrino background. By assuming an increase in high-energy neutrino emission during major BLAZAR flares, in our previous studies, we leveraged the neutrino arrival time to boost the detection power. Here, we utilize the same principle, while substantially increasing the number of BLAZARs in the sample. We searched for the spatiotemporal correlation of 356 IceCube high-energy neutrinos with major optical flares of 3225 radio- and 3814 $γ$-ray-selected BLAZARs. We found that despite the increase in data size, the number of likely spatiotemporal associations remained low and the overall correlation strengths weak. Two individual associations were shown to drive our strongest correlation, namely, the only $>$2$σ$ post-trial spatiotemporal correlation, occurring with the BL Lac objects of the radio-selected BLAZAR sample. We estimated that $\lesssim$8\% of the detected cosmic neutrinos were emitted by BLAZARs during major optical flares. As a complementary analysis, we compared the SYNCHROTRON peak frequency, redshift, Doppler factor, X-ray brightness, and optical variability of spatially neutrino-associated BLAZARs to those of the general BLAZAR population. We found that spatially neutrino-associated BLAZARs have a Doppler factor and X-ray brightness that are higher than average.
[abstract 3 / 41] Wow! (score: 9) - Title: Ultra-thick warm absorbers: Enlarging the parameter space of AGN ionised outflowsAuthors: R. Middei, E. Piconcelli, E. Nardini, A. Marinucci, M. Laurenti, A. Luminari, A. Trindade Falcão, A. Tortosa, M. Perri, S. Puccetti, D. Ł. Król, L. Borrelli,Comments: accepted for publication in A&A, 15 pagesSubjects: astro-ph.HE astro-ph.GACreated: 2026-04-27; Updated: 2026-04-29; Datestamp: 2026-04-29
The analysis of X-ray absorption features in ACTIVE GALACTIC NUCLEi (AGN) provides a wealth of information about the physical properties of the matter surrounding supermassive BLACK HOLEs (SMBHs). While standard correlations between the ionisation state, column density, and velocity typically distinguish between disc winds and warm absorbers, some sources exhibit properties that significantly deviate from these trends. We investigate a class of X-ray absorbers, which we define as ultra-thick warm absorbers (UTWAs), identified in a sample of 12 AGN. These absorbers are characterised by exceptionally high column densities and ionisation parameters (($\log (N_{\rm H}/\rm cm^{-2})\gtrsim22.5$ and $0.5 \lesssim \log(ξ/\rm erg~cm~s^{-1})$ $ \lesssim 2.5$)) that lie outside the typical ranges observed in standard warm absorbers. We performed detailed X-ray spectral analyses of both unpublished and archival {\it XMM-Newton}, {\it NUSTAR}, and {\it SWIFT} datasets to characterise the physical properties of UTWAs in four of these twelve sources. We studied their variability on timescales ranging from days to years and explored their connection with other spectral features. All AGN hosting UTWAs in our sample exhibit extreme soft X-ray variability, in some cases up to an order of magnitude, primarily driven by changes in the absorbing gas. In a subset of these sources (four out of 12), the UTWAs are accompanied by signatures of ultra-fast outflows (UFOs) in the Fe K$α$ energy range. UTWAs represent a rare but crucial phase of AGN feedback. We discuss their physical origin, their potential connection with UFOs, and provide insights into why these high-column density, unusually ionised absorbers appear so rarely in local AGN samples.
[abstract 4 / 41] Yes (score: 6) - Title: Study of Flat Spectrum Radio Quasars and BL Lacertae Objects as Sources of Diffusive Ultra High-Energy Cosmic RaysAuthors: Swaraj Pratim Sarmah, Umananda Dev Goswami,Comments: 14 pages, 4 figuresSubjects: astro-ph.HECreated: 2026-04-27; Updated: 2026-04-29; Datestamp: 2026-04-29
We examine whether Flat Spectrum Radio Quasars (FSRQs) and BL Lacertae objects (BL Lacs) can act as plausible astrophysical sources of diffuse ultra-high-energy COSMIC RAYs (UHECRs). Using realistic luminosity-dependent density evolution (LDDE) functions derived from observed gamma-ray luminosity functions for FSRQs and BL Lacs, we calculate the redshift evolution of the COSMIC RAY source population through integrated luminosity functions. The diffuse UHECRs flux from these sources is modelled by propagating nuclei through extragalactic space, including energy losses from interactions with cosmic photon backgrounds. The resulting UHECRs spectra are compared with observational data from the Pierre Auger Observatory and the Telescope Array, with fluxes normalised at reference energies. We also construct illustrative full skymaps of the integral UHECRs flux from $10$ EeV to $100$ EeV using the \textsc{HEALPix} framework, assuming a uniform distribution of synthetic sources and including energy dependent MAGNETic diffusion. Our results show that although both FSRQs and BL Lac objects can reproduce the observed UHECR flux, the FSRQ scenario is disfavoured by anisotropy and inconsistent source density, while BL Lacs remain consistent with observations.
[abstract 5 / 41] Yes (score: 6) - Title: Rotation Measure Substructures Induced by the Ponderomotive Force of Inertial \alfven WavesAuthors: Qing Zhao, Di Xiao, Xue-Feng Wu,Comments: 11 pages, 4 figures, ApJ acceptedSubjects: astro-ph.HE physics.plasm-phCreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
The rotation measure (RM) and dispersion measure (DM) of fast radio bursts (FRBs) serve as critical probes of the MAGNETo-ionic environments along the line of sight. The significant temporal evolution of RM observed in some repeating FRBs is generally attributed to the local environment of the source, since the intergalactic medium is not expected to vary on such short timescales. Recent observations of repeating FRB 20201124A and FRB 20220529 exhibit complex RM phenomenology, including large-amplitude global fluctuations and short-term substructures. Here, we attribute these short-term RM variations to the ponderomotive force exerted by inertial \alfven~waves (IAWs). We propose that IAWs, generated via MAGNETic RECONNECTion or turbulent cascades in a low-$β$ plasma, induce nonlinear density perturbations in the source environment. We demonstrate that the resulting plasma density redistribution can produce RM suppression consistent with observed substructures. This model presents a physically motivated mechanism for the short-term RM variability observed in active repeaters. It demonstrates that such fluctuations can arise from wave-driven density cavitation within a broad, coupled parameter space involving wave amplitude, plasma density, and temperature, thereby characterizing the localized plasma dynamics required to produce the observed RM jitters.
[abstract 6 / 41] Yes (score: 5) - Title: The case for super-Eddington accretion in JWST broad-line AGN during the first billion yearsAuthors: Erini Lambrides, Rebecca Larson, Kristen Garofali, Andrew Ptak, Marco Chiaberge, Arianna S. Long, Taylor A. Hutchison, Colin Norman, Jed McKinney, Hollis B. Akins, Danielle A. Berg, John Chisholm, Francesca Civano, Aidan P. Cloonan, Ryan Endsley, Andreas L. Faisst, Roberto Gilli, Steven Gillman, Michaela Hirschmann, Jeyhan S. Kartaltepe, Dale D. Kocevski, Vasily Kokorev, Fabio Pacucci, Chris T. Richardson, Massimo Stiavelli, Kelly E. Whalen,Comments: Published (Open Access), https://www.nature.com/articles/s41550-026-02813-w?utm_medium=organic_social&utm_source=partner&utm_content=null&utm_term=null&utm_campaign=CONR_JRNLS_LYLT_GL_PJNL_06PJ3_ARTPROMTKSubjects: astro-ph.HE astro-ph.GACreated: 2026-04-27; Updated: 2026-04-29; Datestamp: 2026-04-29
A multitude of JWST studies reveal a surprising over-abundance of over-massive accreting super-massive BLACK HOLEs (SMBHs) -- leading to a deepening tension between theory and observation in the first billion years of cosmic time. Across X-ray to infrared wavelengths, models built off of pre-JWST predictions fail to easily reproduce observed AGN signatures (or lack thereof), driving uncertainty around the true nature of these sources. Using a sample of JWST AGN identified via their broadened H$α$ emission and covered by the deepest X-ray surveys, we find neither any measurable X-ray emission nor any detection of high-ionization emission lines frequently associated with accreting SMBHs. We propose that these sources are accreting at or beyond the Eddington limit, which reduces the need for efficient production of heavy SMBH seeds at cosmic dawn. Using a theoretical model of super-Eddington accretion, we can produce the observed relative dearth of both X-ray and ultraviolet emission, as well as the high Balmer decrements, without the need for significant dust attenuation. This work indicates that super-Eddington accretion is easily achieved through-out the early Universe, and further study is required to determine what environments are required to trigger this mode of BLACK HOLE growth.
[abstract 7 / 41] Yes (score: 5) - Title: The Emergence of Little Red Dots from Binary Massive Black HolesAuthors: Kohei Inayoshi, Jinyi Shangguan, Xian Chen, Luis C. Ho, Zoltan Haiman,Comments: 19 pages, 8 figures, accepted for publication in ApJ. An analytical expression for the gas-attenuation transmission curve is provided for modeling LRD spectraSubjects: astro-ph.HE astro-ph.GACreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
Little red dots (LRDs) are a newly identified class of broad-line ACTIVE GALACTIC NUCLEi (AGN) with a distinctive v-shape spectrum characterized by red optical and blue UV continuum emission. Their high abundance at redshifts of $z\sim6-8$ and decline at lower redshifts suggest a transient origin. We propose that the spectral shape of LRDs originates from compact binary BLACK HOLE systems, where each BLACK HOLE is surrounded by a mini-disk and embedded in a larger circum-binary disk. With a binary separation of $\lesssim 10^3$ Schwarzschild radii, the Wien tail of a $T\simeq 5000~{\rm K}$ blackbody spectrum at the inner edge of the circum-binary disk produces the red optical emission, while the mini-disks power the UV continuum. Binary torques carve out a gap between the circum-binary disk and mini-disks, setting the turnover wavelength of the v-shaped spectrum around the Balmer limit. This scenario naturally reproduces LRD spectra requiring only modest dust attenuation ($A_V\lesssim 1$ mag), resolving overestimated luminosities for LRDs in previous studies and alleviating a tension with the so-called Soltan argument. This model predicts a distinct spectral evolution as the binary orbit decays through binary-disk interactions and gravitational waves (GWs), linking early-stage "proto-LRD" binaries to the broader AGN population and late-stage "LRD-descendants" to coalescing binaries detectable in GW experiments.
[abstract 8 / 41] Yes (score: 5) - Title: Unprecedented Multipoint Observation of Spatially Varying ICME Turbulence of Different Ages during October 2024 Extreme Solar Storm at 1 AUAuthors: Shibotosh Biswas, Ankush Bhaskar, SG Abitha, Omkar Dhamane, Sanchita Pal, Dibyendu Chakrabarty, Vipin K Yadav,Comments: Accepted in the Astrophysical JournalSubjects: astro-ph.SR physics.plasm-ph physics.space-phCreated: 2026-04-27; Updated: 2026-04-29; Datestamp: 2026-04-29
Understanding turbulence in interplanetary coronal mass ejections (ICMEs) is fundamental to space plasma research and critical for assessing the impact of space weather on geospace. Turbulence governs energy cascade, plasma heating, MAGNETic RECONNECTion, and solar wind MAGNETosphere coupling, thereby influencing both ICME evolution and geoeffectiveness. While previous event based and statistical studies have examined ICME turbulence and its radial evolution in great detail, no significant measurements of ICME MAGNETic turbulence at a single vantage point have been obtained from multiple observatories separated azimuthally. Here, we present the first multipoint analysis of MAGNETohydrodynamic (MHD) turbulence across ICME plasma regions, using four spacecraft at the Sun-Earth L1 point, separated by 80 RE (mesoscale) along the dawn-dusk direction. Using high-resolution MAGNETic field observations from ISRO's Aditya L1, NASA's Wind and ACE, and NOAA's DSCOVR, we analyze turbulence associated with the October 10, 2024, solar storm, which triggered the second strongest geoMAGNETic storm of solar cycle 25. Our results reveal significant variability and differing turbulence maturity across small separations, supported by analysis of field-aligned and perpendicular MAGNETic-field cascades, indicating strong anisotropies. Sheath turbulence is substantially modified by shock induced energy injection. Evidence of compressible turbulence and plasma energization at the flux rope interaction region indicates that internal processes, such as MAGNETic RECONNECTion, strongly influence ICME plasma evolution, highlighting pronounced spatial variability in turbulence and plasma states observed by multiple L1 monitors near Earth and underscoring their potential role in space weather impacts.
[abstract 9 / 41] Yes (score: 5) - Title: Symmetric kiloparsec-scale radio knots in NGC 7213: evidence for a confined weak JET and recurrent nuclear activityAuthors: G. Bruni, F. Panessa, E. Kammoun, A. L. Thakur, C. Reynolds, R. Ricci, M. Wieringa, S. Bianchi, A. De Rosa, G. Matt, F. Nicastro, F. Ursini,Comments: Accepted for publication in A&ASubjects: astro-ph.GA astro-ph.HECreated: 2026-04-27; Updated: 2026-04-29; Datestamp: 2026-04-29
Low-luminosity ACTIVE GALACTIC NUCLEi (LLAGN) often host weak radio JETs whose propagation is shaped by the surrounding interstellar medium. We investigate the nearby LLAGN NGC7213 to assess its ability to launch collimated outflows beyond the nucleus and to characterise the origin and variability of newly identified radio components from parsec to kiloparsec scales. We present new MeerKAT, uGMRT, ATCA, and Australian Long Baseline Array (LBA) observations from 300 MHz to 9 GHz. We analyse the morphology and spectra of the kiloparsec-scale emission and use LBA monitoring to probe the parsec-scale core. We discover a pair of compact radio knots located symmetrically at a projected distance of ~5 kpc north and south of the nucleus. The knots have nearly identical flux densities and flat radio spectra from 300 MHz to at least 5.5 GHz, with no significant spectral or geometric asymmetry. The LBA monitoring shows that the nuclear source remains unresolved at all epochs, constraining the 8 GHz emission to sub-parsec scales, and reveals significant variability on decade-long and month-long timescales, including a flux-density increase of ~40 mJy over six months. The symmetry, spectra, and physical properties of the kiloparsec-scale knots support their interpretation as compact termination shocks of a weak or intermittent JET launched by NGC7213 and confined by the dense, disturbed interstellar medium. The unresolved, variable parsec-scale core indicates that the high-frequency radio variability originates in the innermost JET region, likely linked to a recent increase in nuclear activity. NGC7213 is therefore a nearby example of how weak JETs in low-accretion AGN can produce both compact nuclear variability and symmetric kiloparsec-scale structures in complex environments.
[abstract 10 / 41] Yes (score: 5) - Title: Intergalactic Magnetic Field constraints from detected very high-energy Gamma-Ray Bursts using the Cherenkov Telescope Array ObservatoryAuthors: Ténéman Keita, Renaud Belmont, Thierry Stolarczyk,Comments: 18 pages, 14 figuresSubjects: astro-ph.HE astro-ph.COCreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
Defined as the MAGNETic field permeating cosmic voids, the Intergalactic Magnetic Field (IGMF) is thought to be a relic of the Big Bang, tracing a primordial MAGNETic seed at the origin of all astrophysical fields. Yet, it has thus far escaped detection. Lower limits on the IGMF strength can be established by observing very high-energy (VHE) photons from extragalactic sources. Specifically, this can be achieved by characterising the time-delayed secondary emission induced by highly energetic transient sources, such as GAMMA-RAY BURSTs (GRBs). Most studies exclude values of the IGMF below $10^{-17}\;\mathrm{G}$ by comparing the expected effect to the sensitivity curves of various instruments in the $\mathrm{GeV}$ range or above. In this work, we simulate CTAO observation data under realistic observation conditions and perform spectral-temporal fits to estimate the constraints CTAO will bring on the IGMF once fully deployed. We apply the methodology to simulated sources with properties comparable to the few GRBs detected at VHE. In particular, we show that CTAO will probe strengths up to $\sim 10^{-15}\;\mathrm{G}$ when detecting sources similar to GRBs 221009A and 190114C. We also show that existing observations of GRB 221009A by the first CTAO Large Sized Telescope LST-1 favour a strength of $3\times 10^{-17}\;\mathrm{G}$.
[abstract 11 / 41] Yes (score: 4) - Title: Pair-Rich Corona of an Accreting Kerr Black HoleAuthors: Jonathan Zhang, Christopher Thompson,Comments: 30 pages, 23 figures, submitted to the Astrophysical JournalSubjects: astro-ph.HECreated: 2026-04-27; Updated: 2026-04-29; Datestamp: 2026-04-29
We build a self-consistent model of a warm scattering corona near an accreting BLACK HOLE in Kerr geometry, in the regime of slow ($\sim 0.01$ Eddington) mass accretion. An iterative Monte Carlo procedure is developed that incorporates self-consistently the effects of Compton scattering and electron-positron pair creation, as well as general RELATIVISTIC lensing and frame dragging effects. Soft thermal photons are seeded in the inner disk and the velocity dispersion of the electrons and positrons adjusted to yield a fixed seed luminosity amplification through Compton scattering. A simple kinematic prescription is also added for bulk outflow. Pair creation by photon collisions raises significantly the density of scattering charges in and around the innermost ion disk, which is assumed to be geometrically thick and rarefied compared with the disk outside 10 gravitational radii. The self-consistent pair cloud is concentrated closer to the BH. The spectrum and POLARIZATION of the escaping X-rays are recorded as a function of the observer's orientation. The temperature and Compton parameter measured from the output spectra using the compPS package are consistent with fits to binary BH data in the hardest spectral state; the POLARIZATION degree rises to $4-10\%$ through the 2-8 keV band with allowance for $e^\pm$ upflow from the BH equator.
[abstract 12 / 41] Yes (score: 4) - Title: Constraining the nature of ACTIVE GALACTIC NUCLEi through circumgalactic Lya emission at z=2-3Authors: Shiwu Zhang, Zheng Cai, Fabrizio Arrigoni Battaia, Sebastiano Cantalupo, Mingyu Li, Ben Wang, Yuduo Guo, Aura Obreja, Haibin Zhang, Zihao Li, Donghui Quan,Comments: 23 pages, 14 figures, submitted to the ApJSubjects: astro-ph.GACreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
We present a comprehensive analysis of circumgalactic Lya nebulae around 59 unobscured and 26 obscured QUASARs at z=2-3, observed with the Keck Cosmic Web Imager (KCWI), to constrain the nature of ACTIVE GALACTIC NUCLEi (AGN) at cosmic noon. We find that Lya nebulae around unobscured QUASARs are significantly less symmetric having a symmetry parameter of a_w=0.2-0.6 and more spatially extended having a scale length of r_h=10.7+/-0.5 kpc than those around obscured QUASARs (a_w=0.6-0.8; r_h=6.6-7.7 kpc).Unobscured QUASARs also exhibit steeply declining velocity dispersion profiles with the slope of -4.3+/-0.4 km s^-1 kpc^-1, indicative of large-scale outflows, whereas obscured QUASARs display flat profiles (-0.2+/-0.7 and -0.6+/-0.4 km s^-1 kpc^-1). The degree of QUASAR obscuration appears to be intrinsically linked to nebular asymmetry and extent, a relationship that could be in tension with the standard orientation-based AGN unified model, as it expects unobscured-QUASAR nebulae to be more symmetric and compact. These results naturally fit the evolutionary scenario, where AGN feedback drives a transition from an obscured to an unobscured phase-progressively redistributing gas to larger radii, introducing anisotropy, and driving turbulence. Taken together, our findings favor the evolutionary scenario over the purely orientation-based unified model for QUASARs at cosmic noon.
[abstract 13 / 41] Yes (score: 4) - Title: The GMRT High-Resolution Southern Sky Survey for pulsars and transients -- VIII: Orbital Variability and the Evolution of a 1-Day He-WD Millisecond Pulsar J2101-4208Authors: Ankita Ghosh, Bhaswati Bhattacharyya, David L. Kaplan, David A. Smith, Andrew Lyne, Jayanta Roy, Laila Vleeschower, Gabriella Agazie, Lankeswar Dey, Sangita Kumari, Ujjwal Panda,Comments: Submitted to ApJSubjects: astro-ph.HECreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
We present timing and orbital phase-resolved polarimetry of the millisecond pulsar (MSP) J2101$-$4802, having a spin period of 9.48~ms and dispersion measure (DM) $25.05\ \mathrm{pc\ cm^{-3}}$ discovered with the Giant Meter Radio Telescope (GMRT). From the phase-connected timing of this MSP spanning 3.7 years, we identify that PSR J2101-4802 is in a $\sim$1-day binary orbit with a likely helium-white-dwarf (He-WD) companion having a median companion mass of $\simeq0.15\, M_\odot$, consistent with canonical recycling in the Galactic field. The timing solution further reveals an unusually large orbital period derivative, $\dot{P}_b$ ($\sim10^{-11}\,{\rm s\,s}^{-1}$), compared to typical Galactic-field MSP--HeWD binaries, which cannot be explained by the contributions from kinematic effects (Shklovskii and Galactic acceleration) or general-RELATIVISTIC damping. Using wideband, full-Stokes observations, we also trace the linear and circular POLARIZATION variation across the orbital phase and fit a rotating-vector model (RVM) to its position-angle swing across the pulse phase, yielding constraints on the emission geometry (MAGNETic inclination and impact angle) of this system. The combination of a $\sim$1-day orbit, $\sim0.15\,M_\odot$ companion, modest spin-down power, unusually large $\dot{P}_b$, and phase-locked MAGNETized intrabinary plasma signatures suggests that PSR~J2101$-$4802 represents a transitional system linking redback-like spiders to detached He--WD MSP binaries.
[abstract 14 / 41] (score: 3) - Title: Screening effect of plasma flow on the resonant MAGNETic perturbation penetration in tokamak based on two-fluid modelAuthors: Weikang Tang, Qibin Luan, Hongen Sun, Lai Wei, Shuangshuang Lu, Shuai Jiang, Jian Xu, Zhengxiong Wang,Comments:Subjects: physics.plasm-phCreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
Numerical simulation on the resonant MAGNETic perturbation penetration is carried out by the newly-updated initial value code MDC (MHD@Dalian Code). Based on a set of two-fluid four-field equations, the bootstrap current, parallel and perpendicular transport effects are included appropriately. Taking into account the bootstrap current, a mode penetration like phenomenon is found, which is essentially different from the classical tearing mode model. It may provide a possible explanation for the finite mode penetration threshold at zero rotation detected in experiments. To reveal the influence of diaMAGNETic drift flow on the mode penetration process, $\bf E\times B$ drift flow and diaMAGNETic drift flow are separately applied to compare their effects. Numerical results show that, a sufficiently large diaMAGNETic drift flow can drive a strong stabilizing effect on the neoclassical tearing mode. Furthermore, an oscillation phenomenon of island width is discovered. By analyzing in depth, it is found that, this oscillation phenomenon is due to the negative feedback regulation of pressure on the MAGNETic island. This physical mechanism is verified again by key parameter scanning.
[abstract 15 / 41] (score: 3) - Title: Coupling of neutrino beam-driven MHD waves and resonant instabilities in rotating MAGNEToplasmas with neutrino two-flavor oscillationsAuthors: Jyoti Turi, Amar P. Misra,Comments: 14 pages, 5 figures; Abstract modified, other parts improved with more explanations and discussion, especially in Secs. I and VSubjects: astro-ph.HE physics.plasm-phCreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
We present an analysis of neutrino-driven MAGNETohydrodynamic (MHD) waves and instabilities in a rotating MAGNEToplasma with weak neutrino interactions. We show, for the first time, that neutrino-driven shear Alfv{é}n and oblique MAGNETosonic waves can be coupled by the Coriolis force, forming new wave modes affected by this force, as well as neutrino beam and two neutrino flavor oscillations. Our work extends previous theories by demonstrating that shear Alfv{é}n waves are influenced by neutrino effects and by identifying instabilities resulting from resonant interactions with both a streaming neutrino beam and flavor oscillations. We find that the Coriolis force, as well as plasma density and MAGNETic field strength, significantly affect the profiles of the instability growth rates. Such a growth rate for MAGNETosonic waves appears much higher than the Alfv{é}n wave, implying that MAGNETosonic waves provide a superior mechanism for energy extraction from the neutrino beam. For typical parameters relevant to the protoneutron star surface, the instability time for MAGNETosonic waves may vary in the range 0.09-0.14 s, which is within the predicted time of the neutrino-driven explosion (0.3 s after bounce) reported in the recent three-dimensional MHD simulations of core-collapse SUPERNOVAe. Our findings may shed new light on the physical mechanisms underlying core-collapse SUPERNOVAe.
[abstract 16 / 41] (score: 3) - Title: Diverse Emission Patterns from Precessing Super-Eddington Disks Formed in Tidal Disruption EventsAuthors: Jin-Hong Chen, Lixin Dai, Kan Cheuk Kwan, Tom Man Kwan, Zijian Zhang,Comments: 19 pages, 9 figures, 1 table; Published in ApJSubjects: astro-ph.HE astro-ph.GACreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
A tidal disruption event (TDE) occurs when a star passes within the tidal radius of a supermassive BLACK HOLE (SMBH). In TDEs it is expected that the orbital angular momentum of the disrupted star is generally misaligned with the SMBH spin axis, which should result in a misaligned super-Eddington disk precessing around the SMBH spin axis due to the Lense-Thirring effect. In this paper, we investigate the distinct observational signatures produced from such TDE disks, by performing radiative transfer calculations upon previous super-Eddington disk simulations. We demonstrate that the precession of the disk and wind drive time-dependent obscuration and reprocessing of X-ray radiation. Depending on the orientation of the viewing angle of the observer and the tilt angle of the disk, four main types of variability are induced: 1) The smooth-TDEs: The emissions from these TDEs show no fluctuations; 2) The dimmer: The main emission type (X-ray or optical) stays the same, with small to moderate modulations of brightness; 3) The blinker: X-ray and optical emissions take turns to dominate in one cycle of precession, with dramatic changes in the X-ray fluxes. 4) The siren: X-ray and optical emissions take over each other twice per cycle, possibly with two different peak X-ray fluxes within one cycle. In all three scenarios, we observe an inverse correlation between X-ray and optical emissions. Our model provides a physical framework for interpreting TDE multi-wavelength variability through disk precession dynamics and gives an alternative interpretation to the interesting case of J045650.3-203750 which was suggested to be a repeated partial TDE previously.
[abstract 17 / 41] (score: 3) - Title: CIV wind properties of the SDSS-V X-ray selected QUASARs: strong optical-to-UV emission is key regardless of X-ray strengthAuthors: Amy L. Rankine, David Homan, James Aird, Pranavi Hiremath, Scott F. Anderson, Roberto J. Assef, Franz E. Bauer, W. N. Brandt, Marcella Brusa, Johannes Buchner, Maria Chira, Yaherlyn Díaz, Patrick B. Hall, Anton M. Koekemoer, Mirko Krumpe, Georg Lamer, Teng Liu, Sean Morrison, Blessing Musiimenta, C. A. Negrete, Qingling Ni, Paola Rodríguez Hidalgo, Mara Salvato, Donald P. Schneider, Yue Shen, Matthew J. Temple, Dusán Tubín-Arenas, Dominika Wylezalek,Comments: 20 pages, including 15 figures and 3 appendixes. Accepted for publication in MNRASSubjects: astro-ph.GA astro-ph.HECreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
We present an investigation of the rest-frame optical/UV and X-ray properties for a sample of 3027 X-ray selected QUASARs between $1.5 \leq z \leq 3.5$ detected in the deepest Spectrum Roentgen Gamma/eROSITA data available and observed by the fifth iteration of the Sloan Digital Sky Survey (SDSS-V). We parametrize the CIV$\lambda1549$ emission line to infer the strength of accretion disc winds and perform X-ray spectral fitting. The X-ray spectral properties -- namely, the 2keV monochromatic luminosity (L$_\text{2keV}$) and spectral slope -- are not strongly correlated with wind strength. Despite this result, the X-ray selected sample is shifted towards lower CIV blueshifts and higher equivalent widths than the optically selected sample observed in previous SDSS surveys, and matching in optical luminosity, redshift, and Eddington ratio does not reduce these differences. We estimate the far-UV luminosity using the HeII$\lambda1640$ line luminosity and define the slopes between this and the 2500A monochromatic luminosity ($L_{2500}$) and L$_\text{2keV}$ ($α_\text{ouv}$ and $α_\text{uvx}$, respectively) in a similar manner to the familiar $α_\text{ox}$ parameter, which tracks the spectral slope between $L_{2500}$ and L$_\text{2keV}$. The quantity $α_\text{ouv}$ is more strongly correlated with wind strength in our sample than $α_\text{ox}$. We show that the correlation between $α_\text{ox}$ and wind strength is driven by the relationship between the optical luminosity and wind strength. Our results are consistent with a radiation line-driven wind, whereby the ionising far-UV photons must not over-ionise the gas. The hard X-ray photons are few enough in number to have a negligible effect on the ionisation state of the material.
[abstract 18 / 41] (score: 3) - Title: The trigger and localization system of SVOM-GRMAuthors: Jiang He, Jian-Chao Sun, Yue Huang, Yong-Wei Dong, Shi-Jie Zheng, Xiao-Yun Zhao, Min Gao, Lu Li, Jiang-Tao Liu, Xin Liu, Hao-Li Shi, Li-Ming Song, Wen-Jun Tan, Bo-Bing Wu, Chen-Wei Wang, Jin Wang, Jin-Zhou Wang, Ping Wang, Rui-Jie Wang, Shao-lin Xiong, Juan Zhang, Li Zhang, Shuang-Nan Zhang,Comments: Accepted for publication in SVOM special issue in Research in Astronomy and Astrophysics; 9 pages,11 figuresSubjects: astro-ph.IM astro-ph.HECreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
The Space multi-band Variable Object Monitor (SVOM) is an astronomical satellite jointly developed by China and France, primarily focused on the detection of GAMMA-RAY BURSTs (GRBs) and transient sources. The SVOM satellite was launched on 22nd June, 2024 with four payloads installed onboard. As one of payload, GRM comprises 3 gamma-ray detectors (each detector has an effective area of approximately 200~cm$^{2}$) with distinct pointing directions, enabling the temporal and spectral measurements as well as localization of GRBs in the energy range of 15-5000 keV. This article firstly introduces the on-board localization algorithm design for GRM and presents preliminary test results. Then, leveraging abundant ground-based computational resources, a joint fitting method for spectral and localization analysis using Monte Carlo Markov Chain (MCMC) is implemented. In contrast to the on-board localization algorithm, the on-ground MCMC method comprehensively considers the influence of spectral characteristics, thereby mitigating systematic biases. Finally, a systematic analysis based on this method is provided, highlighting the localization and spectral measurement capabilities of GRM. The preliminary localization analysis result for the on-board detected GRB 240629A by both GRM and FERMI/GBM shows that the localization result (error$\sim$4.14$^{\circ}$) of GRM is consistent with the FERMI/GBM result.
[abstract 19 / 41] (score: 3) - Title: A simple model of current ramp down in the ITER tokamakAuthors: Richard Fitzpatrick,Comments:Subjects: physics.plasm-phCreated: 2026-04-27; Updated: 2026-04-29; Datestamp: 2026-04-29
The controlled ramp down of the toroidal plasma current in the ITER tokamak is simulated using a simple model that employs cylindrical geometry. The MAGNETohydrodynamical (MHD) stability of the plasma throughout the whole current ramp is also calculated. The only potentially unstable MHD mode is the m=2/n=1 classical tearing mode. The envisioned 60 second ramp down of the plasma current in ITER is found to be perfectly feasible, provided that the plasma is sufficiently hot at the start of the ramp. However, attempts to ramp down the current on a significantly faster time scale are predicted to excite 2/1 tearing modes that are likely to lock to the vacuum vessel, and trigger a disruption.
[abstract 20 / 41] (score: 3) - Title: The Impact of Elliptical Broad-Line Regions on Reverberation-Based Black Hole Mass EstimatesAuthors: Jiancheng Wu, Haicheng Feng, Qingwen Wu, Xinwu Cao,Comments: 13 pages, 7 figures, Accepted for publication in ApJSubjects: astro-ph.GA astro-ph.HECreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
The virial factor $f$ is critical for accurate supermassive BLACK HOLE (SMBH) mass measurements using reverberation mapping (RM) and the radius--luminosity ($R$--$L$) relation, yet its value remains highly uncertain. While traditional models assume axisymmetric broad-line region (BLR) geometries, growing evidence suggests that BLRs may possess more complex, asymmetric structures. We systematically investigate the impact of elliptical-disk BLR geometries on SMBH mass determinations through comprehensive numerical simulations. By computing emission-line profiles, emissivity-weighted time lags, and the corresponding virial factor $f$ over a wide range of eccentricities, orientations, and inclinations, we find that even in purely virialized systems, geometric effects alone can cause $f$ to vary by more than an order of magnitude and can mimic observational signatures typically attributed to radiation pressure. Additionally, local broadening introduces further systematic uncertainties in velocity width measurements, biasing $f$ by up to a factor of $\sim$3. Asymmetric BLR configurations also induce a scatter of $\sim$0.18 dex in the $R$--$L$ relation due to projection effects, comparable to the intrinsic scatter observed in RM studies. These results challenge the conventional attribution of RM uncertainties to non-virial motions or radiation pressure, and instead highlight the fundamental role of BLR geometry in SMBH mass measurements.
[abstract 21 / 41] (score: 3) - Title: Theoretical Analysis and PIC Simulations of ElectroMAGNETic Wakefields Excited by Relativistic Beams in Magnetized PlasmasAuthors: Ali Asghar Molavi Choobini, Mehran Shahmansouri,Comments:Subjects: physics.plasm-ph physics.acc-ph physics.comp-phCreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
This study presents theoretical and numerical investigation of the coupled longitudinal and radial wakefields excited by ultraRELATIVISTIC electron beams propagating through a cold plasma channel subjected to an external axial MAGNETic field. A fully causal three dimensional Green function formalism is developed directly from the linearized Maxwell fluid equations in the presence of the MAGNETized plasma dielectric tensor. This unified framework captures the complete electroMAGNETic response, including the induction of a transverse plasma current and the resulting hybridization of longitudinal charge separation dynamics with cyclotron driven transverse motion. The analytical treatment reveals how MAGNETization modifies the effective restoring forces, enhances wake amplitudes, and reshapes the radial focusing defocusing structure of the wake. To validate the theoretical predictions and explore realistic parameter regimes, extensive three dimensional particle in cell simulations are performed using the EPOCH code across wide ranges of plasma density, MAGNETic field strength, beam Lorentz factor, transverse beam radius, and longitudinal current profiles. The simulations demonstrate excellent quantitative agreement with the analytical Green function solutions, confirming that increasing plasma density substantially amplifies the initial wake amplitude while accelerating the damping of higher order oscillations. Application of an external MAGNETic field induces coherent high frequency radial oscillations, strengthens focusing forces, and produces a hybrid eigenmode whose properties are absent in the unMAGNETized limit. Variations in the driver Lorentz factor lead to rapid convergence toward a universal ultraRELATIVISTIC wake structure, while the transverse beam profile controls the radial extent and balance between longitudinal acceleration and transverse focusing.
[abstract 22 / 41] (score: 3) - Title: Enabling real-time multi-messenger follow-up of transient events with Astro-COLIBRIAuthors: Bernardo Cornejo Avila, Sofia Bisero, Mickäel Costa, Antoine Ciric, Ilja Jaroschewski, Weizmann Kiendrébéogo, Fabian Schüssler,Comments: Contribution to the 2026 Very High Energy Phenomena in the Universe session of the 60th Rencontres de MoriondSubjects: astro-ph.IM astro-ph.HECreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
Time-domain astrophysics is a rapidly growing field focused on the study of transient phenomena such as Gamma-Ray Bursts (GRBs), Fast Radio Bursts (FRBs), SUPERNOVAe, novae, and AGN flares. Their characterization increasingly relies on a multi-messenger and multi-wavelength approach, combining gravitational waves, high-energy neutrinos, and electroMAGNETic observations across the spectrum. Such a coordinated strategy requires efficient information sharing and thus tools capable of rapidly compiling and contextualizing key data for each new event. We present Astro-COLIBRI, a well-established platform designed to meet this challenge. Astro-COLIBRI combines a public RESTful API, real-time databases, and a cloud-based alert system. It continuously listens to multiple alert streams, applies user-defined filters, and places each event in its multi-messenger and multi-wavelength context. Through its user-friendly interfaces, including a web application and mobile apps for iOS and Android, the platform provides clear data visualization as well as concise summaries of key event properties and observing conditions for user-defined locations.
[abstract 23 / 41] (score: 3) - Title: Compton-thick AGN Characterisation in a Multi-wavelength Context: Insights from the 70-Month \textit{SWIFT}/BAT CatalogueAuthors: Muhammad Luqman Hakeem Musa, Zamri Zainal Abidin, Masatoshi Imanishi, Yoshiaki Hagiwara, Adlyka Ainul Annuar,Comments: Accepted and published in MNRASSubjects: astro-ph.GA astro-ph.HECreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
We analyse Compton-thick ACTIVE GALACTIC NUCLEi (CT AGNs), a heavily obscured subclass that challenges traditional X-ray diagnostics. Using 243 sources from the 70-Month \textit{SWIFT}/BAT catalogue (26 CT, 217 non-CT), we investigate their properties across radio, infrared (IR), optical, and X-ray bands. VLASS data reveals slightly higher 2--3~GHz mean luminosities in CT AGNs, suggesting active cores attenuated by circumnuclear absorption. Mid-IR diagnostics show redder $W3-W4$ colours in CT AGNs, tracing cooler dust, with significant scatter likely driven by host-galaxy dilution. Most CT AGNs fall outside standard WISE selection wedges, highlighting mid-IR selection limitations. BPT diagnostics show that CT AGNs primarily occupy Seyfert regions, indicating isotropic narrow-line properties. CT AGNs favour significantly higher Eddington ratios ($λ_{\text{Edd}}$), supporting radiation-driven unification where intense accretion maintains high-column density. We also observe a moderate anti-correlation between [NII]/H$α$ and $λ_{\text{Edd}}$. Principal component analysis identifies ionizing power and the accretion-obscuration link as primary variance drivers, though both populations overlap significantly in the PC1--PC2 plane. Machine learning achieved high recall (0.80) using intrinsic X-ray luminosity, [OI]$λ$6300 and H$α$ luminosities, and $W2-W3$ colour. This demonstrates the potential for multi-wavelength signatures to verify CT candidates in future deep surveys where X-ray data is limited. Overall, our findings suggest CT AGNs are driven by high obscuration and accretion rates rather than a simple orientation effect.
[abstract 24 / 41] (score: 3) - Title: Massive Black holes and their galaxiesAuthors: Ricarda S. Beckmann, Rebecca J. Smethurst,Comments: Final draft submitted to the editor for the chapter "Massive black holes and their host galaxies" for submission to the editors for the Encyclopedia of Astrophysics 1st EditionSubjects: astro-ph.GA astro-ph.HECreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
Almost every galaxy in the local Universe is observed to have a massive BLACK HOLE in the centre. The properties of these BLACK HOLEs are observed to tightly correlate with those of their host galaxy which has been interpreted as coevolution regulated by BLACK HOLE feedback. This coevolution spans most of cosmic history, as the first active BLACK HOLEs, so-called ACTIVE GALACTIC NUCLEi, are already observed as early as $z\sim10$. In this chapter, we lay out how we can find supermassive BLACK HOLEs, review what we know about the population of BLACK HOLEs and their host galaxies from observations, and summarise what we have learned about their coevolution across cosmic time from both observations and simulations.
[abstract 25 / 41] (score: 3) - Title: Substructure in redMaPPer clusters and its impact on X-ray morphology and scaling relationsAuthors: R. Tuomainen, A. Finoguenov, J. Comparat, L. Doubrawa,Comments: 10+3 pages, A&A, in pressSubjects: astro-ph.CO astro-ph.HECreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
We statistically quantified the prevalence and properties of substructure in optical galaxy clusters and directly investigated its impact on X-ray morphology and scaling relations, leveraging new data from the DECaLS Legacy Survey and the SRG/eROSITA all-sky survey. We applied the hierarchical density-based clustering algorithm HDBSCAN to the redMaPPer galaxy cluster catalog to identify and characterize substructure from the probabilistic membership assignments. We then cross-matched this sample with the eROSITA X-ray morphology catalog to correlate optical substructure with a comprehensive set of X-ray morphological parameters. Finally, we analyzed the scaling relation between X-ray luminosity and optical richness for clusters with and without substructure. Substructure is a common feature, present in approximately 40% of clusters; a quarter of the full sample exhibits a fractional contribution to richness in excess of 35%. We find a highly significant correlation between optical substructure and disturbed X-ray morphologies, a trend that is strongest for high-mass clusters. The clusters with substructure also drive a stronger redshift evolution in the scatter of the Lx-lambda relation. At low redshifts (z<0.2), they display a systematically higher X-ray luminosity at fixed richness compared to relaxed systems. We attribute the enhanced effect of mergers on X-ray properties at low redshifts to the increased density contrast of low-redshift cool cores and longer substructure survival times, which are possibly due to the suppression of disruptive mixing by effects such as MAGNETic draping. At lower cluster richness, a discordance between X-ray morphology and the merging state indicates a growing relative importance of ACTIVE GALACTIC NUCLEus feedback in governing X-ray morphology.
[abstract 26 / 41] (score: 2) - Title: Schwinger effect in axion inflation on a latticeAuthors: Oksana Iarygina, Evangelos I. Sfakianakis, Axel Brandenburg,Comments: 6 pages, 3 figuresSubjects: astro-ph.CO hep-ph hep-thCreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
We present the first lattice simulations of the nonlinear evolution after axion inflation by self-consistently incorporating currents arising from Schwinger pair production. The tachyonically amplified gauge fields trigger the growth of Schwinger currents, leading to universal values for the conductivity and MAGNETic field at the onset of strong backreaction and subsequent quenching of gauge field production. We show that the Schwinger effect (prematurely) saturates gauge field production, thereby diminishing the prospects of high scale axion inflation MAGNETogenesis as a viable solution for BLAZAR observations.
[abstract 27 / 41] (score: 2) - Title: Spectral Uniformity of Little Red Dots: A Natural Outcome of Coevolving Seed Black Holes and Nascent StarburstsAuthors: Kohei Inayoshi, Kohta Murase, Kazumi Kashiyama,Comments: 25 pages, 9 figures, accepted for publication in ApJSubjects: astro-ph.GACreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
The birth of seeds of massive BLACK HOLEs (BHs) and nascent galaxies at cosmic dawn takes place in dense gaseous environments, which play a crucial role in shaping their coevolution and radiation spectra. We investigate gas accretion during the assembly of massive halos with $M_{\rm h}\gtrsim 10^{10-11}~M_\odot$ at redshifts $z\simeq 4-10$, driving both rapid BH feeding and concurrent nuclear starbursts. As the BH grows to $\sim 10^{6-7}~M_\odot$ via super-Eddington accretion, the accretion power inflates a dense envelope whose effective temperature approaches the Hayashi limit at $T_{\rm eff}\simeq 5000~{\rm K}$, producing red optical emission, while a coeval young stellar population of $\sim 10^7~M_\odot$ provides blue UV emission. This early coevolving system naturally reproduces the characteristic spectral features of the so-called little red dots (LRDs), a population of broad-line ACTIVE GALACTIC NUCLEi (AGNs), including the V-shaped UV-to-optical spectra and weakness of X-ray, infrared, and radio emission. Massive stars in the nuclear starburst soon explode as SUPERNOVAe, injecting energy and momentum that expel gas from the nucleus, quench gas supply to the BH envelope, and ultimately drive a transition into normal AGN phases. For individual LRDs, the optical-to-UV luminosity ratio remains nearly constant at $L_{\rm opt}/L_{\rm UV}\simeq 2-10$ from the onset of accretion bursts for $\simeq 15~{\rm Myr}$, one-third of the Salpeter time, until quenching by stellar feedback. While this ratio is sustained for the LRD population at $z\simeq 4-8$, it declines toward lower redshifts as BHs can no longer maintain red envelopes, thereby losing the LRD characteristics.
[abstract 28 / 41] (score: 2) - Title: Multimodal axion emissions from Abelian-Higgs cosmic stringsAuthors: Naoya Kitajima, Michiru Uwabo-Niibo,Comments: v2: 8 pages, 8 figures; updated to match the version accepted for publication in PRDSubjects: hep-ph astro-ph.CO hep-thCreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
We show that axions can be produced from Abelian-Higgs cosmic strings due to the axion-gauge coupling. The strong MAGNETic field is confined in the string, and the electric field is induced around the moving string, allowing axion productions from the dynamics of cosmic strings. Our numerical analysis on the string collision shows that a sizable number of axions can be produced at the RECONNECTion, and further emissions occur from moving kinks afterward. Large-scale lattice simulations of the string network further reveal multimodal axion emissions in the sense that axions are produced in both the low-energy and high-energy regimes. The former can contribute to the cold DARK MATTER and the latter can be regarded as dark radiation. We found that the axion with GeV or heavier mass can explain the current relic DARK MATTER abundance and simultaneously predicts a sizable amount of dark radiation which can be probed by future observations.
[abstract 29 / 41] (score: 2) - Title: Impact of facility timing and coordination for next-generation gravitational-wave detectorsAuthors: Ssohrab Borhanian, Arianna Renzini, Philippa S. Cole, Costantino Pacilio, Michele Mancarella, Davide Gerosa,Comments: 29 pages, 8 figures, 3 tablesSubjects: gr-qc astro-ph.HECreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
While the Einstein Telescope and Cosmic Explorer proposals for next-generation, ground-based detectors promise vastly improved sensitivities to gravitational-wave signals, only joint observations are expected to enable the full scientific potential of these facilities, making timing and coordination between the efforts crucial to avoid missed opportunities. This study investigates the impact of long-term delays on the scientific capabilities of next-generation detector networks. We use the Fisher information formalism to simulate the performance of a set of detector networks for large, fiducial populations of binary BLACK HOLEs, binary neutron stars, and primordial black-hole binaries. Bootstrapping the simulated populations, we map the expected observation times required to reach a number of observations fulfilling scientific targets for key sensitivity and localization metrics across various network configurations. We also investigate the sensitivity to stochastic backgrounds. We find that purely sensitivity-driven metrics such as the signal-to-noise ratio are not strongly affected by delays between facilities. This is contrasted by the localization metrics, which are very sensitive to the number of detectors in the network and, by extension, to delayed observation campaigns for a detector. Effectively, delays in one detector behave like network-wide interruptions for the localization metrics for networks consisting of two next-generation facilities. We examine the impact of a supporting, current-generation detector such as LIGO India operating concurrently with next-generation facilities and find such an addition will greatly mitigate the negative effects of delays for localization metrics, with important consequences on multi-messenger science and stochastic searches.
[abstract 30 / 41] (score: 2) - Title: Distinguishability of MAGNETic massive BLACK HOLEs from environmental mimics with inspiral gravitational wavesAuthors: Xulong Yuan, Xiangdong Zhang,Comments:Subjects: gr-qcCreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
In this work, we investigate the ppE waveform imprints induced by the external MAGNETic fields of Bertotti-Robinson and Bonnor-Melvin BLACK HOLEs, with the aim of distinguishing such MAGNETic effects from environmental influences. We first compute the ppE frequency-domain waveform for a small BLACK HOLE inspiraling into a massive KBR BLACK HOLE, which corresponds to a Kerr BLACK HOLE embedded in an external MAGNETic field. We find that the leading-order correction arising from the MAGNETic field is at the $-2$ PN order relative to the quadrupole term, while the next-leading-order correction is at $-1.5$ PN, originating from the spin of the BLACK HOLE. We further examine the effects of a spinning KBM BLACK HOLE, whose leading-order MAGNETic correction is at $-3$ PN, whereas its spin-induced correction is also at $-1.5$ PN. The leading-order ppE corrections for both KBR and KBM BLACK HOLEs do not appear degenerate with any modified theory of gravity effects; nonetheless, we demonstrate that they resemble the gravitational pull contributions from additional matter with power-law distributions of index $γ=1$ and 0, respectively. To break the degeneracy with a single event, we adopt the statistic F in former research to discriminate between these two classes of beyond-vacuum GR effects using multiple gravitational wave events. We show even with multiple event statistic, it is not always efficient to distinguish real MAGNETic field effect from corresponding gravitational pull effect, especially for Bertotti-Robinson MAGNETic effect. For Bonnor-Melvin BLACK HOLE, there is a transition value of $ρ_0$ estimated around $10^{-4}\text{kg}/\text{m}^3$ and corresponding $B\sim 10^{4}\text{T}$ above which real MAGNETic effect can be efficiently distinguished from gravitational pull and below the transition value it cannot.
[abstract 31 / 41] (score: 2) - Title: Do little red dots really form a distinct class of astronomical objects?Authors: Jean-Baptiste Billand, David Elbaz, Maximilien Franco, Fabrizio Gentile, Emanuele Daddi, Mauro Giavalisco, Dale D. Kocevski, Joseph S. W. Lewis, Benjamin Magnelli, Valentina Sangalli, Maxime Tarrasse,Comments: Submitted to A&A Version 2: Typo correctedSubjects: astro-ph.GACreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
JWST observations have identified a class of enigmatic sources known as "Little Red Dots" (LRDs). These have been interpreted as a distinct class of ACTIVE GALACTIC NUCLEi (AGN) and host galaxies, potentially involving "quasi-stars" or Black Hole stars (BH*). However, two questions remain: is there a clear discontinuity between LRDs and field galaxies, and do LRDs form a homogeneous population? In this work, we address these issues by introducing a continuous metric to evaluate the "LRDness" of galaxies. We measure their compactness ($δ_{compact}$), the sharpness of the V-shaped spectral energy distribution ($δ_{v-shape}$), and the strength of the broad Balmer line emission. We apply this approach to a sample of ~48,000 galaxies with photometric and ~5,000 with spectroscopic information, selected over ~750 arcmin^2. We find that V-shape prominence correlates strongly with morphology without a clear transition at common LRD selection thresholds: the fraction of compact galaxies rises continuously with V-shape intensity. Similarly, broad H$α$ strength increases with both V-shape sharpness and compactness. The [N II] deficit is not an exclusive feature of LRDs but a global property of compact, metal-poor galaxies. Only the 3% most extreme LRDs present a prominent Balmer break (>3) of potentially non-stellar origin. LRDs and non-LRDs follow similar trends in the evolution of the Balmer decrement with V-shape sharpness, suggesting a shared physical origin, likely dust attenuation. Estimated dust masses (~4-7 x 10^4 M_{sun}) and luminosities are low enough to account for their non-detection by ALMA. We conclude that most LRDs do not represent a separate class of objects, but rather the extreme tail of a continuous distribution of galaxies and broad H$α$ emitters, consistent with a classical broad line region and dust attenuation.
[abstract 32 / 41] (score: 2) - Title: Cosmological discrete self-similarity in primordial BLACK HOLE formationAuthors: Luis E. Padilla, Tomohiro Harada, Ethan Milligan, David Mulryne,Comments: 10 pages, 9 figures. Comments are welcomeSubjects: astro-ph.CO gr-qcCreated: 2026-04-23; Updated: 2026-04-29; Datestamp: 2026-04-29
We demonstrate that discrete self-similarity (DSS), originally discovered in the collapse of a massless scalar field in an asymptotically flat system, survives in primordial BLACK HOLE (PBH) formation within an expanding cosmological background. Using fully RELATIVISTIC numerical simulations of massless scalar-field collapse in an Friedmann-Lemaître-Robertson-Walker universe, we resolve the critical regime down to $|p-p_c|\sim 10^{-8}$, where $p$ and $p_c$ respectively are a parameter of the family of initial data and its threshold value, and find clear log-periodic oscillations in the PBH mass scaling relation. The detailed structure of these oscillations differs from that previously reported in the asymptotically flat case, exhibiting a more pronounced asymmetry between peaks and troughs. Analyzing two distinct families of initial data (Gaussian and piecewise rational curvature profiles), we find critical exponents and DSS periods that differ slightly but are broadly consistent within uncertainties. The presence of DSS implies characteristic log-periodic modulations in the PBH mass spectrum, with potential consequences for PBH abundances and the spectrum of induced gravitational waves.
[abstract 33 / 41] (score: 2) - Title: Bound or blown: the fate of hot gas in galaxy groupsAuthors: R. Seppi, D. Eckert, J. Schaye, J. Braspenning, M. Schaller, B. D. Oppenheimer, E. O'Sullivan, F. Gastaldello, L. Lovisari, M. A. Bourne, M. Sun, A. Finoguenov, H. Khalil, G. Gozaliasl, K. Kolokythas, Y. E. Bahar, R. Santra,Comments: Accepted for publication on A&ASubjects: astro-ph.CO astro-ph.GACreated: 2026-04-27; Updated: 2026-04-29; Datestamp: 2026-04-29
The impact of AGN feedback on the hot gas content of galaxy groups remains a key uncertainty in galaxy formation and its connection to the large scale structure of the Universe. We aim to compare the XMM-Newton Group AGN Project (X-GAP) sample to the hydrodynamical FLAMINGO simulations, which span a wide range of AGN feedback prescriptions. We construct X-GAP analogues by forward-modelling the full selection function, including detection and observational systematics, and generate end-to-end XMM-Newton mock observations analysed consistently with the data. We study multiple observables, including the L--T and Mgas--T relations, number of groups, mean temperature, and velocity dispersion, accounting for their covariance. The forward model accurately recovers input luminosities, gas masses, and core-excised temperatures for regular systems, enabling direct comparison in observable space. The normalisation of the scaling relations is the best discriminator between feedback models, while cosmic variance introduces > 20% fluctuations in the number of detected systems, making counts alone a weak discriminator. Models with intermediate feedback strength provide the best agreement with X-GAP, with the fgas-2sigma model yielding the lowest tension of only 0.8sigma, while the most extreme feedback scenario (fgas-8sigma) is ruled out at > 4sigma. Our results indicate that the thermodynamic properties of galaxy groups favour feedback stronger than the fiducial FLAMINGO calibration, but disfavour the most ejective models. This highlights the importance of combining forward modelling and multi-observable constraints to probe the fate of hot baryons in low-mass haloes.
[abstract 34 / 41] (score: 2) - Title: Can BLR line profile shape improve single-epoch BLACK HOLE mass estimates?Authors: Lizvette Villafaña, Tommaso Treu, Shu Wang, Misty C. Bentz, Brendon J. Brewer, Aaron J. Barth, Jong-Hak Woo, Matthew A. Malkan, Vardha N. Bennert, Vivian U,Comments:Subjects: astro-ph.GACreated: 2026-04-27; Updated: 2026-04-29; Datestamp: 2026-04-29
The virial coefficient ($f$), which is meant to encapsulate broad-line region (BLR) geometry and kinematics, remains one of the largest sources of systematic uncertainty in BLACK HOLE mass estimates for Active Galactic Nuclei (AGNs). While the use of a sample average $\langle f \rangle$ enables BLACK HOLE mass estimates across large samples and cosmological distances, individual AGNs may deviate from this average due to differences in BLR structure and viewing angle. In previous work, we reported marginal evidence for a correlation between $f$ and the shape of the broad H$β$ emission line, $\log_{10}(\mathrm{FWHM}/σ)$. In this work, we update our sample to include ten new sources with CARAMEL BLR dynamical modeling, increasing both the BLACK HOLE mass range and statistical power of our analysis. We find marginal evidence for a correlation between $f$ and $\log_{10}(\mathrm{FWHM}/σ)$, with a slope and intrinsic scatter consistent with previous results. The confirmation of this trend across a larger sample further supports the idea that line profile shape may reflect BLR properties in a way that directly impacts $f$. If confirmed with future BLR dynamical modeling of sources within a wider range of $\log_{10}(\mathrm{FWHM}/σ)$, this relationship could enable empirical estimates of the virial coefficient and improve single-epoch BLACK HOLE mass estimates across cosmic time.
[abstract 35 / 41] (score: 2) - Title: TDCOSMO XXVI: Uniform lens modeling of eight doubly imaged QUASARsAuthors: Ryan Brady, Xiang-Yu Huang, Simon Birrer, Anowar J. Shajib, Nafis Sadik Nihal, Cameron Lemon, Martin Millon, Veronica Motta, Dominique Sluse, Frederic Courbin,Comments: 13 figures, 7 tables, submitted to The Open Journal of AstrophysicsSubjects: astro-ph.CO astro-ph.GACreated: 2026-04-27; Updated: 2026-04-29; Datestamp: 2026-04-29
We present the first uniform gravitational lens modeling analysis of eight doubly imaged QUASARs from multi-band observations with the Hubble Space Telescope. Previous time-delay cosmography analyses by the TDCOSMO Collaboration have primarily relied on quadruply imaged QUASARs, while doubly imaged systems, despite being more abundant, remain underutilized due to their fewer geometric constraints. Using an open-source $\texttt{Lenstronomy}$ framework, we reconstruct the lensing systems with a pipeline tailored for doubles. Comparing our results to the literature, the modeled Einstein radii agree at an average of 1.5$σ$, which is expected given data and modeling heterogeneity, while modeled image separations differ from Gaia DR2 measurements with an r.m.s of only 3.6 mas. We find a strong correlation between Fermat potential precision and the surface brightness of the spatially extended host arcs, establishing that arc surface brightness is the primary driver of mass model precision in doubly imaged systems. To further quantify the information contributed by the lensed arcs, we performed a conjugate point analysis that uses only the QUASAR image positions to constrain the lens mass profiles. The resulting posteriors are substantially broader than those from full image modeling, and a strong anti-correlation between mass parameter hypervolume and arc magnitude additionally confirms that arc brightness determines the degree to which the lens mass profile can be constrained in doubles. A hierarchical cosmographic analysis incorporating time-delay measurements and stellar kinematics to infer $\text{H}_0$ will be presented in a subsequent publication. The uniform pipeline and arc surface brightness trends established here will significantly accelerate the construction of time-delay cosmography samples from the large lens populations expected from LSST, Roman, and Euclid.
[abstract 36 / 41] (score: 2) - Title: Core Collapse Supernova Modeling: The Next Ten YearsAuthors: Anthony Mezzacappa,Comments: Submitted to Classical and Quantum Gravity as part of a Focus Issue on Core Collapse Supernova Gravitational Wave Astronomy and Astrophysics: Past, Present, and Future motivated by the First IGWN Symposium on Core Collapse Supernova Gravitational Wave Theory and Detection held in Warsaw in July 2025Subjects: astro-ph.HECreated: 2026-04-27; Updated: 2026-04-29; Datestamp: 2026-04-29
Core collapse SUPERNOVA modeling has advanced considerably since the first numerical simulations were performed sixty years ago. In particular, the last decade has brought us sophisticated three-dimensional models with significant predictive capabilities -- e.g., for core collapse SUPERNOVA gravitational wave emission. The six decades of modeling have shown us the importance of individual components of these general RELATIVISTIC neutrino radiation MAGNETohydrodynamics events -- specifically, the importance of neutrino kinetics, fluid instabilities, MAGNETic fields, strong gravity, and the nuclear equation of state and neutrino--matter interactions calculated in a manner consistent with the equation of state. They have also shown us that simulation outcomes are sensitive to variations in the treatment of these ingredients, demanding a level of rigor that has not yet been consistently met by modelers. The efficacy of the neutrino shock reheating mechanism for core collapse SUPERNOVAe has been demonstrated. The models now require an improved quantitative predictive capability, which will be achieved through increased sophistication in the treatment of model components, both macroscopic (e.g., strong-field gravity) and microscopic (e.g., neutrino--matter interactions). Advancement of core collapse SUPERNOVA theory will also require the cooperation of modelers in other fields, especially stellar evolution and nuclear theory, to meet the level of rigor required to make the most of the eventuality of a Galactic core collapse SUPERNOVA and its multimessenger emissions.
[abstract 37 / 41] (score: 2) - Title: Thermodynamic Phase Transitions in Einstein-Maxwell-Scalar-Gauss-Bonnet GravityAuthors: Cristián Erices, Stella Kiorpelidi,Comments: 15 pages, 14 figuresSubjects: hep-thCreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
Although asymptotically flat BLACK HOLEs generically lack thermodynamic phase transitions, we show that curvature-induced scalarization of electrically charged BLACK HOLEs in Einstein-Maxwell- Scalar-Gauss-Bonnet theory provides a natural setting for nontrivial thermodynamic behavior, without invoking external confining mechanisms or an extended thermodynamic formalism. Working within the canonical ensemble and employing the Euclidean approach, we identify the coexistence of locally stable scalarized and small Reissner-Nordström thermal states, which promotes free-energy crossings to bona fide phase transitions between equilibrium phases. For weak coupling, a second-order phase transition coincides with the second bifurcation point, at which the scalarized branch RECONNECTs with the Reissner-Nordström branch and scalar hair is spontaneously shed. As the coupling strength increases, this transition becomes zeroth order, the scalarized branch shrinks, and a fish-like structure develops in its Helmholtz free energy, rendering locally stable thermal states partially metastable, and yielding up to three phase transitions. In the strong-coupling limit, the scalarized branch reduces to a Schwarzschild-like solution, and the Reissner-Nordström phase ultimately emerges as the sole thermodynamically preferred configuration
[abstract 38 / 41] (score: 2) - Title: Spectral Evolution and Transient Broad-Line Features in the Isolated AGN UNAM-KIAS 613Authors: Edgar Cortes-Suárez, Paola Marziani, Héctor Manuel Hernández-Toledo, Miguel Ángel Aragón-Calvo, Castalia Alenka Negrete,Comments: 16 pages, 11 figures, 5 tablesSubjects: astro-ph.GACreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
We present multi-epoch optical spectroscopy of the isolated elliptical galaxy UNAM-KIAS 613, hosting a low-luminosity Type 1 AGN. Analysis of archival Sloan Digital Sky Survey (SDSS) data from 2006 reveals a distinctive double-peaked broad H$α$ profile, tentatively modeled by a RELATIVISTIC accretion disk. Follow-up observations in 2018 and 2023 show the disappearance of the red and blue wings, leaving only a single-peaked, central broad component. No significant continuum variability is detected in ASAS-SN and Catalina light curves over 2012-2025, and multi-wavelength data (radio, mid-IR, X-ray) confirm a sub-Eddington, radio-quiet AGN (Eddington ratio $\approx$0.03-0.04, BLACK HOLE mass $\approx$10$^{7.2}$ M$\odot$). We propose that the double-peak structure is in reality transient, and arose from a one-time bipolar outflow event rather than a stable disk or from a Tidal Disruption Event. The mid-IR SED and radio luminosity place UK 613 on the boundary between AGN and STAR FORMATION dominance, suggesting residual STAR FORMATION, while we have found that the isolated environment seems to be prone to the rejuvenation of ellipticals by recent ($\lesssim$ 1 Gyr) cold gas. We also examined its location within the cosmic web with the aim of identifying possible distinctive effects imprinted on its spectroscopic properties. Ultimately, our results are consistent that UNAM-KIAS 613 might have under gone a ''turn-off'' of the accretion disk emitting region or a transition between a radiatively-inefficient and radiatively-efficient accretion mode, and highlight the complex interplay of disk, outflow, host processes and environment in low-accretion, low-BLACK HOLE mass AGNs, an AGN population still largely unexplored to-date.
[abstract 39 / 41] (score: 2) - Title: Augmented reality system for visualising MAGNETic field topology and charged-particle trajectories in MAGNETic fusion plasmasAuthors: Akinobu Matsuyama,Comments: 13 pages, 7 figuresSubjects: physics.plasm-phCreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
A cost-effective augmented reality (AR) system is presented for visualising three-dimensional MAGNETic field structures and charged-particle trajectories in MAGNETically confined fusion plasmas. The system presented in this study integrates an orbit-following simulation code with a marker-based AR framework using a web camera and the OpenCV library. By synchronizing the time step of the simulation with the frame rate of the camera, the trajectories are continuously updated and superimposed in real time onto the camera image. Through the interactive operation of manipulating the web camera, users can observe three-dimensional structures, such as MAGNETic islands, from various positions and viewing angles. Simultaneously, the visualisation results can be shared by multiple people through a display. Such a shared AR environment supports an intuitive understanding of three-dimensional spatial structures that involve a high cognitive load. It also enables collaborative reasoning based on common visual information in research on MAGNETic confinement fusion, where researchers and students have diverse backgrounds in physics, engineering, and related fields.
[abstract 40 / 41] (score: 2) - Title: Fast radio burst dispersion is an unbiased tracer of matter on large scalesAuthors: Shion Andrew, Haochen Wang, Kiyoshi Masui, Josh Borrow, Calvin Leung, Ryan Raikman, Matthieu Schaller, Joop Schaye, James M. Sullivan,Comments:Subjects: astro-ph.CO astro-ph.GA astro-ph.HE gr-qcCreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
The dispersion of fast radio bursts (FRBs) measures the column density of free electrons, tracing the diffuse ionized gas that contains more than $90\%$ of all baryons. On linear scales the FRB dispersion field is an approximately unbiased tracer of the matter distribution, an idea long assumed in the FRB large-scale structure literature and recently formalized by Zhou and Zhang [arXiv:2510.11022]. This follows from baryon-mass conservation, which forces the total baryon field to have unit linear bias, with dispersion inheriting this bias up to small corrections from the stellar and neutral-gas components. We show these corrections can be bounded at the percent level using existing galaxy and 21 cm surveys, and confirm with the FLAMINGO hydrodynamical simulations that the electron bias varies at the percent level across a wide range of feedback prescriptions. The dispersion-galaxy cross-power spectrum at linear scales directly constrains $B_8 \equiv σ_8(Ω_b/0.05)^{1/2}$, a baryonic analog of $S_8$, independently of feedback physics. Because most of the per-object variance in dispersion is cosmological signal rather than noise, $\sim\!10^5$ localized FRBs can match the statistical power of $\sim\!10^8$ weak-lensing galaxy shape measurements. FRB dispersion thus joins weak lensing and redshift-space distortions as a new unbiased tracer of matter on large scales.
[abstract 41 / 41] (score: 2) - Title: Explainable AI for Jet Tagging: A Comparative Study of GNNExplainer, GNNShap, and GradCAM for Jet Tagging in the Lund Jet PlaneAuthors: Pahal D. Patel, Sanmay Ganguly,Comments: 25 pages, 9 figures. Comments are welcomeSubjects: hep-ph cs.LG hep-exCreated: 2026-04-28; Updated: 2026-04-29; Datestamp: 2026-04-29
Graph neural networks such as ParticleNet and transformer based networks on point clouds such as ParticleTransformer achieve state-of-the-art performance on JET tagging benchmarks at the Large Hadron Collider, yet the physical reasoning behind their predictions remains opaque. We present different methods, i.e. perturbation-based (GNNExplainer), Shapley-value-based (GNNShap), and gradient-based (GRADCam); adapted to operate on LundNet's Lund-plane graph representation. Leveraging the fact that each node in the Lund plane corresponds to a physically meaningful parton splitting, we construct Monte Carlo truth explanation masks and introduce a physics-informed evaluation framework that goes beyond standard fidelity metrics. We perform the analysis in three transverse-momentum bins ($\mathrm{p_T} \in [500,700]$, $[800,1000]$, and the inclusive region $[500,1000]$ GeV), revealing how explanation quality and focus shift between non-perturbative and perturbative regimes. We further quantify the correlation between explainer-assigned node importance and classical JET substructure observables -- $N$-subJETtiness ratios $τ_{21}$ and $τ_{32}$ and the energy correlation functions -- establishing the degree to which the model has learned known QCD features. We find that overall the weight assigned by explainability methods has a correlation with analytic observables, with expected shift across different phase space regimes, indicating that a trained neural network indeed learns some aspects of JET-substructure moments. Our open-source implementation enables reproducible explainability studies for graph-based JET taggers.
arXiv:2510.16584 [pdf, ps, other]
arXiv:2510.16585 [pdf, ps, other]
arXiv:2604.24899 [pdf, ps, other]
arXiv:2511.08153 [pdf, ps, other]
arXiv:2604.25469 [pdf, ps, other]
arXiv:2409.13047 [pdf, ps, other]
arXiv:2505.05322 [pdf, ps, other]
arXiv:2602.13644 [pdf, ps, other]
arXiv:2604.25046 [pdf, ps, other]
arXiv:2604.25647 [pdf, ps, other]
arXiv:2604.24961 [pdf, ps, other]
arXiv:2604.25127 [pdf, ps, other]
arXiv:2604.25278 [pdf, ps, other]
arXiv:2108.09621 [pdf, ps, other]
arXiv:2510.19729 [pdf, ps, other]
arXiv:2510.24071 [pdf, ps, other]
arXiv:2603.15075 [pdf, ps, other]
arXiv:2604.18018 [pdf, ps, other]
arXiv:2604.24928 [pdf, ps, other]
arXiv:2604.25163 [pdf, ps, other]
arXiv:2604.25348 [pdf, ps, other]
arXiv:2604.25529 [pdf, ps, other]
arXiv:2604.25543 [pdf, ps, other]
arXiv:2604.25560 [pdf, ps, other]
arXiv:2604.25770 [pdf, ps, other]
arXiv:2506.20538 [pdf, ps, other]
arXiv:2509.19422 [pdf, ps, other]
arXiv:2510.10708 [pdf, ps, other]
arXiv:2510.11861 [pdf, ps, other]
arXiv:2603.05084 [pdf, ps, other]
arXiv:2604.11677 [pdf, ps, other]
arXiv:2604.21520 [pdf, ps, other]
arXiv:2604.24863 [pdf, ps, other]
arXiv:2604.24901 [pdf, ps, other]
arXiv:2604.24908 [pdf, ps, other]
arXiv:2604.24970 [pdf, ps, other]
arXiv:2604.25100 [pdf, ps, other]
arXiv:2604.25219 [pdf, ps, other]
arXiv:2604.25426 [pdf, ps, other]
arXiv:2604.25828 [pdf, ps, other]
arXiv:2604.25885 [pdf, ps, other]