Current date: 2026-06-10

Setting default datestamp limit: 0

Datestamp limit: 2026-06-10 (0 days ago)

Created/updated limit: 2026-06-03 (7 days ago)

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=2026-06-10&until=2026-06-10&set=physics&metadataPrefix=arXiv

Scoring abstracts

Number of records retrieved: 749

Keyword score statistics

score 8 -- 3 abstracts

score 7 -- 1 abstracts

score 6 -- 3 abstracts

score 5 -- 5 abstracts

score 4 -- 5 abstracts

score 3 -- 14 abstracts

score 2 -- 18 abstracts

in total -- 49 abstracts

Articles that appeared on 2026-06-10

[abstract 1 / 49] Wow! (score: 8)
arXiv:2606.10013 [pdf, ps, other]

Title: Limits on primordial BLACK HOLEs from the extragalactic gamma-ray background; current status and future projections

Authors: Ilias Cholis, Iason Krommydas, John Carlini,

Comments: 19 pages, seven figures, one table ZENODO link with simulation files: https://zenodo.org/records/20563575

Subjects: astro-ph.HE astro-ph.CO astro-ph.GA hep-ph

Created: 2026-06-08; Updated: 2026-06-10; Datestamp: 2026-06-10

Primordial BLACK HOLEs (PBHs), possibly formed from the collapse of early universe perturbations, will evaporate via Hawking radiation with a lifetime comparable to the age of the universe, if their mass is $O(10^{14})$ g. Such BLACK HOLEs can contribute to the observed gamma-ray fluxes in the MeV and GeV range. Using the observed extragalactic gamma-ray background (EGRB) from the \textit{FERMI} Large Area Telescope, the \textit{EGRET}, and the \textit{COMPTEL} telescopes that cover gamma-ray energies from 0.5 MeV to 1 TeV, we evaluate limits on the abundance of PBHs with masses of $10^{14}$ to $10^{17}$ g. We study both monochromatic and extended mass distributions of PBHs. To model the EGRB spectrum, we calculate the contribution from extragalactic sources including BLAZARs, star-forming galaxies and RADIO GALAXies and also account for ultra-high-energy COSMIC RAYs that produce gamma rays when interacting with the infrared background. Our EGRB modeling uses information from the \textit{FERMI} gamma-ray point sources catalog, from observations at X-rays, the visible spectrum, the infrared and radio waves, and also accounts for modeling uncertainties and variations on the properties within each class of these sources. Moreover, we use recent work on the modeling of the PBHs' gamma-ray emission, that includes the direct Hawking radiation, gamma rays produced in the hadronization and decay of unstable particles, final state radiation and gamma rays from pair annihilations in the interstellar medium. As the contribution of final state radiation and the annihilation of positrons enhances the low-energy part of the produced gamma-ray spectra from PBHs, we find that the EGRB observations can set the tightest limits on their abundance among all indirect DARK MATTER probes, within the mass range of interest.[abridged]

[abstract 2 / 49] Wow! (score: 8)
arXiv:2606.10527 [pdf, ps, other]

Title: Circular POLARIZATION effects induced by photon-axion mixing in astrophysical environments

Authors: Meng Wang, Nan Ding, Qiusheng Gu, Yunyong Tang, Rui Xue,

Comments: 15 pages, 7 figures. Submitted, under review. Comments welcome

Subjects: astro-ph.HE

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

Axions and axion-like particles (ALPs) are compelling candidates for DARK MATTER and new physics beyond the Standard Model. Photon-axion mixing in external MAGNETic fields modifies the photon energy spectrum and linear POLARIZATION state, and also induces circular POLARIZATION signals. Compared to spectral and linear POLARIZATION methods, circular POLARIZATION benefits from lower astrophysical background contamination, providing an independent probe for axion searches. In this work, we study the circular POLARIZATION induced by photon-axion mixing within the chiral basis framework. By analytically solving the evolution equations under the single-domain approximation, we derive an expression for the circular POLARIZATION degree P_C, applicable in the resonant, strong coupling, and weak coupling regimes. Within single-domain MAGNETic field models, we compare the energy-dependent circular POLARIZATION in four astrophysical environments (AGN JETs, intracluster medium, intergalactic medium, and Galactic MAGNETic fields). We find that the X-ray to MeV band represents the most sensitive observational window. Using the BLAZAR S4 0954+65 as a case study, phase accumulation in random MAGNETic domains causes the circular POLARIZATION degree to fluctuate with redshift and exhibit pronounced energy structures. Using the optical circular POLARIZATION upper limit P_C < 0.184% from this source, we constrain g_{aγγ} <= 5 x 10^{-12} GeV^{-1} for m_a ~ 10^{-16}--10^{-10} eV, with the strongest constraint near m_a ~ 10^{-14} eV. These results establish circular POLARIZATION as a complementary axion probe.

[abstract 3 / 49] Wow! (score: 8)
arXiv:2606.10828 [pdf, ps, other]

Title: A Multiwavelength Interpretation of HESS J1857+026 Emission Using the FERMI-LAT, VERITAS, and HAWC Observatories

Authors: Jordan Eagle, Yu Chen, Ramiro Torres-Escobedo, Youyou Li, Ruo-Yu Shang,

Comments: 24 pages. Accepted for publication in ApJ

Subjects: astro-ph.HE

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

We present a new study on the MeV-TeV gamma-ray origin of HESS J1857+026 using data collected from the FERMI-LAT, VERITAS, and HAWC observatories. A spatial and spectral study of HESS J1857+026 including radiative modeling of the MeV-TeV spectrum determines the likely dominant gamma-ray origin as a pulsar wind nebula (PWN) powered by the energetic pulsar PSR J1856+0245. The MeV-TeV spectrum is further characterized through basic evolutionary radiative modeling assuming a PWN origin to constrain the physical properties of the system such as the MAGNETic field strength and PWN age. The results of the PWN evolutionary model are consistent with the observational constraints of the system, finding an age of the system between t = [16,21]kyr and a MAGNETic field strength between B = [0.4,1.6]muG. These estimates support an evolved PWN scenario where the observed gamma-ray emission is generated by the RELATIVISTIC electrons inverse Compton scattering (ICS) off local photon fields, however the low-energy (E < 10GeV) spectral component could be dominated by hadronic emission originating from a SUPERNOVA remnant (SNR). For a PWN component above 10GeV, we measure the conditions for particle diffusion, finding that the local diffusion (D(50TeV) ~ $10^{28}cm^{-2}s^{-1}$) is suppressed compared to the interstellar medium (ISM) value, in agreement with similar TeV PWNe. By measuring the radial surface brightness profiles of the gamma-ray source across multiple instruments, we demonstrate that the combined MeV-TeV spatial information is a powerful tool to constrain particle diffusion properties.

[abstract 4 / 49] Wow! (score: 7)
arXiv:2606.10447 [pdf, ps, other]

Title: Narrow-Line Seyfert 1 Galaxies in the Dark Energy Spectroscopic Instrument Data Release 1

Authors: Vaidehi S. Paliya, Suvendu Rakshit, Alberto Dominguez, D. J. Saikia, C. S. Stalin,

Comments: ApJS, in press

Subjects: astro-ph.GA astro-ph.CO astro-ph.HE

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

Narrow-line Seyfert 1 (NLSy1) galaxies are peculiar ACTIVE GALACTIC NUCLEi (AGN) known to exhibit a variety of intriguing observational features from low-frequency radio waves to high-energy $γ$~rays. As of now, NLSy1 catalogs are primarily based on optical spectroscopic observations from the Sloan Digital Sky Survey (SDSS). Here we report, for the first time, a new catalog of NLSy1 galaxies using the high-quality optical spectroscopic observations made public in the first data release of the Dark Energy Spectroscopic Instrument (DESI). We performed a detailed spectral decomposition of more than 71,000 optical spectra of AGN not included in the SDSS catalog and located at $z<0.9$. From this sample, we identify 18749 objects as NLSy1 galaxies for the first time. We also supplement the NLSy1 catalog with a sample of broad-line Seyfert 1 galaxies. The NLSy1 galaxies identified in the DESI data tend to have slightly higher bolometric luminosities and lower BLACK HOLE masses (though with large dispersions), leading to the higher Eddington ratios than those of the SDSS-NLSy1 sample matched in redshifts and absolute $B$-band magnitudes. Moreover, the fraction of DESI-NLSy1 galaxies detected in the radio, X-ray, and $γ$-ray catalogs was found to be lower than that of SDSS-NLSy1 sources. We conclude that deeper multiwavelength investigations of these enigmatic AGN will help unravel the low-luminosity end of the NLSy1 population. The catalog has been made available at https://www.ucm.es/BLAZARs/SEYFERT and Zenodo https://doi.org/10.5281/zenodo.20484681.

[abstract 5 / 49] Yes (score: 6)
arXiv:2606.09981 [pdf, ps, other]

Title: The Curious Case of PHL 1811: Heavy Obscuration Versus Intrinsic X-ray Weakness

Authors: B. Luo, Xiaolei Chen, Jian Huang, W. N. Brandt, Qingling Ni,

Comments: 12 pages, 4 figures, accepted for publication in ApJ

Subjects: astro-ph.HE astro-ph.CO astro-ph.GA

Created: 2026-06-08; Updated: 2026-06-10; Datestamp: 2026-06-10

We present a systematic X-ray analysis of the narrow-line Type 1 QUASAR PHL 1811, which has long been regarded as the prototype of intrinsically X-ray weak QUASARs. A critical breakthrough came with the first detection of a bright X-ray flare from this source by the Einstein Probe (EP) in 2024. We utilize archival X-ray observations spanning 2001-2024, including the post-flare EP and SWIFT data. We confirm that PHL 1811 shows X-ray weakness factors $f_{\rm weak} \approx 23$-179 across all epochs before 2024. The 2024 EP flare marks the first detection of an X-ray nominal state with $f_{\rm weak} \approx 0.63$, followed by a rapid flux decline. We identify three key observational signatures that strongly support heavy obscuration: (1) a significant hard X-ray excess above $\approx5$ keV in the 2015 XMM-Newton spectrum; (2) relatively flat spectral shapes in two SWIFT observations; and (3) transitions between X-ray nominal and multiple X-ray weak states without corresponding optical/infrared variability, consistent with expectations from obscuration by a clumpy dust-free absorber. Fitting with a partial-covering obscuration model reproduces all multi-epoch spectra well. The observed steep spectra are dominated by a small leaked/scattered fraction of the intrinsic continuum, and variability is driven by changes in the leakage fraction and column density. Our results strongly favor the scenario where PHL 1811 is obscured by a radiatively driven accretion-disk wind from super-Eddington accretion, unifying PHL 1811 with the broader population of super-Eddington accreting AGNs under a single obscuration framework.

[abstract 6 / 49] Yes (score: 6)
arXiv:2606.10455 [pdf, ps, other]

Title: The Extreme Quasar Main Sequence of Super-Eddington DESI-DR1 NLSy1 Galaxies

Authors: Alberto Domínguez, Suvendu Rakshit, Vaidehi S. Paliya, D. J. Saikia, C. S. Stalin,

Comments: 4 pages, 1 figure; Submitted to A&A Letters

Subjects: astro-ph.GA astro-ph.HE

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

The QUASAR main sequence, or Eigenvector 1 (EV1), describes the optical diversity of ACTIVE GALACTIC NUCLEi (AGN), with Narrow-Line Seyfert 1 (NLSy1) galaxies anchoring the high-accretion end. Recent discoveries of overly massive BLACK HOLEs in the early Universe highlight the need to study local, low-mass super-Eddington accretors as analogs of rapid BLACK HOLE growth. We map a population of 18,749 NLSy1 galaxies identified in the Dark Energy Spectroscopic Instrument Data Release 1 (DESI DR1) onto the EV1 plane to determine whether they represent a distinct population of super-accretors. We compare the spectral properties of the DESI DR1 NLSy1 sample with the SDSS DR17 NLSy1 catalog. We extract key parameters, including the broad H-beta full width at half maximum (FWHM) and Fe II strength (R4570). To evaluate their accretion states, we derive single-epoch virial BLACK HOLE masses using an Fe II strength-dependent scaling relation and an Eddington rate-dependent fundamental plane. The DESI DR1 NLSy1 population shows a shift toward the extreme end of the EV1 parameter space, with stronger Fe II emission (median log R4570 = -0.03) than the SDSS sample (-0.31). Furthermore, the DESI sources host less massive BLACK HOLEs (median log BLACK HOLE mass ~6.73) than the SDSS objects (6.77-6.91). Given comparable continuum luminosities, a larger fraction of the DESI sample (43.8%-47.7%) exceeds the Eddington limit (log Eddington ratio > 0) than the SDSS sample (20.6%-37.4%). The sensitivity of DESI has unveiled a large population of low-mass, super-Eddington accreting AGN largely missing from previous surveys. These extreme EV1 objects naturally produce the observed intense Fe II emission. This unique sample provides a statistical dataset of local super-Eddington accretors for understanding early-Universe BLACK HOLE growth.

[abstract 7 / 49] Yes (score: 6)
arXiv:2606.10519 [pdf, ps, other]

Title: Gamma-Ray Emission from the Crab Pulsar: A 17-Year FERMI-LAT Reanalysis

Authors: Liancheng Zhou, Yun-Lu Gong, Jun Fang, Li Zhang,

Comments: 11 pages, 6 figures, Accepted for publication in Research in Astronomy and Astrophysics

Subjects: astro-ph.HE

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

We present a reanalysis of 17 years of FERMI Large Area Telescope (LAT) observations of the Crab pulsar obtained between 2008 August and 2025 August. Using monthly Jodrell Bank radio ephemerides, we assigned pulse phases to the LAT events and aligned the phase zero across the full data set. From this phase-aligned data set, we derived pulse profiles over 100 MeV to 300 GeV. The pulsed emission remains clearly detectable in the 10 to 20 GeV and 20 to 30 GeV bands, with H-test significances of 32.36 sigma and 11.59 sigma, respectively, but is not significantly detected in the 30 to 300 GeV band. Phase-resolved likelihood analysis was performed over 100 MeV to 30 GeV using 14 phase bins with comparable pulsed statistics. The fixed-window fractional fluxes show that the contribution of Peak 1 (P1) decreases steadily with energy, while those of Peak 2 (P2) and the Bridge increase, with P2 exceeding P1 above 10 GeV. Finally, the same phase-assignment framework also enables an off-pulse analysis from 100 MeV to 1 TeV, confirming the SYNCHROTRON and inverse-Compton components that dominate the emission in the selected off-pulse interval.

[abstract 8 / 49] Yes (score: 5)
arXiv:2606.09992 [pdf, ps, other]

Title: EP260321a/SN 2026gzf: The Faintest Shock Breakout Associated with a Broad-Lined Supernova

Authors: Brendan O'Connor, Xander J. Hall, Malte Busmann, Daniel Gruen, Alberto Floris, Tomas Cabrera, Ziyuan Zhu, Antonella Palmese, Dylan Green, John Banovetz, Julius Gassert, Christopher L. Fryer, Roberto Ricci, Eleonora Troja, Surya Shivaprasad, Gregory R. Zeimann, Ariel J. Amsellem, Stephen Bailey, Segev BenZvi, Simone Dichiara, Hendrik van Eerten, Jeremy Hare, Lei Hu, Christopher M. Irwin, Keerthi Kunnumkai, Konstantin Malanchev, Mitra Maleki, Michael J. Moss, Adam D. Myers, Dheeraj Pasham, Christoph Ries, Geoffrey Ryan, David Schlegel, Michael Schmidt, Silona Wilke, Yu-Han Yang,

Comments: Submitted to ApJL

Subjects: astro-ph.HE

Created: 2026-06-08; Updated: 2026-06-10; Datestamp: 2026-06-10

The explosion of a star is first marked by the shock wave breaking out of the stellar surface, producing a burst of ultraviolet and X-ray radiation. These events are observationally rare, despite likely accompanying the majority of SUPERNOVAe. Here, we report on our multi-wavelength observing campaign of the closest Einstein Probe fast X-ray transient EP260321a at $z=0.0344$. The thermal ($kT=160$ eV) X-ray emission with peak luminosity $2.2\times10^{44}$ erg s$^{-1}$ points to a shock breakout origin. We demonstrate that EP260321a is accompanied by a broad-lined Type Ic SUPERNOVA, SN 2026gzf. The SUPERNOVA properties, including its spectral evolution, lightcurve evolution, and expansion velocities, are all typical of the energetic stripped-envelope SUPERNOVAe associated with GAMMA-RAY BURSTs. However, deep X-ray upper limits obtained with the \textit{Chandra X-ray Observatory} do not detect an X-ray afterglow, and instead exclude the afterglow of known GAMMA-RAY BURSTs or fast X-ray transients. If the stellar explosion launched a successful RELATIVISTIC JET, we require that it had both a low Lorentz factor $Γ_0$\,$<$\,$30$ and a kinetic energy $E_\textrm{kin}$\,$<$\,$10^{49}$ erg for a stellar wind density of $A_*$\,$\gtrsim$\,$1$. We propose that EP260321a originated from a mildly RELATIVISTIC, weak outflow that was choked by the progenitor star. This scenario is capable of naturally explaining its low X-ray luminosity and lack of prompt gamma-ray emission. EP260321a bridges the gap between SN 2008D and low-luminosity GRBs, suggesting a greater diversity in the physical parameters of stripped stars as they undergo terminal collapse.

[abstract 9 / 49] Yes (score: 5)
arXiv:2606.10840 [pdf, ps, other]

Title: FERMI-LAT Gamma-ray Emission Discovered from the Composite Supernova Remnant B0453-685 in the Large Magellanic Cloud

Authors: Jordan Eagle,

Comments: Published in Proceedings of Science Multifrequency Behaviour of High Energy Cosmic Sources XIV 2023: https://pos.sissa.it/447/

Subjects: astro-ph.HE

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

A second extragalactic pulsar wind nebula (PWN) is discovered in the MeV-GeV band using the FERMI-LAT. Faint, point-like gamma-ray emission is detected at the location of the composite SUPERNOVA remnant (SNR) B0453-685 from energies 300MeV-2TeV. The FERMI-LAT data analysis of the new gamma-ray source is presented together with a detailed multi-wavelength investigation to understand the nature of the observed emission. The observational evidence and physical implications from broadband modeling do not support an SNR gamma-ray origin. Semi-analytic radiative evolutionary models are explored to understand the potential for any pulsar or PWN component responsible for the observed gamma-ray emission. The modeling results favor an evolved PWN ($τ\sim 14,000$ years) that has been impacted by the return of the SNR reverse shock with a possible substantial pulsar component below $5$GeV. The particle acceleration mechanisms and their efficiency within B0453-685 have important implications for the role PWNe play in generating Cosmic Rays (CRs), but constraints on the SYNCHROTRON cut-off are required to accurately characterize the underlying particle properties.

[abstract 10 / 49] Yes (score: 5)
arXiv:2606.10855 [pdf, ps, other]

Title: Pulsar Wind Nebulae (PWNe) -- A Review

Authors: Jordan Eagle,

Comments: To be published in the Multifrequency Behaviour of High Energy Cosmic Sources - XV Proceedings of Science 2025 issue: https://pos.sissa.it/506/

Subjects: astro-ph.HE

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

Pulsar Wind Nebulae (PWNe) are RELATIVISTIC, MAGNETic winds comprised of radiating electrons and positrons, powered by an energetic pulsar. The pulsar continuously injects particles into the PWN that are accelerated at the termination shock. As the RELATIVISTIC particles enter the PWN, they radiate away the energy received at the shock as they interact with the PWN environment, generating SYNCHROTRON emission from interactions with the MAGNETic field of the PWN and Inverse Compton Scattering (ICS) from interactions with the local photon fields. Synchrotron emission is observed from the majority of known PWNe from radio to X-ray energies, and the ICS is observed in the $γ$-ray bands, from MeV to TeV energies. The particle acceleration processes at the termination shock and elsewhere within the PWN remain to be understood. Recent progress in theoretical studies have provided the capability to explain broadband observations of several PWNe including their spectral and spatial features. This work reviews some of the most compelling outcomes of recent literature, outlining the outstanding questions that remain to be answered, and how the future prospects of $γ$-ray astronomy will be instrumental in advancing the current understanding of PWNe.

[abstract 11 / 49] Yes (score: 5)
arXiv:2606.10926 [pdf, ps, other]

Title: Time lags as proxy of spectral evolution in GAMMA-RAY BURSTs

Authors: C. Maraventano, F. Daigne, R. Mochkovitch, L. Nava, G. Ghirlanda, T. Di Salvo,

Comments: 13 pages, 6 figures, 4 tables, Accepted for publication in Astronomy & Astrophysics (A&A)

Subjects: astro-ph.HE

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

Positive lags in GAMMA-RAY BURSTs (GRBs), where hard photons anticipate softer ones, provide a unique window into the temporal evolution of their prompt emission. Negative lags, when hard photons are delayed, are instead more enigmatic to interpret. Disentangling the effects that produce both kinds of lags is critical for identifying the physical mechanisms at work in the prompt and early afterglow phases of GRBs. We investigate the potential of time lags for distinguishing different emission components at different energy bands. Using data from the FERMI Gamma-ray Burst Monitor (GBM) and the LAT Low Energy(LLE) technique, we perform a time-resolved joint spectral analysis in the range 10 keV-100 MeV for two exceptionally bright bursts, GRB 160625B and GRB 190114C. Time lags between the lowest-energy band (10-100 keV) and progressively higher-energy bands up to 30-100 MeV were computed across their distinct emission episodes via the cross-correlation function. For GRB 160625B, the spectra are described by a single component with clear hard-to-soft evolution, and the time lags are always positive. Analysis of the high-energy exponential cutoff, likely originating above the photosphere, yields bulk Lorentz factor estimates of $Γ\sim 120-250$. GRB 190114C exhibits negative lags in the 30-100 MeV band, coinciding with a delayed high-energy powerlaw component that dominates the LLE range after ~2.5 s. Comparison with multi-wavelength observations shows some compatibility with the early afterglow, though its origin remains open, leaving room for external shocks or internal dissipation. Time lags are effective diagnostic tools for the spectral evolution of GRBs: positive lags trace the softening of the prompt emission, whereas negative lags indicate the appearance of a new, independent high-energy spectral component.

[abstract 12 / 49] Yes (score: 5)
arXiv:2606.10964 [pdf, ps, other]

Title: The link between obscured accretion and mildly RELATIVISTIC precessing JETs

Authors: Rob Fender, Sara Motta,

Comments: Accepted for publication in MNRAS. Link to published version of Fender & Motta (Nature Astronomy, 2025) on which this builds, is here: https://www.nature.com/articles/s41550-025-02665-w

Subjects: astro-ph.HE

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

We have recently shown evidence that the most RELATIVISTIC JETs (with Lorentz factor >2) from stellar-mass BLACK HOLEs in X-ray binary systems may be locked to a fixed axis, likely the spin axis of the BLACK HOLE. Slower, mildly RELATIVISTIC JETs (with velocities typically ~ 0.3c) are often seen to precess and can be associated with both neutron stars and BLACK HOLEs. In this paper we demonstrate an additional clear link between highly obscured systems and these lower-velocity, precessing JETs. We speculate that this link may be due to mass-loading of the JETs close to their launch sites, since these obscured systems are likely to be examples of (sometimes persistent, other times transient) super-Eddington accretion. The fastest RELATIVISTIC JETs are now seen to be both locked to a fixed direction, likely the BLACK HOLE spin axis, and to be launched in low-density environments, while JETs launched in dense environments are generally slower and very likely to precess.

[abstract 13 / 49] Yes (score: 4)
arXiv:2509.07352 [pdf, ps, other]

Title: Directed searches for gravitational waves from ultralight vector BOSON clouds around merger remnant and galactic BLACK HOLEs during the first part of the fourth LIGO-Virgo-KAGRA observing run

Authors: The LIGO Scientific Collaboration, the Virgo Collaboration, the KAGRA Collaboration, A. G. Abac, I. Abouelfettouh, F. Acernese, K. Ackley, C. Adamcewicz, S. Adhicary, D. Adhikari, N. Adhikari, R. X. Adhikari, V. K. Adkins, S. Afroz, A. Agapito, D. Agarwal, M. Agathos, N. Aggarwal, S. Aggarwal, O. D. Aguiar, I. -L. Ahrend, L. Aiello, A. Ain, P. Ajith, T. Akutsu, S. Albanesi, W. Ali, S. Al-Kershi, C. Alléné, A. Allocca, S. Al-Shammari, P. A. Altin, S. Alvarez-Lopez, W. Amar, O. Amarasinghe, A. Amato, F. Amicucci, C. Amra, A. Ananyeva, S. B. Anderson, W. G. Anderson, M. Andia, M. Ando, M. Andrés-Carcasona, T. Andrić, J. Anglin, S. Ansoldi, J. M. Antelis, S. Antier, M. Aoumi, E. Z. Appavuravther, S. Appert, S. K. Apple, K. Arai, A. Araya, M. C. Araya, M. Arca Sedda, J. S. Areeda, N. Aritomi, F. Armato, S. Armstrong, N. Arnaud, M. Arogeti, S. M. Aronson, K. G. Arun, G. Ashton, Y. Aso, L. Asprea, M. Assiduo, S. Assis de Souza Melo, S. M. Aston, P. Astone, F. Attadio, F. Aubin, K. AultONeal, G. Avallone, E. A. Avila, S. Babak, C. Badger, S. Bae, S. Bagnasco, L. Baiotti, R. Bajpai, T. Baka, A. M. Baker, K. A. Baker, T. Baker, G. Baldi, N. Baldicchi, M. Ball, G. Ballardin, S. W. Ballmer, S. Banagiri, B. Banerjee, D. Bankar, T. M. Baptiste, P. Baral, M. Baratti, J. C. Barayoga, B. C. Barish, D. Barker, N. Barman, P. Barneo, F. Barone, B. Barr, L. Barsotti, M. Barsuglia, D. Barta, A. M. Bartoletti, M. A. Barton, I. Bartos, A. Basalaev, R. Bassiri, A. Basti, M. Bawaj, P. Baxi, J. C. Bayley, A. C. Baylor, P. A. Baynard, M. Bazzan, V. M. Bedakihale, F. Beirnaert, M. Bejger, D. Belardinelli, A. S. Bell, D. S. Bellie, L. Bellizzi, W. Benoit, I. Bentara, J. D. Bentley, M. Ben Yaala, S. Bera, F. Bergamin, B. K. Berger, S. Bernuzzi, M. Beroiz, D. Bersanetti, T. Bertheas, A. Bertolini, J. Betzwieser, D. Beveridge, G. Bevilacqua, N. Bevins, R. Bhandare, R. Bhatt, D. Bhattacharjee, S. Bhattacharyya, S. Bhaumik, V. Biancalana, A. Bianchi, I. A. Bilenko, G. Billingsley, A. Binetti, S. Bini, C. Binu, S. Biot, O. Birnholtz, S. Biscoveanu, A. Bisht, M. Bitossi, M. -A. Bizouard, S. Blaber, J. K. Blackburn, L. A. Blagg, C. D. Blair, D. G. Blair, N. Bode, N. Boettner, G. Boileau, M. Boldrini, G. N. Bolingbroke, A. Bolliand, L. D. Bonavena, R. Bondarescu, F. Bondu, E. Bonilla, M. S. Bonilla, A. Bonino, R. Bonnand, A. Borchers, S. Borhanian, V. Boschi, S. Bose, V. Bossilkov, Y. Bothra, A. Boudon, L. Bourg, M. Boyle, A. Bozzi, C. Bradaschia, P. R. Brady, A. Branch, M. Branchesi, I. Braun, T. Briant, A. Brillet, M. Brinkmann, P. Brockill, E. Brockmueller, A. F. Brooks, B. C. Brown, D. D. Brown, M. L. Brozzetti, S. Brunett, G. Bruno, R. Bruntz, J. Bryant, Y. Bu, F. Bucci, J. Buchanan, O. Bulashenko, T. Bulik, H. J. Bulten, A. Buonanno, K. Burtnyk, R. Buscicchio, D. Buskulic, C. Buy, R. L. Byer, G. S. Cabourn Davies, R. Cabrita, V. Cáceres-Barbosa, L. Cadonati, G. Cagnoli, C. Cahillane, A. Calafat, T. A. Callister, E. Calloni, S. R. Callos, M. Canepa, G. 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Pirello, M. D. Pitkin, A. Placidi, E. Placidi, M. L. Planas, W. Plastino, C. Plunkett, R. Poggiani, E. Polini, J. Pomper, L. Pompili, J. Poon, E. Porcelli, E. K. Porter, C. Posnansky, R. Poulton, J. Powell, G. S. Prabhu, M. Pracchia, B. K. Pradhan, T. Pradier, A. K. Prajapati, K. Prasai, R. Prasanna, P. Prasia, G. Pratten, G. Principe, G. A. Prodi, P. Prosperi, P. Prosposito, A. C. Providence, A. Puecher, J. Pullin, P. Puppo, M. Pürrer, H. Qi, J. Qin, G. Quéméner, V. Quetschke, P. J. Quinonez, N. Qutob, R. Rading, I. Rainho, S. Raja, C. Rajan, B. Rajbhandari, K. E. Ramirez, F. A. Ramis Vidal, M. Ramos Arevalo, A. Ramos-Buades, S. Ranjan, K. Ransom, P. Rapagnani, B. Ratto, A. Ravichandran, A. Ray, V. Raymond, M. Razzano, J. Read, T. Regimbau, S. Reid, C. Reissel, D. H. Reitze, A. I. Renzini, B. Revenu, A. Revilla Peña, R. Reyes, L. Ricca, F. Ricci, M. Ricci, A. Ricciardone, J. Rice, J. W. Richardson, M. L. Richardson, A. Rijal, K. Riles, H. K. Riley, S. Rinaldi, J. Rittmeyer, C. Robertson, F. Robinet, M. Robinson, A. Rocchi, L. Rolland, J. G. Rollins, A. E. Romano, R. Romano, A. Romero, I. M. Romero-Shaw, J. H. Romie, S. Ronchini, T. J. Roocke, L. Rosa, T. J. Rosauer, C. A. Rose, D. Rosińska, M. P. Ross, M. Rossello-Sastre, S. Rowan, S. K. Roy, S. Roy, D. Rozza, P. Ruggi, N. Ruhama, E. Ruiz Morales, K. Ruiz-Rocha, S. Sachdev, T. Sadecki, P. Saffarieh, S. Safi-Harb, M. R. Sah, S. Saha, T. Sainrat, S. Sajith Menon, K. Sakai, Y. Sakai, M. Sakellariadou, S. Sakon, O. S. Salafia, F. Salces-Carcoba, L. Salconi, M. Saleem, F. Salemi, M. Sallé, S. U. Salunkhe, S. Salvador, A. Salvarese, A. Samajdar, A. Sanchez, E. J. Sanchez, L. E. Sanchez, N. Sanchis-Gual, J. R. Sanders, E. M. Sänger, F. Santoliquido, F. Sarandrea, T. R. Saravanan, N. Sarin, P. Sarkar, A. Sasli, P. Sassi, B. Sassolas, R. Sato, S. Sato, Yukino Sato, Yu Sato, O. Sauter, R. L. Savage, T. Sawada, H. L. Sawant, S. Sayah, V. Scacco, D. Schaetzl, M. Scheel, A. Schiebelbein, M. G. Schiworski, P. Schmidt, S. Schmidt, R. Schnabel, M. Schneewind, R. M. S. Schofield, K. Schouteden, B. W. Schulte, B. F. Schutz, E. Schwartz, M. Scialpi, J. Scott, S. M. Scott, R. M. Sedas, T. C. Seetharamu, M. Seglar-Arroyo, Y. Sekiguchi, D. Sellers, N. Sembo, A. S. Sengupta, E. G. Seo, J. W. Seo, V. Sequino, M. Serra, A. Sevrin, T. Shaffer, U. S. Shah, M. A. Shaikh, L. Shao, A. K. Sharma, Preeti Sharma, Prianka Sharma, Ritwik Sharma, S. Sharma Chaudhary, P. Shawhan, N. S. Shcheblanov, E. Sheridan, Z. -H. Shi, M. Shikauchi, R. Shimomura, H. Shinkai, S. Shirke, D. H. Shoemaker, D. M. Shoemaker, R. W. Short, S. ShyamSundar, A. Sider, H. Siegel, N. Siemonsen, D. Sigg, L. Silenzi, L. Silvestri, M. Simmonds, L. P. Singer, Amitesh Singh, Anika Singh, D. Singh, N. Singh, S. Singh, A. M. Sintes, V. Sipala, V. Skliris, B. J. J. Slagmolen, D. A. Slater, T. J. Slaven-Blair, J. Smetana, J. R. Smith, L. Smith, R. J. E. Smith, W. J. Smith, S. Soares de Albuquerque Filho, M. Soares-Santos, K. Somiya, I. Song, S. Soni, V. Sordini, F. Sorrentino, H. Sotani, F. Spada, V. Spagnuolo, A. P. Spencer, P. Spinicelli, A. K. Srivastava, F. Stachurski, C. J. Stark, D. A. Steer, N. Steinle, J. Steinlechner, S. Steinlechner, N. Stergioulas, P. Stevens, M. StPierre, M. D. Strong, A. Strunk, A. L. Stuver, M. Suchenek, S. Sudhagar, Y. Sudo, N. Sueltmann, L. Suleiman, K. D. Sullivan, J. Sun, L. Sun, S. Sunil, J. Suresh, B. J. Sutton, P. J. Sutton, K. Suzuki, M. Suzuki, B. L. Swinkels, A. Syx, M. J. Szczepańczyk, P. Szewczyk, M. Tacca, H. Tagoshi, K. Takada, H. Takahashi, R. Takahashi, A. Takamori, S. Takano, H. Takeda, K. Takeshita, I. Takimoto Schmiegelow, M. Takou-Ayaoh, C. Talbot, M. Tamaki, N. Tamanini, D. Tanabe, K. Tanaka, S. J. Tanaka, S. Tanioka, D. B. Tanner, W. Tanner, L. Tao, R. D. Tapia, E. N. Tapia San Martín, C. Taranto, A. Taruya, J. D. Tasson, J. G. Tau, D. Tellez, R. Tenorio, H. Themann, A. Theodoropoulos, M. P. Thirugnanasambandam, L. M. Thomas, M. Thomas, P. Thomas, J. E. Thompson, S. R. Thondapu, K. A. Thorne, E. Thrane, J. Tissino, A. Tiwari, Pawan Tiwari, Praveer Tiwari, S. Tiwari, V. Tiwari, M. R. Todd, M. Toffano, A. M. Toivonen, K. Toland, A. E. Tolley, T. Tomaru, V. Tommasini, T. Tomura, H. Tong, C. Tong-Yu, A. Torres-Forné, C. I. Torrie, I. Tosta e Melo, E. Tournefier, M. Trad Nery, K. Tran, A. Trapananti, R. Travaglini, F. Travasso, G. Traylor, M. Trevor, M. C. Tringali, A. Tripathee, G. Troian, A. Trovato, L. Trozzo, R. J. Trudeau, T. Tsang, S. Tsuchida, L. Tsukada, K. Turbang, M. Turconi, C. Turski, H. Ubach, N. Uchikata, T. Uchiyama, R. P. Udall, T. Uehara, K. Ueno, V. Undheim, L. E. Uronen, T. Ushiba, M. Vacatello, H. Vahlbruch, N. Vaidya, G. Vajente, A. Vajpeyi, J. Valencia, M. Valentini, S. A. Vallejo-Peña, S. Vallero, V. Valsan, M. van Dael, E. Van den Bossche, J. F. J. van den Brand, C. Van Den Broeck, M. van der Sluys, A. Van de Walle, J. van Dongen, K. Vandra, M. VanDyke, H. van Haevermaet, J. V. van Heijningen, P. Van Hove, J. Vanier, M. VanKeuren, J. Vanosky, N. van Remortel, M. Vardaro, A. F. Vargas, V. Varma, A. N. Vazquez, A. Vecchio, G. Vedovato, J. Veitch, P. J. Veitch, S. Venikoudis, R. C. Venterea, P. Verdier, M. Vereecken, D. Verkindt, B. Verma, Y. Verma, S. M. Vermeulen, F. Vetrano, A. Veutro, A. Viceré, S. Vidyant, A. D. Viets, A. Vijaykumar, A. Vilkha, N. Villanueva Espinosa, V. Villa-Ortega, E. T. Vincent, J. -Y. Vinet, S. Viret, S. Vitale, H. Vocca, D. Voigt, E. R. G. von Reis, J. S. A. von Wrangel, W. E. Vossius, L. Vujeva, S. P. Vyatchanin, J. Wack, L. E. Wade, M. Wade, K. J. Wagner, L. Wallace, E. J. Wang, H. Wang, J. Z. Wang, W. H. Wang, Y. F. Wang, G. Waratkar, J. Warner, M. Was, T. Washimi, N. Y. Washington, D. Watarai, B. Weaver, S. A. Webster, N. L. Weickhardt, M. Weinert, A. J. Weinstein, R. Weiss, L. Wen, K. Wette, J. T. Whelan, B. F. Whiting, C. Whittle, E. G. Wickens, D. Wilken, A. T. Wilkin, B. M. Williams, D. Williams, M. J. Williams, N. S. Williams, J. L. Willis, B. Willke, M. Wils, L. Wilson, C. W. Winborn, J. Winterflood, C. C. Wipf, G. Woan, J. Woehler, N. E. Wolfe, H. T. Wong, I. C. F. Wong, K. Wong, T. Wouters, J. L. Wright, M. Wright, B. Wu, C. Wu, D. S. Wu, H. Wu, K. Wu, Q. Wu, Y. Wu, Z. Wu, E. Wuchner, D. M. Wysocki, V. A. Xu, Y. Xu, N. Yadav, H. Yamamoto, K. Yamamoto, T. S. Yamamoto, T. Yamamoto, R. Yamazaki, T. Yan, K. Z. Yang, Y. Yang, Z. Yarbrough, J. Yebana, S. -W. Yeh, A. B. Yelikar, X. Yin, J. Yokoyama, T. Yokozawa, S. Yuan, H. Yuzurihara, M. Zanolin, M. Zeeshan, T. Zelenova, J. -P. Zendri, M. Zeoli, M. Zerrad, M. Zevin, L. Zhang, N. Zhang, R. Zhang, T. Zhang, C. Zhao, Yue Zhao, Yuhang Zhao, Z. -C. Zhao, Y. Zheng, H. Zhong, H. Zhou, H. O. Zhu, Z. -H. Zhu, A. B. Zimmerman, L. Zimmermann, M. E. Zucker, J. Zweizig,

Comments: 34 pages, 4 figures

Subjects: gr-qc astro-ph.HE hep-ph

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

We present the first directed searches for long-transient and continuous gravitational waves from ultralight vector BOSON clouds around known BLACK HOLEs (BHs). We use LIGO data from the first part of the fourth LIGO-Virgo-KAGRA observing run. The searches target two distinct types of BHs and use two new semicoherent methods: hidden Markov model (HMM) tracking for the remnant BHs of the mergers GW230814_230901 and GW231123_135430 (referred to as GW230814 and GW231123 in this study), and a dedicated method using the Band Sampled Data (BSD) framework for the galactic BH in the Cygnus X-1 binary system. Without finding evidence of a signal from vector BOSONs in the data, we estimate the mass range that can be constrained. For the HMM searches targeting the remnants from GW231123 and GW230814, we disfavor vector BOSON masses in the ranges $[0.94, 1.08]$ and $[2.75, 3.28] \times 10^{-13}$ eV, respectively, at 30% confidence, assuming a 1% false alarm probability. Although these searches are only marginally sensitive to signals from merger remnants at relatively large distances, future observations are expected to yield more stringent constraints with high confidence. For the BSD search targeting the BH in Cygnus X-1, we exclude vector BOSON masses in the range $[0.85, 1.59] \times 10^{-13}$ eV at 95% confidence, assuming an initial BH spin larger than 0.5.

[abstract 14 / 49] Yes (score: 4)
arXiv:2602.21291 [pdf, ps, other]

Title: Collapse of Magnetized White Dwarfs as site of Heavy Element Formation and Kilonova Signal

Authors: Tetyana Pitik, David Radice, Daniel Kasen, Fabio Magistrelli, Patrick Chi-Kit Cheong, Sebastiano Bernuzzi,

Comments: 14 pages, 13 figures. Published on MNRAS; added 2 figures and one appendix, conclusions unchanged

Subjects: astro-ph.HE nucl-th

Created: 2026-06-08; Updated: 2026-06-10; Datestamp: 2026-06-10

We present the first end-to-end calculation connecting the accretion-induced collapse (AIC) of a MAGNETized, rapidly rotating white dwarf to observable kilonova signatures, combining 2D general-RELATIVISTIC neutrino-MAGNETohydrodynamic simulations, followed by radiation hydrodynamics with in-situ nuclear network and 2D Monte Carlo radiative transfer with spatially resolved heating rates. Unlike all previous unMAGNETized AIC models - which predicted proton-rich, $^{56}$Ni-dominated ejecta - strong MAGNETic fields eject ${\sim 0.2 M_\odot}$ of neutron-rich material $(\langle Y_e \rangle \sim 0.24)$ on dynamical timescales, before neutrino irradiation can raise the electron fraction, enabling strong $r$-process nucleosynthesis up to and beyond the third peak. The resulting kilonova is lanthanide-rich $(X_{\rm lan} \approx 8\%)$ and dominated by near-infrared emission. We compute synthetic light curves in the LSST and JWST bands and find striking agreement, without parameter tuning, between the observations of AT 2023vfi/GRB 230307A and our broadband light curves for polar viewing angles. These results establish MAGNETized AIC as a viable channel for heavy $r$-process element production and a compelling progenitor candidate for long-duration GAMMA-RAY BURSTs with kilonova signatures.

[abstract 15 / 49] Yes (score: 4)
arXiv:2606.10002 [pdf, ps, other]

Title: Failed JET breakout in the metal-poor broad-lined type Ic SUPERNOVA 2026gzf

Authors: Antonio Martin-Carrillo, Christina C. Thöne, James K. Leung, Gregory Corcoran, Antonio de Ugarte Postigo, Peter G. Jonker, Luca Izzo, Andrew J. Levan, Benjamin P. Gompertz, Stéphane Basa, Nikhil Sarin, Jonathan Quirola-Vásquez, Rob A. J. Eyles-Ferris, Riccardo Brivio, Alan M. Watson, Laura Cotter, Jennifer Alexandra Chacón, Andrea Rossi, Andrea Melandri, Piramon Kumnurdmanee, Nial R. Tanvir, Anshika Gupta, Franz E. Bauer, Jean-Grégoire Ducoin, Andrea Reguitti, Kuntal Misra, Dong Xu, Susanna D. Vergani, Wen-fai Fong, Kendall Ackley, Edilberto Aguilar-Ruiz, Dalya Akl, Miguel Ángel Aloy, Jie An, Camila Angulo-Valdez, Sarah Antier, Jean-Luc Atteia, Rosa L. Becerra, Rene P. Breton, Nathaniel R. Butler, Sergio Campana, Francesco Carotenuto, Jorge Casares Velázquez, Ashley A. Chrimes, Valerio D'Elia, Joyce N. D. van Dalen, Fabio De Colle, Massimiliano De Pasquale, Vik S. Dhillon, Damien Dornic, Martin J. Dyer, Matteo Ferro, Morgan Fraser, Andrew S. Fruchter, Francis Fortin, Duncan K. Galloway, Leonardo García-García, Stefan Geier, Ramandeep Gill, Noémie Globus, Roberto Gualandi, Marion Guelfand, Francesco Guidolin, Dieter H. Hartmann, Agnes P. C. van Hoof, Pall Jakobsson, Divyanshu Janghel, Tom L. Killestein, Sylvio Klose, Shiho Kobayashi, Rubina Kotak, Amit Kumar, Asuka Kuwata, Tanmoy Laskar, William H. Lee, Massimiliano Lincetto, Gianluca Lombardi, Diego López-Cámara, Joseph D. Lyman, Elisabetta Maiorano, Keiichi Maeda, Nikos Mandarakas, Francesco Magnani, Jirong Mao, Enrique Moreno Méndez, Ana María Nicuesa Guelbenzu, Kanthanakorn Noysena, Laura K. Nuttall, Paul T. O'Brien, David O'Neill, Paolo Ochner, Margarita Pereyra, Giovanna Pugliese, Gavin Ramsay, Lauren Rhodes, Andrea Saccardi, Ruben Salvaterra, Fredd Sánchez Álvarez, Benjamin Schneider, Steve Schulze, Rhaana L. C. Starling, Danny Steeghs, Kzrysztof Ulaczyk, Chiara Ventura, Tayyaba Zafar, Zi-Pei Zhu,

Comments: 53 pages, 17 figures. Submitted to journal

Subjects: astro-ph.HE

Created: 2026-06-08; Updated: 2026-06-10; Datestamp: 2026-06-10

A long-standing question in the death of massive stars is the role of RELATIVISTIC JETs. While many GAMMA-RAY BURSTs and some fast X-ray transients seem to be associated with broad-lined type Ic SUPERNOVAe, the opposite is not true. The lack of observable JET emission in those Ic-BL SNe can be explained by invoking off-axis JETs, choked JETs that inject all their energy into the stellar envelope, baryon-loaded JETs for which the prompt high-energy emission is strongly suppressed, or non-JETted SNe. The lack of exact explosion time in the majority of SNe presents an obstacle to distinguish between these scenarios. Here we report the properties of SN 2026gzf associated with the X-ray thermal Einstein Probe shock-breakout EP260321a at z=0.0343. The absence of compelling shocked cocoon and radio emission up to 54 days, combined with initial expansion velocities of ~30,000 km/s and a circumstellar shell of ~0.07 M$_\odot$, favour a scenario for SN 2026gzf in which a JET was choked in the circumstellar shell. Our high-spatial resolution images of the SN environment show that the progenitor was located between two highly star-forming regions with a metallicity lower than any previously known Ic-BL SN. As the first case of a Ic-BL SN associated with high-energy prompt emission without the signature of a JET, SN 2026gzf provides a unique perspective to understand the successful launch of RELATIVISTIC JETs during the deaths of massive stars.

[abstract 16 / 49] Yes (score: 4)
arXiv:2606.10506 [pdf, ps, other]

Title: Phase-drifting with emitting plasma temperature in the quasi-periodic pulsations of an X-class solar flare

Authors: Libo Fu, Valery M. Nakariakov, Ding Yuan, Suraj Sahu, Song Feng, Ehsan Tavabi,

Comments:

Subjects: astro-ph.SR astro-ph.HE

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

Recent multi-wavelength observations of solar flares have provided new constraints on the physical origin of quasi-periodic pulsations (QPPs). In an X-class flare, we detect a short-lived $\sim$5-minute QPP simultaneously in hard X-rays, extreme-ultraviolet (EUV), and soft X-ray emissions, exhibiting a clear phase-drifting behavior with emitting plasma temperature. Based on phase-resolved timing analysis, it is found that (i) the QPPs in all diagnostics share nearly identical oscillation periods, (ii) a systematic temperature-dependent phase drifting is present, with the phase delay relative to the hard X-ray emission increases systematically from the hottest to cooler EUV channels, and (iii) the QPP persists for only a few cycles during the impulsive phase. These properties imply that periodic MAGNETic RECONNECTion, possibly triggered by the leakage of 5-minute oscillations from the lower atmosphere, modulates the non-thermal electrons responsible for the leading Hard X-ray QPPs. Subsequently, plasma heating and cooling processes manifest sequentially across passbands with different temperature responses, resulting in the observed temperature-dependent phase drifting. These results provide novel observational evidence supporting the use of multi-temperature, multi-wavelength phase relationships to constrain the temporal evolution of flare energy release and the origins of QPPs.

[abstract 17 / 49] Yes (score: 4)
arXiv:2606.11084 [pdf, ps, other]

Title: High-Resolution ALMA Imaging for a Gravitationally-lensed Quasar at $z=6.5$: Constraining the AGN Contribution to Galactic-Scale Dust Heating

Authors: Minghao Yue, Xiaohui Fan, Anna-Christina Eilers, Jinyi Yang, Feige Wang, Jianwei Lyu, James W. Nightingale, Ann Zabludoff, Ran Wang,

Comments: Accepted by ApJL

Subjects: astro-ph.GA

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

We present high-resolution (beam size $0\farcs076\times0\farcs040$) Atacama Large Millimeter/submillimeter Array (ALMA) observations of the far-infrared $(λ_\text{rest}=162.7μ\rm{m})$ dust continuum of J0439+1634, a gravitationally lensed QUASAR at $z=6.52$. We perform pixelated lens modeling for the visibility data, finding that J0439+1634 is well-described by a singular isothermal ellipsoid plus an external shear lensing model. The best-fit lensing potential exhibits a naked-cusp configuration, confirming the finding in Fan et al. (2019). The reconstructed source plane continuum emission shows a compact bright core, with size $\lesssim200$ pc and peak brightness $\sim0.6 \text{ Jy arcsec}^{-2}$. The total continuum flux at 245 GHz is $3.36\pm0.02$ mJy. The flux magnification is {$4.63\pm0.03$}, indicating an average source-plane resolution of $0\farcs019$ (equivalent to 104 pc). The spatial resolution around the supermassive BLACK HOLE reaches $\sim36$ pc. %Using the new lensing model, we re-fit the Hubble Space Telescope image for J0439+1634, and find that the position of the optical QUASAR is consistent with the brightest pixel in the dust continuum map. Leveraging the exceptional source-plane resolution, we build a radiative transfer model to describe the observed dust emission profile. The best-fit model indicates that heated dust from the ACTIVE GALACTIC NUCLEus (AGN) dominates the sub-millimeter emission at $r\lesssim100$ pc and that star-heated dust dominates the outer region of the host galaxy. AGN heating contributes {$\sim13\%$} to the observed sub-mm flux. Therefore, previous far-infrared-based STAR FORMATION rate measurements for most high-redshift QUASARs are likely mildly overestimated.

[abstract 18 / 49] (score: 3)
arXiv:2505.18067 [pdf, ps, other]

Title: A Comprehensive Analytical Model of the Dynamic Z-Pinch

Authors: Alejandro Mesa Dame, Eric S. Lavine, David A. Hammer,

Comments: 10 pages, 14 figures

Subjects: physics.plasm-ph

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

We present an analytical 1D axisymmetric model describing the evolution of the dynamic z-pinch. This model is capable of predicting the trajectories of the imploding sheath's MAGNETic piston and preceding shock front, along with the velocity, pressure, density, and MAGNETic field profiles, for any time-dependent current, spatially varying initial density profile, and weak initial axial field. The implosion is divided into stages, with each stage described by a set of coupled ordinary differential equations derived from the ideal MHD equations. Comparisons with experimental data from the COBRA pulsed-power facility are quite promising and imply this model could prove useful in designing and analyzing future pulsed-power experiments.

[abstract 19 / 49] (score: 3)
arXiv:2604.03429 [pdf, ps, other]

Title: The VLBI spectrum of the persistent radio source associated with FRB 20190417A

Authors: G. Bruni, L. Piro, Y. -P. Yang, L. Nicastro, A. Rossi, E. Palazzi, E. Maiorano, S. Savaglio, B. Zhang,

Comments: Accepted for publication in A&A Letters

Subjects: astro-ph.HE astro-ph.SR

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

We aim to confirm the compact nature and constrain the radio spectra of candidate persistent radio sources (PRSs) associated with repeating fast radio bursts (FRBs). We performed European VLBI Network (EVN) observations at 5 and 8 GHz targeting two candidates identified in a recent VLA survey. We measured flux densities and upper limits at milliarcsecond resolution and combined them with published VLBI data at lower frequencies to derive spectral constraints. We detect a compact source associated with FRB 20190417A at 5 GHz with a flux density of $150\pm45$ uJy, while no detection is obtained at 8 GHz. The source is unresolved and has a brightness temperature $T_{\rm b}>10^{5}$ K, confirming its non-thermal nature. Combining our measurement with VLBI data at 1.4 GHz, we derive a spectral index $α= -0.19 \pm 0.29$, consistent with a nearly flat spectrum. This makes FRB 20190417A only the second PRS with a spectral index constrained using VLBI data. The inferred luminosity places the source on the proposed $L_ν$-|RM| relation. Including this source yields a scatter of $σ_Δ= 0.65$, corresponding to $\hatα|ε| = 1.5 \pm 0.7$, consistent with forward shocks in the free-expansion phase or young pulsar wind nebulae. For the candidate PRS associated with FRB 20181030A, we report upper limits of 80 uJy at 5 GHz and 150 uJy at 8 GHz, corresponding to $L_{5\,\mathrm{GHz}} \lesssim 3.8 \times 10^{25}\ {\rm erg\ s^{-1}\ Hz^{-1}}$, and implying a steep spectral index ($α\lesssim -1.2$) if the VLA emission arises from a compact component. Our results highlight the importance of VLBI in isolating compact emission from FRB engines and provide one of the few spectral constraints for PRSs at milliarcsecond resolution. The consistency of FRB 20190417A with the $L_ν$-|RM| relation supports a nebular origin for the persistent emission.

[abstract 20 / 49] (score: 3)
arXiv:2604.21974 [pdf, ps, other]

Title: The Effects of Complex Accretion Disk Geometry on Broadened Iron K$α$ Lines

Authors: William Surgent, Daniel R. Wilkins,

Comments:

Subjects: astro-ph.HE

Created: 2026-06-08; Updated: 2026-06-10; Datestamp: 2026-06-10

X-rays are emitted from the corona above the orbiting matter of the accretion disk and travel either directly to us or illuminate the disk. This illumination of the inner disk is enhanced by gravitational light bending, which focuses the rays towards the BLACK HOLE and therefore towards the inner radii of the disk. These rays that hit the inner radii are reflected back to us, and we observe them in the X-ray reflection spectrum. In this work, we create novel general-RELATIVISTIC ray-tracing simulations to investigate the effects of altering the geometry of the accretion disks of BLACK HOLEs on the most dominant part of the reflection spectrum, the iron K$α$ line. Work demonstrating the effect of disk geometry on the iron line has been performed, though many previous analyses have assumed a simplistic system, consisting of a point-source corona with a flat and infinitesimally thin accretion disk. We extend these models to more realistic accretion disk approximations. These include a constant-aspect-ratio disk, a radiation-pressure-dominated Shakura-Sunyaev disk, an expanded inner disk that has a nonnegligible scale height in its inner regions due to radiation pressure, as well as various warped-disk configurations. Using measurement uncertainties from XRISM, we find that nonnegligible thickness in accretion disks underestimates the BLACK HOLE spin, coronal height, and inclination angle if fitted with a flat-disk model. The warped-disk model could not be fit with the flat-disk approximation.

[abstract 21 / 49] (score: 3)
arXiv:2605.15313 [pdf, ps, other]

Title: The Millimeter/X-ray Relation in Rapidly Accreting Supermassive Black Holes at $z < 0.16$

Authors: Sophie M. Venselaar, Claudio Ricci, Santiago Del Palacio, Kriti K. Gupta, Chin-Shin Chang, Roberto Serafinelli, Macon A. Magno, Richard Mushotzky, Elena Shablovinskaya, Taiki Kawamuro, Ezequiel Treister, Jacob S. Elford, Susanne Aalto, George C. Privon, Michael J. Koss,

Comments: 25 pages, 11 figures. Accepted for publication in ApJ

Subjects: astro-ph.HE astro-ph.GA

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

A tight correlation between nuclear millimeter and X-ray emission has recently been found in nearby ($z < 0.01$) and low-Eddington ratio ($\rm λ_{Edd} < 0.1$) radio-quiet Active Galactic Nuclei (AGN), suggesting a common origin in the hot X-ray corona. We test this relation in nine more distant RQ AGN ($z \sim 0.06-0.16$) with higher bolometric luminosities ($\log(L_{\rm bol}/\mathrm{erg\,s^{-1}})=45.3-46.3$), Eddington ratios ($\rm λ_{Edd} = 0.19-0.85$), and X-ray bolometric corrections ($κ_{2-10}=29-194$), selected from the Burst Alert Telescope (BAT) survey. We obtained quasi-simultaneous observations with SWIFT at 2-10 keV and the Atacama Large Millimeter/submillimeter Array (ALMA) at 100 GHz and with high angular resolution ($<0.14$"). We find that these high-luminosity AGN lie above the millimeter/X-ray correlation defined by lower-luminosity sources. A joint fit to both samples yields a second-degree polynomial with an intrinsic scatter of 0.32 dex. Furthermore, the millimeter emission correlates linearly with both the UV disk luminosity and $L_{\rm bol}$, with intrinsic scatters of 0.45 and 0.35 dex, respectively. We propose that the deviation from the linear millimeter/X-ray relation arises from a two-component coronal electron population: thermal electrons that produce X-rays, but become less efficient at higher luminosities, and nonthermal electrons that produce millimeter emission and remain tied to $L_{\rm bol}$. Additional millimeter emission from outflow-driven shocks may also contribute, though spectral energy distribution modeling and spectral index studies favor a coronal origin.

[abstract 22 / 49] (score: 3)
arXiv:2606.10011 [pdf, ps, other]

Title: A Multi-Wavelength View of the First Type Ic-BL Supernova with an Einstein Probe X-ray Shock Breakout

Authors: Jillian C. Rastinejad, Gokul Srinivasaragavan, Nikhil Sarin, Tanner O'Dwyer, S. Bradley Cenko, James K. Leung, Anya E. Nugent, Daniel A. Perley, Genevieve Schroeder, Shreya Anand, Tomas Ahumada, Igor Andreoni, Aleksandra Bochenek, Alessandra Corsi, Christoffer Fremling, Anna Y. Q. Ho, Mansi M. Kasliwal, Geoffrey Mo, Anirudh Salgundi, Kendall I. Sippy, J. Sollerman, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, Michael C. Davis, Fabio De Colle, Danielle Frostig, Christopher L. Fryer, Michael J. Graham, Xander J. Hall, K. -R. Hinds, Luca Izzo, Wynn Jacobson-Galan, Nathan P. Lourie, Keiichi Maeda, Josiah Purdum, Ben Rusholme, Avinash Singh, Robert Stein,

Comments: Submitted to ApJL

Subjects: astro-ph.HE

Created: 2026-06-08; Updated: 2026-06-10; Datestamp: 2026-06-10

In March 2026, the Einstein Probe (EP) discovered its most nearby (z = 0.0343) Fast X-ray Transient (FXT), EP260321a, the first EP FXT to provide a strong match to expectations for X-ray ''shock breakout'' (SBO) emission. Here, we present our multi-wavelength follow-up campaign of EP260321a and its broad-line Type Ic (Ic-BL) SUPERNOVA (SN) counterpart, SN 2026gzf, the first Type Ic-BL SN with a definitive X-ray SBO. We show that our radio follow-up extending over 5.8 - 54.5 days post-FXT rules out an on-axis JET counterpart of isotropic-equivalent kinetic energy $E_{K} > 10^{49}$ erg for circumburst densities $n > 10^{-2}~{\rm cm}^{-3}$ and constrains radio SYNCHROTRON emission from the fastest-moving SN ejecta. In addition, we derive the properties of SN 2026gzf and its host galaxy from our well-sampled optical data and compare them with those of optically discovered Type Ic-BL SNe, finding that SN2026gzf is well within the 90% confidence interval across all properties. We further fit SN 2026gzf's light curve with five different physical models, and determine that combined emission from both interaction with circumstellar material (CSM) and $^{56}$Ni radioactive decay provides the best fit with plausible model parameters. Finally, using the rate of Ic-BL SNe from the ZTF Bright Transient Survey and assuming all Type Ic-BL SNe produce EP260321a-like FXTs, we infer an expected rate of EP-detected SBOs of 4.4 - 16 year$^{-1}$. This is inconsistent at the 90% confidence level with current EP detection rates, potentially indicating that most Type Ic-BL SNe produce less luminous X-ray SBO signals compared to EP 260321a.

[abstract 23 / 49] (score: 3)
arXiv:2606.10160 [pdf, ps, other]

Title: Aether-SHELLQs: JWST integral-field spectroscopy of candidate obscured QUASARs at z ~ 6

Authors: Yoshiki Matsuoka, Roberto Decarli, Emanuele Paolo Farina, Anniek J. Gloudemans, Eduardo Bañados, Fabrizio Arrigoni Battaia, Anna-Christina Eilers, Chiara Mazzucchelli, Michael A. Strauss, Hyewon Suh, Maxime Trebitsch, Fabian Walter, Feige Wang, Kentaro Aoki, Junya Arita,

Comments: Accepted for publication in ApJ

Subjects: astro-ph.GA

Created: 2026-06-08; Updated: 2026-06-10; Datestamp: 2026-06-10

We present James Webb Space Telescope (JWST) NIRSpec integral field unit (IFU) observations of six galaxies at $z \sim 6$, obtained as part of the Aether project (General Observers program 5645). The targets were originally identified by the Subaru High-$z$ Exploration of Low-Luminosity Quasars (SHELLQs) survey, as candidate obscured QUASARs with luminous ($\gtrsim10^{43}$ erg s$^{-1}$) but narrow ($\lesssim500$ km s$^{-1}$) Ly$α$ emission. Two objects exhibit a broad component in their Balmer lines (FWHM $>3000$ km s$^{-1}$), indicating the presence of ACTIVE GALACTIC NUCLEi (AGNs), while the remaining four show similar profiles in permitted and forbidden lines. Combining these data with similar SHELLQs objects reported previously, we find that the presence of broad lines is strongly correlated with Ly$α$ luminosity ($L_{\rm Lyα}$); the inferred AGN fraction is $>$77 % and $<$15 % above and below $L_{\rm Lyα} =10^{44}$ erg s$^{-1}$, respectively. Dust-extinction corrections inferred from the Balmer decrement would imply unrealistically high Ly$α$ luminosities, suggesting that the line-emitting gas consists of multiple zones. The IFU data reveal diverse spatial structures. The AGN hosts are compact, whereas the other galaxies show extended ionized gas on scales up to 10 kpc and STAR FORMATION rates of 60 - 600 $M_\odot$ yr$^{-1}$. One of the extended objects exhibits a signature of rotation, while most of the others show little ordered kinematics, with velocity widths (FWHM) up to 200 - 300 km s$^{-1}$. These objects populate the intermediate luminosity regime between classical luminous QUASARs and the low-luminosity AGNs discovered by JWST, including Little Red Dots, potentially linking the two populations.

[abstract 24 / 49] (score: 3)
arXiv:2606.10189 [pdf, ps, other]

Title: Radio precursors of monster shocks: a mechanism for fast radio bursts from SGR 1935+2154

Authors: Andrei M. Beloborodov,

Comments: 21 pages, 6 figures, submitted to ApJ

Subjects: astro-ph.HE

Created: 2026-06-08; Updated: 2026-06-10; Datestamp: 2026-06-10

Kilohertz perturbations in active MAGNETars evolve into monster radiative shocks at radii $r\sim 10^8$ cm. The shock generates X-rays and a semi-coherent radio precursor, which strongly interacts with the MAGNETospheric plasma ahead of the shock. We show that this interaction self-regulates the precursor emission and find its self-consistent frequency and luminosity. The precursor frequency falls in the GHz band and its production peaks when the shock expands to $r\approx 10^9$ cm. The resulting GHz burst has a sub-millisecond duration and energy ${\cal E}_{\rm FRB}\approx 10^{34}{\cal E}_{38}^{0.2}$ erg where ${\cal E}$ is the energy of the primary MAGNETosonic disturbance that launched the shock. As the GHz burst propagates to the light cylinder $R_{\rm LC}\sim 10^{10}$ cm, it faces a threat of being absorbed by the MAGNETosphere. The burst escapes if the local plasma density at $R_{\rm LC}$ is $\sim 30$ times lower than typically expected for active MAGNETars, so distant observers need some luck to see the radio burst. The shock X-rays follow the radio waves with a millisecond delay. Shocks from kilohertz disturbances with energies ${\cal E}\sim 10^{38}$ erg generate X-ray and radio bursts similar to the activity detected in SGR 1935+2154.

[abstract 25 / 49] (score: 3)
arXiv:2606.10215 [pdf, ps, other]

Title: LEAP: A Rapid Neural Surrogate of Multi-Fluid MHD at Europa

Authors: Sachin Alexander Reddy, Abigail R. Azari, Corey J. Cochrane, Xianzhe Jia, Tom A. Nordheim, Lukas Mandrake, Steven D. Vance, Camilla Harris, Ioana Ciucǎ,

Comments:

Subjects: physics.space-ph physics.plasm-ph

Created: 2026-06-08; Updated: 2026-06-10; Datestamp: 2026-06-10

Characterizing Europa's subsurface ocean is a key objective of the Europa Clipper and JUICE missions in the search for life beyond Earth. Although the ocean's induced MAGNETic field provides key constraints on habitability, interpretation is complicated by perturbations arising from Jupiter's plasma interaction with Europa. Physics-based models (e.g. MAGNETohydrodynamic, MHD) required to characterize these effects are physically comprehensive, but have a prohibitive computational cost. To address this, we introduce Learning Europa's Atmosphere and Plasma (LEAP), a transformer-based surrogate trained on outputs from a state-of-the-art multi-fluid MHD code to predict MAGNETic field perturbations along spacecraft trajectories. LEAP evaluates in milliseconds on a laptop, whereas MHD takes 12 hrs on a high-performance computer (~40,000x speed-up). The model has test set errors of -/+ 2.6 nT, and for the Galileo E4 and E14 flybys of Europa it matches the parent MHD model in accuracy. Its enhanced speed enables large-scale parameter surveys and probabilistic estimations of plasma conditions, establishing a new framework for accelerated plasma interaction modeling. LEAP can also inform future MHD simulations while learning from them. Beyond Europa, this framework could be expanded to planning future missions or to other high-priority bodies, including Uranus and Neptune.

[abstract 26 / 49] (score: 3)
arXiv:2606.10283 [pdf, ps, other]

Title: First Principles Magnetohydrodynamical Theory for the Expanding Box Model

Authors: Sebastián Saldivia, Nicolás Villarroel-Sepúlveda, Sebastián Echeverría-Veas, Felipe A. Asenjo, Pablo S. Moya,

Comments: 12 pages, 1 figure

Subjects: physics.plasm-ph astro-ph.SR

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

The Expanding Box Model (EBM) has been widely employed to simulate multiscale plasma phenomena in the expanding solar wind by transforming the MHD equations to a co-moving, non-inertial frame. However, traditional formulations have suffered from historical ambiguity regarding the physical separation between the co-moving and inertial reference frames, primarily arising from a classical approximation of an invariant MAGNETic field between them. To resolve this inconsistency, we reformulate the EBM from first principles using a fully covariant approach. Here, we model the expanding solar wind frame as an anisotropic expanding spacetime metric, allowing us to incorporate radial acceleration profiles and differential transverse expansion, ensuring that all physical fields are correctly transformed by expansion. We demonstrate that the mathematical artifacts and structural asymmetries identified in previous EBM-MHD literature are direct consequences of neglecting the tensorial scaling of the MAGNETic field. Our covariant treatment eliminates these residues, restoring symmetry in the co-moving frame. Projecting our system back into the inertial frame recovers the established observational scaling and analogous physics, clarifies the mathematical distinction between local plasma dynamics and global expansion, and reveals the macroscopic anisotropy of the Parker spiral as a purely geometric projection. Furthermore, linear wave analysis demonstrates that macroscopic acceleration governs the evolution of Alfvén wave amplitude, acting either as geometric damping or as an energy source. Further, we write the EBM-MHD system using compressible Elsässer variables. This formulation provides a consistent and clean foundation for future numerical simulations of accelerating astrophysical plasmas.

[abstract 27 / 49] (score: 3)
arXiv:2606.10292 [pdf, ps, other]

Title: Constraints on axion-like particles from ultra-high-energy observations of M87 with the HAWC observatory

Authors: R. Alfaro, C. Alvarez, A. Andrés, E. Anita-Rangel, M. Araya, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, P. Bangale, E. Belmont-Moreno, A. Bernal, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, F. Carreón, S. Casanova, U. Cotti, J. Cotzomi, P. Desiati, E. De la Fuente, N. Di Lalla, R. Diaz Hernandez, M. A. DuVernois, J. C. Díaz-Vélez, T. Ergin, C. Espinoza, N. Fraija, S. Fraija, J. A. García-González, F. Garfias, N. Ghosh, A. Gonzalez Muñoz, M. M. González, J. A. González, J. A. Goodman, J. Gyeong, J. P. Harding, I. Herzog, D. Huang, F. Hueyotl-Zahuantitla, A. Iriarte, S. Kaufmann, D. Kieda, A. Lara, W. H. Lee, J. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, H. Martínez-Huerta, J. A. Matthews, P. Miranda-Romagnoli, P. E. Mirón-Enriquez, J. A. Morales-Soto, E. Moreno, M. Mostafá, M. Najafi, A. Nayerhoda, L. Nellen, M. U. Nisa, R. Noriega-Papaqui, L. Olivera-Nieto, N. Omodei, M. Osorio-Archila, E. Ponce, Y. Pérez Araujo, E. G. Pérez-Pérez, A. Pratts, C. D. Rho, A. Rodriguez Parra, D. Rosa-González, M. Roth, D. Salazar-Gallegos, A. Sandoval, M. Schneider, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, E. Varela, L. Villaseñor, X. Wang, Z. Wang, I. J. Watson, H. Wu, S. Yu, X. Zhang, H. Zhou, C. de León,

Comments: Content: 12 pages and 5 figures

Subjects: astro-ph.HE hep-ph

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

In this work, we perform an indirect search for axion-like particles (ALPs) through their hypothesized mixing with photons in the presence of MAGNETic fields. ALPs are a well-motivated dark-matter candidate class, and the photon-ALP conversion mechanism provides a unique channel to constrain their mass and coupling constant using very-high-energy gamma-ray observations. The photon-ALP mixing could alter the observed gamma-ray spectrum from extragalactic sources by effectively reducing the apparent attenuation due to extragalactic-background-light absorption. We analyze 7.5 years of data from the High Altitude Water Cherenkov (HAWC) Observatory, targeting the nearby RADIO GALAXy M87. This source is located within the Virgo cluster and is an ideal environment for photon-ALP conversion due to its low redshift and the large-scale, strongly MAGNETized medium of the cluster. We find no evidence for a photon-ALP conversion signal and, consequently, set constraints on the ALP mass and photon-ALP coupling constant with emission from M87 which are consistent with previous results. Our analysis places competitive constraints on the ALP parameter space, defining an exclusion region in the mass range of approximately $10^{-8}$ to $10^{-6}$ eV for coupling constants above $5\times10^{-12}$ GeV$^{-1}$, complementing previous constraints from other gamma-ray observatories.

[abstract 28 / 49] (score: 3)
arXiv:2606.10655 [pdf, ps, other]

Title: Optical-morphology-based assessment of astrometric quality in Gaia-CRF3 QUASARs

Authors: Qiqi Wu, Shilong Liao, Zhaoxiang Qi, Qi Xu, Ye Ding, Keyu Zhu,

Comments: 16 pages, 14 figures Submitted to Astronomy & Astrophysics

Subjects: astro-ph.GA

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

Context. Several studies have shown that host-galaxy structure or extended optical morphology in AGNs can induce spurious parallaxes and proper motions in Gaia DR3. However, it remains unclear whether source morphology also introduces systematic errors into the celestial reference frame constructed from Gaia data. Aims. We aim to provide a Gaia-independent external morphological indicator for Gaia-CRF3 sources and to use it to quantify the astrometric systematics associated with source morphology. Methods. Using morphological parameters derived from DESI, SDSS, and SkyMapper, together with the PS1-PSC point-source score as a common reference scale, we used XGBoost to infer external morphological scores for Gaia-CRF3 sources. We then developed a multi-survey fusion scheme to combine the four survey-based point-source scores into a single composite score that measures the degree to which each source departs from the morphology of an ideal point source. Results. We obtained morphological scores for 1,607,490 Gaia-CRF3 sources, corresponding to a completeness of 99.59\% with respect to the full Gaia-CRF3 catalogue. The score ranges from 0 to 1 and remains reliable for sources with $G<20.85$ mag. Based on this indicator, we find that AGNs with strongly non-point-like morphology induce a parallax zero-point shift of about $-43.7\,μ$as, which cannot be effectively removed by the current parallax zero-point correction model. We also find that reference-source subsamples selected in different score ranges exhibit significantly different all-sky proper motion fields. For the high-purity point-source subsample with \texttt{point\_score} > 0.95, the total frame spin amplitude is reduced by 15.8\% relative to that of the full Gaia-CRF3 sample.

[abstract 29 / 49] (score: 3)
arXiv:2606.10710 [pdf, ps, other]

Title: Hubble as a Unique Discovery Engine of the Fate of Massive Stars and Black Hole Formation

Authors: Avishai Gilkis, Eva Laplace, Charles D. Kilpatrick, Maria R. Drout, Anna J. G. O'Grady, Christopher A. Tout,

Comments: 5 pages, 2 figures; white paper submitted in response to the Space Telescope Science Institute call: Building a Roadmap for Hubble science into the 2030s

Subjects: astro-ph.HE astro-ph.GA

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

How stellar-mass BLACK HOLEs are formed is an open question in astrophysics, with very limited observational constraints. It is not known which types of stars are more likely to produce BLACK HOLEs, and whether the formation process is accompanied by strong or weak electroMAGNETic transients - or none at all - and this issue remains a critical missing piece in the puzzle of the fate of massive stars. Recent theoretical work predicts that many stellar-mass BLACK HOLEs form from hot, UV-luminous massive stars, including Wolf-Rayet-like progenitors, and searches focused primarily on luminous cool supergiants may therefore miss a substantial fraction of black-hole formation events. While the coming decade will bring major advances in time-domain astronomy through Rubin/LSST, Roman, JWST, and wide-field transient surveys, none of these combines UV sensitivity, sub-arcsecond imaging, and decade-long continuity. HST uniquely enables direct searches for disappearing hot massive stars associated with black-hole formation. We outline a roadmap for extending HST's role in this area into the 2030s through a dedicated, large program to re-image nearby galaxies in the UV and identify candidate disappearing stars and unusual low-luminosity transients identified by complementary surveys. Theoretical event rates imply that the nearby galaxy population accessible to HST should yield of order one detectable black-hole-forming disappearance event per year. Extending HST operations into the 2030s would therefore provide crucial insights into the unsolved problem of BLACK HOLE formation.

[abstract 30 / 49] (score: 3)
arXiv:2606.10823 [pdf, ps, other]

Title: AGN-driven BBH mergers: Black hole populations and hierarchical growth across the AGN parameter space

Authors: Maria Paola Vaccaro, Michela Mapelli, Alessandro Alberto Trani, Boyuan Liu,

Comments: 19 pages, 14 figures

Subjects: astro-ph.GA astro-ph.CO astro-ph.HE

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

Active galactic nuclei (AGNs) have been proposed as efficient environments for the formation of binary BLACK HOLEs (BBHs). We present an updated semi-analytical framework for BBH formation and evolution in AGN disks, following the capture, migration, pair-up, gas-driven hardening, binary--single encounters, and merger of stellar-origin BLACK HOLEs. We systematically explore the dependence of the resulting BBH merger population on the main AGN parameters, namely the supermassive BLACK HOLE mass $M_\bullet$, the Eddington ratio $λ_\bullet$, and the disk viscosity parameter $α$, and construct an intrinsic BBH population by weighting the simulations according to observed low-redshift AGN properties. We find that AGN disks can produce repeated mergers and build a high-mass tail extending beyond the pair-instability mass gap and into the intermediate-mass range. Hierarchical growth is more efficient in lower-viscosity disks, with $α=0.01$, while higher-viscosity disks suppress the formation of massive remnants. The merger efficiency generally increases with $λ_\bullet$, but its dependence on $M_\bullet$ is non-trivial. The AGN-assisted BBH population is characterized by increasingly unequal mass ratios at high primary mass, a correlation between primary mass and $|χ_{\rm eff}|$, and an effective-spin distribution that depends strongly on the fraction of binaries born in prograde or retrograde configurations. We find that the AGN channel can reproduce systems broadly consistent with the massive BBH events GW190521 and GW231123. We test several variations of the physical model, including different formalisms for migration torques, gas hardening, and three-body encounters. The general properties of the population are robust across these variations, with the high-mass tail and spin signatures persisting in all cases except when gas hardening is switched off.

[abstract 31 / 49] (score: 3)
arXiv:2606.11133 [pdf, ps, other]

Title: Resolving SLX 1744-299 and SLX 1744-300 in the hard X-ray band: implications for their ultracompact nature

Authors: Enzo A. Saavedra, Montserrat Armas Padilla, Teo Muñoz-Darias,

Comments: 10 pages, 7 figures. Accepted for publication in Astronomy & Astrophysics

Subjects: astro-ph.HE

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

Persistent, low-luminosity low-mass X-ray binaries (LMXBs) offer a unique opportunity to study accretion in this poorly understood regime, as well as to unveil new members of the ultracompact X-ray binary (UCXB) family, characterised by orbital periods ($P_{\rm orb}$) shorter than $\sim 80$ min. We report on a NUSTAR archival observation that, for the first time above 10 keV, spatially resolves the Galactic Centre pair SLX 1744$-$299 and SLX 1744$-$300. We find SLX 1744$-$300 to be slightly brighter, with a flux ratio of $\sim 1.15$, increasing to $\sim 1.3$ when extrapolated to 0.5$-$10 keV. Both the timing (root-mean-square variability) and spectral properties (well described in both cases by a thermal Comptonisation model) indicate that the systems were in the hard state. The two sources, however, display markedly different behaviour throughout the observation. SLX 1744$-$299 shows a gradual flux decline consistent with a decrease in the mass-accretion rate, whereas SLX 1744$-$300 remains steady but exhibits two short-recurrence Type-I X-ray bursts indicative of mixed H/He burning. Combining our results with previously reported upper limits on the distance, we derive low persistent X-ray luminosities of $L_{\rm X}\lesssim 1.1\times10^{36}$ erg s$^{-1}$ and $L_{\rm X}\lesssim 2.6\times10^{36}$ erg s$^{-1}$ (3$-$78 keV) for SLX 1744$-$299 and SLX 1744$-$300, respectively. The corresponding mass-accretion rates, when compared with the critical values from the disc instability model, favour $P_{\rm orb}\lesssim 90$ min and $P_{\rm orb}\lesssim 105-155$ min. Although both limits are formally compatible with the UCXB regime, the case of SLX 1744$-$299 appears significantly more compelling, also considering the previously reported intermediate-duration burst.

[abstract 32 / 49] (score: 2)
arXiv:2509.18271 [pdf, ps, other]

Title: Small-scale Lyman alpha forest cosmology with PRIYA: Constraints from XQ100 and KODIAQ-SQUAD one-dimensional flux power spectra

Authors: Ming-Feng Ho, Mahdi Qezlou, Simeon Bird, Yanhui Yang, Camille Avestruz, M. A. Fernandez, Vid Iršič,

Comments: 44 pages, 24 figures. Accepted version, matched to JCAP

Subjects: astro-ph.CO astro-ph.GA

Created: 2026-06-08; Updated: 2026-06-10; Datestamp: 2026-06-10

We present a new cosmological analysis of the small-scale Lyman alpha forest 1D flux power spectrum (P1D) using high-resolution QUASAR spectra from XQ100 and KODIAQ-SQUAD, interpreted through the PRIYA emulator. PRIYA is a suite of galaxy formation simulations spanning a range of cosmological and inhomogeneous HeII reionization parameters, enabling few-percent-level predictions of the P1D. These datasets, probing down to $k \sim 6\,h\,\mathrm{Mpc}^{-1}$ at $z = 2-5$, offer access to non-linear scales inaccessible to large-volume surveys like eBOSS. We find that the XQ100 P1D yields constraints on the primordial power spectrum parameters $(A_P, n_P)$ at pivot scale $k_0 = 0.78\,\mathrm{Mpc}^{-1}$ that are consistent with PRIYA results from eBOSS DR14 and Planck CMB, albeit with broader uncertainties. Notably, this is achieved without external IGM temperature data, showing that XQ100 alone provides stronger constraints on thermal history than eBOSS DR14. In contrast, the KODIAQ-SQUAD P1D favors a significantly higher $A_P$ value, driven by the selection bias toward high-column density absorbers (HCDs). We also find that the P1D at $k > 0.045\,\mathrm{s/km}$ is more sensitive to Lyman limit system contamination and thermal history. When imposing a prior on $(A_P, n_P)$, the reduced $χ^2$ remains unchanged and the inferred mean IGM temperature is unaffected, suggesting that cosmological and thermal parameters are largely sensitive to different scales. The XQ100 P1D therefore provides complementary information on thermal nuisance parameters, which can be jointly fit with eBOSS or DESI P1D measurements to improve cosmological constraints.

[abstract 33 / 49] (score: 2)
arXiv:2511.20083 [pdf, ps, other]

Title: Covariant equations of motion of massive spinning particles in a background Yang-Mills field

Authors: Jie Zhou, Ying Shan Zhao, Yifeng Sun,

Comments: 14 pages

Subjects: nucl-th hep-th

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

The dynamics of a spinning colored particle in a background non-Abelian Yang-Mills field is of broad interest in many areas of physics. A physically important application arises in RELATIVISTIC heavy-ion collisions, where hard probes such as heavy QUARKs and JETs propagate through the strong early-time classical color fields collectively referred to as the glasma. The standard framework for describing the classical dynamics of colored particles in a background Yang-Mills field is provided by the Wong equations, but it does not incorporate spin degrees of freedom. Although several extensions of the Wong equations have been proposed to include spin, they generally fail to satisfy all the necessary requirements simultaneously, such as Lorentz covariance, allowance for an arbitrary chromoMAGNETic moment, and preservation of the required physical constraints. In this work, we extend the framework of a RELATIVISTIC classical spinning particle in an electroMAGNETic field to describe spin-1/2 QUARKs propagating in a generic background non-Abelian Yang-Mills field. By systematically applying the Dirac-Bergmann algorithm, we derive a self-consistent set of equations of motion for the particle's coordinates, momenta, spin, and color charge that satisfies all these requirements. This formalism provides a more complete and physically consistent description of spinning colored particles in background Yang-Mills fields, and offers a suitable framework for studying momentum diffusion and spin POLARIZATION phenomena of hard probes in heavy-ion collisions, particularly in the glasma.

[abstract 34 / 49] (score: 2)
arXiv:2512.11958 [pdf, ps, other]

Title: Modeling the Milky Way Circumnuclear Disk: Rosettes and Rings

Authors: Asad Ukani, Lena Murchikova, Mark D. Gorski,

Comments: v2: Accepted to ApJ. 2 subsections, minor corrections, and several clarifications added. 12 pages, 3 figures, 2 tables, and 1 appendix; v1: 10 pages, 3 figures, 2 tables, and 1 appendix

Subjects: astro-ph.GA

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

The Milky Way Galactic Center hosts a $\sim4\times10^{6}\,M_\odot$ supermassive BLACK HOLE (SMBH), Sagittarius A* (Sgr A*). The dominant structures in its immediate vicinity are the nuclear star cluster (NSC), whose enclosed mass at 2 pc is approximately half that of the SMBH, and the circumnuclear disk (CND)/ring, which extends between $\sim0.5$ pc and $\sim3$ pc from Sgr A* and is the largest reservoir of molecular gas in this region. Existing models of the CND commonly use one circular orbit to describe the motion of its gas. Here, we explore a much broader range of models. In the combined potential of Sgr A* and the NSC, we consider non-Keplerian rosette orbits as well as a circular disk, which is formed using a finely spaced set of concentric rings. For both systems, we test various inner/outer radii, inclinations, and position angles, sampling a total of $\sim3.3 \times 10^{5}$ models. We then conduct mock observations of all models to construct velocity maps, which we compare with HCN ($J=1{-}0$) observations of the CND. We find that the best-fitting model is a circular disk with inner and outer radii of 1.0 pc and 2.9 pc, an inclination of $i=60^{\circ}$, and a position angle of $\text{PA} = 35^{\circ}.$

[abstract 35 / 49] (score: 2)
arXiv:2512.24003 [pdf, ps, other]

Title: Machine-learning approaches to dispersion measure estimation for fast radio bursts

Authors: Hosein Rajabi, Zhejian Liu, Fereshteh Rajabi, Martin Houde,

Comments: 14 pages, 6 figures, and 8 tables

Subjects: astro-ph.HE

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

Fast radio bursts (FRBs) are bright, mostly millisecond-duration transients of extragalactic origin whose emission mechanisms remain unknown. As FRB signals propagate through ionized media, they experience frequency-dependent delays quantified by the dispersion measure (DM), a key parameter for inferring source distances and local plasma conditions. Accurate DM estimation is therefore essential for characterizing FRB sources and testing physical models, yet current dedispersion methods can be computationally intensive and prone to human bias. In this proof-of-concept study, we develop and benchmark three deep-learning architectures, a conventional convolutional neural network (CNN), a fine-tuned ResNet-50, and a hybrid CNN-LSTM model, for automated DM estimation. All models are trained and validated on a large set of synthetic FRB dynamic spectra generated using CHIME/FRB-like specifications. The hybrid CNN-LSTM achieves the highest accuracy and stability while maintaining low computational cost across the investigated DM range. Although trained on simulated data, these models can be fine-tuned on real CHIME/FRB observations and extended to future facilities, providing a pathway toward real-time, data-driven DM estimation in large FRB surveys with further development.

[abstract 36 / 49] (score: 2)
arXiv:2604.09160 [pdf, ps, other]

Title: Joining forces: 30 years of optical monitoring of the Einstein Cross

Authors: V. N. Shalyapin, L. J. Goicoechea, R. Gil-Merino, A. Esteban-Gutiérrez, C. W. Morgan, E. Mediavilla, A. Yonehara, A. Sergeyev,

Comments: Accepted to A&A; 18 pages, 6 long tables (Tables C.1-C.6) are available at the CDS [minor change to the title]

Subjects: astro-ph.GA

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

We present an extended optical monitoring of the quadruply-imaged gravitationally lensed QUASAR QSO 2237+0305, the Einstein Cross, including observations from different observatories in both hemispheres and using a new photometric technique. This technique uses a region far enough from the lens system to determine accurately the sky background level, and minimises contamination from the lensing galaxy by combining analytical and numerical modeling of its structure. The resulting light curves of the four QUASAR images describe variations across practically the entire optical spectrum and span about 9000 days in the $VRI$ bands. The multi-band microlensing variability is captured with an unprecedented level of detail, and a preliminary microlensing analysis reveals an almost linear scaling of source radius with wavelength, providing direct evidence for the wavelength-dependent structure of the region contributing to optical passband fluxes. Specifically, assuming a mean microlens mass $\langle M \rangle$ = 0.3 $\rm{M_{\odot}}$ and concentric Gaussian sources that move according to the velocity distribution peaks (speed and direction) reported in a previous microlensing analysis, we find that the half-light radius of the $g$-band source is 9.6 $\pm$ 2.7 lt-day and the size of the sources grows with wavelength with a power-law index of $α$ = 0.94 $\pm$ 0.05. We conclude that these long-term light curves set stringent empirical constraints on models of QUASAR emission and microlensing physics.

[abstract 37 / 49] (score: 2)
arXiv:2605.12356 [pdf, ps, other]

Title: Reproducing morphological features in the SUPERNOVA remnant G11.2-0.3 by simulating jittering JETs

Authors: Muhammad Akashi, Noam Soker,

Comments: Publications of the Astronomical Society of the Pacific

Subjects: astro-ph.HE

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

We hydrodynamically simulate a core-collapse SUPERNOVA (CCSN) explosion by launching three pairs of JETs in the framework of the jittering-JETs explosion mechanism (JJEM), and reproduce a morphology of two opposite circum-JET rings and a bar of dense gas perpendicular to the rings' axis, resembling these morphological features in the CCSN remnant SNR G11.2-0.3. The first pair of wide JETs is very energetic; it triggers the explosion and inflates two bubbles that compress the material in an expanding shell. The bubbles also compress material in a plane perpendicular to the JET axis. The second pair of wide JETs removes material from this plane, beside along a bar that is on an axis perpendicular to the two pairs' axes. The JETs of the third pair, now of narrow JETs, penetrate the expanding shell and compress material to their sides to form two opposite rings. These morphological features are qualitatively similar to those observed in the point-symmetric CCSN remnant G11.2-0.3. As competing theoretical CCSN explosion mechanisms cannot explain point-symmetric CCSN remnants, our study provides some support for the claim that the JJEM is the primary explosion mechanism of CCSNe.

[abstract 38 / 49] (score: 2)
arXiv:2606.10000 [pdf, ps, other]

Title: From Dense Gas Clouds to Supermassive Black Hole Seeds: Hybrid Hydro/Direct $N$-body Simulations of Runaway Collision-driven Intermediate-mass Black Hole Formation

Authors: Eunwoo Chung, Yongseok Jo, Ji-hoon Kim, Minyong Jung, Oh-kyoung Kwon,

Comments: Accepted for publication in ApJ, 23 pages, 15 figures. For summary video, see https://youtu.be/nJnj6wwB0D4

Subjects: astro-ph.GA

Created: 2026-06-08; Updated: 2026-06-10; Datestamp: 2026-06-10

A population of dense stellar systems at high redshift has recently been uncovered by the JWST. To investigate the formation of supermassive BLACK HOLE (SMBH) seeds in these dense environments without invoking any \textit{ad hoc} seeding mechanisms, we present star cluster-scale simulations performed with an updated version of the hydrodynamics code \texttt{Enzo-Abyss}, which self-consistently integrates the gravity using a direct $N$-body method coupled with stellar evolution. By modeling initially dense, metal-poor gas clouds with varying turbulence, we consistently find the formation of dense clusters resembling early-stage nuclear star clusters (NSCs), as well as the formation of very massive stars (VMSs) ranging from $343\;\mathrm{M_\odot}$ to $5108\;\mathrm{M_\odot}$ via runaway collisions, irrespective of stellar wind feedback strength. Following the direct collapse of these VMSs, the resulting intermediate-mass BLACK HOLEs (IMBHs) grow through Eddington-limited gas accretion and tidal disruption events (TDEs). In our most optimistic model, we find a mass accretion rate of $1.64\times10^{-4}\;\mathrm{M_\odot\;yr^{-1}}$, with TDEs contributing $23\%$ of the total accretion over $\sim10\;\mathrm{Myr}$. Assuming a steady gas supply into the NSC driven by rapid structural assembly in the high-redshift environment, together with a constant TDE rate, we project that an IMBH with an initial mass of $6747\;\mathrm{M_\odot}$ at the center of the NSC can grow to $\sim62000\;\mathrm{M_\odot}$ within $100\;\mathrm{Myr}$ of its formation. Our numerical study, conducted within a single self-consistent framework that incorporates the essential physical processes, suggests that VMSs can form in dense gas clouds, collapse into IMBHs, and subsequently provide viable seeds for the SMBHs observed at high redshift.

[abstract 39 / 49] (score: 2)
arXiv:2606.10036 [pdf, ps, other]

Title: Learning the Universe at High Redshifts: Impact of Accretion Modeling on Early Black Hole Growth

Authors: Jonathan Kho, Aklant K. Bhowmick, Rainer Weinberger, Paul Torrey, Laura Blecha, Lars Hernquist, Greg L. Bryan, Alex M. Garcia, Niusha Ahvazi, Alejandro Saravia, Boon Kiat Oh,

Comments: 19 pages, 7 figures, submitted to ApJ

Subjects: astro-ph.GA

Created: 2026-06-08; Updated: 2026-06-10; Datestamp: 2026-06-10

JWST discoveries of the earliest ($z \gtrsim 9$) supermassive BLACK HOLEs (BHs, $M_\bullet \gtrsim 10^6\,\rm{M}_\odot$) challenge the BH seeding and accretion models of most cosmological simulations. In this work, we compare early BH growth arising from three different accretion prescriptions characterized by distinct scalings between the accretion rate ($\dot{M}_{\rm \bullet}$) and the BH mass ($M_{\rm \bullet}$): the commonly used Bondi-Hoyle model ($\dot{M}_{\rm \bullet}\propto M_{\rm \bullet}^2$), and two free-fall models with shallower scalings ($\dot{M}_{\rm \bullet}\propto M_{\rm \bullet}^{1/2}$ and $M_{\rm \bullet}$). Bondi accretion tends to produce stronger runaway growth than the free-fall models when using heavy ($\sim10^5\,\rm{M}_\odot$) seeds owing to the steeper $M_\bullet$ scaling, but its sensitivity to the local gas sound speed makes it more susceptible to suppression from temperature increases due to AGN and stellar feedback. The free-fall models tend to produce stronger growth for lower-mass seeds ($\sim10^{3-4}\,\rm{M}_\odot$) as they are less dependent on the BH's mass to accrete effectively, however in this regime BH growth remains negligible for all accretion models in the presence of fiducial stellar feedback. Enhancing early BH growth via many BH-BH mergers disproportionately enhances subsequent accretion-driven growth for Bondi due to the steeper $M_{\rm \bullet}$ dependence. Our simulations can thus assemble BHs with masses of $\sim10^6-10^7 M_{\odot}$ at $z\gtrsim9$, as inferred by JWST, under two circumstances: 1) abundant heavy-seed formation that drives BH-BH mergers, or 2) Bondi accretion with weak feedback.

[abstract 40 / 49] (score: 2)
arXiv:2606.10104 [pdf, ps, other]

Title: The Fifth RIT Catalog of Binary Black Hole Simulations: Multiple-Resolution Studies of Eccentric Orbits

Authors: Giuseppe Ficarra, James Healy, Carlos O. Lousto,

Comments: 26 pages, 2 figures, 19 tables

Subjects: gr-qc astro-ph.HE

Created: 2026-06-08; Updated: 2026-06-10; Datestamp: 2026-06-10

This fifth release of the RIT public catalog of numerical relativity binary BLACK HOLE waveforms http://ccrg.rit.edu/~RITCatalog introduces an additional 248 configurations, prioritizing 197 newly simulated eccentric orbits. This update brings the catalog to a total of 2129 cases. All waveforms are corrected for center-of-mass drift and extrapolated to future null infinity. To rigorously estimate waveform errors, we conduct multiple-resolution convergence studies on 10 eccentric simulations (up to 33 orbits to merger) using three global resolutions increasing by factors of 1.2, plus a comprehensive six-resolution study for a single 18-orbit configuration. We evaluate waveform accuracy by computing mismatches against theoretical infinite-resolution extrapolations. Additionally, we analyze the convergence properties of key physical observables: merger times, number of orbits, final masses, final spins, recoil velocities, and the peak amplitude, frequency, and luminosity of the gravitational radiation.

[abstract 41 / 49] (score: 2)
arXiv:2606.10175 [pdf, ps, other]

Title: Gravitational Wave Energy Emitted in the Head-On Collision of Two Black Holes

Authors: Nesibe Derin Sivrioglu, Robert R. Caldwell,

Comments: 4 pages, 2 figures

Subjects: gr-qc

Created: 2026-06-08; Updated: 2026-06-10; Datestamp: 2026-06-10

What is the spectrum of gravitational radiation produced by the head-on collision of two equal-mass BLACK HOLEs? The emission is dominated by low frequency bremsstrahlung, producing a flat energy spectrum. But where does the spectrum turn over? We propose that the lowest quasinormal mode of the final BLACK HOLE marks the end of the low-frequency domain. The result is an analytic model of the total emitted energy as a function of the BLACK HOLE velocity in the center of mass frame. With no free parameters, the model predicts that 13.8% of the total initial energy is emitted in gravitational radiation, in good agreement with numerical relativity. This result also enables calculation of the nonlinear contribution to the memory, a persistent distortion of the spacetime after passage of the gravitational wave burst. Advances in numerical relativity simulations will enable tests of our model for increasingly RELATIVISTIC speeds, providing insight into this extreme collision.

[abstract 42 / 49] (score: 2)
arXiv:2606.10490 [pdf, ps, other]

Title: Systematic comparison of VMEC and HINT equilibrium calculations for finite-beta LHD plasmas

Authors: Albert Civit-Bertran, Yasuhiro Suzuki, Shimpei Futatani,

Comments: 2 pages, 2 figures, Rapid communication

Subjects: physics.plasm-ph

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

A systematic comparison between VMEC and HINT equilibrium calculations has been carried out for Large Helical Device plasmas to clarify the influence of the assumption of the nested flux surfaces at finite beta.Three vacuum MAGNETic-axis configurations, $R_{\rm axV} = \SI{3.53}{\, m}$, $\SI{3.60}{\, m}$, $\SI{3.85}{\, m}$, are examined for the beta values on the axis in the range $β_0 \in [0.0\%, 5.0\%]$. The MAGNETic-axis position, the rotational transform on the axis, and the plasma volume enclosed by the last closed flux surface are compared between the two codes. At low-$β_0$, VMEC and HINT give consistent equilibria, indicating that the nested flux surfaces are largely preserved. Above a configuration-dependent critical $β_0$, however, the two solutions begin to diverge, indicating that the nested flux surfaces assumption is compromised. In HINT, the enclosed plasma volume decreases at higher beta because the stochastic MAGNETic field evolves near the plasma edge, whereas VMEC cannot represent this flux surface breaking due to its assumption of nested flux surfaces. These results show that the 3D equilibrium responses in LHD equilibria become increasingly important from inward- to outward-shifted configurations, mainly through Pfirsch-Schlüter current-driven perturbations of the MAGNETic field and the resulting edge stochasticity.

[abstract 43 / 49] (score: 2)
arXiv:2606.10505 [pdf, ps, other]

Title: Solar flare ribbons structured by uncombed chromospheric loops

Authors: L. P. Chitta, E. R. Priest, David Orozco Suárez, Azaymi L. Siu-Tapia, Jose Carlos del Toro Iniesta, Francisco Javier Bailén, Julian Blanco Rodríguez, Alberto Álvarez-Herrero, Maria Balaguer Jiménez, Esteban Sanchis Kilders, Ignacio Torralbo, Christoph Kuckein, Sami K. Solanki, Andreas Lagg, Achim Gandorfer, Yukio Katsukawa, Pietro Bernasconi, Thomas Berkefeld, Alex Feller, Tino L. Riethmüller, Masahito Kubo, H. N. Smitha, Bianca Grauf, Michael Carpenter, Alexander Bell, Valentín Martínez Pillet, Juan Sebastián Castellanos Durán, Edvarda Harnes, Johannes Hoelken, Francisco A. Iglesias, Ryohtaroh T. Ishikawa, Yusuke Kawabata, Takuma Matsumoto, Takayoshi Oba, Hanna Strecker, Dušan Vukadinović,

Comments: Accepted for publication in the Astrophysical Journal Letters (Part of the SUNRISE III Focus Issue). Online animations available from the corresponding author

Subjects: astro-ph.SR physics.plasm-ph physics.space-ph

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

A part of the MAGNETic energy released during a flare is transported to the lower atmosphere. High-resolution observations show that flare ribbons, sites of energy deposition at the footpoints of flaring loops which appear bright in the chromosphere and transition region, are structured on small spatial scales on the order of 100 km. Based on idealized numerical models of flares it is suggested that the ribbon fine-structures could originate from a tearing instability and the development of plasmoids in current sheets. Here we report on Fe I 5250.6 Å and Mg I b2 5173 Å spectral observations of a solar flare from the Tunable Magnetograph onboard the SUNRISE III balloon-borne mission that reveal an intricate link between the flare ribbon structure and the ambient chromosphere. We identified uncombed chromospheric loops and non-flaring fine-structures that are interspersed among brighter flare ribbon threads. These loops remain stable on timescales of minutes. Spectral lines from these regions show reduced emission or self-reversal in the line core compared with the immediately adjacent flare ribbons. We discuss the potential role of these structures in the onset of a flare. Furthermore, we suggest that irrespective of the complexities in the flaring current sheet, uncombed chromospheric loops and nonflaring fine-structure might play a role in spatially modulating the flare energy deposition in the lower atmosphere.

[abstract 44 / 49] (score: 2)
arXiv:2606.10538 [pdf, ps, other]

Title: Updating the PATH framework with FRB host galaxy models

Authors: C. W. James, N. Loudas, M. Woodland, B. C. Andersen, J. X. Prochaska, J. L. Hoffmann, L. Marnoch, S. D. Ryder,

Comments: 20 pages, 13 figures, 5 Tables, accepted by PASA

Subjects: astro-ph.HE astro-ph.GA

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

Over a hundred fast radio burst (FRB) host galaxies have now been identified, enabling both comparisons of host redshift with FRB dispersion measure to study the cosmological distribution of ionised gas, and analyses of host properties in order to identify FRB progenitors. The standard method for determining the most likely FRB host galaxy in an optical image is the Bayesian framework Probabilistic Association of Transients to their Hosts (PATH), which accounts for uncertainties in the radio localisation, and simplified prior distributions on the host being observable. In this work we extend PATH, incorporating physically-motivated priors that are based on expectations about FRB host galaxy magnitudes. We develop three different models for the apparent r-band magnitude distribution based on an FRB's expected host galaxy redshift, $P(m_r|z)$ and combine these with expectations for redshift based on an FRB's dispersion measure, $P(z|DM)$. We fit the parameters of these prior models using host galaxy candidates for 32 FRBs detected by the Australian SKA Pathfinder (ASKAP) in incoherent sum (ICS) mode by the Commensal Real-time ASKAP Fast Transients (CRAFT) survey. Employing PATH with the new priors on the host magnitudes, we find increased confidence in the most probable hosts of all ASKAP ICS FRB host galaxies. All three models predict similar distributions of FRB host magnitudes at low redshift $(z \sim 0.1)$, and we confirm previous results that the true FRB host galaxy distribution is fainter than expected for a star-formation-weighted distribution (p-value of 0.12%). However, a mass-weighted distribution provides an even worse fit (p-value of $10^{-9}$). Tests against more FRBs in the $z > 0.5$ range, where the models differ, and extensions of the models to account for e.g. host metallicity, may help to resolve these uncertainties in the FRB host distribution.

[abstract 45 / 49] (score: 2)
arXiv:2606.10561 [pdf, ps, other]

Title: MeV-GeV Gamma-Ray Astrophysics in the Multimessenger Era

Authors: Alessandro De Angelis,

Comments:

Subjects: physics.gen-ph

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

Gamma-ray astrophysics probes the most extreme particle accelerators and explosive transients in the Universe. From pioneering theoretical predictions in the 1950s and the first space-borne detections in the 1960s, mostly exploring the sub-MeV region, the field has evolved into a mature, multi-decade enterprise that spans nine orders of magnitude in photon energy up to PeV energies and interfaces naturally with neutrino and gravitational-wave astronomy. Yet the energy range from a few hundred keV to a few GeV -- the "MeV gap", constraining progress on nucleosynthesis, positron annihilation, transient physics, dark-matter signatures, and electroMAGNETic counterparts to high-energy neutrinos and gravitational waves - remains sensitivity-limited. In this paper, we survey the scientific motivations for gamma-ray astrophysics, sketch a concise history from the first ideas to key milestones in space- and ground- based gamma-ray astronomy, and discuss programmatic attempts to close the MeV gap.

[abstract 46 / 49] (score: 2)
arXiv:2606.10566 [pdf, ps, other]

Title: Discovery of EP J175257.3-351923 as a Candidate Black Hole Low-Mass X-ray Binary

Authors: G. L. Huang, Q. C. Zhao, L. Tao, A. Coleiro, A. Rau, S. Brennan, C . Y. Dai, R. Soria, F. Cangemi, F. Coti Zelati, A. Marino, L. Zhang, S. Guillot, H. Q. Cheng, H. Feng, D. Götz, Y. Huang, Y. F. Huang, D. Y. Li, Z. S. Li, P. Maggi, R. C. Ma, X. Ma, H. W. Pan, N. Rea, J. Wang, Q. Y. Wu, L. P. Xin, W. M. Yuan, Z. H. Yao, G. B. Zhang, W. D. Zhang, S. N. Zhang,

Comments: Submitted to A&A Letters on April 8, 2026

Subjects: astro-ph.HE

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

We report the discovery of a new X-ray transient, EP~J175257.3--351923 (EP250916a), by the \textit{Einstein Probe} (EP) near the Galactic plane. The outburst lasted for at least $\gtrsim 40$~days, reached a peak 2--10 keV flux of $\sim 4 \times 10^{-10}$~erg~cm$^{-2}$~s$^{-1}$, and exhibited a fast-rise, exponential-decay (FRED) profile typical of X-ray binary outbursts. The source remained in the hard state throughout the outburst, with only modest variations in the photon index ($\sim 1.6$--$2.2$) and no evidence for a spectral state transition. Broadband spectral modeling suggests a truncated disk, a weak reflection component, and a high-energy cutoff at $\sim 217$~keV, consistent with hard-state accretion in black-hole systems. No reliable optical counterpart is detected within the SWIFT/XRT error circle in SVOM/VT, SWIFT/UVOT and GROND observations, and the inferred X-ray-to-optical flux ratio, $ξ\gtrsim 21.75$, is consistent with a low-mass companion. No pulsations or significant aperiodic variability are detected. Although the compact object cannot yet be firmly identified, the timing, spectral, and optical evidence favors EP~J175257.3--351923 as a black-hole low-mass X-ray binary candidate, highlighting EP's potential to uncover a faint, previously hidden population of X-ray binaries.

[abstract 47 / 49] (score: 2)
arXiv:2606.10739 [pdf, ps, other]

Title: Potential detection of ~ 4.2 keV emission line from GRS 1747-312

Authors: Amom Lanchenbi Chanu, Akash Garg, Ranjeev Misra, A. Senorita Devi,

Comments:

Subjects: astro-ph.HE

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

We present a broadband spectral analysis of the neutron star LMXB GRS 1747-312 using $\sim 40$ ks AstroSat data. The source was observed during the decay phase of the 2017 outburst, with an absorbed 1.0--5.5 keV flux of $1.67^{+0.04}*{-0.07} \times 10^{-11}$ erg s$^{-1}$ cm$^{-2}$, corresponding to a luminosity of $\sim (0.9-1.80) \times 10^{35}$ erg s$^{-1}$. The continuum is modeled with thermal Comptonization of blackbody emission and interstellar absorption. A mildly broad iron line at $\sim 6.4$ keV is fitted with a disc reflection component. Narrow lines below 2 keV are described by a hot plasma using the XSPEC model APEC. Additionally, there is a potential detection of an emission line at $4.19^{+0.12}*{-0.10}$ keV with width $σ= 0.2 \pm 0.2~\mathrm{keV}$ and line flux = $13^{+10}*{-9} \times 10^{-5}$ erg s$^{-1}$ cm$^{-2}$. Examination of several short duration ($\sim$ few kiloseconds) SWIFT observations at few times the AstroSat source flux, provided upper limits to the line flux $< 30 \times 10^{-5}$ erg s$^{-1}$ cm$^{-2}$. The 4.2 keV line likely originates from reflection off the neutron star surface. Shifting the neutral Fe $K*α$ line from its rest energy of 6.4 to 4.2 keV requires a redshift of $z \sim 0.6$, consistent with that expected from the surface of a non-spinning $1.4 M_\odot$, 10 km radius neutron star. If confirmed, this feature provides a potential direct measurement of gravitational redshift, allowing us to place strong constraints on the neutron star's mass-to-radius ratio and gain valuable insights into the equation of state (EOS) of dense matter.

[abstract 48 / 49] (score: 2)
arXiv:2606.10863 [pdf, ps, other]

Title: Isochrones in primordial MAGNETic field evolution

Authors: Axel Brandenburg, Mattia Cielo, Oksana Iarygina, Franco Vazza,

Comments: 11 pages, 14 figures, 2 tables, submitted to A&A

Subjects: astro-ph.CO

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

During the radiation-dominated era of the Universe, a primordial MAGNETic field undergoes a turbulent decay while its length scale increases due to an inverse cascade. At later times, the size of the largest processed eddy scales with the Alfvén speed and it describes an isochrone that moves toward larger scales with increasing time. Different MAGNETogenesis mechanisms produce different initial length scales and field strengths, independently of the nominal generation time. However, we show that for any initial field, a proper time can be determined such that the isochrones at early times are parallel to those at late times. We use two-dimensional numerical simulations of decaying MHD turbulence and vary the initial position of the peak of the MAGNETic energy spectrum. In this case, the evolution is governed by the conservation of anastrophy. A fit to the Alfvén time yields an accurate estimate of the factor by which the decay time is longer than the Alfvén time, while the offset in the fit provides an additional estimate of the proper time that needs to be added to the nominal time since the beginning of each simulation. We also find that the presence of an initial velocity field of realistic strength helps producing a more straight track. The MAGNETic field parameters lie on universal isochrones even for early times.

[abstract 49 / 49] (score: 2)
arXiv:2606.11089 [pdf, ps, other]

Title: MusE GAs FLOw and Wind (MEGAFLOW) XIV: Background-Galaxy Absorption Reveals Kiloparsec-Scale Structure in the Cool Circumgalactic Medium

Authors: Yucheng Guo, Nicolas F. Bouché, Martin Wendt, Timothy Heckman, Joop Schaye, Sanchayeeta Borthakur, Johannes Zabl, Maxime Cherrey, Sowgat Muzahid, Ismael Pessa, Ramona Augustin, Daria Kozlova,

Comments: Submitted to A&A

Subjects: astro-ph.GA

Created: 2026-06-09; Updated: 2026-06-10; Datestamp: 2026-06-10

The properties of the cool ($T\sim10^4$~K) gas in the circumgalactic medium (CGM) are closely linked to the physical mechanisms that create and maintain this multiphase medium. The cool CGM is thought to consist of discrete clouds, whose characteristic size is unknown. Here we present a geometric and direct approach to constrain the coherence scale of these cool structures using stacked MgII absorption lines measured against extended background galaxies and effectively point-like background QUASARs, whose sizes are a few kpc and $\lesssim$ 0.01 pc, respectively. When the background-source size is smaller than the coherence scale of the foreground clouds, incomplete covering lowers the detection fraction and causes the median stacked absorption to differ from the mean. For stacked MgII absorption against background galaxies, the mean and median equivalent width (EW) profiles are broadly consistent. For stacked MgII absorption against background QUASARs, by contrast, the median and mean EW profiles differ significantly, and more so as the impact parameter increases beyond 100 kpc. Furthermore, we find a tentative trend that the median and mean EW profiles are broadly consistent for large background galaxies (median half-light radius $\approx 6.6$ kpc), but differ for small background galaxies ($\approx 1.5$ kpc). This indicates that MgII clouds have a coherence length of $\sim$2-7~kpc. Using a toy model in which the CGM is populated with discrete cool clouds, we show that the observed differences arise naturally from the combination of partial covering and beam averaging. Our results provide a new geometry-based measure of the small-scale structure of cool CGM gas.