Showing 1–50 of 203 results for author: Vereš, P

AT2025agpz in Rubin commissioning data: distinguishing a luminous interacting supernova from nuclear transients in compact galaxies

Authors: C. R. Angus, M. Quilt, H. F. Stevance, M. Nicholl, S. J. Smartt, P. Wiseman, A. Möller, C. T. Murphey, P. J. Pessi, K. Auchettl, M. Dennefeld, M. Dominik, C. Frohmaier, P. Francis, M. Gromadzki, A. Lawrence, G. Leloudas, C. Lidman, D. Magill, I. Mandel, B. Martin, S. Mattila, G. Narayan, F. Onori, S. R. Oates , et al. (15 additional authors not shown)

Abstract: The Vera C. Rubin Observatory's Legacy Survey of Space and Time will discover unprecedented numbers of rare, long-lived optical transients, many of which will be too faint or too numerous for comprehensive spectroscopic follow-up. Characterising objects that span the boundaries between established transient classes is therefore essential for improving photometric classification. We present AT2025a… ▽ More The Vera C. Rubin Observatory's Legacy Survey of Space and Time will discover unprecedented numbers of rare, long-lived optical transients, many of which will be too faint or too numerous for comprehensive spectroscopic follow-up. Characterising objects that span the boundaries between established transient classes is therefore essential for improving photometric classification. We present AT2025agpz, a luminous transient at $z=0.147$, discovered around peak by ATLAS but extensively monitored during Rubin commissioning observations of the Euclid Deep Field South. The transient is coincident with the nucleus of a faint dwarf galaxy, exhibits a rest-frame rise time of $77.9\pm1.3$ d, and reaches a peak bolometric luminosity of $6.3\times10^{43}$ erg s$^{-1}$. The exceptional depth and cadence of the Rubin commissioning data, combined with complementary DECam imaging, tightly constrain the explosion epoch and yield an early-time power-law rise of $n=3.33^{+0.33}_{-0.28}$. Follow-up spectroscopy reveals remarkably slow spectral evolution dominated by narrow Balmer emission, while high-resolution X-shooter observations resolve broad electron-scattering wings and multiple H$α$ emission components characteristic of interaction-powered supernovae. Spectral energy distribution modelling indicates a low-mass, moderately star-forming host galaxy. Although AT2025agpz occupies observational parameter space shared by the recently identified Ambiguous Nuclear Transient population, its colour evolution, host environment, and emission-line morphology favour an interaction-powered luminous supernova. More broadly, this event highlights the growing observational overlap between luminous interacting supernovae and nuclear transients, illustrating both the challenges and opportunities for transient classification in the Rubin era. △ Less

Submitted 5 August, 2026; originally announced August 2026.

Comments: 14 pages, 10 figures, submitted to MNRAS

Can We Find the Emission Mechanism Behind the Extremely Bright GRB 230812B?

Authors: Utkarsh Pathak, Sameer K. Patil, Hitesh Tanenia, Yashowardhan Rai, Viswajeet Swain, Anuraag Arya, Gaurav Waratkar, Anirudh Salgundi, Mehul Goyal, Varun Bhalerao, Igor Andreoni, Sarah Antier, G. C. Anupama, Sudhanshu Barway, Dipankar Bhattacharya, Tanmoy Chattopadhyay, Michael Coughlin, Anirban Dutta, Christoffer Fremling, Nidhal Guessoum, Mansi Kasliwal, Oliver J. Roberts, Gokul P. Srinivasaragavan, Rishabh Singh Teja, Santosh Vadawale , et al. (1 additional authors not shown)

Abstract: GRB 230812B is a bright long-duration GRB with a luminous, long-lived afterglow and an AstroSat/CZTI polarization measurement during the prompt phase, enabling a joint study of its prompt spectral evolution, polarization, and broadband afterglow. Time-resolved spectroscopy of the prompt emission shows that during the rising phase, the low-energy Band-function index exceeds the synchrotron line of… ▽ More GRB 230812B is a bright long-duration GRB with a luminous, long-lived afterglow and an AstroSat/CZTI polarization measurement during the prompt phase, enabling a joint study of its prompt spectral evolution, polarization, and broadband afterglow. Time-resolved spectroscopy of the prompt emission shows that during the rising phase, the low-energy Band-function index exceeds the synchrotron line of death, favoring the presence of an additional thermal component. At later times, from $T_0+2$ s to $T_0+32$ s, the prompt spectra are consistent with predominantly non-thermal emission. Polarization analysis of the prompt emission in the $300$-$600$ keV band yields a marginal lower limit on the polarization fraction of $Π\gtrsim 50\%$ at the $1σ$ level. The long X-ray monitoring of the afterglow shows no jet break over the observed baseline. Multiwavelength afterglow modeling favors a wide jet with an inferred half-opening angle of $θ_j = 15^{+6}_{-4}$ degrees observed close to the jet axis with a viewing angle of $θ_v = 0.9^{+1.8}_{-0.6}$ degrees. The inferred circumburst density is low, $n_0 = 1.2^{+0.3}_{-0.1}\times10^{-4}\,\textrm{cm}^{-3}$, and the isotropic-equivalent kinetic energy of the jet is $E_{{\rm k}, iso} = 4.0^{+1.5}_{-0.8} \times 10^{53}$ erg. Taken together, the prompt spectral evolution favors an early phase with a thermal contribution followed by a later phase dominated by non-thermal emission. The polarization constraint in the late prompt phase is consistent with synchrotron emission, although a higher-significance polarization measurement will be required to robustly constrain the magnetic-field geometry and the relative contribution of photospheric emission. △ Less

Submitted 20 July, 2026; originally announced July 2026.

Comments: 16 pages, 7 figures, 3 Tables. Submitted to ApJ

GRB 260310A / SN 2026fgk: A Multi-Wavelength Study of a Nearby Underluminous Long GRB and SN with a Complex Afterglow

Authors: Ramandeep Gill, Rosa L. Becerra, Antonio de Ugarte Postigo, Christina C. Thöne, Alan M. Watson, Noémie Globus, Jean-Grégoire Ducoin, Peter Veres, Stanley E. Kurtz, Asuka Kuwata, Antonio Martín-Carrillo, Luca Izzo, Christophe Adami, Enrique Moreno Méndez, Nikos Mandarakas, Camila Angulo-Valdez, Stéphane Basa, William H. Lee, Edilberto Aguilar-Ruiz, Dalya Akl, Margo F. Aller, Miguel Ángel Aloy, Jie An, Sarah Antier, Jean-Luc Atteia , et al. (32 additional authors not shown)

Abstract: We present a comprehensive multi-wavelength study of GRB 260310A / SN 2026fgk, a nearby ($z=0.153$), long-duration gamma-ray burst (GRB) with an exceptionally underluminous prompt $γ$-ray emission and a Comptonized spectrum. The burst occurred at the edge of a blue host galaxy at a projected distance of 15 kpc, which is one of the largest offsets reported for a long GRB. The bright optical aftergl… ▽ More We present a comprehensive multi-wavelength study of GRB 260310A / SN 2026fgk, a nearby ($z=0.153$), long-duration gamma-ray burst (GRB) with an exceptionally underluminous prompt $γ$-ray emission and a Comptonized spectrum. The burst occurred at the edge of a blue host galaxy at a projected distance of 15 kpc, which is one of the largest offsets reported for a long GRB. The bright optical afterglow, with dense coverage from COLIBRÍ, likely peaked at a few to several hours post-burst, followed by a shallow decay not expected from canonical afterglow models. Both the optical and X-ray light curves show a brief chromatic plateau from $4-7$ days. We show that the subsequent rebrightening observed at $\sim20$ days is best explained by the combined contribution of the associated Type Ic-BL supernova, identified in GTC spectra, and a late-time refreshed shock. The broadband optical to X-ray spectral energy distribution is well described by synchrotron emission from the forward shock, while the radio observations demand an additional emission component. We model the afterglow using (a) an on-axis uniform jet from a dirty fireball with late-time energy injection and (b) a misaligned jet with power-law angular structure, both having material emitting along our line-of-sight (LOS) moving with an initial Lorentz factor of $Γ_0\sim20-35$. We conclude that at more typical GRB distances ($z\gtrsim0.5$) the prompt $γ$-ray emission from this source would likely have escaped detection, whereas its optical afterglow would have remained observable, making the event appear as an orphan afterglow or a gamma-ray quiet fast X-ray transient. △ Less

Submitted 18 August, 2026; v1 submitted 25 May, 2026; originally announced May 2026.

Comments: Accepted to MNRAS

Reanalysing large-scale structure using an updated gamma-ray burst spatial density approach

Authors: Istvan Horvath, Zsolt Bagoly, Jon Hakkila, Lajos G. Balazs, Janos Horvath, Sandor Pinter, Istvan I. Racz, Peter Veres, L. Viktor Toth

Abstract: In the past few decades, large universal structures have been found that challenge the homogeneity and isotropy expected in standard cosmological models. This study examines burst clustering in both galactic hemispheres using a recently developed methodology, using spheres in 3D space for testing regularities. Using our new method in both hemisphere we find only one deviation from isotropy. A smal… ▽ More In the past few decades, large universal structures have been found that challenge the homogeneity and isotropy expected in standard cosmological models. This study examines burst clustering in both galactic hemispheres using a recently developed methodology, using spheres in 3D space for testing regularities. Using our new method in both hemisphere we find only one deviation from isotropy. A small one in the Southern and a huge one in the Northern hemisphere. This itself suggests that the two deviations do not likely to come from statistical fluctuation. The northern huge group contains app. 125 gamma-ray bursts (GRBs) corresponds with the so - called Hercules-Corona Borealis Great Wall. The southern group contains 4-5 GRBs locating very close to each other. Two of them (GRB050822 and GRB050318) are close not just in redshift and the angular position but they are very close in observing time (5 months). We concluded that the third important result of this work that this method could not find other overdensity deviation from homogeneity in the GRBs spatial distribution. We have shown that the large-scale density increase in the spatial distribution of gamma-ray bursts does not necessarily violate the cosmological principle. △ Less

Submitted 29 April, 2026; v1 submitted 15 April, 2026; originally announced April 2026.

Comments: accepted for publication

Journal ref: Monthly Notices of the Royal Astronomical Society, Volume 548, Issue 3, id.stag666, 7 pp. May 2026

Bayesian parameter study of the Seyfert-starburst composite galaxies NGC 1068 and NGC 7469

Authors: Björn Eichmann, Silvia Salvatore, Santiago del Palacio, Giacomo Sommani, Crystal Mele, Patrik M. Veres, Julia Becker Tjus

Abstract: Multimessenger observation of the Seyfert-starburst composite galaxies NGC 1068 and NGC 7469 indicate a characteristic feature in the radio band (the so-called mm-bump) as well as indication of high-energy neutrinos by the AGN corona. Moreover, also the starburst ring of these sources is bright in the radio and hence, a potential source of $γ$-rays and neutrinos. We aim to explain the non-therma… ▽ More Multimessenger observation of the Seyfert-starburst composite galaxies NGC 1068 and NGC 7469 indicate a characteristic feature in the radio band (the so-called mm-bump) as well as indication of high-energy neutrinos by the AGN corona. Moreover, also the starburst ring of these sources is bright in the radio and hence, a potential source of $γ$-rays and neutrinos. We aim to explain the non-thermal features of these two sources with our homogeneous steady-state Seyfert-starburst composite model, which we refined in this work. Hereby, we account for stochastic diffuse acceleration and energy losses within the corona and $γγ$-pair attenuation of the escaping $γ$-rays. Since the non-thermal features of Seyfert sources contribute only marginally to the electromagnetic spectrum, only few data points can be assigned to the starburst ring or the AGN corona. Hence, prior information on the physical parameters is incorporated within a Markov Chain Monte Carlo approach to avoid overfitting. Based on this Bayesian parameter study we show, that the non-thermal features of NGC 1068 can be explained well. Still a more detailed treatment of the spatial inhomogeneities in the central region of the AGN could further improve the fit results. This manifests itself even more clearly in the case of NGC 7469, where the mm-bump needs to emerge from a coronal size $R_{\rm c}>100\,\mathcal{R}_{\rm s}$, whereas (TeV-PeV)-neutrino emission requires $R_{\rm c}< 10\,\mathcal{R}_{\rm s}$. Similar to what has previously been shown in other wavebands, our analysis highlights that the spatial extension of the so-called AGN corona depends the considered energy of the messenger. Hence, it seems that there is not a unique edge of the corona and a substantial progress in the understanding of these phenomena is expected if future analysis account for these spatial inhomogeneities. △ Less

Submitted 17 February, 2026; originally announced February 2026.

Precursors in tidal disruption events: repeating, fast, and AGN-hosted TDEs

Authors: Patrik Milán Veres

Abstract: Context. Tidal disruption events (TDEs) are rare transients that provide important insights into the physics of galactic nuclei. A recently identified feature in their optical light curves is the presence of early bump-like structures (precursors) that appear before the onset of the main flare or during its rise. Aims. We aim to build and study the first sample of precursor TDEs in order to improv… ▽ More Context. Tidal disruption events (TDEs) are rare transients that provide important insights into the physics of galactic nuclei. A recently identified feature in their optical light curves is the presence of early bump-like structures (precursors) that appear before the onset of the main flare or during its rise. Aims. We aim to build and study the first sample of precursor TDEs in order to improve our understanding of these features, which could be key to revealing the origin of the optical emission in TDEs. Methods. We compiled all known precursor TDEs from the literature, searched for additional candidates, and analyzed them as a sample. Results. We find that precursor TDEs predominantly fall within the repeating TDE, fast TDE, and TDE in active galactic nucleus (AGN) subclasses. We reveal a positive correlation between the occurrence time of the precursors relative to the main peak and the central black hole mass. Conclusions. We suggest that the precursors appear due to interactions between the incoming stellar debris and the disk or leftover material from an earlier disruption (repeating and fast TDEs) or a stable pre-existing disk (TDEs in AGNs). Precursors are therefore potentially key signatures of repeating partial TDEs in previously quiescent galaxies. △ Less

Submitted 23 February, 2026; v1 submitted 12 February, 2026; originally announced February 2026.

Comments: Accepted for publication in A&A Letters. No changes to v_1

Journal ref: A&A 707, L19 (2026)

Astrometric follow-up of near-Earth asteroid 2024 YR4 during a Torino scale level 3 alert

Authors: Marco Micheli, Maxime Devogèle, Larry Denneau, Eileen V. Ryan, William H. Ryan, Petr Pravec, Kamil Hornoch, Hana Kučáková, Petr Fatka, Melissa J. Brucker, Cassandra Lejoly, Nicholas Moskovitz, Mikael Granvik, Zuri Gray, Grigori Fedorets, Anlaug Amanda Djupvik, Carson Fuls, David Rankin, Kacper Wierzchoś, Bill Gray, Tim Lister, Richard J. Wainscoat, Robert Weryk, Olivier R. Hainaut, Federica Spoto , et al. (16 additional authors not shown)

Abstract: The discovery of 2024 YR4 presented the planetary defense community with the most significant impact threat in almost two decades, reaching level 3 on the Torino scale. The community, now mature and well-organized, responded with a global observational effort. Astrometric measurements, forming the basis for orbital refinement and impact prediction, were a central component of this response. In thi… ▽ More The discovery of 2024 YR4 presented the planetary defense community with the most significant impact threat in almost two decades, reaching level 3 on the Torino scale. The community, now mature and well-organized, responded with a global observational effort. Astrometric measurements, forming the basis for orbital refinement and impact prediction, were a central component of this response. In this paper, we present the astrometric data collected by the international community, from the time of discovery until the object became too faint for all existing observational assets, including JWST. We also discuss the coordination role played by the International Asteroid Warning Network, and the importance of publicly available image archives to enable precovery searches. △ Less

Submitted 6 February, 2026; originally announced February 2026.

Journal ref: J Astronaut Sci 73, 8 (2026)

Fastest or Significant: A Systematic Framework for Validating Global Minimum Variability Timescale Measurements of Gamma-ray Bursts

Authors: S. Bala, P. Veres, A. Goldstein, R. Sonawane, R. Samanta, S. Iyyani

Abstract: The minimum variability timescale (MVT) is a key observable used to probe the central engines of Gamma-Ray Bursts (GRBs) by constraining the emission region size and the outflow Lorentz factor. However, its interpretation is often ambiguous: statistical noise and analysis choices can bias measurements, making it difficult to distinguish genuine source variability from artifacts. Here we perform a… ▽ More The minimum variability timescale (MVT) is a key observable used to probe the central engines of Gamma-Ray Bursts (GRBs) by constraining the emission region size and the outflow Lorentz factor. However, its interpretation is often ambiguous: statistical noise and analysis choices can bias measurements, making it difficult to distinguish genuine source variability from artifacts. Here we perform a comprehensive suite of simulations to establish a quantitative framework for validating Haar-based MVT measurements. We show that in multi--component light curves, the MVT returns the most statistically significant structure in the interval, which is not necessarily the fastest intrinsic timescale, and can therefore converge to intermediate values. Reliability is found to depend jointly on the MVT value and its signal-to-noise ratio ($\mathrm{SNR}_{\mathrm{MVT}}$), with shorter intrinsic timescales requiring proportionally higher $\mathrm{SNR}_{\mathrm{MVT}}$ to be resolved. We use this relation to define an empirical MVT Validation Curve, and provide a practical workflow to classify measurements as robust detections or upper limits. Applying this procedure to a sample of Fermi-GBM bursts shows that several published MVT values are better interpreted as upper limits. These results provide a path toward standardizing MVT analyses and highlight the caution required when inferring physical constraints from a single MVT measurement in complex events. △ Less

Submitted 11 February, 2026; v1 submitted 18 December, 2025; originally announced December 2025.

Comments: Accepted in ApJ

Constraints on the intergalactic magnetic field from Fermi-LAT observations of GRB 221009A

Authors: Lea Burmeister, Paolo Da Vela, Francesco Longo, Guillem Marti-Devesa, Manuel Meyer, Francesco Saturni, Antonio Stamerra, Peter Veres

Abstract: A cosmological origin of the magnetic fields in large scale structures of the Universe would require a non-negligible magnetic field in cosmic voids, which, however, remains undetected. Gamma-ray emission from gamma-ray bursts (GRBs) offers the opportunity to indirectly probe such an intergalactic magnetic field (IGMF), as gamma rays interact with cosmic radiation fields, producing electron-positr… ▽ More A cosmological origin of the magnetic fields in large scale structures of the Universe would require a non-negligible magnetic field in cosmic voids, which, however, remains undetected. Gamma-ray emission from gamma-ray bursts (GRBs) offers the opportunity to indirectly probe such an intergalactic magnetic field (IGMF), as gamma rays interact with cosmic radiation fields, producing electron-positron pairs, and initiate an electromagnetic cascade. The deflection of the pairs in the IGMF results in a time-delayed signal at GeV energies. Using observations with the Fermi Large Area Telescope of the GRB 221009A, we are able to derive the most stringent constraints to date from the non-observation of the cascade and rule out magnetic fields B < 2.5 x 10^{-17} G at 95% confidence level for a coherence length larger than 1 Mpc. Our results are comparable to limits obtained from blazar observations but do not suffer from assumptions on the duty cycle of the gamma-ray source or whether inverse-Compton scattering losses dominate over the development of plasma instabilities. △ Less

Submitted 23 February, 2026; v1 submitted 11 December, 2025; originally announced December 2025.

Comments: Published in PRD. 14 pages, 9 figures, 2 tables

Hidden No More: Spotlight on tidal disruption events in active galactic nuclei

Authors: Patrik Milán Veres

Abstract: Tidal disruption events (TDEs) are typically discovered in previously quiescent galaxies. However, earlier studies have revealed a handful of TDEs occurring in pre-existing active galactic nuclei (AGNs). We discuss AT2019aalc, a promising TDE candidate in an AGN, and compare it to similar sources. We also explore Bowen fluorescence flares, a newly identified class of flaring supermassive black hol… ▽ More Tidal disruption events (TDEs) are typically discovered in previously quiescent galaxies. However, earlier studies have revealed a handful of TDEs occurring in pre-existing active galactic nuclei (AGNs). We discuss AT2019aalc, a promising TDE candidate in an AGN, and compare it to similar sources. We also explore Bowen fluorescence flares, a newly identified class of flaring supermassive black holes, as potential members of the TDE in AGN transient class. We aim to connect the observed properties of these flares with the expectations of TDE-in-AGN simulations. △ Less

Submitted 11 December, 2025; originally announced December 2025.

Comments: Proceedings of "X-ray Quasi-Periodic Eruptions and Repeating Nuclear Transients", 16-19 June 2025, ESAC, Madrid. Submitted to Astronomische Nachrichten

An Extremely Luminous Flare Recorded from a Supermassive Black Hole

Authors: Matthew J. Graham, Barry McKernan, K. E. Saavik Ford, Daniel Stern, Matteo Cantiello, Andrew J. Drake, Yuanze Ding, Mansi Kasliwal, Mike Koss, Raffaella Margutti, Sam Rose, Jean Somalwar, Phil Wiseman, S. G. Djorgovski, Patrik M. Veres, Eric C. Bellm, Tracy X. Chen, Steven L. Groom, Shrinivas R. Kulkarni, Ashish Mahabal

Abstract: Since their discovery more than 60 years ago, accreting supermassive black holes in active galactic nuclei (AGN) were recognized as highly variable sources, requiring an extremely compact, dynamic environment. Their variability traces to multiple phenomena, including changing accretion rates, temperature changes, foreground absorbers, and structural changes to the accretion disk. Spurred by a new… ▽ More Since their discovery more than 60 years ago, accreting supermassive black holes in active galactic nuclei (AGN) were recognized as highly variable sources, requiring an extremely compact, dynamic environment. Their variability traces to multiple phenomena, including changing accretion rates, temperature changes, foreground absorbers, and structural changes to the accretion disk. Spurred by a new generation of time-domain surveys, the extremes of black hole variability are now being probed. We report the discovery of an extreme flare by the AGN J224554.84+374326.5, which brightened by more than a factor of 40 in 2018. The source has slowly faded since then. The total emitted UV/optical energy to date is $\sim10^{54}$ erg, i.e., the complete conversion of approximately one solar mass into electromagnetic radiation. This flare is 30 times more powerful than the previous most powerful AGN transient. Very few physical events in the Universe can liberate this much electromagnetic energy. We discuss potential mechanisms, including the tidal disruption of a high mass $(>30\, M_\odot)$ star, gravitational lensing of an AGN flare or supernova, or a supermassive (pair instability) supernova in the accretion disk of an AGN. We favor the tidal disruption of a massive star in a prograde orbit in an AGN disk. △ Less

Submitted 3 November, 2025; originally announced November 2025.

Comments: 41 pages, 12 figures, accepted by Nature Astronomy

Late-afterglow Emission from a Quasi-spherical Outflow in a stratified environment

Authors: Nissim Fraija, Boris Betancourt-Kamenetskaia, Antonio Galván, Alvaro Montalvo, A. C. Caligula Do E. S. Pedreira, Peter Veres, Rosa Leticia Becerra, Maria G. Dainotti, Simone Dichiara, Hermes León Vargas

Abstract: Gamma-ray bursts (GRBs) are cosmic events occurring at large distances beyond our galaxy. They provide a unique opportunity to study electromagnetic patterns not seen elsewhere. When the collimated GRB outflow interacts with the outer layers of a star or the wind generated by a binary neutron star merger, it releases energy, forming a quasi-spherical outflow around it. This broad outflow begins to… ▽ More Gamma-ray bursts (GRBs) are cosmic events occurring at large distances beyond our galaxy. They provide a unique opportunity to study electromagnetic patterns not seen elsewhere. When the collimated GRB outflow interacts with the outer layers of a star or the wind generated by a binary neutron star merger, it releases energy, forming a quasi-spherical outflow around it. This broad outflow begins to radiate once it has transferred enough energy to the surrounding medium. We have developed a new analytical model that describes the synchrotron afterglow scenario of the quasi-spherical outflow, including factors such as stratified density, self-absorption regime, and the fraction of electrons accelerated by the shock front. We also successfully describe the multiwavelength observations of a sample of llGRB afterglows (GRB 980425, 031203, 060218, 100316D, 130603B, 150101B and 171205A) that exhibited a late component, analyzed in both stellar wind and constant-density environments. Our analysis shows that a constant-density environment is favored. Additionally, we consider the multiwavelength upper limits of the short bursts reported in the Swift-BAT database. △ Less

Submitted 30 September, 2025; originally announced October 2025.

Comments: 26 pages, 9 figures, 5 tables, Accepted in MNRAS

GRB 250702B: Discovery of a Gamma-Ray Burst from a Black Hole Falling into a Star

Authors: Eliza Neights, Eric Burns, Chris L. Fryer, Dmitry Svinkin, Suman Bala, Rachel Hamburg, Ramandeep Gill, Michela Negro, Megan Masterson, James DeLaunay, David J. Lawrence, Sophie E. D. Abrahams, Yuta Kawakubo, Paz Beniamini, Christian Aa. Diget, Dmitry Frederiks, John Goldsten, Adam Goldstein, Alexander D. Hall-Smith, Erin Kara, Alison M. Laird, Gavin P. Lamb, Oliver J. Roberts, Ryan Seeb, V. Ashley Villar , et al. (30 additional authors not shown)

Abstract: Gamma-ray bursts are the most luminous electromagnetic events in the universe. Their prompt gamma-ray emission has typical durations between a fraction of a second and several minutes. A rare subset of these events have durations in excess of a thousand seconds, referred to as ultra-long gamma-ray bursts. Here, we report the discovery of the longest gamma-ray burst ever seen with a ~25,000 s gamma… ▽ More Gamma-ray bursts are the most luminous electromagnetic events in the universe. Their prompt gamma-ray emission has typical durations between a fraction of a second and several minutes. A rare subset of these events have durations in excess of a thousand seconds, referred to as ultra-long gamma-ray bursts. Here, we report the discovery of the longest gamma-ray burst ever seen with a ~25,000 s gamma-ray duration, GRB 250702B, and characterize this event using data from four instruments in the InterPlanetary Network and the Monitor of All-sky X-ray Image. We find a hard spectrum, subsecond variability, and high total energy, which are only known to arise from ultrarelativistic jets powered by a rapidly-spinning stellar-mass central engine. These properties and the extreme duration are together incompatible with all confirmed gamma-ray burst progenitors and nearly all models in the literature. This burst is naturally explained with the helium merger model, where a field binary ends when a black hole falls into a stripped star and proceeds to consume and explode it from within. Under this paradigm, GRB 250702B adds to the growing evidence that helium stars expand and that some ultra-long GRBs have similar evolutionary pathways as collapsars, stellar-mass gravitational wave sources, and potentially rare types of supernovae. △ Less

Submitted 26 September, 2025; originally announced September 2025.

Comments: Will submit to MNRAS

Journal ref: Mon Not R Astron Soc (2025)

Upper Limit on the Non-Gravitational Acceleration and Lower Limits on the Nucleus Mass and Diameter of 3I/ATLAS

Authors: Richard Cloete, Abraham Loeb, Peter Vereš

Abstract: We use astrometric data on 3I/ATLAS compiled by the Minor Planet Center from May 15 to September 23, 2025, and derive an upper limit on any statistically significant deviation from the best-fit gravity-based trajectory. The residuals imply that the non-gravitational acceleration is smaller than $\sim 3 \times 10^{-10}\,{\rm au\,d^{-2}}$. Based on the total mass-loss rate and outflow speed inferred… ▽ More We use astrometric data on 3I/ATLAS compiled by the Minor Planet Center from May 15 to September 23, 2025, and derive an upper limit on any statistically significant deviation from the best-fit gravity-based trajectory. The residuals imply that the non-gravitational acceleration is smaller than $\sim 3 \times 10^{-10}\,{\rm au\,d^{-2}}$. Based on the total mass-loss rate and outflow speed inferred from JWST data on August 6, 2025, we derive lower limits on the mass and diameter of 3I/ATLAS of $3.3 \times 10^{16}\,{\rm g}$ and $5\,{\rm km}$, respectively. △ Less

Submitted 24 September, 2025; originally announced September 2025.

Monte Carlo parameter study for Seyfert AGN-starburst composite galaxies NGC1068 and NGC7469

Authors: Silvia Salvatore, Björn Eichmann, Giacomo Sommani, Santiago del Palacio, Patrik M. Veres, Julia Becker Tjus

Abstract: Seyfert-starburst composite galaxies host two promising phenomena of non-thermal high-energy radiation. In this regard the IceCube observation of high-energy neutrinos from the direction of the Seyfert-starburst composite galaxy NGC 1068 is not surprising. More recently, another Seyfert-starburst composite galaxy, NGC 7469, has shown hints for neutrino emission at even higher energies. Theoretical… ▽ More Seyfert-starburst composite galaxies host two promising phenomena of non-thermal high-energy radiation. In this regard the IceCube observation of high-energy neutrinos from the direction of the Seyfert-starburst composite galaxy NGC 1068 is not surprising. More recently, another Seyfert-starburst composite galaxy, NGC 7469, has shown hints for neutrino emission at even higher energies. Theoretical investigations could clarify that their so-called AGN corona is the most-likely origin of these neutrinos due to the need of being partially $γ$-ray opaque. In this work, we present an updated version of our Seyfert-starburst composite model from 2022, that accounts for a proper treatment of the stochastic acceleration processes in the AGN corona and the secondary electrons and positrons from leptonic radiation processes. Moreover, we use a Markov Chain Monte Carlo (MCMC) approach to study the parameter space of these two potential high-energy neutrino sources under consideration of the given prior knowledge. In the case of NGC 1068, we can successfully explain its non-thermal observational features, where both its AGN corona and starburst ring are needed to account for the observations at high- energies. In the case of NGC 7469, the high-energy signatures can only be explained assuming a small coronal radius and the including external $γγ$-pair attenuation. In general, both sources exhibit a strong influence of the $γ$-ray opaqueness on the results, highlighting the need for an accurate treatment of the intrinsic coronal X-ray field and the spatial extent of the $γ$-ray production site. △ Less

Submitted 22 September, 2025; originally announced September 2025.

Deciphering the Physical Origin of GRB 240825A: A Long GRB Lacking a Bright Supernova

Authors: Rahul Gupta, Judith L. Racusin, R. Sanchez-Ramirez, Y. Hu, Andrea Rossi, Maria Dolores Caballero Garcia, Pi Nuessle, Alberto J. Castro-Tirado, Samantha Oates, Pragyan P. Bordoloi, Amar Aryan, Simone Dichiara, Peter Veres, Noel Klingler, Nicola Omodei, Elisabetta Maiorano, Donggeun Tak, S. Shilling, Jose E. Adsuara, P. H. Connell, E. Fernandez Garcia, Guillermo Garcia-Segura, Ankur Ghosh, Ersin Göğüs, Francisco J. Gordillo-Vazquez , et al. (30 additional authors not shown)

Abstract: We present a comprehensive multiwavelength analysis of GRB 240825A, a bright gamma-ray burst (GRB) detected by Fermi and Swift, with a prompt duration ($T_{\rm 90}$ ~ 4 sec in 50-300 keV) near the boundary separating short and long GRBs, prompting a detailed investigation into its classification and progenitor. Using classical prompt metrics (duration, minimum variability timescale (MVT), lag, and… ▽ More We present a comprehensive multiwavelength analysis of GRB 240825A, a bright gamma-ray burst (GRB) detected by Fermi and Swift, with a prompt duration ($T_{\rm 90}$ ~ 4 sec in 50-300 keV) near the boundary separating short and long GRBs, prompting a detailed investigation into its classification and progenitor. Using classical prompt metrics (duration, minimum variability timescale (MVT), lag, and spectral hardness) and modern classification techniques (machine-learning (ML) based t-SNE, support vector machine, energy-hardness-duration, and $ε\equiv E_{γ,\mathrm{iso},52} / E_{p,z,2}^{5/3}$), we find GRB 240825A exhibits hybrid characteristics. The short MVT (13.830 $\pm$ 1.574 ms), rest-frame duration, and ML-based classification indicate a merger-like or ambiguous nature, while its energetics and position on the Amati relation favor a collapsar origin. We conducted deep optical and NIR photometric and spectroscopic late-time search for an associated supernova (SN)/kilonova (KN) and the host galaxy using 10.4 m GTC and 8.4 m binocular LBT telescopes. No bright SN (like SN 1998bw) is detected down to stringent limits (e.g., $m_r > 26.1$ mag at 17.59 days), despite a redshift of $z$ = 0.659 measured from GTC spectroscopy. Host galaxy SED modeling with Prospector indicates a massive, dusty, and star-forming galaxy-typical of collapsar GRB hosts, though with low sSFR and large offset. We compare these findings with hybrid events like GRB 211211A, GRB 230307A, GRB 200826A, including SNe-GRBs, and conclude that GRB 240825A likely originated from a massive star collapse, with the associated supernova obscured by a dusty host environment or low luminosity SN with absolute magnitude M$_{V}$ fainter than -18.0. This study emphasizes the need for multiwavelength follow-up and a multi-layered classification to determine GRB progenitors. △ Less

Submitted 31 July, 2025; originally announced August 2025.

Comments: 34 pages, 21 figures, 6 tables, submitted, Comments/Suggestions are very welcome

GRB 241105A: A test case for GRB classification and rapid r-process nucleosynthesis channels

Authors: Dimple, B. P. Gompertz, A. J. Levan, D. B. Malesani, T. Laskar, S. Bala, A. A. Chrimes, K. Heintz, L. Izzo, G. P. Lamb, D. O'Neill, J. T. Palmerio, A. Saccardi, G. E. Anderson, C. De Barra, Y. Huang, A. Kumar, H. Li, S. McBreen, O. Mukherjee, S. R. Oates, U. Pathak, Y. Qiu, O. J. Roberts, R. Sonawane , et al. (63 additional authors not shown)

Abstract: Gamma-ray bursts (GRBs) offer a powerful window to probe the progenitor systems responsible for the formation of heavy elements through the rapid neutron capture (r-) process, thanks to their exceptional luminosity, which allows them to be observed across vast cosmic distances. GRB 241105A, observed at a redshift of z = 2.681, features a short initial spike (1.5 s) and a prolonged weak emission la… ▽ More Gamma-ray bursts (GRBs) offer a powerful window to probe the progenitor systems responsible for the formation of heavy elements through the rapid neutron capture (r-) process, thanks to their exceptional luminosity, which allows them to be observed across vast cosmic distances. GRB 241105A, observed at a redshift of z = 2.681, features a short initial spike (1.5 s) and a prolonged weak emission lasting about 64 s, positioning it as a candidate for a compact binary merger and potentially marking it as the most distant merger-driven GRB observed to date. However, the emerging ambiguity in GRB classification necessitates further investigation into the burst's true nature. Prompt emission analyses, such as hardness ratio, spectral lag, and minimum variability timescales, yield mixed classifications, while machine learning-based clustering places GRB 241105A near both long-duration mergers and collapsar GRBs. We conducted observations using the James Webb Space Telescope (JWST) to search for a potential supernova counterpart. Although no conclusive evidence was found for a supernova, the host galaxy's properties derived from the JWST observations suggest active star formation with low metallicity, and a sub-kpc offset of the afterglow from the host, which appears broadly consistent with a collapsar origin. Nevertheless, a compact binary merger origin cannot be ruled out, as the burst may plausibly arise from a fast progenitor channel. This would have important implications for heavy element enrichment in the early Universe. △ Less

Submitted 15 September, 2025; v1 submitted 21 July, 2025; originally announced July 2025.

Comments: Accepted for publication in the Monthly Notices of the Royal Astronomical Society

Journal ref: Mon Not R Astron Soc (2025) 548-571

NSF-DOE Vera C. Rubin Observatory Observations of Interstellar Comet 3I/ATLAS (C/2025 N1)

Authors: Colin Orion Chandler, Pedro H. Bernardinelli, Mario Jurić, Devanshi Singh, Henry H. Hsieh, Ian Sullivan, R. Lynne Jones, Jacob A. Kurlander, Dmitrii Vavilov, Siegfried Eggl, Matthew Holman, Federica Spoto, Megan E. Schwamb, Lauren A. MacArthur, Rahil Makadia, Marco Micheli, Aren Heinze, Eric J. Christensen, Wilson Beebe, Aaron Roodman, Kian-Tat Lim, Tim Jenness, James Bosch, Brianna M. Smart, Eric Bellm , et al. (283 additional authors not shown)

Abstract: We report on the observation and measurement of astrometry, photometry, morphology, and activityof the interstellar object 3I/ATLAS, also designated C/2025 N1 (ATLAS) with the NSF-DOE Vera C. Rubin Observatory. Comet 3I/ATLAS, the third known interstellar object, was discovered on UT 2025 July 1. Rubin Observatory had coincidentally collected images of the object's region of the sky during routine… ▽ More We report on the observation and measurement of astrometry, photometry, morphology, and activityof the interstellar object 3I/ATLAS, also designated C/2025 N1 (ATLAS) with the NSF-DOE Vera C. Rubin Observatory. Comet 3I/ATLAS, the third known interstellar object, was discovered on UT 2025 July 1. Rubin Observatory had coincidentally collected images of the object's region of the sky during routine commissioning. Facilitated by Rubin's high resolution and large aperture, we successfully recovered object detections from Rubin observations spanning UT 2025 June 21 (10 days before discovery, when 3I/ATLAS was 4.5 au from the Sun) through the date of discovery, and we acquired additional images through UT 2025 July 20 as part of commissioning. We measure on-sky locations of 3I/ATLAS in Rubin ugrizy bands, with a typical precision of about 70 mas, and briefly describe the reason this is coarser than our measured static source astrometric precision of about 3 mas in Rubin images. We measure grizy magnitudes of 3I/ATLAS photometry at about 0.01 mag precision, detecting no short-term photometric variability above 0.01 mag. We derive an estimated near-nucleus dust-to-nucleus scattering cross-section ratio of eta >= 13 on UT 2025 July 2 based on Rubin photometry and an upper limit nucleus size computed from Hubble Space Telescope observations. We find Rubin colors of g - r = (0.657 +/- 0.013) mag, r - i = (0.235 +/- 0.018) mag, i - z = (0.147 +/- 0.042) mag, z - y = (0.047 +/- 0.052) mag. These data represent the earliest observations of this object by a large (>=8-meter class) telescope and illustrate the type of measurements (and discoveries) Rubin's Legacy Survey of Space and Time (LSST) will begin to provide after it begins in early 2026. △ Less

Submitted 7 April, 2026; v1 submitted 17 July, 2025; originally announced July 2025.

Comments: Collaboration between the NSF-DOE Vera C. Rubin Observatory and the LSST Solar System Science Collaboration (SSSC)

Fermi-GBM Observations of GRB 230307A: An Exceptionally Bright Long-Duration Gamma-ray Burst with an Associated Kilonova

Authors: S. Dalessi, P. Veres, C. M. Hui, S. Bala, S. Lesage, M. S. Briggs, A. Goldstein, E. Burns, C. A. Wilson-Hodge, C. Fletcher, O. J. Roberts, P. N. Bhat, E. Bissaldi, W. H. Cleveland, M. M. Giles, M. Godwin, R. Hamburg, B. A. Hristov, D. Kocevski, B. Mailyan, C. Malacaria, O. Mukherjee, L. Scotton, A. von Kienlin, J. Wood

Abstract: On March 7th, 2023 the \textit{Fermi} Gamma-ray Burst Monitor observed the second highest fluence gamma-ray burst (GRB) ever, GRB~230307A. With a duration beyond 100~s, GRB~230307A contains a multitude of rapidly-varying peaks, and was so bright it caused instrumental effects in the GBM detectors. The high fluence of this burst, (6.02 $\pm$ 0.02)$\times$10$^{-3}$ erg cm$^{-2}$, prompted rapid foll… ▽ More On March 7th, 2023 the \textit{Fermi} Gamma-ray Burst Monitor observed the second highest fluence gamma-ray burst (GRB) ever, GRB~230307A. With a duration beyond 100~s, GRB~230307A contains a multitude of rapidly-varying peaks, and was so bright it caused instrumental effects in the GBM detectors. The high fluence of this burst, (6.02 $\pm$ 0.02)$\times$10$^{-3}$ erg cm$^{-2}$, prompted rapid follow-up across the electro magnetic spectrum including the discovery of an associated kilonova. GRB~230307A is one of a few long GRBs with an associated compact merger origin. Three main temporal regions of interest are identified for fine time-resolution spectral analysis: triggering pulse, main emission, and late emission, and the parameter evolution is traced across these regions. The high flux of the burst allowed for the statistical preference of a more complex, physically-motivated model, the Double Smoothly Broken Power Law, over typical spectral fitting functions for GRBs. From this model the evolution of the parameters was found to be in accordance with those expected for synchrotron radiation in the fast-cooling regime. Additionally, it was found that the flux experiences a steep decline in late time intervals, a feature which is often attributed to high-latitude emission, which follows the dissipation episodes. Furthermore, GRB~230307A was found to have one of the highest inferred bulk Lorentz factors of $Γ= 1600$. GRB~230307A is a noteworthy burst in terms of flux alone, but additionally provides a unique insight into the possible temporal and spectral characteristics of a new long merger class of GRBs. △ Less

Submitted 16 July, 2025; originally announced July 2025.

Comments: 17 Pages, 10 figures

Optical polarization of stellar-fed active and quiescent supermassive black holes

Authors: N. Jordana-Mitjans, A. Franckowiak, E. Ramírez-Ruiz, C. G. Mundell, N. Valtonen-Mattila, R. Stein, P. Milán Veres

Abstract: Using the MOPTOP polarimeter on the 2-meter Liverpool Telescope, we conducted a monitoring campaign targeting three optically-discovered TDEs (AT2024bgz, AT2024pvu, and AT2024wsd) and two Bowen flares in AGN (AT2020afhd and AT2019aalc). The three thermal TDEs showed low intrinsic polarization levels ($ΔP \approx 0$-$6\%$) with stable polarization angles. The Bowen flares also showed variable polar… ▽ More Using the MOPTOP polarimeter on the 2-meter Liverpool Telescope, we conducted a monitoring campaign targeting three optically-discovered TDEs (AT2024bgz, AT2024pvu, and AT2024wsd) and two Bowen flares in AGN (AT2020afhd and AT2019aalc). The three thermal TDEs showed low intrinsic polarization levels ($ΔP \approx 0$-$6\%$) with stable polarization angles. The Bowen flares also showed variable polarization degree ($ ΔP \approx 0$-$8\%$), but significant polarization angle variability: AT2020afhd exhibited a $Δθ= 83 \pm 8 \,^\circ$ shift at 150 days post-optical peak, while the AT2019aalc displayed quasi-periodic swings of $Δθ\approx 40 \, ^\circ$ amplitude starting 190 days after peak brightness. The TDEs of this study are well described by models invoking rapid disk formation and reprocessed emission from optically thick outflows, whereas the Bowen flares reveal more complex reprocessing geometries, potentially consistent with TDEs occurring in AGN gas-rich environments. We find that moderate polarization is observed at later times for TDEs with low-Eddington ratios and highly extended photospheres. This implies that, as the accretion level declines, we expect more asymmetric reprocessing layers along a given viewing angle. Since the outflow density and velocity depend sensitively on the inclination angle, we expect TDEs with low-Eddington ratios and highly extended photospheres to exhibit varying levels of polarization. The polarization of AT2019aalc (Seyfert 1) hints at a clumpy, asymmetric outflow and the presence of a tilted, precessing accretion disk, while the polarization of AT2020afhd (AGN type 2) is consistent with the detection of a scattered light echo. △ Less

Submitted 8 July, 2025; originally announced July 2025.

Journal ref: A&A 704, A250 (2025)

Apache Point rapid response characterization of primitive imminent impactor 2024 RW$_1$

Authors: Carl Ingebretsen, Bryce T. Bolin, Robert Jedicke, Peter Vereš, Christine H. Chen, Carey M. Lisse, Russet McMillan, Torrie Sutherland, Amanda J. Townsend

Abstract: Imminent impactors may be detected only a few hours before their impact with Earth, providing a brief opportunity to characterize them before impact. We describe the characterization of imminent impactor 2024 RW$_1$, which was discovered by the Catalina Sky Survey on 2024 September 4 at 05:43 UTC, before it entered the atmosphere near the northern Philippines at 16:39 UTC. We observed 2024 RW$_1$… ▽ More Imminent impactors may be detected only a few hours before their impact with Earth, providing a brief opportunity to characterize them before impact. We describe the characterization of imminent impactor 2024 RW$_1$, which was discovered by the Catalina Sky Survey on 2024 September 4 at 05:43 UTC, before it entered the atmosphere near the northern Philippines at 16:39 UTC. We observed 2024 RW$_1$ with the Astrophysical Research Consortium Telescope Imaging Camera on the Apache Point Astrophysical Research Consortium's 3.5-m telescope on 2024 September 4 10:16 UTC. We obtained g, r, i, and z photometry of 2024 RW$_1$, yielding color indices of g-r = 0.47$\pm$0.04, r-i = 0.13$\pm$0.04, i-z = -0.11$\pm$0.07, and g-i = 0.60$\pm$0.04, corresponding to a spectral slope of 0.67$\pm$0.40~$\%$/100 nm. The closest match to an asteroid spectral type is with B-type asteroids from the C-complex. We detect variations in the time series photometry of the asteroid with an amplitude of $\sim$0.75, and a double-peaked rotation period of $\sim$1900 s. Assuming a visible albedo of 0.07$\pm$0.03, a density of $\sim$1500 kg/m$^3$, and a calculated absolute magnitude of 30.92$\pm$0.05, we estimate that the asteroid has a diameter of 3.3$\pm$0.7 m and a total mass of $\sim$28,000 kg. Comparing our astrometric orbital solutions to NEOMOD3, the most likely source of 2024 RW$_1$ is the 3:1 main belt mean motion resonance (77\% probability) followed by the $ν_6$ resonance (13\% probability), consistent with its organic B-type nature. △ Less

Submitted 15 September, 2025; v1 submitted 29 May, 2025; originally announced May 2025.

Comments: 12 pages, 5 figures, 1 table, submitted to AJ

Improving the discovery of near-Earth objects with machine-learning methods

Authors: Peter Vereš, Richard Cloete, Matthew J. Payne, Abraham Loeb

Abstract: We present a comprehensive analysis of the digest2 parameters for candidates of the Near-Earth Object Confirmation Page (NEOCP) that were reported between 2019 and 2024. Our study proposes methods for significantly reducing the inclusion of non-NEO objects on the NEOCP. Despite the substantial increase in near-Earth object (NEO) discoveries in recent years, only about half of the NEOCP candidates… ▽ More We present a comprehensive analysis of the digest2 parameters for candidates of the Near-Earth Object Confirmation Page (NEOCP) that were reported between 2019 and 2024. Our study proposes methods for significantly reducing the inclusion of non-NEO objects on the NEOCP. Despite the substantial increase in near-Earth object (NEO) discoveries in recent years, only about half of the NEOCP candidates are ultimately confirmed as NEOs. Therefore, much observing time is spent following up on non-NEOs. Furthermore, approximately 11% of the candidates remain unconfirmed because the follow-up observations are insufficient. These are nearly 600 cases per year. To reduce false positives and minimize wasted resources on non-NEOs, we refine the posting criteria for NEOCP based on a detailed analysis of all digest2 scores. We investigated 30 distinct digest2 parameter categories for candidates that were confirmed as NEOs and non-NEOs. From this analysis, we derived a filtering mechanism based on selected digest2 parameters that were able to exclude 20% of the non-NEOs from the NEOCP while maintaining a minimal loss of true NEOs. We also investigated the application of four machine-learning (ML) techniques, that is, the gradient-boosting machine (GBM), the random forest (RF) classifier, the stochastic gradient descent (SGD) classifier, and neural networks (NN) to classify NEOCP candidates as NEOs or non-NEOs. Based on digest2 parameters as input, our ML models achieved a precision of approximately 95% in distinguishing between NEOs and non-NEOs. Results. Combining the digest2 parameter filter with an ML-based classification model, we demonstrate a significant reduction in non-NEOs on the NEOCP that exceeds 80%, while limiting the loss of NEO discovery tracklets to 5.5%. Importantly, we show that most follow-up tracklets of initially misclassified NEOs are later correctly identified as NEOs. △ Less

Submitted 17 May, 2025; originally announced May 2025.

Comments: 13 pages, 16 figures, 11 tables

Scanning the Universe for Large-Scale Structures using Gamma-Ray Bursts

Authors: Istvan Horvath, Zsolt Bagoly, Lajos G. Balazs, Jon Hakkila, Bendeguz Koncz, Istvan I. Racz, Peter Veres, Sandor Pinter

Abstract: In the past few decades, large universal structures have been found that challenge the homogeneity and isotropy expected in standard cosmological models. The largest of these, identified as the Hercules-Corona Borealis Great Wall, was found in 2014 in the northern galactic hemisphere in the redshift range of 1.6 < z < 2.1. Subsequent studies used an increasing gamma-ray burst database to show that… ▽ More In the past few decades, large universal structures have been found that challenge the homogeneity and isotropy expected in standard cosmological models. The largest of these, identified as the Hercules-Corona Borealis Great Wall, was found in 2014 in the northern galactic hemisphere in the redshift range of 1.6 < z < 2.1. Subsequent studies used an increasing gamma-ray burst database to show that the cluster was unlikely to have been caused by statistical sampling uncertainties. This study re-examines burst clustering in the northern galactic hemisphere using a recently developed methodology. Evidence is provided that the Hercules-Corona Borealis Great Wall cluster is larger than previously thought, with members potentially spanning the redshift range of 0.33 < z < 2.43. The extension of this cluster's size does not appear to have been due to statistical variations or sampling biases. △ Less

Submitted 7 April, 2025; originally announced April 2025.

Comments: submitted

Journal ref: Universe 2025, 11(4), 121

Reprocessing the NEAT Dataset: Preliminary Results

Authors: C. R. Nugent, J. M. Bauer, O. Benitez, M. Blain, N. D'Souza, S. Garimella, M. Goldwater, Y. Kim, H. C. G. Larsen, T. Linder, K. Mackowiak, Z. McGinnis, E. Pan, C. C. Pedersen, P. Sadhwani, F. Spoto, N. J. Tan, P. Vereš, C. Xue

Abstract: We have created a new image analysis pipeline to reprocess images taken by the Near Earth Asteroid Tracking survey and have applied it to ten nights of observations. This work is the first large-scale reprocessing of images from an asteroid discovery survey in which thousands of archived images are re-calibrated, searched for minor planets, and resulting observations are reported to the Minor Plan… ▽ More We have created a new image analysis pipeline to reprocess images taken by the Near Earth Asteroid Tracking survey and have applied it to ten nights of observations. This work is the first large-scale reprocessing of images from an asteroid discovery survey in which thousands of archived images are re-calibrated, searched for minor planets, and resulting observations are reported to the Minor Planet Center. We describe the software used to extract, calibrate, and clean sources from the images, including specific techniques that accommodate the unique features of these archival images. This pipeline is able to find fainter asteroids than the original pipeline. △ Less

Submitted 25 March, 2025; originally announced March 2025.

Comments: 13 pages, 7 figures

The La Silla Schmidt Southern Survey

Authors: Adam A. Miller, Natasha S. Abrams, Greg Aldering, Shreya Anand, Charlotte R. Angus, Iair Arcavi, Charles Baltay, Franz E. Bauer, Daniel Brethauer, Joshua S. Bloom, Hemanth Bommireddy, Marcio Catelan, Ryan Chornock, Peter Clark, Thomas E. Collett, Georgios Dimitriadis, Sara Faris, Francisco Forster, Anna Franckowiak, Christopher Frohmaier, Lluıs Galbany, Renato B. Galleguillos, Ariel Goobar, Claudia P. Gutierrez, Saarah Hall , et al. (53 additional authors not shown)

Abstract: We present the La Silla Schmidt Southern Survey (LS4), a new wide-field, time-domain survey to be conducted with the 1 m ESO Schmidt telescope. The 268 megapixel LS4 camera mosaics 32 2k$\times$4k fully depleted CCDs, providing a $\sim$20 deg$^2$ field of view with $1''$ pixel$^{-1}$ resolution. The LS4 camera will have excellent performance at longer wavelengths: in a standard 45 s exposure the e… ▽ More We present the La Silla Schmidt Southern Survey (LS4), a new wide-field, time-domain survey to be conducted with the 1 m ESO Schmidt telescope. The 268 megapixel LS4 camera mosaics 32 2k$\times$4k fully depleted CCDs, providing a $\sim$20 deg$^2$ field of view with $1''$ pixel$^{-1}$ resolution. The LS4 camera will have excellent performance at longer wavelengths: in a standard 45 s exposure the expected 5$σ$ limiting magnitudes in $g$, $i$, $z$ are $\sim$21.5, $\sim$20.9, and $\sim$20.3 mag (AB), respectively. The telescope design requires a novel filter holder that fixes different bandpasses over each quadrant of the detector. Two quadrants will have $i$ band, while the other two will be $g$ and $z$ band and color information will be obtained by dithering targets across the different quadrants. The majority (90%) of the observing time will be used to conduct a public survey that monitors the extragalactic sky at both moderate (3 d) and high (1 d) cadence, as well as focused observations within the Galactic bulge and plane. Alerts from the public survey will be broadcast to the community via established alert brokers. LS4 will run concurrently with the Vera C. Rubin Observatory's Legacy Survey of Space and Time (LSST). The combination of LS4+LSST will enable detailed holistic monitoring of many nearby transients: high-cadence LS4 observations will resolve the initial rise and peak of the light curve while less-frequent but deeper observations by LSST will characterize the years before and after explosion. Here, we summarize the primary science objectives of LS4 including microlensing events in the Galaxy, extragalactic transients, the search for electromagnetic counterparts to multi-messenger events, and cosmology. △ Less

Submitted 18 March, 2025; originally announced March 2025.

Comments: (to be submitted to PASP)

Machine Learning Methods for Automated Interstellar Object Classification with LSST

Authors: Richard Cloete, Peter Vereš, Abraham Loeb

Abstract: The Legacy Survey of Space and Time, to be conducted with the Vera C. Rubin Observatory, is poised to revolutionize our understanding of the Solar System by providing an unprecedented wealth of data on various objects, including the elusive interstellar objects (ISOs). Detecting and classifying ISOs is crucial for studying the composition and diversity of materials from other planetary systems. Ho… ▽ More The Legacy Survey of Space and Time, to be conducted with the Vera C. Rubin Observatory, is poised to revolutionize our understanding of the Solar System by providing an unprecedented wealth of data on various objects, including the elusive interstellar objects (ISOs). Detecting and classifying ISOs is crucial for studying the composition and diversity of materials from other planetary systems. However, the rarity and brief observation windows of ISOs, coupled with the vast quantities of data to be generated by LSST, create significant challenges for their identification and classification. This study aims to address these challenges by exploring the application of machine learning algorithms to the automated classification of ISO tracklets in simulated LSST data. We employed various machine learning algorithms, including random forests (RFs), stochastic gradient descent (SGD), gradient boosting machines (GBMs), and neural networks (NNs), to classify ISO tracklets in simulated LSST data. We demonstrate that GBM and RF algorithms outperform SGD and NN algorithms in accurately distinguishing ISOs from other Solar System objects. RF analysis shows that many derived Digest2 values are more important than direct observables in classifying ISOs from the LSST tracklets. The GBM model achieves the highest precision, recall, and F1 score, with values of 0.9987, 0.9986, and 0.9987, respectively. These findings lay the foundation for the development of an efficient and robust automated system for ISO discovery using LSST data, paving the way for a deeper understanding of the materials and processes that shape planetary systems beyond our own. The integration of our proposed machine learning approach into the LSST data processing pipeline will optimize the survey's potential for identifying these rare and valuable objects, enabling timely follow-up observations and further characterization. △ Less

Submitted 2 December, 2024; originally announced December 2024.

Comments: 11 pages, 4 figures, 6 tables

Report number: Astronomy & Astrophysics, Volume 691, November 2024

Strong Nongravitational Accelerations and the Potential for Misidentification of Near-Earth Objects

Authors: Aster G. Taylor, Darryl Z. Seligman, Matthew J. Holman, Peter Veres, Davide Farnocchia, Nikole Lewis, Marco Micheli, Jason T. Wright

Abstract: Nongravitational accelerations in the absence of observed activity have recently been identified on NEOs, opening the question of the prevalence of anisotropic mass-loss in the near-Earth environment. Motivated by the necessity of nongravitational accelerations to identify 2010 VL$_{65}$ and 2021 UA$_{12}$ as a single object, we investigate the problem of linking separate apparitions in the presen… ▽ More Nongravitational accelerations in the absence of observed activity have recently been identified on NEOs, opening the question of the prevalence of anisotropic mass-loss in the near-Earth environment. Motivated by the necessity of nongravitational accelerations to identify 2010 VL$_{65}$ and 2021 UA$_{12}$ as a single object, we investigate the problem of linking separate apparitions in the presence of nongravitational perturbations. We find that nongravitational accelerations on the order of $10^{-9}$ au/d$^2$ can lead to a change in plane-of-sky positions of $\sim10^3$ arcsec between apparitions. Moreover, we inject synthetic tracklets of hypothetical nongravitationally-accelerating NEOs into the Minor Planet Center orbit identification algorithms. We find that at large nongravitational accelerations ($|A_i|\geq10^{-8}$ au/d$^2$) these algorithms fail to link a significant fraction of these tracklets. We further show that if orbits can be determined for both apparitions, the tracklets will be linked regardless of nongravitational accelerations, although they may be linked to multiple objects. In order to aid in the identification and linkage of nongravitationally accelerating objects, we propose and test a new methodology to search for unlinked pairs. When applied to the current census of NEOs, we recover the previously identified case but identify no new linkages. We conclude that current linking algorithms are generally robust to nongravitational accelerations, but objects with large nongravitational accelerations may potentially be missed. While current algorithms are well-positioned for the anticipated increase in the census population from future survey missions, it may be possible to find objects with large nongravitational accelerations hidden in isolated tracklet pairs. △ Less

Submitted 11 October, 2024; v1 submitted 9 October, 2024; originally announced October 2024.

Comments: 16 pages, 5 figures and 5 appendix figures. Accepted to ApJ

Fermi-GBM Team Analysis on The Ravasio Line

Authors: Eric Burns, Stephen Lesage, Adam Goldstein, Michael S. Briggs, Peter Veres, Suman Bala, Cuan de Barra, Elisabetta Bissaldi, William H Cleveland, Misty M Giles, Matthew Godwin, Boyan A. Hristov, C. Michelle Hui, Daniel Kocevski, Bagrat Mailyan, Christian Malacaria, Sheila McBreen, Robert Preece, Oliver J. Roberts, Lorenzo Scotton, A. von Kienlin, Colleen A. Wilson-Hodge, Joshua Wood

Abstract: The prompt spectra of gamma-ray bursts are known to follow broadband continuum behavior over decades in energy. GRB 221009A, given the moniker the brightest of all time (BOAT), is the brightest gamma-ray burst identified in half a century of observations, and was first identified by the Fermi Gamma-ray Burst Monitor (GBM). On behalf of the Fermi-GBM Team, Lesage et al. (2023) described the initial… ▽ More The prompt spectra of gamma-ray bursts are known to follow broadband continuum behavior over decades in energy. GRB 221009A, given the moniker the brightest of all time (BOAT), is the brightest gamma-ray burst identified in half a century of observations, and was first identified by the Fermi Gamma-ray Burst Monitor (GBM). On behalf of the Fermi-GBM Team, Lesage et al. (2023) described the initial GBM analysis. Ravasio et al. (2024) report the identification of a spectral line in part of the prompt emission of this burst, which they describe as evolving over 80 s from $\sim$12 MeV to 6 MeV. We report a GBM Team analysis on the Ravasio Line: 1) We cannot identify an instrumental effect that could have produced this signal, and 2) our method of calculating the statistical significance of the line shows it easily exceeds the 5$σ$ discovery threshold. We additionally comment on the claim of the line beginning at earlier time intervals, up to 37 MeV, as reported in Zhang et al. (2024). We find that it is reasonable to utilize these measurements for characterization of the line evolution, with caution. We encourage theoretical studies exploring this newly discovered gamma-ray burst spectral feature, unless any rigorous alternative explanation unrelated to the emission from GRB 221009A is identified. △ Less

Submitted 30 September, 2024; originally announced October 2024.

Synchrotron self-Compton in a radiative-adiabatic fireball scenario: Modelling the multiwavelength observations in some Fermi/LAT bursts

Authors: Nissim Fraija, P. Veres, B. Betancourt Kamenetskaia, A. Galvan-Gamez, M. G. Dainotti, Simone Dichiara, R. L. Becerra

Abstract: Energetic GeV photons expected from the closest and the most energetic Gamma-ray bursts (GRBs) provide an unique opportunity to study the very-high-energy emission as well as the possible correlations with lower energy bands in realistic GRB afterglow models. In the standard GRB afterglow model, the relativistic homogeneous shock is usually considered to be fully adiabatic, however, it could be pa… ▽ More Energetic GeV photons expected from the closest and the most energetic Gamma-ray bursts (GRBs) provide an unique opportunity to study the very-high-energy emission as well as the possible correlations with lower energy bands in realistic GRB afterglow models. In the standard GRB afterglow model, the relativistic homogeneous shock is usually considered to be fully adiabatic, however, it could be partially radiative. Based on the external forward-shock scenario in both stellar wind and constant-density medium. We present a radiative-adiabatic analytical model of the synchrotron self-Compton (SSC) and synchrotron processes considering an electron energy distribution with a power-law index of 1 < p < 2 and 2 $\leq$ p. We show that the SSC scenario plays a relevant role in the radiative parameter $ε$, leading to a prolonged evolution during the slow cooling regime. In a particular case, we derive the Fermi/LAT light curves together with the photons with energies $\geq$ 100 MeV in a sample of nine bursts from the second Fermi/LAT GRB catalog that exhibited temporal and spectral indices with $\geq$ 1.5 and $\approx$ 2, respectively. These events can hardly be described with closure relations of the standard synchrotron afterglow model, and also exhibit energetic photons above the synchrotron limit. We have modeled the multi-wavelength observations of our sample to constrain the microphysical parameters, the circumburst density, the bulk Lorentz factor and the mechanism responsible for explaining the energetic GeV photons. △ Less

Submitted 18 September, 2024; originally announced September 2024.

Comments: Accepted in MNRAS. 26 pages, 7 figures, 6 tables

Extragalactic Magnetar Giant Flare GRB 231115A: Insights from Fermi/GBM Observations

Authors: Aaron C. Trigg, Rachael Stewart, Alex Van Kooten, Eric Burns, Matthew G. Baring, Dmitry D. Frederiks, Daniela Huppenkothen, Brendan O'Connor, Oliver J. Roberts, Zorawar Wadiasingh, George Younes, Narayana Bhat, Michael S. Briggs, Malte Busmann, Adam Goldstein, Daniel Gruen, Lei Hu, Chryssa Kouveliotou, Michela Negro, Antonella Palmese, Arno Riffeser, Lorenzo Scotton, Dmitry S. Svinkin, Peter Veres, Raphael Zöller

Abstract: We present the detection and analysis of GRB 231115A, a candidate extragalactic magnetar giant flare (MGF) observed by Fermi/GBM and localized by INTEGRAL to the starburst galaxy M82. This burst exhibits distinctive temporal and spectral characteristics that align with known MGFs, including a short duration and a high peak energy. Gamma-ray analyses reveal significant insights into this burst, sup… ▽ More We present the detection and analysis of GRB 231115A, a candidate extragalactic magnetar giant flare (MGF) observed by Fermi/GBM and localized by INTEGRAL to the starburst galaxy M82. This burst exhibits distinctive temporal and spectral characteristics that align with known MGFs, including a short duration and a high peak energy. Gamma-ray analyses reveal significant insights into this burst, supporting conclusions already established in the literature: our time-resolved spectral studies provide further evidence that GRB 231115A is indeed a MGF. Significance calculations also suggest a robust association with M82, further supported by a high Bayes factor that minimizes the probability of chance alignment with a neutron star merger. Despite extensive follow-up efforts, no contemporaneous gravitational wave or radio emissions were detected. The lack of radio emission sets stringent upper limits on possible radio luminosity. Constraints from our analysis show no fast radio bursts (FRBs) associated with two MGFs. X-ray observations conducted post-burst by Swift/XRT and XMM/Newton provided additional data, though no persistent counterparts were identified. Our study underscores the importance of coordinated multi-wavelength follow-up and highlights the potential of MGFs to enhance our understanding of short GRBs and magnetar activities in the cosmos. Current MGF identification and follow-up implementation are insufficient for detecting expected counterparts; however, improvements in these areas may allow for the recovery of follow-up signals with existing instruments. Future advancements in observational technologies and methodologies will be crucial in furthering these studies. △ Less

Submitted 8 June, 2025; v1 submitted 9 September, 2024; originally announced September 2024.

GRB 221009A: the B.O.A.T Burst that Shines in Gamma Rays

Authors: M. Axelsson, M. Ajello, M. Arimoto, L. Baldini, J. Ballet, M. G. Baring, C. Bartolini, D. Bastieri, J. Becerra Gonzalez, R. Bellazzini, B. Berenji, E. Bissaldi, R. D. Blandford, R. Bonino, P. Bruel, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, E. Cavazzuti, C. C. Cheung, G. Chiaro, N. Cibrario, S. Ciprini, G. Cozzolongo , et al. (129 additional authors not shown)

Abstract: We present a complete analysis of Fermi Large Area Telescope (LAT) data of GRB 221009A, the brightest Gamma-Ray Burst (GRB) ever detected. The burst emission above 30 MeV detected by the LAT preceded by 1 s the low-energy (< 10 MeV) pulse that triggered the Fermi Gamma-Ray Burst Monitor (GBM), as has been observed in other GRBs. The prompt phase of GRB 221009A lasted a few hundred seconds. It was… ▽ More We present a complete analysis of Fermi Large Area Telescope (LAT) data of GRB 221009A, the brightest Gamma-Ray Burst (GRB) ever detected. The burst emission above 30 MeV detected by the LAT preceded by 1 s the low-energy (< 10 MeV) pulse that triggered the Fermi Gamma-Ray Burst Monitor (GBM), as has been observed in other GRBs. The prompt phase of GRB 221009A lasted a few hundred seconds. It was so bright that we identify a Bad Time Interval (BTI) of 64 seconds caused by the extremely high flux of hard X-rays and soft gamma rays, during which the event reconstruction efficiency was poor and the dead time fraction quite high. The late-time emission decayed as a power law, but the extrapolation of the late-time emission during the first 450 seconds suggests that the afterglow started during the prompt emission. We also found that high-energy events observed by the LAT are incompatible with synchrotron origin, and, during the prompt emission, are more likely related to an extra component identified as synchrotron self-Compton (SSC). A remarkable 400 GeV photon, detected by the LAT 33 ks after the GBM trigger and directionally consistent with the location of GRB 221009A, is hard to explain as a product of SSC or TeV electromagnetic cascades, and the process responsible for its origin is uncertain. Because of its proximity and energetic nature, GRB 221009A is an extremely rare event. △ Less

Submitted 6 September, 2024; originally announced September 2024.

Comments: 60 pages, 38 figures, 9 tables

Back from the dead: AT2019aalc as a candidate repeating TDE in an AGN

Authors: Patrik Milán Veres, Anna Franckowiak, Sjoert van Velzen, Bjoern Adebahr, Sam Taziaux, Jannis Necker, Robert Stein, Alexander Kier, Ancla Mueller, Dominik J. Bomans, Nuria Jordana-Mitjans, Marek Kowalski, Erica Hammerstein, Elena Marci-Boehncke, Simeon Reusch, Simone Garrappa, Sam Rose, Kaustav Kashyap Das

Abstract: Context. To date, three nuclear transients have been associated with high-energy neutrino events. These transients are generally thought to be powered by tidal disruptions of stars (TDEs) by massive black holes. However, AT2019aalc, hosted in a Seyfert-1 galaxy, was not yet classified due to a lack of multiwavelength observations. Interestingly, the source has re-brightened 4 years after its disco… ▽ More Context. To date, three nuclear transients have been associated with high-energy neutrino events. These transients are generally thought to be powered by tidal disruptions of stars (TDEs) by massive black holes. However, AT2019aalc, hosted in a Seyfert-1 galaxy, was not yet classified due to a lack of multiwavelength observations. Interestingly, the source has re-brightened 4 years after its discovery. Aims. Our aim is to constrain the physical mechanism responsible for the second optical flare, which may also provide clues to the origin of the initial event. Methods. We conducted a multi-wavelength monitoring program (from radio to X-rays) of AT2019aalc during its re-brightening in 2023/2024. Results. The observations revealed multiple X-ray flares during the second optical flaring episode of the transient and a uniquely bright UV counterpart. The second flare, similarly to the first one, is also accompanied by IR dust echo emission. A long-term radio flare is found with an inverted spectrum. Optical spectroscopic observations reveal the presence of Bowen Fluorescence lines and strong high-ionization coronal lines indicating an extreme level of ionization in the system. Conslusions. The results suggest that the transient can be classified as a Bowen Fluorescence Flare (BFF), a relatively new sub-class of flaring active galactic nuclei (AGN). AT2019aalc can be also classified as an extreme coronal line emitter (ECLE). We found that, in addition to AT2019aalc, another BFF AT2021loi is spatially coincident with a high-energy neutrino event. We propose a repeating TDE scenario within an AGN framework to explain the multi-wavelength properties of AT2019aalc and suggest a possible connection among ECLEs, BFFs, and TDEs occurring in AGNs. △ Less

Submitted 1 December, 2025; v1 submitted 30 August, 2024; originally announced August 2024.

Comments: Accepted for publication in A&A. 23 pages, 19 figures, 3 tables

Journal ref: A&A 706, A324 (2026)

Non-detection of Neutrinos from the BOAT: Improved Constraints on the Parameters of GRB 221009A

Authors: P. Veres, N. Fraija, S. Lesage, A. Goldstein, M. S. Briggs, P. N. Bhat

Abstract: The IceCube neutrino observatory detects the diffuse astrophysical neutrino background with high significance, but the contribution of different classes of sources is not established. Because of their non-thermal spectrum, gamma-ray bursts (GRBs) are prime particle acceleration sites and one of the candidate classes for significant neutrino production. Exhaustive searches, based on stacking analys… ▽ More The IceCube neutrino observatory detects the diffuse astrophysical neutrino background with high significance, but the contribution of different classes of sources is not established. Because of their non-thermal spectrum, gamma-ray bursts (GRBs) are prime particle acceleration sites and one of the candidate classes for significant neutrino production. Exhaustive searches, based on stacking analysis of GRBs however could not establish the link between neutrinos and GRBs. Gamma-ray burst GRB 221009A had the highest time integrated gamma-ray flux of any detected GRB so far. The total fluence exceeds the sum of all Fermi Gamma-ray Burst Monitor (GBM) detected GRBs by a factor of two. Because it happened relatively nearby, it is one of the most favorable events for neutrino production from GRBs yet no neutrinos were detected. We calculate neutrino fluxes for this GRB in the TeV-PeV range using the most accurate, time-resolved spectral data covering the brightest intervals. We place limits on the physical parameters (Lorentz factor, baryon loading or emission radius) of the burst that are better by a factor of 2 compared to previous limits. The neutrino non-detection indicates a bulk Lorentz factor greater than 500 and possibly even 800, consistent with other observations. △ Less

Submitted 22 July, 2026; v1 submitted 29 August, 2024; originally announced August 2024.

Comments: 11 pages, 3 figures, 1 table. Minor revision: corrected notation, typos. Accepted in ApJ

Polarization Measurement of Gamma-ray Bursts with Fermi-GBM: The Case of GRB 180720B

Authors: P. Veres, W. Duvall, A. Goldstein, M. S. Briggs, J. E. Grove

Abstract: To achieve confident non-zero polarization measurements for gamma-ray bursts (GRBs) we need sensitive polarimeters and bright GRBs. Here we report on the polarimetric analysis of the bright GRB 180720B using the \Fermi Gamma-ray Burst Monitor (GBM). We rely on the detection of photons that scattered off Earth's atmosphere and into GBM from this burst. Polarized gamma-rays will exhibit a characteri… ▽ More To achieve confident non-zero polarization measurements for gamma-ray bursts (GRBs) we need sensitive polarimeters and bright GRBs. Here we report on the polarimetric analysis of the bright GRB 180720B using the \Fermi Gamma-ray Burst Monitor (GBM). We rely on the detection of photons that scattered off Earth's atmosphere and into GBM from this burst. Polarized gamma-rays will exhibit a characteristic pattern when scattering off the atmosphere that differs from an unpolarized beam. We compare the measured photon counts in the GBM detectors with extensive simulations of polarized beams to derive the most probable polarization degree (PD) and angle (PA). For the entire GRB, we find PD$=72^{+24}_{-30}\% ~(1σ)$ and PA$=91^{+11}_{-9}$ deg ($1σ$, equatorial frame). Interestingly, the PA value is broadly consistent with an early optical PA measurement by the Kanata telescope, starting shortly after the end of the prompt emission. The consistency of PAs lends support for this method. The relatively high polarization degree (albeit with large uncertainties) agrees with similar past measurements suggesting that some GRBs might be highly polarized. This will be confirmed or refuted by the upcoming dedicated GRB polarimeters. △ Less

Submitted 21 July, 2026; v1 submitted 23 August, 2024; originally announced August 2024.

Comments: 10 pages, 7 figures, accepted in ApJ, added estimate of systematics, lightcurves and detailed effective area. Conclusions unchanged

Debiasing astro-Photometric Observations with Corrections Using Statistics (DePhOCUS)

Authors: Tobias Hoffmann, Marco Micheli, Juan Luis Cano, Maxime Devogèle, Davide Farnocchia, Petr Pravec, Peter Vereš, Björn Poppe

Abstract: Photometric measurements allow the determination of an asteroid's absolute magnitude, which often represents the sole means to infer its size. Photometric observations can be obtained in a variety of filters that can be unique to a specific observatory. Those observations are then calibrated into specific bands with respect to reference star catalogs. In order to combine all the different measurem… ▽ More Photometric measurements allow the determination of an asteroid's absolute magnitude, which often represents the sole means to infer its size. Photometric observations can be obtained in a variety of filters that can be unique to a specific observatory. Those observations are then calibrated into specific bands with respect to reference star catalogs. In order to combine all the different measurements for evaluation, photometric observations need to be converted to a common band, typically V-band. Current band-correction schemes in use by IAU's Minor Planet Center, JPL's Center for Near Earth Object Studies and ESA's NEO Coordination Centre use average correction values for the apparent magnitude derived from photometry of asteroids as the corrections are dependent on the typically unknown spectrum of the object to be corrected. By statistically analyzing the photometric residuals of asteroids, we develop a new photometric correction scheme that does not only consider the band, but also accounts for reference catalog and observatory. We describe a new statistical photometry correction scheme for asteroid observations with debiased corrections. Testing this scheme on a reference group of asteroids, we see a 36% reduction in the photometric residuals. Moreover, the new scheme leads to a more accurate and debiased determination of the H-G magnitude system and, in turn, to more reliable inferred sizes. We discuss the significant shift in the corrections with this "DePhOCUS" debiasing system, its limitations, and the impact for photometric and physical properties of all asteroids, especially Near-Earth Objects. △ Less

Submitted 10 October, 2024; v1 submitted 14 August, 2024; originally announced August 2024.

Journal ref: Icarus (2024)

High-resolution imaging of the evolving bipolar outflows in symbiotic novae: The case of the RSOphiuchi 2021 nova outburst

Authors: R. Lico, M. Giroletti, U. Munari, T. J. O'Brien, B. Marcote, D. R. A. Williams, J. Yang, P. Veres, P. Woudt

Abstract: The recurrent and symbiotic nova RS Ophiuchi (RSOph) underwent a new outburst phase during August 2021, about 15 years after the last event that occurred in 2006. This outburst represents the first nova event ever detected at very high energies (VHE, E>100\,GeV), and a whole set of coordinated multiwavelength observations were triggered by this event. The main goals of this work are to characteriz… ▽ More The recurrent and symbiotic nova RS Ophiuchi (RSOph) underwent a new outburst phase during August 2021, about 15 years after the last event that occurred in 2006. This outburst represents the first nova event ever detected at very high energies (VHE, E>100\,GeV), and a whole set of coordinated multiwavelength observations were triggered by this event. The main goals of this work are to characterize the evolving morphology of the expanding bipolar ejecta with high accuracy and to determine the physical conditions of the surrounding medium in which they propagate. By means of high-resolution very long baseline interferometry (VLBI) radio observations, we monitored RSOph with the European VLBI Network (EVN) and e-MERLIN at 1.6 and 5\,GHz during multiple epochs from 14 to 65 days after the explosion. We reveal an evolving source structure consisting of a central and compact core and two elongated bipolar outflows expanding on opposite sides of the core in the east-west direction. The ejecta angular separation with time is consistent with a linear expansion with an average projected speed of $\sim7000$ km s$^{-1}$. We find clear evidence of a radial dependence of the density along the density enhancement on the orbital plane (DEOP), going from 1$\times$10$^7$ ~cm$^{-3}$ close to the central binary to 9$\times$10$^5$~cm$^{-3}$ at $\sim400$~AU. Thanks to the accurate source astrometric position provided by \textit{Gaia} DR3, in this work we draw a detailed scenario of the geometry and physics of the RSOph evolving source structure after the most recent nova event. We conclude that most of the mass lost by the red giant companion goes into the DEOP, for which we estimate a total mass of $6.4 \times 10^{-6} ~~\mathrm{M_\odot}$, and into the circumstellar region, while only a small fraction (about one-tenth) is accreted by the white dwarf. △ Less

Submitted 3 December, 2024; v1 submitted 8 July, 2024; originally announced July 2024.

Comments: 8 pages, 6 figures, 4 tables

Journal ref: A&A 692, A107 (2024)

Flaires: A Comprehensive Catalog of Dust-Echo-like Infrared Flares

Authors: Jannis Necker, Eleni Graikou, Marek Kowalski, Anna Franckowiak, Jakob Nordin, Teresa Pernice, Sjoert van Velzen, Patrik M. Veres

Abstract: Context: Observations of transient emission from extreme accretion events onto supermassive black holes can reveal conditions in the center of galaxies and the black hole itself. Most recently, they have been suggested to be emitters of high-energy neutrinos. If it is suddenly rejuvenated accretion or a tidal disruption event (TDE) is not clear in most cases. Aims: We expanded on existing samples… ▽ More Context: Observations of transient emission from extreme accretion events onto supermassive black holes can reveal conditions in the center of galaxies and the black hole itself. Most recently, they have been suggested to be emitters of high-energy neutrinos. If it is suddenly rejuvenated accretion or a tidal disruption event (TDE) is not clear in most cases. Aims: We expanded on existing samples of infrared flares to compile the largest and most complete list available. A large sample size is necessary to provide high enough statistics for far away and faint objects to estimate their rate. Our catalog is large enough to facilitate a preliminary study of the rate evolution with redshift for the first time. Methods: We compiled a sample of 40 million galaxies, and, using a custom, publicly available pipeline, analyzed the WISE light curves for these 40 million objects using the Bayesian Blocks algorithm. We selected promising candidates for dust echos of transient accretion events and inferred the luminosity, extension, and temperature of the hot dust by fitting a blackbody spectrum. Results: We established a clean sample of 823 dust-echo-like infrared flares, of which we can estimate the dust properties for 568. After removing 70 objects with possible contribution by synchrotron emission, the luminosity, extension, and temperature are consistent with dust echos. Estimating the dust extension from the light curve shape revealed that the duration of the incident flare is broadly compatible with the duration of TDEs. The resulting rate per galaxy is consistent with the latest measurements of infrared-detected TDEs and appears to decline at increasing redshift. Conclusions: Although systematic uncertainties may impact the calculation of the rate evolution, this catalog will enable further research in phenomena related to dust-echos from TDEs and extreme accretion flares. △ Less

Submitted 1 July, 2024; originally announced July 2024.

Comments: 23 pages, 11 figures, to be submitted to A&A

Journal ref: A&A 695, A228 (2025)

Constraining possible $γ$-ray burst emission from GW230529 using Swift-BAT and Fermi-GBM

Authors: Samuele Ronchini, Suman Bala, Joshua Wood, James Delaunay, Simone Dichiara, Jamie A. Kennea, Tyler Parsotan, Gayathri Raman, Aaron Tohuvavohu, Naresh Adhikari, Narayana P. Bhat, Sylvia Biscoveanu, Elisabetta Bissaldi, Eric Burns, Sergio Campana, Koustav Chandra, William H. Cleveland, Sarah Dalessi, Massimiliano De Pasquale, Juan García-Bellido, Claudio Gasbarra, Misty M. Giles, Ish Gupta, Dieter Hartmann, Boyan A. Hristov , et al. (13 additional authors not shown)

Abstract: GW230529 is the first compact binary coalescence detected by the LIGO-Virgo-KAGRA collaboration with at least one component mass confidently in the lower mass-gap, corresponding to the range 3-5$M_{\odot}$. If interpreted as a neutron star-black hole merger, this event has the most symmetric mass ratio detected so far and therefore has a relatively high probability of producing electromagnetic (EM… ▽ More GW230529 is the first compact binary coalescence detected by the LIGO-Virgo-KAGRA collaboration with at least one component mass confidently in the lower mass-gap, corresponding to the range 3-5$M_{\odot}$. If interpreted as a neutron star-black hole merger, this event has the most symmetric mass ratio detected so far and therefore has a relatively high probability of producing electromagnetic (EM) emission. However, no EM counterpart has been reported. At the merger time $t_0$, Swift-BAT and Fermi-GBM together covered 100$\%$ of the sky. Performing a targeted search in a time window $[t_0-20 \text{s},t_0+20 \text{s}]$, we report no detection by the Swift-BAT and the Fermi-GBM instruments. Combining the position-dependent $γ-$ray flux upper limits and the gravitational-wave posterior distribution of luminosity distance, sky localization and inclination angle of the binary, we derive constraints on the characteristic luminosity and structure of the jet possibly launched during the merger. Assuming a top-hat jet structure, we exclude at 90$\%$ credibility the presence of a jet which has at the same time an on-axis isotropic luminosity $\gtrsim 10^{48}$ erg s$^{-1}$, in the bolometric band 1 keV-10 MeV, and a jet opening angle $\gtrsim 15$ deg. Similar constraints are derived testing other assumptions about the jet structure profile. Excluding GRB 170817A, the luminosity upper limits derived here are below the luminosity of any GRB observed so far. △ Less

Submitted 17 May, 2024; originally announced May 2024.

Comments: 18 pages, 1 table, 11 figures

Future Perspectives for Gamma-ray Burst Detection from Space

Authors: Enrico Bozzo, Lorenzo Amati, Wayne Baumgartner, Tzu-Ching Chang, Bertrand Cordier, Nicolas De Angelis, Akihiro Doi, Marco Feroci, Cynthia Froning, Jessica Gaskin, Adam Goldstein, Diego Götz, Jon E. Grove, Sylvain Guiriec, Margarita Hernanz, C. Michelle Hui, Peter Jenke, Daniel Kocevski, Merlin Kole, Chryssa Kouveliotou, Thomas Maccarone, Mark L. McConnell, Hideo Matsuhara, Paul O'Brien, Nicolas Produit , et al. (13 additional authors not shown)

Abstract: Since their first discovery in the late 1960s, Gamma-ray bursts have attracted an exponentially growing interest from the international community due to their central role in the most highly debated open questions of the modern research of astronomy, astrophysics, cosmology, and fundamental physics. These range from the intimate nuclear composition of high density material within the core of ultra… ▽ More Since their first discovery in the late 1960s, Gamma-ray bursts have attracted an exponentially growing interest from the international community due to their central role in the most highly debated open questions of the modern research of astronomy, astrophysics, cosmology, and fundamental physics. These range from the intimate nuclear composition of high density material within the core of ultra-dense neuron stars, to stellar evolution via the collapse of massive stars, the production and propagation of gravitational waves, as well as the exploration of the early Universe by unveiling first stars and galaxies (assessing also their evolution and cosmic re-ionization). GRBs have stimulated in the past $\sim$50 years the development of cutting-edge technological instruments for observations of high energy celestial sources from space, leading to the launch and successful operations of many different scientific missions (several of them still in data taking mode nowadays). In this review, we provide a brief description of the GRB-dedicated missions from space being designed and developed for the future. The list of these projects, not meant to be exhaustive, shall serve as a reference to interested readers to understand what is likely to come next to lead the further development of GRB research and associated phenomenology. △ Less

Submitted 17 April, 2024; originally announced April 2024.

Comments: Accepted for publication on Universe. Invited review, contribution to the Universe Special Issue "Recent Advances in Gamma Ray Astrophysics and Future Perspectives", P. Romano eds. (https://www.mdpi.com/journal/universe/special_issues/7299902Z97)

European VLBI Network observations of the peculiar radio source 4C 35.06 overlapping with a compact group of nine galaxies

Authors: Patrik Milán Veres, Krisztina Éva Gabányi, Sándor Frey, Zsolt Paragi, Tao An, Joydeep Bagchi, Ákos Bogdán, K. G. Biju, Emma Kun, Joe Jacob, Björn Adebahr

Abstract: Context. According to the hierarchical structure formation model, brightest cluster galaxies (BCGs) evolve into the most luminous and massive galaxies in the Universe through multiple merger events. The peculiar radio source 4C 35.06 is located at the core of the galaxy cluster Abell 407, overlapping with a compact group of nine galaxies. Low-frequency radio observations have revealed a helical, s… ▽ More Context. According to the hierarchical structure formation model, brightest cluster galaxies (BCGs) evolve into the most luminous and massive galaxies in the Universe through multiple merger events. The peculiar radio source 4C 35.06 is located at the core of the galaxy cluster Abell 407, overlapping with a compact group of nine galaxies. Low-frequency radio observations have revealed a helical, steep-spectrum, kiloparsec-scale jet structure and inner lobes with less steep spectra, compatible with a recurring active galactic nucleus (AGN) activity scenario. However, the host galaxy of the AGN responsible for the detected radio emission remained unclear. Aims. We aim to identify the host of 4C 35.06 by studying the object at high angular resolution and thereby confirm the recurrent AGN activity scenario. Methods. To reveal the host of the radio source, we carried out very long baseline interferometry (VLBI) observations with the European VLBI Network of the nine galaxies in the group at 1.7 and 4.9 GHz. Results. We detected compact radio emission from an AGN located between the two inner lobes at both observing frequencies. In addition, we detected another galaxy at 1.7 GHz, whose position appears more consistent with the principal jet axis and is located closer to the low-frequency radio peak of 4C 35.06. The presence of another radio-loud AGN in the nonet sheds new light on the BCG formation and provides an alternative scenario in which not just one but two AGNs are responsible for the complex large-scale radio structure △ Less

Submitted 20 February, 2024; originally announced February 2024.

Comments: accepted for publication in Astronomy & Astrophysics (A&A), 7 pages, 4 figures, 2 tables

Mapping the Universe with Gamma-Ray Bursts

Authors: Istvan Horvath, Zsolt Bagoly, Lajos G. Balazs, Jon Hakkila, Zsuzsa Horvath, Andras Peter Joo, Sandor Pinter, L. Viktor Tóth, Peter Veres, Istvan I. Racz

Abstract: We explore large-scale cosmic structure using the spatial distribution of 542 gamma-ray bursts (GRBs) having accurately measured positions and spectroscopic redshifts. Prominent cosmological clusters are identified in both the northern and southern galactic hemispheres (avoiding extinction effects in the plane of the Milky Way) using the Bootstrap Point-Radius method. The Northern Galactic hemisph… ▽ More We explore large-scale cosmic structure using the spatial distribution of 542 gamma-ray bursts (GRBs) having accurately measured positions and spectroscopic redshifts. Prominent cosmological clusters are identified in both the northern and southern galactic hemispheres (avoiding extinction effects in the plane of the Milky Way) using the Bootstrap Point-Radius method. The Northern Galactic hemisphere contains a significant group of four GRBs in the redshift range 0.59 < z < 0.62 (with a Bootstrap probability of p = 0.012) along with the previously-identified Hercules-Corona Borealis GreatWall (in the revised redshift range 0.9 < z < 2.1, p = 0.017). The Southern Galactic hemisphere contains the previously-identified Giant GRB Ring (p = 0.022) along with another possible cluster of 7 - 9 GRBs at 1.179 < z < 1.444 (p = 0.031). Additionally, both the Hercules-Corona Borealis Great Wall and the Giant GRB Ring have become more prominent as the GRB sample size has grown. The approach used here underscores the potential value of GRB clustering as a probe of large-scale cosmic structure, complementary to galaxy and quasar clustering. Because of the vast scale on which GRB clustering provides valuable insights, it is important that optical GRB monitoring continue so that additional spectroscopic redshift measurements should be obtained. △ Less

Submitted 2 December, 2023; originally announced December 2023.

Comments: 11 pages, 15 figures, submitted to MNRAS

Exploring Physically-Motivated Models to Fit Gamma-Ray Burst Spectra

Authors: Suraj Poolakkil, Robert Preece, Peter Veres

Abstract: We explore fitting gamma-ray burst spectra with three physically-motivated models, and thus revisit the viability of synchrotron radiation as the primary source of GRB prompt emission. We pick a sample of 100 bright GRBs observed by the Fermi Gamma-ray Burst Monitor (GBM), based on their energy flux values. In addition to the standard empirical spectral models used in previous GBM spectroscopy cat… ▽ More We explore fitting gamma-ray burst spectra with three physically-motivated models, and thus revisit the viability of synchrotron radiation as the primary source of GRB prompt emission. We pick a sample of 100 bright GRBs observed by the Fermi Gamma-ray Burst Monitor (GBM), based on their energy flux values. In addition to the standard empirical spectral models used in previous GBM spectroscopy catalogs, we also consider three physically-motivated models; (a) a Thermal Synchrotron model, (b) a Band model with a High-energy Cutoff, and (c) a Smoothly Broken Power Law (SBPL) model with a Multiplicative Broken Power Law (MBPL). We then adopt the Bayesian information criterion (BIC) to compare the fits obtained and choose the best model. We find that 42% of the GRBs from the fluence spectra and 23% of GRBs from the peak-flux spectra have one of the three physically-motivated models as their preferred one. From the peak-flux spectral fits, we find that the low-energy index distributions from the empirical model fits for long GRBs peak around the synchrotron value of -2/3, while the two low-energy indices from the SBPL+MBPL fits of long GRBs peak close to the -2/3 and -3/2 values expected for a synchrotron spectrum below and above the cooling frequency. △ Less

Submitted 22 November, 2023; originally announced November 2023.

Comments: arXiv admin note: text overlap with arXiv:2103.13528

GRB 180128A: A Second Magnetar Giant Flare Candidate from the Sculptor Galaxy

Authors: Aaron C. Trigg, Eric Burns, Oliver J. Roberts, Michela Negro, Dmitry S. Svinkin, Matthew G. Baring, Zorawar Wadiasingh, Nelson L. Christensen, Igor Andreoni, Michael S. Briggs, Niccolo Di Lalla, Dmitry D. Frederiks, Vladimir M. Lipunov, Nicola Omodei, Anna V. Ridnaia, Peter Veres, Alexandra L. Lysenko

Abstract: Magnetars are slowly rotating neutron stars that possess the strongest magnetic fields ($10^{14}-10^{15} \mathrm{G}$) known in the cosmos. They display a range of transient high-energy electromagnetic activity. The brightest and most energetic of these events are the gamma-ray bursts (GRBs) known as magnetar giant flares (MGFs), with isotropic energy $E\approx10^{44}-10^{46} \mathrm{erg}$. There a… ▽ More Magnetars are slowly rotating neutron stars that possess the strongest magnetic fields ($10^{14}-10^{15} \mathrm{G}$) known in the cosmos. They display a range of transient high-energy electromagnetic activity. The brightest and most energetic of these events are the gamma-ray bursts (GRBs) known as magnetar giant flares (MGFs), with isotropic energy $E\approx10^{44}-10^{46} \mathrm{erg}$. There are only seven detections identified as MGFs to date: three unambiguous events occurred in our Galaxy and the Magellanic Clouds, and the other four MGF candidates are associated with nearby star-forming galaxies. As all seven identified MGFs are bright at Earth, additional weaker events remain unidentified in archival data. We conducted a search of the Fermi Gamma-ray Burst Monitor (GBM) database for candidate extragalactic MGFs and, when possible, collected localization data from the Interplanetary Network (IPN) satellites. Our search yielded one convincing event, GRB 180128A. IPN localizes this burst with NGC 253, commonly known as the Sculptor Galaxy. This event is the second MGF in modern astronomy to be associated with this galaxy and the first time two bursts are associated with a single galaxy outside our own. Here, we detail the archival search criteria that uncovered this event and its spectral and temporal properties, which are consistent with expectations for a MGF. We also discuss the theoretical implications and finer burst structures resolved from various binning methods. Our analysis provides observational evidence for an eighth identified MGF. △ Less

Submitted 15 November, 2023; originally announced November 2023.

Comments: 15 pages, 8 figures

Journal ref: A&A 694, A323 (2025)

An Explanation of GRB Fermi-LAT Flares and High-Energy Photons in Stratified Afterglows

Authors: Nissim Fraija, Boris Betancourt Kamenetskaia, Antonio Galván-Gámez, Peter Veres, Rosa L. Becerra, Simone Dichiara, Maria G. Dainotti, Francisco Lizcano, Edilberto Aguilar-Ruiz

Abstract: The second {\itshape Fermi}/LAT gamma-ray burst (GRB) catalog (2FLGC) spanning the first decade of operations by the LAT collaboration was recently released. The closure relations of the synchrotron forward shock (FS) model are not able to reproduce a sizeable portion of the afterglow-phase light curves in this collection, indicating that there may be a large contribution from some other mechanism… ▽ More The second {\itshape Fermi}/LAT gamma-ray burst (GRB) catalog (2FLGC) spanning the first decade of operations by the LAT collaboration was recently released. The closure relations of the synchrotron forward shock (FS) model are not able to reproduce a sizeable portion of the afterglow-phase light curves in this collection, indicating that there may be a large contribution from some other mechanism. Recently, synchrotron self-Compton (SSC) light curves from the reverse shock (RS) regions were derived in the thick- and thin-shell regime for a constant-density medium, and it was demonstrated that analytical light curves could explain the~GeV flare observed in several bursts from 2FLGC, including GRB 160509A. Here, we generalise the SSC RS scenario from the constant density to a stratified medium, and show that this contribution helps to describe the early light curves exhibited in some {\itshape Fermi}/LAT-detected bursts. As a particular case, we model a sample of eight bursts that exhibited a short-lasting emission with the synchrotron and SSC model from FS and RS regions, evolving in a stellar-wind environment, constraining the microphysical parameters, the circumburst density, the bulk Lorentz factor, and the fraction of shock-accelerated electrons. We demonstrate that the highest-energy photons can only be described by the SSC from the forward-shock region. △ Less

Submitted 3 November, 2023; originally announced November 2023.

Comments: 35 pages, 12 figures, 4 tables, accepted in mnras

Improvement of digest2 NEO Classification Code -- utilizing the Astrometry Data Exchange Standard

Authors: Peter Vereš, Richard Cloete, Robert Weryk, Abraham Loeb, Matthew J. Payne

Abstract: We describe enhancements to the digest2 software, a short-arc orbit classifier for heliocentric orbits. Digest2 is primarily used by the Near-Earth Object (NEO) community to flag newly discovered objects for a immediate follow-up and has been a part of NEO discovery process for more than 15 years. We have updated the solar system population model used to weight the digest2 score according to the 2… ▽ More We describe enhancements to the digest2 software, a short-arc orbit classifier for heliocentric orbits. Digest2 is primarily used by the Near-Earth Object (NEO) community to flag newly discovered objects for a immediate follow-up and has been a part of NEO discovery process for more than 15 years. We have updated the solar system population model used to weight the digest2 score according to the 2023 catalog of known solar system orbits and extended the list of mean uncertainties for 140 observatory codes. Moreover, we have added Astrometry Data Exchange Standard (ADES) input format support to digest2, which provides additional information for the astrometry, such as positional uncertainties for each detection. The digest2 code was also extended to read the roving observer astrometric format as well as the ability to compute a new parameter from the provided astrometric uncertainties ($RMS'$) that can serve as an indicator of in-tracklet curvature when compared with tracklet's great-circle fit RMS. Comparison with the previous version of digest2 confirmed the improvement in accuracy of NEO identification and found that using ADES XML input significantly reduces the computation time of the digest2. △ Less

Submitted 28 September, 2023; originally announced September 2023.

Comments: 14 pages, 8 tables, 6 figures, appendix

A Joint Fermi-GBM and Swift-BAT Analysis of Gravitational-Wave Candidates from the Third Gravitational-wave Observing Run

Authors: C. Fletcher, J. Wood, R. Hamburg, P. Veres, C. M. Hui, E. Bissaldi, M. S. Briggs, E. Burns, W. H. Cleveland, M. M. Giles, A. Goldstein, B. A. Hristov, D. Kocevski, S. Lesage, B. Mailyan, C. Malacaria, S. Poolakkil, A. von Kienlin, C. A. Wilson-Hodge, The Fermi Gamma-ray Burst Monitor Team, M. Crnogorčević, J. DeLaunay, A. Tohuvavohu, R. Caputo, S. B. Cenko , et al. (1674 additional authors not shown)

Abstract: We present Fermi Gamma-ray Burst Monitor (Fermi-GBM) and Swift Burst Alert Telescope (Swift-BAT) searches for gamma-ray/X-ray counterparts to gravitational wave (GW) candidate events identified during the third observing run of the Advanced LIGO and Advanced Virgo detectors. Using Fermi-GBM on-board triggers and sub-threshold gamma-ray burst (GRB) candidates found in the Fermi-GBM ground analyses,… ▽ More We present Fermi Gamma-ray Burst Monitor (Fermi-GBM) and Swift Burst Alert Telescope (Swift-BAT) searches for gamma-ray/X-ray counterparts to gravitational wave (GW) candidate events identified during the third observing run of the Advanced LIGO and Advanced Virgo detectors. Using Fermi-GBM on-board triggers and sub-threshold gamma-ray burst (GRB) candidates found in the Fermi-GBM ground analyses, the Targeted Search and the Untargeted Search, we investigate whether there are any coincident GRBs associated with the GWs. We also search the Swift-BAT rate data around the GW times to determine whether a GRB counterpart is present. No counterparts are found. Using both the Fermi-GBM Targeted Search and the Swift-BAT search, we calculate flux upper limits and present joint upper limits on the gamma-ray luminosity of each GW. Given these limits, we constrain theoretical models for the emission of gamma-rays from binary black hole mergers. △ Less

Submitted 25 August, 2023; originally announced August 2023.

A Radio Flare in the Long-Lived Afterglow of the Distant Short GRB 210726A: Energy Injection or a Reverse Shock from Shell Collisions?

Authors: Genevieve Schroeder, Lauren Rhodes, Tanmoy Laskar, Anya Nugent, Alicia Rouco Escorial, Jillian C. Rastinejad, Wen-fai Fong, Alexander J. van der Horst, Péter Veres, Kate D. Alexander, Alex Andersson, Edo Berger, Peter K. Blanchard, Sarah Chastain, Lise Christensen, Rob Fender, David A. Green, Paul Groot, Ian Heywood, Assaf Horesh, Luca Izzo, Charles D. Kilpatrick, Elmar Körding, Amy Lien, Daniele B. Malesani , et al. (10 additional authors not shown)

Abstract: We present the discovery of the radio afterglow of the short $γ$-ray burst (GRB) 210726A, localized to a galaxy at a photometric redshift of $z\sim 2.4$. While radio observations commenced $\lesssim 1~$day after the burst, no radio emission was detected until $\sim11~$days. The radio afterglow subsequently brightened by a factor of $\sim 3$ in the span of a week, followed by a rapid decay (a "radi… ▽ More We present the discovery of the radio afterglow of the short $γ$-ray burst (GRB) 210726A, localized to a galaxy at a photometric redshift of $z\sim 2.4$. While radio observations commenced $\lesssim 1~$day after the burst, no radio emission was detected until $\sim11~$days. The radio afterglow subsequently brightened by a factor of $\sim 3$ in the span of a week, followed by a rapid decay (a "radio flare"). We find that a forward shock afterglow model cannot self-consistently describe the multi-wavelength X-ray and radio data, and underpredicts the flux of the radio flare by a factor of $\approx 5$. We find that the addition of substantial energy injection, which increases the isotropic kinetic energy of the burst by a factor of $\approx 4$, or a reverse shock from a shell collision are viable solutions to match the broad-band behavior. At $z\sim 2.4$, GRB 210726A is among the highest redshift short GRBs discovered to date as well as the most luminous in radio and X-rays. Combining and comparing all previous radio afterglow observations of short GRBs, we find that the majority of published radio searches conclude by $\lesssim 10~$days after the burst, potentially missing these late rising, luminous radio afterglows. △ Less

Submitted 19 July, 2024; v1 submitted 21 August, 2023; originally announced August 2023.

Comments: 29 pages, 10 figures, accepted to ApJ

Gamma-ray Transient Network Science Analysis Group Report

Authors: Eric Burns, Michael Coughlin, Kendall Ackley, Igor Andreoni, Marie-Anne Bizouard, Floor Broekgaarden, Nelson L. Christensen, Filippo D'Ammando, James DeLaunay, Henrike Fleischhack, Raymond Frey, Chris L. Fryer, Adam Goldstein, Bruce Grossan, Rachel Hamburg, Dieter H. Hartmann, Anna Y. Q. Ho, Eric J. Howell, C. Michelle Hui, Leah Jenks, Alyson Joens, Stephen Lesage, Andrew J. Levan, Amy Lien, Athina Meli , et al. (12 additional authors not shown)

Abstract: The Interplanetary Network (IPN) is a detection, localization and alert system that utilizes the arrival time of transient signals in gamma-ray detectors on spacecraft separated by planetary baselines to geometrically locate the origin of these transients. Due to the changing astrophysical landscape and the new emphasis on time domain and multi-messenger astrophysics (TDAMM) from the Pathways to D… ▽ More The Interplanetary Network (IPN) is a detection, localization and alert system that utilizes the arrival time of transient signals in gamma-ray detectors on spacecraft separated by planetary baselines to geometrically locate the origin of these transients. Due to the changing astrophysical landscape and the new emphasis on time domain and multi-messenger astrophysics (TDAMM) from the Pathways to Discovery in Astronomy and Astrophysics for the 2020s, this Gamma-ray Transient Network Science Analysis Group was tasked to understand the role of the IPN and high-energy monitors in this new era. The charge includes describing the science made possible with these facilities, tracing the corresponding requirements and capabilities, and highlighting where improved operations of existing instruments and the IPN would enhance TDAMM science. While this study considers the full multiwavelength and multimessenger context, the findings are specific to space-based high-energy monitors. These facilities are important both for full characterization of these transients as well as facilitating follow-up observations through discovery and localization. The full document reports a brief history of this field, followed by our detailed analyses and findings in some 68 pages, providing a holistic overview of the role of the IPN and high-energy monitors in the coming decades. △ Less

Submitted 5 October, 2023; v1 submitted 8 August, 2023; originally announced August 2023.

Comments: Terms of Reference and additional information on the Science Analysis Group are available at https://pcos.gsfc.nasa.gov/sags/gtn-sag.php

Extreme Variability in a Long Duration Gamma-ray Burst Associated with a Kilonova

Authors: P. Veres, P. N. Bhat, E. Burns, R. Hamburg, N. Fraija, D. Kocevski, R. Preece, S. Poolakkil, N. Christensen, M. A. Bizouard, T. Dal Canton, S. Bala, E. Bissaldi, M. S. Briggs, W. Cleveland, A. Goldstein, B. A. Hristov, C. M. Hui, S. Lesage, B. Mailyan, O. J. Roberts, C. A. Wilson-Hodge

Abstract: The recent discovery of a kilonova from the long duration gamma-ray burst, GRB 211211A, challenges classification schemes based on temporal information alone. Gamma-ray properties of GRB 211211A reveal an extreme event, which stands out among both short and long GRBs. We find very short variations (few ms) in the lightcurve of GRB 211211A and estimate ~1000 for the Lorentz factor of the outflow. W… ▽ More The recent discovery of a kilonova from the long duration gamma-ray burst, GRB 211211A, challenges classification schemes based on temporal information alone. Gamma-ray properties of GRB 211211A reveal an extreme event, which stands out among both short and long GRBs. We find very short variations (few ms) in the lightcurve of GRB 211211A and estimate ~1000 for the Lorentz factor of the outflow. We discuss the relevance of the short variations in identifying similar long GRBs resulting from compact mergers. Our findings indicate that in future gravitational wave follow-up campaigns, some long duration GRBs should be treated as possible strong gravitational wave counterparts. △ Less

Submitted 20 May, 2023; originally announced May 2023.

Comments: 10 pages 5 figures, submitted to AAS journals

Journal ref: ApJL 954 L5 (2023)

Fermi-GBM Discovery of GRB 221009A: An Extraordinarily Bright GRB from Onset to Afterglow

Authors: S. Lesage, P. Veres, M. S. Briggs, A. Goldstein, D. Kocevski, E. Burns, C. A. Wilson-Hodge, P. N. Bhat, D. Huppenkothen, C. L. Fryer, R. Hamburg, J. Racusin, E. Bissaldi, W. H. Cleveland, S. Dalessi, C. Fletcher, M. M. Giles, B. A. Hristov, C. M. Hui, B. Mailyan, C. Malacaria, S. Poolakkil, O. J. Roberts, A. von Kienlin, J. Wood , et al. (115 additional authors not shown)

Abstract: We report the discovery of GRB 221009A, the highest flux gamma-ray burst ever observed by the Fermi Gamma-ray Burst Monitor (GBM). This GRB has continuous prompt emission lasting more than 600 seconds which smoothly transitions to afterglow visible in the GBM energy range (8 keV--40 MeV), and total energetics higher than any other burst in the GBM sample. By using a variety of new and existing ana… ▽ More We report the discovery of GRB 221009A, the highest flux gamma-ray burst ever observed by the Fermi Gamma-ray Burst Monitor (GBM). This GRB has continuous prompt emission lasting more than 600 seconds which smoothly transitions to afterglow visible in the GBM energy range (8 keV--40 MeV), and total energetics higher than any other burst in the GBM sample. By using a variety of new and existing analysis techniques we probe the spectral and temporal evolution of GRB 221009A. We find no emission prior to the GBM trigger time (t0; 2022 October 9 at 13:16:59.99 UTC), indicating that this is the time of prompt emission onset. The triggering pulse exhibits distinct spectral and temporal properties suggestive of the thermal, photospheric emission of shock-breakout, with significant emission up to $\sim$15 MeV. We characterize the onset of external shock at t0+600 s and find evidence of a plateau region in the early-afterglow phase which transitions to a slope consistent with Swift-XRT afterglow measurements. We place the total energetics of GRB 221009A in context with the rest of the GBM sample and find that this GRB has the highest total isotropic-equivalent energy ($\textrm{E}_{γ,\textrm{iso}}=1.0\times10^{55}$ erg) and second highest isotropic-equivalent luminosity ($\textrm{L}_{γ,\textrm{iso}}=9.9\times10^{53}$ erg/s) based on redshift of z = 0.151. These extreme energetics are what allowed us to observe the continuously emitting central engine of GBM from the beginning of the prompt emission phase through the onset of early afterglow. △ Less

Submitted 12 July, 2023; v1 submitted 24 March, 2023; originally announced March 2023.

Comments: 26 pages 7 figures - accepted for publication in ApJL