Discovery and confirmation of the shortest gamma-ray burst from a collapsar

Ahumada, Tomás; Singer, L. P.; Anand, S.; Coughlin, M. W.; Kasliwal, M. M.; Ryan, Geoffrey; Andreoni, Igor; Cenko, S. Bradley; Fremling, C.; Kumar, Harsh; Pang, P. T. H.; Burns, E.; Cunningham, Virginia; Dichiara, S.; Dietrich, Tim; Svinkin, D.; Almualla, Mouza; Castro‐Tirado, Alberto J.; De, Kishalay; Dunwoody, Rachel; Gatkine, Pradip; Hammerstein, Erica; Iyyani, Shabnam; Mangan, Joseph; Perley, D. A.; Purkayastha, Sonalika; Bellm, Eric C.; Bhalerao, V.; Bolin, Bryce; Bulla, Mattia; Cannella, Christopher; Chandra, Poonam; Duev, Dmitry A.; Frederiks, D.; Gal‐Yam, A.; Graham, M. J.; Ho, Anna Y. Q.; Hurley, K.; Karambelkar, Viraj; Kool, Erik C.; Kulkarni, S. R.; Mahabal, A.; Masci, Frank J.; McBreen, S.; Pandey, S. B.; Reusch, Simeon; Ridnaia, A.; Rosnet, P.; Rusholme, B.; Carracedo, Ana Sagués; Smith, Roger; Soumagnac, Maayane T.; Stein, R.; Troja, E.; Tsvetkova, A. E.; Walters, Richard; Valeev, A. F.

doi:10.1038/s41550-021-01428-7

Cited by 111 publications

(115 citation statements)

References 153 publications

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“…The 10-800 keV-band light curve, as detected by GBM, is shown in Figure 1a. The duration in the same energy range of the burst is measured as T 90 ∼ 0.96 +0.06 −0.07 s (see Table 1 for a collection of all the measured parameters of GRB 200826A, and see the details of data analysis in Methods), which is consistent with the value of T 90 = 1.14 ± 0.13 in 50-300 keV energy range 11 . The lightcurve pulse profile is quite sharp.…”

supporting

confidence: 76%

“…Finally, a Type II origin of GRB 200826 is further supported by the follow-up observations by Gemini-North 8-meter telescope 11 (see Extended Data Figure 5), which revealed a possible optical bump at 25.45 ± 0.15 mag in i-band. This bump could be consistent with a supernova, a signature of a massive star core collapse event.…”

supporting

confidence: 57%

“…Short GRBs, on the other hand, typically show negligible lags 18 . The (10)(11)(12)(13)(14)(15)(16)(17)(18)(19)(20) keV to (250-300) keV spectral lag of GRB 200826A is 0.157±0.051 s (See Methods and Extended Data Figure 4). This is at odds for short GRBs but is typical for long GRBs.…”

mentioning

confidence: 99%

“…Our results are consistent with those in ref. 11 . Due to kicks at the births of neutron stars from SNe explosions, these mergers also usually occur at a site far away from star formation regions, often in the outskirts or even outside their host galaxies 20,22 .…”

mentioning

confidence: 99%

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A Genuinely Short Gamma-Ray Burst from Massive Star Core Collapse

Zhang

Liu

Peng

et al. 2020

Preprint

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Gamma-ray bursts have been phenomenologically classified into long and short populations based on whether the observed duration is longer or shorter than two seconds. Multi-wavelength and multi-messenger observations in recent years have revealed that in general long GRBs originate from massive star core collapse events, whereas short GRBs originate from binary neutron star mergers. It has been known that the duration criterion is sometimes unreliable, and multi-wavelength criteria are needed to identify the physical origin of a particular GRB. Some apparently long GRBs have been suggested to have a neutron star merger origin, whereas some apparently short GRBs have been attributed to genuinely long GRBs whose short, bright emission is above the detector's sensitivity threshold. Still, there has been no known case that a GRB is genuinely short but originates from death of a massive star. Here we report the comprehensive analysis of the multi-wavelength data of a bright short GRB 200826A. This burst has a sharp 1-second spike, which is not part of an underlying long-duration event. Its other observational properties are, however, inconsistent with those of other short GRBs believed to originate from binary neutron star mergers. Rather, these properties resemble those of long GRBs. This burst presents a challenge to the traditional GRB classification scheme and reveals a class of core-collapse-origin GRBs with genuinly short durations.

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supporting

confidence: 76%

supporting

confidence: 57%

mentioning

confidence: 99%

mentioning

confidence: 99%

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A Genuinely Short Gamma-Ray Burst from Massive Star Core Collapse

Zhang

Liu

Peng

et al. 2020

Preprint

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“…It is also observed that some GRBs with T 90 values favourable to long GRBs have afterglow and host properties similar to the short GRBs (Gal-Yam et al, 2006). On the other hand, other GRBs with T 90 less than 2 sec show properties identical to long GRBs (Antonelli et al, 2009;Ahumada et al, 2021).…”

Section: Introductionmentioning

confidence: 85%

GRB 210217A: A short or a long GRB?

Dimple¹,

Misra²,

Ghosh³

et al. 2022

Preprint

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Gamma-ray bursts are traditionally classified as short and long bursts based on their T 90 value (the time interval during which an instrument observes 5% to 95% of gamma-ray/hard X-ray fluence). However, T 90 is dependent on the detector sensitivity and the energy range in which the instrument operates. As a result, different instruments provide different values of T 90 for a burst. GRB 210217A is detected with different duration by Swift and Fermi. It is classified as a long/soft GRB by Swift-BAT with a T 90 value of 3.76 sec. On the other hand, the sub-threshold detection by Fermi-GBM classified GRB 210217A as a short/hard burst with a duration of 1.024 sec. We present the multi-wavelength analysis of GRB 210217A (lying in the overlapping regime of long and short GRBs) to identify its actual class using multi-wavelength data. We utilized the T 90 -hardness ratio, T 90 -E p , and T 90 -t mvts distributions of the GRBs to find the probability of GRB 210217A being a short GRB. Further, we estimated the photometric redshift of the burst by fitting the joint XRT/UVOT SED and place the burst in the Amati plane. We found that GRB 210217A is an ambiguous burst showing properties of both short and long class of GRBs.

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Comprehension of Jet Physics from the Analysis of the Gamma‐Ray Burst Afterglow Parameter Distributions

et al. 2022

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The discovery of a short gamma‐ray burst (GRB), GRB170817A, in association with a gravitational wave (GW) and a bright kilonova started a new era in the high‐energy astrophysics. The observation of GRB170817A and more recently, GRB200826A and GRB211211A, a short and a long burst, respectively, with a possible kilonova, reinforce the concern about new ways of classification. For this reason, a new machine learning technique is applied to Swift‐BAT data, searching for morphological similarities in the light curves. The resulting map is characterized by two distinct groups, although still correlated with standard T90 duration. Since a jet viewed off‐axis could explain the emission from GRB170817A, the modeling of this kind of sources is of great importance. A public code called JetFit, based on the “boosted fireball” model, is applied to fit Swift‐XRT afterglow light curves of short and long GRBs, with known red‐shift, from 2005 to 2021. JetFit does not model the flaring activity. For this purpose, a new technique to remove the time flaring phases, is developed. This analysis provides a comprehensive study of the prompt and of the afterglow phase, trough the study of the best‐fit parameters.

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Discovery and confirmation of the shortest gamma-ray burst from a collapsar

Cited by 111 publications

References 153 publications

A Genuinely Short Gamma-Ray Burst from Massive Star Core Collapse

A Genuinely Short Gamma-Ray Burst from Massive Star Core Collapse

GRB 210217A: A short or a long GRB?

Comprehension of Jet Physics from the Analysis of the Gamma‐Ray Burst Afterglow Parameter Distributions

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