dc.contributor.author |
Kumar, Harsh |
|
dc.contributor.author |
Gupta, Rahul |
|
dc.contributor.author |
Saraogi, Divita |
|
dc.contributor.author |
Ahumada, Tomás |
|
dc.contributor.author |
Andreoni, Igor |
|
dc.contributor.author |
Anupama, G. C |
|
dc.contributor.author |
Aryan, Amar |
|
dc.contributor.author |
Barway, Sudhanshu |
|
dc.contributor.author |
Bhalerao, Varun |
|
dc.contributor.author |
Chandra, Poonam |
|
dc.contributor.author |
Coughlin, Michael W |
|
dc.contributor.author |
Dimple |
|
dc.contributor.author |
Dutta, Anirban |
|
dc.contributor.author |
Ghosh, Ankur |
|
dc.contributor.author |
Ho, Anna Y. Q |
|
dc.contributor.author |
Kool, E. C |
|
dc.contributor.author |
Kumar, Amit |
|
dc.contributor.author |
Medford, Michael S |
|
dc.contributor.author |
Misra, Kuntal |
|
dc.contributor.author |
Pandey, Shashi B |
|
dc.contributor.author |
Perley, Daniel A |
|
dc.contributor.author |
Riddle, Reed |
|
dc.contributor.author |
Ror, Amit Kumar |
|
dc.contributor.author |
Setiadi, Jason M |
|
dc.contributor.author |
Yao, Yuhan |
|
dc.date.accessioned |
2022-08-23T06:12:52Z |
|
dc.date.available |
2022-08-23T06:12:52Z |
|
dc.date.issued |
2022-06 |
|
dc.identifier.citation |
Monthly Notices of the Royal Astronomical Society, Vol. 513, No. 2, pp. 2777–2793 |
en_US |
dc.identifier.issn |
1365-2966 |
|
dc.identifier.uri |
http://hdl.handle.net/2248/8018 |
|
dc.description |
Restricted Access |
en_US |
dc.description.abstract |
We present results from extensive broadband follow-up of GRB 210204A over the period of 30 d. We detect optical flares in the
afterglow at 7.6 × 105 s and 1.1 × 106 s after the burst: the most delayed flaring ever detected in a GRB afterglow. At the source
redshift of 0.876, the rest-frame delay is 5.8 × 105 s (6.71 d). We investigate possible causes for this flaring and conclude that
the most likely cause is a refreshed shock in the jet. The prompt emission of the GRB is within the range of typical long bursts:
it shows three disjoint emission episodes, which all follow the typical GRB correlations. This suggests that GRB 210204A
might not have any special properties that caused late-time flaring, and the lack of such detections for other afterglows might be
resulting from the paucity of late-time observations. Systematic late-time follow-up of a larger sample of GRBs can shed more
light on such afterglow behaviour. Further analysis of the GRB 210204A shows that the late-time bump in the light curve is
highly unlikely due to underlying SNe at redshift (z) = 0.876 and is more likely due to the late-time flaring activity. The cause
of this variability is not clearly quantifiable due to the lack of multiband data at late-time constraints by bad weather conditions.
The flare of GRB 210204A is the latest flare detected to date. |
en_US |
dc.language.iso |
en |
en_US |
dc.publisher |
Oxford University Press on behalf of Royal Astronomical Society |
en_US |
dc.relation.uri |
https://doi.org/10.1093/mnras/stac1061 |
|
dc.rights |
© Royal Astronomical Society |
|
dc.subject |
Methods: data analysis |
en_US |
dc.subject |
Gamma-ray burst: general |
en_US |
dc.subject |
Gamma-ray burst: individual: GRB 210204A |
en_US |
dc.title |
The long-active afterglow of GRB 210204A: detection of the most delayed flares in a gamma-ray burst |
en_US |
dc.type |
Article |
en_US |