Revealing nature of GRB 210205A, ZTF21aaeyldq (AT2021any) and follow-up observations with the 4K × 4K CCD imager + 3.6m DOT

DOI: 
10.1007/s12036-021-09794-4
Publication date: 
01/06/2022
Main author: 
Gupta R.
IAA authors: 
Castro-Tirado, A. J.;Hu, Y. D.;Fernández-García, E.;Caballero-García, M. D.;Castro-Tirado, M.
Authors: 
Gupta, Rahul;Kumar, Amit;Pandey, Shashi Bhushan;Castro-Tirado, A. J.;Ghosh, Ankur;Dimple, ;Hu, Y. D.;Fernández-García, E.;Caballero-García, M. D.;Castro-Tirado, M.;Hedrosa, R. P.;Hermelo, I.;Vico, I.;Misra, Kuntal;Kumar, Brajesh;Aryan, Amar;Tiwari, Sugriva Nath
Journal: 
Journal of Astrophysics and Astronomy
Refereed: 
Yes
Publication type: 
Article
Volume: 
43.0
Pages: 
11
Number: 
11
Abstract: 
Optical follow-up observations of optical afterglows of gamma-ray bursts are crucial to probe the geometry of outflows, emission mechanisms, energetics and burst environments. We performed the follow-up observations of GRB 210205A and ZTF21aaeyldq (AT2021any) using the 3.6m Devasthal optical telescope (DOT) around one day after the burst to deeper limits due to the longitudinal advantage of the place. This paper presents our analysis of the two objects using data from other collaborative facilities, i.e., 2.2m Calar Alto Astronomical Observatory (CAHA) and other archival data. Our analysis suggests that GRB 210205A is a potential dark burst once compared with the X-ray afterglow data. Also, comparing results with other known and well-studied dark GRBs samples indicate that the reason for the optical darkness of GRB 210205A could either be intrinsic faintness or a high redshift event. Based on our analysis, we also found that ZTF21aaeyldq is the third known orphan afterglow with a measured redshift except for ZTF20aajnksq (AT2020blt) and ZTF19abvizsw (AT2019pim). The multiwavelength afterglow modeling of ZTF21aaeyldq using the afterglowpy package demands a forward shock model for an ISM-like ambient medium with a rather wider jet opening angle. We determine circumburst density of n= 0.87 cm- 3, kinetic energy Ek= 3.80 × 10 52 erg and the afterglow modeling also indicates that ZTF21aaeyldq is observed on-axis (θobs< θcore) and a gamma-ray counterpart was missed by GRBs satellites. Our results emphasize that the 3.6m DOT has a unique capability for deep follow-up observations of similar and other new transients for deeper observations as a part of time-domain astronomy in the future.
Database: 
SCOPUS
ADS
URL: 
https://ui.adsabs.harvard.edu/#abs/2022JApA...43...11G/abstract
ADS Bibcode: 
2022JApA...43...11G
Keywords: 
Gamma-ray burst: general—gamma-ray burst: individual: GRB 210205A and ZTF21aaeyldq—methods: data analysis—telescope