GRB 171010A/SN 2017htp: a GRB-SN at z = 0.33

Melandri, A.; Malesani, D.; Izzo, L.; Japelj, J.; Vergani, S. D.; Schady, P.; Carracedo, Ana Sagués; Postigo, A. de Ugarte; Anderson, J. P.; Barbarino, C.; Bolmer, J.; Breeveld, A. A.; Calissendorff, Per; Campana, S.; Cano, Z.; Carini, R.; Covino, S.; D’Avanzo, P.; D’Elia, V.; Valle, M. Della; Pasquale, M. de; Fynbo, J. P. U.; Gromadzki, M.; Hammer, F.; Hartmann, D. H.; Heintz, K. E.; Inserra, C.; Jakobsson, P.; Канн, Д. А.; Kotilainen, Jari; Maguire, K.; Masetti, N.; Nicholl, M.; E, F Olivares; Pugliese, G.; Rossi, A.; Salvaterra, R.; Sollerman, J.; Stone, M.; Tagliaferri, G.; Tomasella, L.; Thöne, C. C.; Xu, D.; Young, D. R.

doi:10.1093/mnras/stz2900

Cited by 23 publications

(20 citation statements)

References 74 publications

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“…Many of these GRBs are associated with broad-line Type Ic supernovae. The list of such GRBssupernovae include some of the well studied cases such as, GRB 980425/SN 1998bw (z = 0.00866, Galama et al 1998), GRB 030329/SN 2003dh (z = 0.1685, Hjorth et al 2003, GRB 031203/SN 2003lw (z = 0.1055, Malesani et al 2004), GRB 060218/SN 2006aj (z = 0.0335, Campana et al 2006), GRB 100316D/SN 2010bh (z = 0.0591, Starling et al 2011), GRB 111209A/SN 2011kl (z = 0.677, Gao et al 2016), GRB 120422A/SN 2012bz (z = 0.283, Melandri et al 2012), GRB 130427A/SN 2013cq (z = 0.3399, Melandri et al 2014), GRB 130702A/SN 2013dx (z = 0.145, Cenko et al 2013), GRB 161219B/SN 2016jca (z = 0.1475, Cano et al 2017b), GRB 171010A/SN 2017htp (z = 0.33, Melandri et al 2019), GRB 190829A/ SN 2019oyu (z = 0.08, Terreran et al 2019, although only the five are nearby, z 0.1 (Cano et al 2017a, and references therein).…”

Section: Introductionmentioning

confidence: 99%

1000 days of lowest frequency emission from the low-luminosity GRB 171205A

Maity,

Chandra

2020

Preprint

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We report the lowest frequency measurements of gamma-ray burst (GRB) 171205A with the upgraded Giant Metrewave Radio Telescope (uGMRT) covering a frequency range from 250-1450 MHz and a period of 4 − 937 days. It is the first GRB afterglow detected at 250-500 MHz frequency range and the second brightest GRB detected with the uGMRT. Even though the GRB is observed for nearly 1000 days, there is no evidence of transition to non-relativistic regime. We also analyse the archival Chandra X-ray data on day ∼ 70 and day ∼ 200. We also find no evidence of a jet break from the analysis of combined data. We fit synchrotron afterglow emission arising from a relativistic, isotropic, self-similar deceleration as well as from a shock-breakout of wide-angle cocoon. Our data also allow us to discern the nature and the density of the circumburst medium. We find that the density profile deviates from a standard constant density medium and suggests that the GRB exploded in a stratified wind like medium. Our analysis shows that the lowest frequency measurements covering the absorbed part of the light curves are critical to unravel the GRB environment. Our data combined with other published measurements indicate that the radio afterglow has contribution from two components: a weak, possibly slightly off-axis jet and a surrounding wider cocoon, consistent with the results of Izzo et al. (2019). The cocoon emission likely dominates at early epochs, whereas the jet starts to dominate at later epochs, resulting in flatter radio lightcurves.

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Section: Introductionmentioning

confidence: 99%

1000 days of lowest frequency emission from the low-luminosity GRB 171205A

Maity,

Chandra

2020

Preprint

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“…More than 1400 bursts have been discovered by the Neil Gehrels Swift Observatory (Swift hereafter) in the last 16 years, among which only 40-50 GRBs have an associated SN identified by late bumps in their optical afterglow light curves, and to date, just 28 have been spectroscopically confirmed (A. Rossi et al 2022, in preparation;Cano et al 2017a;Izzo et al 2019;Melandri et al 2022 and references therein;Cano et al 2017b;Ashall et al 2019;Klose et al 2019;Melandri et al 2019;Hu et al 2021). The burst duration for all these events is more than 2 s; therefore they are considered LGRBs.…”

Section: Introductionmentioning

confidence: 99%

The Peculiar Short-duration GRB 200826A and Its Supernova*

Rossi

Rothberg

Palazzi

et al. 2022

ApJ

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Gamma-ray bursts (GRBs) are classified into long and short events. Long GRBs (LGRBs) are associated with the end states of very massive stars, while short GRBs (SGRBs) are linked to the merger of compact objects. GRB 200826A was a peculiar event, because by definition it was an SGRB, with a rest-frame duration of ∼0.5 s. However, this event was energetic and soft, which is consistent with LGRBs. The relatively low redshift (z = 0.7486) motivated a comprehensive, multiwavelength follow-up campaign to characterize its host, search for a possible associated supernova (SN), and thus understand the origin of this burst. To this aim we obtained a combination of deep near-infrared (NIR) and optical imaging together with spectroscopy. Our analysis reveals an optical and NIR bump in the light curve whose luminosity and evolution are in agreement with several SNe associated to LGRBs. Analysis of the prompt GRB shows that this event follows the E p,i–E iso relation found for LGRBs. The host galaxy is a low-mass star-forming galaxy, typical of LGRBs, but with one of the highest star formation rates, especially with respect to its mass ( log M * / M ⊙ = 8.6 , SFR ∼ 4.0 M ⊙ yr−1). We conclude that GRB 200826A is a typical collapsar event in the low tail of the duration distribution of LGRBs. These findings support theoretical predictions that events produced by collapsars can be as short as 0.5 s in the host frame and further confirm that duration alone is not an efficient discriminator for the progenitor class of a GRB.

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“…According to the observation of prompt emission duration, GRBs is divided into long-duration bursts (LGRBs) and shortduration bursts (SGRBs) with a dividing line of ∼2 s (Kouveliotou et al 1993). The observations and analysis for some dozen supernovae (SNe) associated with LGRBs (Hjorth et al 2003;Matheson et al 2003;Stanek et al 2003;Malesani et al 2004;Deng et al 2005;Campana et al 2006;Mirabal et al 2006;Modjaz et al 2006;Sollerman et al 2006;Maeda et al 2007;Chornock et al 2010;Starling et al 2011;Bufano et al 2012;Melandri et al 2012Melandri et al , 2014Melandri et al , 2019Olivares et al 2012;Singer et al 2013;Schulze et al 2014;D'Elia et al 2015;Toy et al 2016;Cano et al 2017a;Volnova et al 2017;Ashall et al 2019;Hu et al 2021) indicate that most LGRBs are produced by the explosions of massive stars. On the other hand, the confirmation of SSS17a/AT2017gfo, which is a kilonova associated with GW170817 that is a gravitational wave emitted by a merger of a neutron star binary and GRB 170817A that is an SGRB (Abbott et al 2017;Arcavi et al 2017;Coulter et al 2017;Shappee et al 2017), supports the conjecture that at least a fraction of SGRBs are produced by the mergers of compact binary stars.…”

Section: Introductionmentioning

confidence: 99%

Modeling the Multiband Light Curves of the Afterglows of Three Gamma-Ray Bursts and their Associated Supernovae

Lian

Wang

Gan

et al. 2022

ApJ

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Some dozen supernovae (SNe) associated with long gamma-ray bursts (GRBs) have been confirmed. Most of the previous studies derive the physical properties of the GRB-SNe by fitting the constructed (pseudo-)bolometric light curves. However, many GRB-SNe only have a few filter data, for which the (pseudo-)bolometric light curves are very difficult to construct. Additionally, constructing (pseudo-)bolometric light curves rely on some assumptions. In this paper, we use the multiband broken power-law plus 56Ni model to fit the multiband light curves of the afterglows and the SNe (SN 2001ke, SN 2013dx, and SN 2016jca) associated with three GRBs (GRB 011121, GRB 130702A, and GRB 161219B). We find our model can account for the multiband light curves of the three GRB-SNe (except for the late-time z-band light curve of two events), indicating that the model is a reliable model. The 56Ni masses we derive are higher than those in the literature. This might be due to the fact that the 56Ni masses in the literature are usually obtained by fitting the pseudo-bolometric light curves whose luminosities are usually (significantly) underestimated. We suggest that the multiband model can not only be used to fit the multiband light curves of GRB-SNe that have many filter observations, but also fit those having sparse data.

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GRB 171010A/SN 2017htp: a GRB-SN at z = 0.33

Cited by 23 publications

References 74 publications

1000 days of lowest frequency emission from the low-luminosity GRB 171205A

1000 days of lowest frequency emission from the low-luminosity GRB 171205A

The Peculiar Short-duration GRB 200826A and Its Supernova*

Modeling the Multiband Light Curves of the Afterglows of Three Gamma-Ray Bursts and their Associated Supernovae

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