2017A&A...600A..98D


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.14CET19:15:58

2017A&A...600A..98D - Astronomy and Astrophysics, volume 600A, 98-98 (2017/4-1)

A study of gamma ray bursts with afterglow plateau phases associated with supernovae.

DAINOTTI M.G., NAGATAKI S., MAEDA K., POSTNIKOV S. and PIAN E.

Abstract (from CDS):

Context. The analysis of 176 gamma ray burst (GRB) afterglow plateaus observed by Swift from GRBs with known redshifts revealed that the subsample of long GRBs associated with supernovae (LONG-SNe), comprising 19 events, presents a very high correlation coefficient between the luminosity at the end of the plateau phase LX(Ta)=La and the end time of the plateau T*a. Furthermore, these SNe Ib/c associated with GRBs also obey the peak-magnitude stretch relation, which is similar to that used to standardize the SNe Ia.
Aims. Our aim is to investigate a category of GRBs with plateau and associated with SNe to compare our correlation for this sample with the correlation for long GRBs for which no associated SN has been observed (hereafter LONG-NO-SNe, 128 GRBs) and to check whether there is a difference among these subsamples.
Methods. We first adopted a nonparametric statistical method to take redshift evolution into account and to check if and how this effect may steepen the slope for the LONG-NO-SNe sample. This procedure is necessary because this sample is observed at much higher redshift than the GRB-SNe sample. Therefore, removing selection bias is the first step before any comparison among samples observed at different redshifts could be properly performed. Then, we applied the T-student test to evaluate a statistical difference between the slopes of the two samples.
Results. We demonstrate that there is no evolution for the slope of the LONG-NO-SNe sample and no evolution is expected for GRBs observed at small redshifts such as those present in the LONG-SNe sample. The difference between the slope of the LONG-NO-SNe and the slope of LONG-SNe, i.e., those with firm spectral detection of SN components, is statistically significant (P=0.005).
Conclusions. This possibly suggests that, unlike LONG-NO-SNe, LONG-SNe with firm spectroscopic features of the associated SNe might not require a standard energy reservoir in the plateau phase. Therefore, this analysis may open new perspectives in future theoretical investigations of the GRBs with plateau emission and that are associated with SNe.

Abstract Copyright: © ESO, 2017

Journal keyword(s): gamma rays: stars - methods: observational - methods: statistical - methods: statistical

Simbad objects: 25

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Number of rows : 25

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 SN 2010ma SN* 00 48 55.35 -34 33 59.5           SNIc 109 1
2 GRB 050824 gB 00 48 56.100 +22 36 32.00 19.66 21.03 20.46     ~ 151 0
3 GRB 120729A gB 00 52 17.84 +49 56 23.1           ~ 65 0
4 SN 2009nz SN* 02 26 19.87 -18 57 08.6           SN.? 218 1
5 SN 2006aj SN* 03 21 39.670 +16 52 02.27 17.96 19.11 17.40     SN.Ic-bl 810 1
6 GRB 060729 gB 06 21 31.850 -62 22 12.69           ~ 242 0
7 SN 2003lw SN* 08 02 30.1 -39 51 03       20.23   SN.Ic: 498 0
8 SN 2012bz SN* 09 07 38.38 +14 01 07.5           SNIb/c 125 1
9 GRB 111228A gB 10 00 16.04 +18 17 52.2           ~ 127 0
10 SN 2003dh SN* 10 44 50.030 +21 31 18.15     16.2     SN.IcPec 1098 2
11 GRB 050416 gB 12 33 54.600 +21 03 26.69     19.12     ~ 246 1
12 GRB 090424 gB 12 38 07.40 +16 49 45.9           ~ 194 0
13 GRB 070809 gB 13 35 04.2 -22 07 07           ~ 100 0
14 GRB 080319B gB 14 31 41.04 +36 18 09.2           ~ 417 0
15 GRB 100418A gB 17 05 26.96 +11 27 41.9           ~ 134 0
16 GRB 050525A gB 18 32 32.560 +26 20 22.34 14.19 15.17 13.91     SN.Ic: 342 1
17 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1618 2
18 GRB 090618 gB 19 36 01.80 +78 21 07.1           ~ 262 0
19 GRB 100621A gB 21 01 13.12 -51 06 22.5           ~ 140 0
20 GRB 060614 gB 21 23 32.140 -53 01 36.10 18.89 20.12 19.54     ~ 491 1
21 GRB 060505 gB 22 07 03.440 -27 48 51.89           ~ 215 1
22 GRB 061110A gB 22 25 09.800 -02 15 30.70 21.43         ~ 112 0
23 SN 2008hw SN* 22 39 50.39 -40 08 49.1           SNIc 138 1
24 GRB 051109B gB 23 01 50.330 +38 40 46.51           ~ 68 0
25 SN 2013fu SN* 23 54 29.91 +29 25 47.6           SNIb/c 90 1

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2019.12.14-19:15:58

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