# 2011A&A...529A.130D

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 Query : 2011A&A...529A.130D

2011A&A...529A.130D - Astronomy and Astrophysics, volume 529A, 130-130 (2011/5-1)

On the nature of GRB 050509b: a disguised short GRB.

DE BARROS G., AMATI L., BERNARDINI M.G., BIANCO C.L., CAITO L., IZZO L., PATRICELLI B. and RUFFINI R.

Abstract (from CDS):

GRB 050509b, detected by the Swift satellite, is the first case where an X-ray afterglow has been observed associated with a short gamma-ray burst (GRB). Within the fireshell model, the canonical GRB light curve presents two different components: the proper-GRB (P-GRB) and the extended afterglow. Their relative intensity is a function of the fireshell baryon loading parameter B and of the CircumBurst Medium (CBM) density (nCBM). In particular, the traditionally called short GRBs can be either genuine'' short GRBs (with B≲10–5, where the P-GRB is energetically predominant) or disguised'' short GRBs (with B>3.0x10–4 and nCBM≪1, where the extended afterglow is energetically predominant). We verify whether GRB 050509b can be classified as a genuine'' short or a disguised'' short GRB, in the fireshell model. We investigate two alternative scenarios. In the first, we start from the assumption that this GRB is a genuine'' short burst. In the second attempt, we assume that this GRB is a disguised'' burst. If GRB 050509b were a genuine short GRB, there should initially be very hard emission, which is ruled out by the observations. The analysis that assumes that this is a disguised short GRB is compatible with the observations. The theoretical model predicts a value of the extended afterglow energy peak that is consistent with the Amati relation. GRB 050509b cannot be classified as a genuine'' short GRB. The observational data are consistent with a disguised'' short GRB classification, i.e., a long burst with a weak extended afterglow deflated'' by the low density of the CBM. We expect that all short GRBs with measured redshifts are disguised short GRBs because of a selection effect: if there is enough energy in the afterglow to measure the redshift, then the proper GRB must be less energetic than the afterglow. The Amati relation is found to be fulfilled only by the extended afterglow excluding the P-GRB.

Journal keyword(s): gamma-ray burst: individual: GRB 050509b - gamma-ray burst: general - black hole physics - binaries: general - supernovae: general

CDS comments: Fig.1 Galaxy G1 = 2MASX J12361286+2858580

Full paper

 Number of rows : 17
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 GRB 071227 gB 03 52 31.09 -55 59 03.3           ~ 160 0
2 GRB 970228 gB 05 01 46.7 +11 46 53           ~ 630 1
3 [CSB2005b] S6 G 12 33 13.63 +28 59 07.7           ~ 5 0
4 2MASXI J1236128+285858 BiC 12 36 12.8803407000 +28 58 58.780075656           ~ 23 1
5 [BFP2005] J3 ? 12 36 13.435 +28 58 56.88           ~ 3 0
6 [BFP2005] J2 ? 12 36 13.464 +28 59 05.18           ~ 3 0
7 [BFP2005] J4 ? 12 36 13.471 +28 59 06.87           ~ 3 0
8 [BFP2005] J1 ? 12 36 13.574 +28 59 03.84           ~ 3 0
9 [CSB2005b] S1 G 12 36 13.7 +28 58 57           ~ 7 0
10 [CSB2005b] S4 ? 12 36 13.7 +28 59 03           ~ 6 0
11 [CSB2005b] S5 ? 12 36 13.88 +28 59 01.0           ~ 6 0
12 [CSB2005b] S3 ? 12 36 14.0 +28 59 01           ~ 7 0
13 [CSB2005b] S2 G 12 36 14.1 +28 59 00           ~ 7 0
14 [BFP2005] J5 ? 12 36 14.237 +28 59 05.39           ~ 2 0
15 GRB 050509B gB 12 36 18.000 +29 01 24.00           ~ 294 1
16 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1737 2
17 GRB 060614 gB 21 23 32.140 -53 01 36.10 18.89 20.12 19.54     ~ 540 1

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2022.08.08-02:40:15