2015A&A...583A.129Y


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.14CEST19:41:51

2015A&A...583A.129Y - Astronomy and Astrophysics, volume 583A, 129-129 (2015/11-1)

The sharpness of gamma-ray burst prompt emission spectra.

YU H.-F., VAN EERTEN H.J., GREINER J., SARI R., BHAT P.N., VON KIENLIN A., PACIESAS W.S. and PREECE R.D.

Abstract (from CDS):

We study the sharpness of the time-resolved prompt emission spectra of gamma-ray bursts (GRBs) observed by the Gamma-ray Burst Monitor (GBM) on board the Fermi Gamma-ray Space Telescope. We aim to obtain a measure of the curvature of time-resolved spectra that can be compared directly to theory. This tests the ability of models such as synchrotron emission to explain the peaks or breaks of GBM prompt emission spectra. We take the burst sample from the official Fermi GBM GRB time-resolved spectral catalog. We re-fit all spectra with a measured peak or break energy in the catalog best-fit models in various energy ranges, which cover the curvature around the spectral peak or break, resulting in a total of 1113 spectra being analyzed. We compute the sharpness angles under the peak or break of the triangle constructed under the model fit curves and compare them to the values obtained from various representative emission models: blackbody, single-electron synchrotron, synchrotron emission from a Maxwellian or power-law electron distribution. We find that 35% of the time-resolved spectra are inconsistent with the single-electron synchrotron function, and 91% are inconsistent with the Maxwellian synchrotron function. The single temperature, single emission time, and location blackbody function is found to be sharper than all the spectra. No general evolutionary trend of the sharpness angle is observed, neither per burst nor for the whole population. It is found that the limiting case, a single temperature Maxwellian synchrotron function, can only contribute up to 58–18+23% of the peak flux. Our results show that even the sharpest but non-realistic case, the single-electron synchrotron function, cannot explain a large fraction of the observed GRB prompt spectra. Because any combination of physically possible synchrotron spectra added together will always further broaden the spectrum, emission mechanisms other than optically thin synchrotron radiation are likely required in a full explanation of the spectral peaks or breaks of the GRB prompt emission phase.

Abstract Copyright:

Journal keyword(s): gamma rays: stars - gamma-ray burst: general - radiation mechanisms: non-thermal - radiation mechanisms: thermal - methods: data analysis

Simbad objects: 70

goto Full paper

goto View the reference in ADS

Number of rows : 70

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 GRB 110428A gB 00 21 50.62 +64 48 53.3           ~ 20 0
2 GRB 110921B gB 01 12 -27.8           ~ 10 0
3 GRB 100322A gB 01 33 -10.2           ~ 15 0
4 GRB 101014A gB 01 47.8 -51 04           ~ 19 0
5 GRB 120129A gB 02 02 +59.3           ~ 10 0
6 SN 2009nz SN* 02 26 19.87 -18 57 08.6           ~ 226 1
7 GRB 100324B gB 02 39 -19.3           ~ 16 0
8 GRB 081125 gB 02 51 -18.9           ~ 25 0
9 GRB 110825A gB 02 59 11.59 +15 25 38.4           ~ 21 0
10 GRB 120526A gB 04 25 -32.2           ~ 9 0
11 GRB 090530B gB 04 53 +13.8           ~ 20 0
12 GRB 101126A gB 05 39 -22.6           ~ 14 0
13 GRB 110920A gB 05 50 +38.8           ~ 19 0
14 GRB 090820 gB 05 51 +27.1           ~ 34 0
15 GRB 100728A gB 05 55 01.99 -15 15 20.1           ~ 99 0
16 GRB 100829A gB 06 02 +30.3           ~ 13 0
17 GRB 090328 gB 06 02 39.69 -41 52 55.1           ~ 140 1
18 GRB 090809B gB 06 21 +00.2           ~ 25 0
19 GRB 110407B gB 06 30 -11.9           ~ 6 0
20 GRB 100511A gB 07 17.2 -04 39           ~ 18 0
21 GRB 120426A gB 07 26 -65.6           ~ 11 0
22 GRB 081207 gB 07 29.6 +70 30           ~ 22 0
23 GRB 100719D gB 07 33 +05.4           ~ 8 0
24 GRB 100724B gB 07 58 +75.9           ~ 74 0
25 GRB 080916C gB 07 59 23.24 -56 38 16.8           ~ 315 0
26 GRB 120119A gB 08 00 06.940 -09 04 53.83           ~ 116 0
27 GRB 081215A gB 08 22 +54.0           ~ 46 0
28 GRB 091128 gB 08 31 +01.7           ~ 15 0
29 GRB 090804A gB 08 42 -11.3           ~ 17 0
30 GRB 101123A gB 08 45.0 +06 31           ~ 18 0
31 GRB 110622A gB 08 56 +19.5           ~ 8 0
32 GRB 080817 gB 10 05 09.600 -19 15 36.00           ~ 22 0
33 GRB 090626 gB 11 17.2 -36 03           ~ 48 0
34 GRB 120624B gB 11 23 32.27 +08 55 41.5           ~ 58 0
35 GRB 111216A gB 12 24 +05.8           ~ 7 0
36 GRB 090424 gB 12 38 07.40 +16 49 45.9           ~ 202 0
37 GRB 101231A gB 12 47 +17.6           ~ 8 0
38 GRB 100414A gB 12 48 30.0 +08 41 35           ~ 96 0
39 GRB 081224A gB 13 26.8 +75 06           ~ 25 0
40 GRB 091120 gB 15 07.2 -21 47           ~ 27 0
41 GRB 120328B gB 15 12 +22.8           ~ 14 0
42 GRB 110301A gB 15 17.4 +29 24           ~ 34 0
43 GRB 080825C gB 15 28.8 -04 54           ~ 60 0
44 GRB 100910A gB 15 52.4 -34 37           ~ 10 0
45 GRB 091003A gB 16 46 04.680 +36 37 31.08           ~ 102 0
46 GRB 090902B gB 17 39 45.26 +27 19 28.1           ~ 327 0
47 GRB 111220A gB 17 50 -56.0           ~ 6 0
48 GRB 090718B gB 18 16 -36.4           ~ 18 0
49 GRB 111003A gB 18 27 -62.3           ~ 8 0
50 GRB 110731A gB 18 42 00.99 -28 32 13.8           ~ 121 0
51 GRB 100826A gB 18 56 -23.2           ~ 52 0
52 GRB 110625A gB 19 06 55.85 +06 45 19.2           ~ 49 0
53 GRB 120707A gB 19 24 -34.4           ~ 11 0
54 GRB 120204A gB 19 30 -03.6           ~ 6 0
55 GRB 090618 gB 19 36 01.80 +78 21 07.1           ~ 269 0
56 GRB 091010 gB 19 54 40.510 -22 32 17.36           ~ 42 0
57 GRB 120226A gB 20 12 +48.7           ~ 13 0
58 GRB 100918A gB 20 34 -46.0           ~ 9 0
59 GRB 090528B gB 20 49 +32.7           ~ 24 0
60 GRB 110717B gB 20 51 -14.8           ~ 7 0
61 GRB 101023A gB 21 11 51.26 -65 23 17.7           ~ 56 0
62 GRB 090829A gB 21 56.8 -34 12           ~ 24 0
63 GRB 110721A gB 22 10 -38.6           ~ 109 0
64 GRB 110817A gB 22 24 09 -45 50.0           ~ 13 0
65 GRB 090719 gB 22 45 -67.9           ~ 32 0
66 GRB 100707A gB 23 24 -06.6           ~ 36 0
67 GRB 100612B gB 23 28 -01.8           ~ 18 0
68 GRB 090131 gB 23 29.2 +21 12           ~ 31 0
69 GRB 110729A gB 23 34 +05.0           ~ 7 0
70 GRB 090926A gB 23 33 36.18 -66 19 25.9           ~ 250 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2015A&A...583A.129Y and select 'bookmark this link' or equivalent in the popup menu


2020.07.14-19:41:51

© Université de Strasbourg/CNRS

    • Contact