2013A&A...558A..22H


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.03CEST22:50:39

2013A&A...558A..22H - Astronomy and Astrophysics, volume 558A, 22-22 (2013/10-1)

Progenitor delay-time distribution of short gamma-ray bursts: constraints from observations.

HAO J.-M. and YUAN Y.-F.

Abstract (from CDS):

The progenitors of short gamma-ray bursts (SGRBs) have not yet been well identified. The most popular model is the merger of compact object binaries (NS-NS/NS-BH). However, other progenitor models cannot be ruled out. The delay-time distribution of SGRB progenitors, which is an important property to constrain progenitor models, is still poorly understood. We aim to better constrain the luminosity function of SGRBs and the delay-time distribution of their progenitors with newly discovered SGRBs. We present a low-contamination sample of 16 Swift SGRBs that is better defined by a duration shorter than 0.8s. By using this robust sample and by combining a self-consistent star formation model with various models for the distribution of time delays, the redshift distribution of SGRBs is calculated and then compared to the observational data. We find that the power-law delay distribution model is disfavored and that only the lognormal delay distribution model with the typical delay τ≥3Gyr is consistent with the data. Comparing Swift SGRBs with T90>0.8s to our robust sample (T90<0.8s), we find a significant difference in the time delays between these two samples. Our results show that the progenitors of SGRBs are dominated by relatively long-lived systems (τ≥3Gyr), which contrasts the results found for Type Ia supernovae. We therefore conclude that primordial NS-NS systems are not favored as the dominant SGRB progenitors. Alternatively, dynamically formed NS-NS/BH and primordial NS-BH systems with average delays longer than 5Gyr may contribute a significant fraction to the overall SGRB progenitors.

Abstract Copyright:

Journal keyword(s): gamma-ray burst: general - binaries: close - stars: evolution - stars: formation - stars: neutron - black hole physics

Simbad objects: 27

goto Full paper

goto View the reference in ADS

Number of rows : 27

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 070810B gB 00 35 48.4 +08 49 18           ~ 45 0
2 GRB 100117A gB 00 45 04.56 -01 35 41.7           ~ 109 0
3 GRB 111117A gB 00 50 46.220 +23 00 39.22           ~ 81 0
4 GRB 070724A gB 01 51 14.08 -18 35 38.8           ~ 145 0
5 GRB 100206A gB 03 08 38.94 +13 09 25.5           ~ 103 0
6 GRB 070729 gB 03 45 16.04 -39 19 19.9           ~ 58 0
7 GRB 070714B gB 03 51 22.30 +28 17 51.3           ~ 169 1
8 GRB 071227 gB 03 52 31.09 -55 59 03.3           ~ 145 0
9 GRB 101219A gB 04 58 20.43 -02 32 23.0           ~ 99 0
10 GRB 061006 gB 07 24 07.660 -79 11 55.10           ~ 162 1
11 GRB 061217 gB 10 41 39.320 -21 07 22.11           ~ 107 0
12 GRB 090515 gB 10 56 41.0 +14 27 22           ~ 83 0
13 GRB 130603B gB 11 28 48.16 +17 04 18.2           ~ 265 0
14 GRB 050509B gB 12 36 18.000 +29 01 24.00           ~ 278 1
15 GRB 070809 gB 13 35 04.2 -22 07 07           ~ 112 0
16 GRB 060801 gB 14 12 01.290 +16 58 54.00           ~ 135 0
17 GRB 050813 gB 16 07 57.190 +11 14 57.80           ~ 122 1
18 GRB 050724 gB 16 24 44.400 -27 32 27.90     19.70     ~ 383 1
19 GRB 060502B gB 18 35 46.060 +52 37 51.45           ~ 121 1
20 GRB 080905A gB 19 10 39.10 -18 51 55.4           ~ 135 0
21 GRB 070429B gB 21 52 03.820 -38 49 42.20           ~ 94 0
22 GRB 051221 gB 21 54 48.626 +16 53 27.16 19.49         ~ 307 1
23 GRB 051210 gB 22 00 40.930 -57 36 47.10           ~ 109 0
24 GRB 061201 gB 22 08 32.060 -74 34 47.90           ~ 155 0
25 GRB 090510 gB 22 14 12.60 -26 35 51.1           ~ 408 1
26 GRB 080123 gB 22 35 46.100 -64 54 03.24           ~ 69 0
27 GRB 100816A gB 23 26 57.56 +26 34 42.6           ~ 118 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2013A&A...558A..22H and select 'bookmark this link' or equivalent in the popup menu


2020.07.03-22:50:39

© Université de Strasbourg/CNRS

    • Contact