2019A&A...623A..26P


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.27CET18:38:11

2019A&A...623A..26P - Astronomy and Astrophysics, volume 623A, 26-26 (2019/3-1)

Are long gamma-ray bursts biased tracers of star formation? Clues from the host galaxies of the Swift/BAT6 complete sample of bright LGRBs. III. Stellar masses, star formation rates, and metallicities at z > 1.

PALMERIO J.T., VERGANI S.D., SALVATERRA R., SANDERS R.L., JAPELJ J., VIDAL-GARCIA A., D'AVANZO P., CORRE D., PERLEY D.A., SHAPLEY A.E., BOISSIER S., GREINER J., LE FLOC'H E. and WISEMAN P.

Abstract (from CDS):


Aims. Long gamma-ray bursts (LGRB) have been proposed as promising tracers of star formation owing to their association with the core-collapse of massive stars. Nonetheless, previous studies we carried out at z<1 support the hypothesis that the conditions necessary for the progenitor star to produce an LGRB (e.g. low metallicity), were challenging the use of LGRBs as star-formation tracers, at least at low redshift. The goal of this work is to characterise the population of host galaxies of LGRBs at 1<z<2, investigate the conditions in which LGRBs form at these redshifts and assess their use as tracers of star formation.
Methods. We performed a spectro-photometric analysis to determine the stellar mass, star formation rate, specific star formation rate and metallicity of the complete, unbiased host galaxy sample of the Swift/BAT6 LGRB sample at 1<z<2. We compared the distribution of these properties to the ones of typical star-forming galaxies from the MOSDEF and COSMOS2015 Ultra Deep surveys, within the same redshift range.
Results. We find that, similarly to z<1, LGRBs do not directly trace star formation at 1<z<2, and they tend to avoid high-mass, high-metallicity host galaxies. We also find evidence for an enhanced fraction of starbursts among the LGRB host sample with respect to the star-forming population of galaxies. Nonetheless we demonstrate that the driving factor ruling the LGRB efficiency is metallicity. The LGRB host distributions can be reconciled with the ones expected from galaxy surveys by imposing a metallicity upper limit of logOH∼8.55. We can determine upper limits on the fraction of super-solar metallicity LGRB host galaxies of ∼20%, 10% at z<1, 1<z<2, respectively.
Conclusions. Metallicity rules the LGRB production efficiency, which is stifled at Z≥0.7Z. Under this hypothesis we can expect LGRBs to trace star formation at z>3, once the bulk of the star forming galaxy population are characterised by metallicities below this limit. The role played by metallicity can be explained by the conditions necessary for the progenitor star to produce an LGRB. The moderately high metallicity threshold found is in agreement with the conditions necessary to rapidly produce a fast-rotating Wolf-Rayet stars in close binary systems, and could be accommodated by single star models under chemically homogeneous mixing with very rapid rotation and weak magnetic coupling.

Abstract Copyright: © J. T. Palmerio et al. 2019

Journal keyword(s): gamma-ray burst: general - galaxies: star formation - galaxies: abundances

Simbad objects: 29

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Number of rows : 29

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9661 1
2 GRB 081221 gB 01 03 10.2 -24 32 53           ~ 122 0
3 GRB 080602 gB 01 16 42.18 -09 13 55.4           ~ 49 0
4 GRB 081222 gB 01 30 57.76 -34 05 44.0           ~ 153 0
5 GRB 091208B gB 01 57 38.50 +16 52 50.7           ~ 156 0
6 GRB 060908 gB 02 07 18.360 +00 20 31.20 16.99 18.34 16.85     ~ 177 0
7 GRB 060306 gB 02 44 22.830 -02 08 55.00           ~ 95 0
8 GRB 100728B gB 02 56 13.44 +00 16 51.5           ~ 101 0
9 GRB 090926B gB 03 05 14.30 -38 59 50.9           ~ 114 1
10 GRB 061007 gB 03 05 19.510 -50 30 02.50 14.28 14.40 12.95     ~ 272 1
11 GRB 050318 gB 03 18 51.000 -46 23 43.61 18.10 18.68 17.58     ~ 159 0
12 GRB 070328 gB 04 20 27.680 -34 04 00.60 20.29         ~ 76 0
13 GRB 081121 gB 05 57 07.70 -60 36 42.1           ~ 111 0
14 GRB 090201 gB 06 08 12.30 -46 36 16.1           ~ 50 0
15 GRB 080517 gB 06 48 58.00 +50 44 06.3           ~ 41 1
16 GRB 061121 gB 09 48 54.570 -13 11 42.68 17.19 17.71 17.02     ~ 291 0
17 GRB 070306 gB 09 52 23.220 +10 28 55.20           ~ 180 1
18 GRB 100615A gB 11 48 49.25 -19 28 52.2           ~ 89 0
19 GRB 050802 gB 14 37 05.820 +27 47 12.62 16.85 17.38 16.97     ~ 160 0
20 GRB 060814 gB 14 45 21.480 +20 35 11.80           ~ 188 0
21 GRB 080721 gB 14 57 55.76 -11 43 24.9           ~ 141 0
22 GRB 050401 gB 16 31 28.84 +02 11 14.5           ~ 305 0
23 GRB 080605 gB 17 28 30.04 +04 00 56.9           ~ 154 0
24 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1671 2
25 GRB 050922C gB 21 09 33.000 -08 45 30.10 15.15 15.86 14.69     ~ 254 0
26 GRB 080413B gB 21 44 34.62 -19 58 51.2           ~ 150 0
27 GRB 080804 gB 21 54 41.90 -53 11 20.2           ~ 120 0
28 GRB 071117 gB 22 20 10.40 -63 26 36.6           ~ 89 0
29 GRB 090812 gB 23 32 48.5 -10 36 17           ~ 123 0

    Equat.    Gal    SGal    Ecl

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2021.01.27-18:38:11

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