2022A&A...666A..14S


Query : 2022A&A...666A..14S

2022A&A...666A..14S - Astronomy and Astrophysics, volume 666A, 14 (2022/10-1)

Are the host galaxies of long gamma-ray bursts more compact than star-forming galaxies of the field?

SCHNEIDER B., LE FLOC'H E., ARABSALMANI M., VERGANI S.D. and PALMERIO J.T.

Abstract (from CDS):


Context. Long gamma-ray bursts (GRBs) offer a promising tool for tracing the cosmic history of star formation, especially at high redshift, where conventional methods are known to suffer from intrinsic biases. Previous studies of GRB host galaxies at low redshift showed that high surface density of stellar mass and high surface density of star formation rate (SFR) can potentially enhance the GRB production. Evaluating the effect of such stellar densities at high redshift is therefore crucial to fully control the ability of long GRBs for probing the activity of star formation in the distant Universe.
Aims. We assess how the size, stellar mass, and star formation rate surface densities of distant galaxies affect the probability of their hosting a long GRB, using a sample of GRB hosts at z > 1 and a control sample of star-forming sources from the field.
Methods. We gathered a sample of 45 GRB host galaxies at 1 < z < 3.1 observed with the Hubble Space Telescope WFC3 camera in the near-infrared. Our subsample at 1 < z < 2 has cumulative distributions of redshift and stellar mass consistent with the host galaxies of known unbiased GRB samples, while our GRB host selection at 2 < z < 3.1 has lower statistics and is probably biased toward the high end of the stellar mass function. Using the GALFIT parametric approach, we modeled the GRB host light profile with a Sérsic component and derived the half-light radius for 35 GRB hosts, which we used to estimate the star formation rate and stellar mass surface densities of each object. We compared the distribution of these physical quantities to the SFR-weighted properties of a complete sample of star-forming galaxies from the 3D-HST deep survey at a comparable redshift and stellar mass.
Results. We show that similarly to z < 1, GRB hosts are smaller in size and they have higher stellar mass and star formation rate surface densities than field galaxies at 1 < z < 2. Interestingly, this result is robust even when separately considering the hosts of GRBs with optically bright afterglows and the hosts of dark GRBs, as the two subsamples share similar size distributions. At z > 2, however, GRB hosts appear to have sizes and stellar mass surface densities more consistent with those characterizing the field galaxies. This may reveal an evolution with redshift of the bias between GRB hosts and the overall population of star-forming sources, although we cannot exclude that our result at z > 2 is also affected by the prevalence of dark GRBs in our selection.
Conclusions. In addition to a possible trend toward a low-metallicity environment, other environmental properties such as stellar density appear to play a role in the formation of long GRBs, at least up to z ∼ 2. This might suggest that GRBs require special environments to enhance their production.

Abstract Copyright: © B. Schneider et al. 2022

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

Simbad objects: 53

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Number of rows : 53
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 GRB 071031 gB 00 25 37.40 -58 03 33.9           ~ 167 0
2 Fermi bn081221681 gB 01 03 10.2 -24 32 53           ~ 159 0
3 GRB 060719 gB 01 13 43.380 -48 22 55.09           ~ 96 0
4 Fermi bn091208410 gB 01 57 38.50 +16 52 50.7           ~ 193 0
5 Fermi bn090113778 gB 02 08 16.00 +33 26 08.4           ~ 81 0
6 GRB 080707 gB 02 10 28.48 +33 06 35.1           ~ 73 0
7 GRB 050406 gB 02 17 52.200 -50 11 15.81     18.83     ~ 122 0
8 GRB 070802 gB 02 27 35.91 -55 31 39.1           ~ 153 0
9 GRB 061007 gB 03 05 19.510 -50 30 02.50 14.28 14.40 12.95     ~ 291 1
10 NAME GOODS Southern Field reg 03 32 28.0 -27 48 30           ~ 1347 1
11 NAME Hubble Ultra Deep Field reg 03 32 39.0 -27 47 29           ~ 1675 0
12 GRB 090407 gB 04 35 54.98 -12 40 45.5           ~ 73 0
13 GRB 060124 gB 05 08 25.900 +69 44 26.98   18.91 17.35     ~ 265 0
14 GRB 081121 gB 05 57 07.70 -60 36 42.1           ~ 133 0
15 Fermi bn080928628 gB 06 20 16.85 -55 11 59.3           ~ 166 0
16 GRB 070125 gB 07 51 17.80 +31 09 04.8           ~ 182 0
17 Fermi bn120119170 gB 08 00 06.940 -09 04 53.83           ~ 161 0
18 Fermi bn150314205 gB 08 26 40.82 +63 50 03.4           ~ 92 0
19 GRB 140331A gB 08 59 27.46 +02 43 02.3           ~ 24 0
20 GRB 070306 gB 09 52 23.220 +10 28 55.20           ~ 207 1
21 NAME COSMOS Field reg 10 00 28.60 +02 12 21.0           ~ 2981 0
22 GRB 110709B gB 10 58 37.2 -23 27 18           ~ 83 0
23 GRB 080603B gB 11 46 07.46 +68 03 38.5           ~ 138 0
24 Fermi bn100615083 gB 11 48 49.25 -19 28 52.2           ~ 114 0
25 GRB 050408 gB 12 02 17.320 +10 51 10.00           ~ 151 0
26 GRB 090426 gB 12 36 19.49 +32 59 05.5           ~ 206 0
27 NGC 4698 Sy2 12 48 22.9082830584 +08 29 14.667552276   13.24 12.27     ~ 485 0
28 Fermi bn100414097 gB 12 48 30.0 +08 41 35           ~ 120 0
29 GRB 080607A gB 12 59 47.14 +15 55 09.6           ~ 235 0
30 GRB 060512 gB 13 03 05.810 +41 11 27.21 19.12 19.63 17.20     ~ 134 0
31 GRB 070208 gB 13 11 32.607 +61 57 54.37 20.79 20.79 19.86     ~ 108 0
32 GRB 080207 gB 13 50 03.02 +07 30 08.0           ~ 104 0
33 GRB 060814 gB 14 45 21.480 +20 35 11.80           ~ 219 0
34 GRB 090404 gB 15 56 55.80 +35 31 03.4           ~ 70 0
35 GRB 060502A gB 16 03 42.480 +66 36 02.49     18.65     ~ 133 0
36 GRB 070521 gB 16 10 38.600 +30 15 22.70           ~ 149 0
37 GRB 050401 gB 16 31 28.84 +02 11 14.5           ~ 336 0
38 GRB 080319C gB 17 15 55.48 +55 23 31.7           ~ 159 0
39 GRB 080605 gB 17 28 30.04 +04 00 56.9           ~ 178 0
40 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 14463 0
41 GRB 090418A gB 17 57 15.17 +33 24 21.1           ~ 88 0
42 GRB 071122 gB 18 26 25.26 +47 04 29.5           ~ 75 0
43 GRB 080325 gB 18 31 34.40 +36 31 26.1           ~ 71 0
44 GRB 080603A gB 18 37 37.95 +62 44 39.6           ~ 83 0
45 Fermi bn081008832 gB 18 39 52.40 -57 25 58.8           ~ 199 0
46 GRB 080520 gB 18 40 46.50 -54 59 30.4           ~ 64 0
47 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1827 2
48 GRB 050315 gB 20 25 54.100 -42 36 02.19           ~ 216 0
49 Fermi bn160509374 gB 20 47 00.90 +76 06 30.1           ~ 111 0
50 GRB 080805 gB 20 56 55.30 -62 25 58.8           ~ 92 0
51 GRB 100621A gB 21 01 13.12 -51 06 22.5           ~ 185 0
52 GRB 071021 gB 22 42 34.33 +23 43 05.4           ~ 97 0
53 GRB 111215A gB 23 18 13.33 +32 29 38.5           ~ 64 0

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