2021A&A...656A.136T


Query : 2021A&A...656A.136T

2021A&A...656A.136T - Astronomy and Astrophysics, volume 656A, 136-136 (2021/12-1)

Outflows from GRB hosts are ubiquitous: Kinematics of z < 0.3 GRB-SN hosts resolved with FLAMES.

THONE C.C., IZZO L., FLORES H., DE UGARTE POSTIGO A., VERGANI S.D., AGUI FERNANDEZ J.F., KANN D.A., CHRISTENSEN L., COVINO S., DELLA VALLE M., HAMMER F., MELANDRI A., PUECH M., RODRIGUES M.A. and GOROSABEL J.

Abstract (from CDS):

The hosts of long duration gamma-ray bursts (GRBs) are predominantly starburst galaxies at subsolar metallicity. At redshifts z < 1, this implies that most of them are low-mass galaxies similar to the populations of blue compact dwarfs and dwarf irregulars. What triggers the massive star-formation needed for producing a GRB progenitor is still largely unknown, as are the resolved gas properties and kinematics of these galaxies and their formation history. Here we present a sample of six spatially resolved GRB hosts at z < 0.3 observed with 3D spectroscopy at high spectral resolution (R = 8000-13 000) using FLAMES/VLT. We analyzed the resolved gas kinematics of the full sample and the abundances in a subsample with strong enough emission lines. Only two galaxies show a regular disk-like rotation field, another two are dispersion-dominated, and the remaining ones have two narrow emission components associated with different parts of the galaxy but no regular rotation field, which might indicate a recent merger. All galaxies show evidence for broad components underlying the main emission peak with σ of 50-110 km s–1. This broad component is more metal-rich than the narrow components, it is blueshifted in most cases, and it follows a different velocity structure. We find a weak correlation between the star-formation rate and the width of the broad component, its flux compared to the narrow component, and the maximum outflow velocity of the gas, but we do not find any correlation with the star-formation density, metallicity or stellar mass. We hence associate this broad component with a metal-rich outflow from star-forming regions in the host. The GRB is not located in the brightest region of the host, but is always associated with some star-forming region showing a clear wind component. Our study shows the great potential of 3D spectroscopy to study the star-formation processes and history in galaxies hosting extreme transients, the need for high signal-to-noise, and the perils using unresolved or only partially resolved data for these kinds of studies.

Abstract Copyright: © ESO 2021

Journal keyword(s): gamma-ray burst: general - galaxies: starburst - galaxies: kinematics and dynamics

Simbad objects: 30

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Number of rows : 30
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 ESO 350-38 AGN 00 36 52.489 -33 33 17.23   14.31 14.41 13.49   ~ 345 0
2 NGC 244 bCG 00 45 46.4165696064 -15 35 48.392605716   14.1   13.04 13.4 ~ 82 0
3 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10530 1
4 QSO B0125-0635 QSO 01 27 35.5248944352 -06 19 35.432857848 14.75 15.05 14.48 14.06 13.70 ~ 100 0
5 SN 2019oyw SN* 02 58 10.510 -08 57 27.20           ~ 94 0
6 SN 2006aj SN* 03 21 39.670 +16 52 02.27 17.96 19.11 17.40     SNIc-BL 901 1
7 NGC 1569 IG 04 30 49.186 +64 50 52.52 11.72 11.86 11.03     ~ 1211 3
8 GRB 990705 gB 05 09 54.5 -72 07 53           ~ 219 1
9 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16509 1
10 GRB 050826 gB 05 51 01.590 -02 38 35.40           ~ 120 0
11 SN 2010bh SN* 07 10 30.63 -56 15 19.7           SNIc 267 1
12 SN 2003lw SN* 08 02 30.1 -39 51 03       20.23   SNIc: 526 0
13 SN 2012bz SN* 09 07 38.38 +14 01 07.5           SNIb/c 149 1
14 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5677 6
15 SN 2003dh SN* 10 44 50.030 +21 31 18.15     16.2     SNIcpec 1177 1
16 SN 2010dh SN* 10 56 37.19 +20 14 41.9           ~ 12 1
17 SN 2017iuk SN* 11 09 39.49 -12 35 18.7           ~ 127 0
18 Mrk 1304 IG 11 42 12.253 +00 20 03.68   14.16 13.67 13.41 13.03 ~ 174 0
19 NGC 4449 EmG 12 28 11.118 +44 05 36.81 10.11 9.98 9.64 9.45   ~ 1086 1
20 GRB 090426 gB 12 36 19.49 +32 59 05.5           ~ 188 0
21 Fermi bn090323002 gB 12 42 50.28 +17 03 11.9           ~ 201 1
22 GRB 111005A gB 14 53 15.60 -19 43 19.1           ~ 55 0
23 GRB 060418 gB 15 45 42.600 -03 38 20.00 15.73 16.19 14.98     ~ 349 0
24 GRB 100418A gB 17 05 26.96 +11 27 41.9           ~ 167 0
25 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1764 2
26 GRB 060505 gB 22 07 03.440 -27 48 51.89           ~ 246 1
27 GRB 050820A gB 22 29 38.110 +19 33 37.10 18.33 19.00 18.47     ~ 372 0
28 GRB 020903 gB 22 48 42.34 -20 46 09.3           ~ 227 1
29 NGC 7552 GiP 23 16 10.767 -42 35 05.39 11.34 11.22 10.57 10.08 11.1 ~ 535 3
30 Fermi bn080810549 gB 23 47 08.00 +00 18 35.1           ~ 203 0

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2023.01.31-00:36:36

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