2018A&A...617A.141C


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.10CEST02:11:40

2018A&A...617A.141C - Astronomy and Astrophysics, volume 617A, 141-141 (2018/9-1)

Investigation of dust attenuation and star formation activity in galaxies hosting GRBs.

CORRE D., BUAT V., BASA S., BOISSIER S., JAPELJ J., PALMERIO J., SALVATERRA R., VERGANI S.D. and ZAFAR T.

Abstract (from CDS):


Context. The gamma-ray bursts hosts (GRBHs) are excellent targets to study the extinction properties of dust and its effects on the global emission of distant galaxies. The dust extinction curve is measured along the GRB afterglow line of sight and the analysis of the spectral energy distribution (SED) of the host galaxy gives access to the global dust attenuation of the stellar light.
Aims. In this pilot study we gather information on dust extinction in GRBHs to compare the properties of the extinction curve to those of the dust obscuration affecting the total stellar light of the host galaxy. Assuming the extinction curve to be representative of the dust properties, we aim to investigate which dust-stars geometries and local dust distribution in the inter stellar medium (ISM) can reproduce the observed attenuation curve.
Methods. We selected a sample of 30 GRBs for which the extinction curve along the GRB afterglow line-of-sight (l.o.s.) is measured in the rest-frame ultraviolet (UV) up to optical and we analysed the properties of the extinction curve as a function of the host galaxy properties. From these 30 GRBs, we selected seven GRBHs with a good rest-frame UV to near-infrared (NIR) spectral coverage for the host. The attenuation curve was derived by fitting the SEDs of the GRBH sample with the CIGALE SED fitting code. Different star formation histories (SFH) were studied to recover the star formation rates (SFR) derived using Hα luminosities. Implications for the dust-stars geometries in the ISM are inferred by a comparison with radiative transfer simulations.
Results. The most extinguished GRBs are preferentially found in the more massive hosts and the UV bump is preferentially found in the most extinguished GRB l.o.s. Five out of seven hosts are best fitted with a recent burst of star formation, leading to lower stellar mass estimates than previously found. The average attenuation in the host galaxies is about 70% of the amount of extinction along the GRB l.o.s. We find a great variety in the derived attenuation curves of GRBHs, the UV slope can be similar, flatter or even steeper than the extinction curve slope. Half of the attenuation curves are consistent with the Calzetti attenuation law and there is evidence of a UV bump in only one GRBH. We find that the flatter (steeper) attenuation curves are found in galaxies with the highest (lowest) SFR and stellar masses. The comparison of our results with radiative transfer simulations leads to a uniform distribution of dust and stars in a very clumpy ISM for half the GRBHs and various dust-stars geometries for the second half of the sample.

Abstract Copyright: © ESO 2018

Journal keyword(s): gamma-ray burst: general - dust, extinction - galaxies: starburst - galaxies: star formation - galaxies: high-redshift - galaxies: ISM

Simbad objects: 34

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Number of rows : 34

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 080710 gB 00 33 05.68 +19 30 05.8           ~ 103 0
2 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 10904 1
3 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9446 1
4 GRB 100814A gB 01 29 53.61 -17 59 43.6           ~ 149 0
5 GRB 081222 gB 01 30 57.76 -34 05 44.0           ~ 151 0
6 GRB 100901A gB 01 49 03.56 +22 45 30.6           ~ 125 0
7 GRB 091018 gB 02 08 46 -57 33.0           ~ 117 0
8 GRB 070802 gB 02 27 35.91 -55 31 39.1           ~ 136 0
9 [EFH2009] GRB 070802 host G G 02 27 35.91 -55 31 39.1       25.03   ~ 3 0
10 GRB 071112C gB 02 36 50.89 +28 22 16.9           ~ 129 0
11 GRB 060904B gB 03 52 50.520 -00 43 30.61 18.27 19.14 18.37     ~ 162 0
12 GRB 091029 gB 04 00 40.00 -55 57 12.7           ~ 117 0
13 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14832 1
14 GRB 081121 gB 05 57 07.70 -60 36 42.1           ~ 110 0
15 GRB 120119A gB 08 00 06.940 -09 04 53.83           ~ 116 0
16 GRB 090102 gB 08 32 59.50 +33 06 25.7           ~ 184 0
17 GRB 061121 gB 09 48 54.570 -13 11 42.68 17.19 17.71 17.02     ~ 287 0
18 GRB 090424 gB 12 38 07.40 +16 49 45.9           ~ 202 0
19 [CPW2010] GRB 080607 host G G 12 59 47.14 +15 55 09.6           ~ 3 0
20 GRB 080607 gB 12 59 47.14 +15 55 09.6           ~ 209 0
21 M 51 GiP 13 29 52.698 +47 11 42.93   9.26 8.36 8.40   ~ 3782 4
22 GRB 060418 gB 15 45 42.600 -03 38 20.00 15.73 16.19 14.98     ~ 322 1
23 GRB 080210 gB 16 45 04.03 +13 49 36.3           ~ 92 0
24 GRB 080319C gB 17 15 55.48 +55 23 31.7           ~ 137 0
25 GRB 080605 gB 17 28 30.04 +04 00 56.9           ~ 153 0
26 [KGS2011] GRB 080605 host G G 17 28 30.05 +04 00 56.0           ~ 3 0
27 GRB 120815A gB 18 15 54.40 -52 07 29.0           ~ 65 0
28 GRB 090618 gB 19 36 01.80 +78 21 07.1           ~ 269 0
29 [KGS2011] GRB 080805 host G G 20 56 53.43 -62 26 39.3     25.7 25.5   ~ 2 0
30 GRB 080805 gB 20 56 55.30 -62 25 58.8           ~ 79 0
31 GRB 080804 gB 21 54 41.90 -53 11 20.2           ~ 117 0
32 GRB 060607 gB 21 58 50.400 -22 29 46.70 18.49 16.67 15.09     ~ 258 1
33 GRB 050820A gB 22 29 38.110 +19 33 37.10 18.33 19.00 18.47     ~ 338 1
34 NAME Local Group GrG ~ ~           ~ 6973 0

    Equat.    Gal    SGal    Ecl

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2020.07.10-02:11:40

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