2013A&A...560A..88D


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.16CEST18:44:30

2013A&A...560A..88D - Astronomy and Astrophysics, volume 560A, 88-88 (2013/12-1)

Dust-to-metal ratios in damped Lyman-α absorbers. Fresh clues to the origins of dust and optical extinction towards γ-ray bursts.

DE CIA A., LEDOUX C., SAVAGLIO S., SCHADY P. and VREESWIJK P.M.

Abstract (from CDS):

Motivated by the anomalous dust-to-metal ratios derived in the literature for γ-ray burst (GRB) damped Lyman-α absorbers (DLAs), we measure these ratios using the dust-depletion pattern observed in UV/optical afterglow spectra associated with the interstellar medium (ISM) at the GRB host-galaxy redshifts. Our sample consists of 20 GRB absorbers and a comparison sample of 72 DLAs toward quasars (QSOs) with redshift 1.2<z<4.0 and down to Z=0.002Z metallicities. The dust-to-metal ratio in QSO- and GRB-DLAs increases both with metallicity and metal column density, spanning ∼10-110% of the Galactic value and pointing to a nonuniversal dust-to-metal ratio. The low values of dust-to-metal ratio suggest that low-metallicity systems have lower dust fractions than typical spiral galaxies and, perhaps, that the dust in these systems is produced inefficiently, i.e. by grain growth in the low-metallicity regime with negligible contribution from supernovae (SNe) and asymptotic giant branch (AGB) stars. On the other hand, some GRB- and QSO-DLAs show high dust-to-metal ratio values out to z∼4, requiring rapid dust production, such as in SN ejecta, but also in AGB winds and via grain growth for the highest metallicity systems. GRB-DLAs overall follow the dust-to-metal-ratio properties of QSO-DLAs, GRBs probing larger column and volume densities. For comparison, the dust-to-metal ratio that we derive for the SMC and LMC are ∼82-100% and ∼98% of the Galactic value, respectively. The literature dust-to-metal ratio of the low-metallicity galaxy I Zw 18 (<37%) is consistent with the distribution that we find. The dust extinction AV increases steeply with the column density of iron in dust, N(Fe)dust, calculated from relative metal abundances, confirming that dust extinction is mostly occurring in the host galaxy ISM. Most GRB-DLAs display logN(Fe)dust>14.7, above which several QSO-DLAs reveal molecular hydrogen, making GRB-DLAs promising candidates for molecular detection and study.

Abstract Copyright:

Journal keyword(s): gamma-ray burst: general - ISM: abundances - dust, extinction - quasars: absorption lines

Simbad objects: 31

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Number of rows : 31

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 071031 gB 00 25 37.40 -58 03 33.9           ~ 142 0
2 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9448 1
3 HD 5980 WR* 00 59 26.5847969465 -72 09 53.927725716   11.13 11.31   11.029 WN4+O7I: 359 1
4 RMC 31 WR* 01 03 25.2276668802 -72 06 43.858552056   12.11 12.30     WN3:h+O5.5V+O5.5If+O7.5V 109 0
5 SK 155 * 01 14 50.2609110337 -73 20 17.853632425 11.35 12.33 12.48     O9Ib 53 0
6 GRB 070802 gB 02 27 35.91 -55 31 39.1           ~ 136 0
7 HD 18100 * 02 53 40.8048620088 -26 09 20.426284938   8.23 8.44     B5II/III 86 0
8 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5670 1
9 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14838 1
10 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4485 2
11 Mrk 116 PaG 09 34 02.1 +55 14 25           ~ 997 1
12 GRB 030323 gB 11 06 09.4 -21 46 13           ~ 125 1
13 GRB 080330 gB 11 17 06.70 +30 36 24.1           ~ 119 0
14 GRB 030226 gB 11 33 04.9 +25 53 56           ~ 186 2
15 GRB 090323 gB 12 42 50.28 +17 03 11.9           ~ 183 1
16 GRB 080607 gB 12 59 47.14 +15 55 09.6           ~ 209 0
17 GRB 050730 gB 14 08 17.090 -03 46 18.90   20.32 17.68     ~ 282 1
18 QSO J1443+2724 QSO 14 43 31.1702656971 +27 24 36.772847043     19.3     ~ 72 0
19 GRB 010222 gB 14 52 12.55 +43 01 06.3           ~ 335 2
20 GRB 990123 gB 15 25 29 +44 45.0     8.95     ~ 963 1
21 GRB 060418 gB 15 45 42.600 -03 38 20.00 15.73 16.19 14.98     ~ 322 1
22 GRB 050401 gB 16 31 28.84 +02 11 14.5           ~ 302 0
23 GRB 000926 gB 17 04 15 +51 46.0           ~ 341 2
24 HD 167756 * 18 18 40.1582210207 -42 17 18.223418445 5.18 6.143 6.290     B0Ia/ab 98 0
25 GRB 080413A gB 19 09 11.73 -27 40 39.6           ~ 123 0
26 GRB 020813A gB 19 46 41.874 -19 36 04.81           ~ 285 1
27 GRB 050922C gB 21 09 33.000 -08 45 30.10 15.15 15.86 14.69     ~ 250 0
28 GRB 050820A gB 22 29 38.110 +19 33 37.10 18.33 19.00 18.47     ~ 338 1
29 GRB 051111A gB 23 12 33.170 +18 22 28.80 19.77 20.08 19.50     ~ 185 1
30 GRB 090926A gB 23 33 36.18 -66 19 25.9           ~ 250 0
31 NAME Local Group GrG ~ ~           ~ 6977 0

    Equat.    Gal    SGal    Ecl

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2020.07.16-18:44:30

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