J/A+A/681/A64 DLA QSO, GRB and stars column densities (Konstantopoulou+, 2024)
Dust depletion of metals from local to distant galaxies.
II. Cosmic dust-to-metal ratio and dust composition.
Konstantopoulou C., De Cia A., Ledoux C., Krogager J.-K., Mattsson L.,
Watson D., Heintz K.E., Peroux C., Noterdaeme P., Andersen A.C.,
Fynbo J.P.U., Jermann I., Ramburuth-Hurt T.
<Astron. Astrophys., 681, A64 (2024)>
=2024A&A...681A..64K 2024A&A...681A..64K (SIMBAD/NED BibCode)
ADC_Keywords: QSOs ; GRB ; Milky Way ; Magellanic Clouds ; Abundances ;
Interstellar medium ; Optical ; Ultraviolet
Keywords: dust, extinction - galaxies: abundances - galaxies: evolution -
galaxies: ISM - Local Group - quasars: absorption lines
Abstract:
The evolution of cosmic dust content and the cycle between metals and
dust in the interstellar medium (ISM) play a fundamental role in
galaxy evolution. The chemical enrichment of the Universe can be
traced through the evolution of the dust-to-metal ratio (DTM) and the
dust-to-gas ratio (DTG) with metallicity. The physical processes
through which dust is created and eventually destroyed remain to be
elucidated. We use a novel method to determine mass estimates of the
DTM, DTG, and dust composition in terms of the fraction of dust mass
contributed by element X (fMX) based on our previous measurements of
the depletion of metals in different environments (the Milky Way, the
Magellanic Clouds, and damped Lyman-α absorbers (DLAs) towards
quasars (QSOs) and towards gamma-ray bursts (GRBs)), which were
calculated from the relative abundances of metals in the ISM through
absorption-line spectroscopy column densities observed mainly from
VLT/UVES and X-shooter, and HST/STIS. We also derive the dust
extinction from the estimated dust depletion (AV,depl) for GRB-DLAs,
the Magellanic Clouds, and the Milky Way, and compare it with the AV
estimated from extinction (AV,ext). We find that the DTM and DTG
ratios increase with metallicity and with the dust tracer [Zn/Fe].
This suggests that grain growth in the ISM is the dominant process of
dust production, at least in the metallicity range
(-2≤[M/H]tot≤0.5) and redshift range (0.6<z<6.3) that we are
studying. The increasing trend in the DTM and DTG with metallicity is
in good agreement with a dust production and evolution hydrodynamical
model. Our data suggest that the stellar dust yield is much lower
(about 1%) than the metal yield and thus that the overall amount of
dust in the warm neutral medium that is produced by stars is much
lower than previously estimated. The global neutral gas metallicity is
decreasing over cosmic time and is traced similarly by quasar-DLAs and
GRB-DLAs. We find that, overall, AV,depl is lower than AV,ext for
the Milky Way and in a few lines of sight for the Magellanic Clouds, a
discrepancy that is likely related to the presence of carbonaceous
dust associated with dense clumps of cold neutral gas. For the other
environments studied here, we find good agreement overall between the
AV,ext and AV,depl. We show that the main elements (fMX>1%) that
contribute to the dust composition, by mass, are O, Fe, Si, Mg, C, S,
Ni, and Al for all the environments, with Si, Mg, and C being
equivalent contributors. There are nevertheless variations in the dust
composition depending on the overall amount of dust. The abundances
measured at low dust regimes in quasar- and GRB-DLAs suggest the
presence of pyroxene and metallic iron in dust. These results give
important information on the dust and metal content of galaxies across
cosmic times, from the Milky Way up to z=6.3.
Description:
QSO-DLAs, GRB-DLAs, Milky Way, LMC and SMC dust properties.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tableb1.dat 127 108 QSO-DLAs dust properties
tableb2.dat 121 37 Milky Way dust properties
tableb3.dat 124 31 LMC dust properties
tableb4.dat 124 18 SMC dust properties
tableb5.dat 127 36 GRB-DLAs dust properties
--------------------------------------------------------------------------------
See also:
J/ApJ/700/1299 : Gas-phase element depletions in the ISM (Jenkins, 2009)
J/MNRAS/452/4326 : Metal-rich damped Lyα systems at z∼2 (Berg+, 2015)
J/ApJ/910/95 : METAL Hubble prog. II. LMC dust-to-gas ratio
(Roman-Duval+, 2021)
J/A+A/666/A12 : QSO-DLA and MW stars column densities
(Konstantopoulou+, 2022)
Byte-by-byte Description of file: tableb1.dat tableb5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- Name QSO or GRB name
16- 21 F6.4 --- zabs Absorption redshift
23- 27 F5.2 [-] logNHI ?=- HI column density
29- 32 F4.2 [-] e_logNHI ? HI column density error
34- 38 F5.2 [-] logNH2 ?=- H2 column density
40- 43 F4.2 [-] e_logNH2 ? H2 column density error
45- 49 F5.2 [-] [Zn/Fe] Abundance [Zn/Fe]
51- 55 F5.3 [-] e_[Zn/Fe] Abundance [Zn/Fe] error
58- 64 F7.5 --- DTM ?=- Dust-to-metal ratio (this work)
66- 71 F6.4 --- e_DTM ? Dust-to-metal ratio error (this work)
72- 79 E8.3 --- DTG ?=- Dust-to-gas ratio (this work)
81- 88 E8.3 --- e_DTG ? Dust-to-gas ratio error (this work)
90- 95 F6.4 --- DTMN ?=- DTM in terms of column density (this work)
97-101 F5.3 --- e_DTMN ? DTM in terms of column density error
(this work)
103-107 F5.3 mag AVdepl ?=- Dust extinction from the estimated dust
depletion (this work)
109-113 F5.3 mag e_AVdepl ? Dust extinction from the estimated dust
depletion error (this work)
115-119 F5.2 [-] [M/H]tot ?=- Total dust-corrected metallicity
from De Cia et al. (2018A&A...611A..76D 2018A&A...611A..76D,
Cat. J/A+A/611/A76) in table B1
121-124 F4.2 [-] e_[M/H]tot ? Total dust-corrected metallicity error
126-127 I2 --- r_logNHI References logNHI and logNH2 (1)
--------------------------------------------------------------------------------
Note (1): References as follows:
11 = De Cia et al. (2016A&A...596A..97D 2016A&A...596A..97D)
12 = Berg et al. (2015MNRAS.452.4326B 2015MNRAS.452.4326B, Cat. J/MNRAS/452/4326)
51 = Heintz et al. (2023A&A...679A..91H 2023A&A...679A..91H)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tableb2.dat tableb3.dat tableb4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- Name QSO or GRB name
17- 21 F5.2 [-] logNHI ?=- HI column density
23- 26 F4.2 [-] e_logNHI ? HI column density error
28- 32 F5.2 [-] logNH2 ?=- H2 column density
34- 37 F4.2 [-] e_logNH2 ? H2 column density error
39- 43 F5.2 [-] [Zn/Fe] Abundance [Zn/Fe]
45- 49 F5.3 [-] e_[Zn/Fe] Abundance [Zn/Fe] error
52- 58 F7.5 --- DTM ?=- Dust-to-metal ratio (this work)
60- 65 F6.4 --- e_DTM ? Dust-to-metal ratio error (this work)
66- 73 E8.3 --- DTG ?=- Dust-to-gas ratio (this work)
75- 82 E8.3 --- e_DTG ? Dust-to-gas ratio error (this work)
84- 89 F6.4 --- DTMN ?=- DTM in terms of column density (this work)
91- 95 F5.3 --- e_DTMN ? DTM in terms of column density error
(this work)
97-101 F5.3 mag AVdepl ?=- Dust extinction from the estimated dust
depletion (this work)
103-107 F5.3 mag e_AVdepl ? Dust extinction from the estimated dust
depletion error (this work)
109-113 F5.2 [-] [M/H]tot ?=- Total dust-corrected metallicity (1)
115-118 F4.2 [-] e_[M/H]tot ? Total dust-corrected metallicity error
120-124 A5 --- r_logNHI References logNHI and logNH2 (2)
--------------------------------------------------------------------------------
Note (1): from De Cia et al. (2021Natur.597..206D 2021Natur.597..206D) in table B2,
from De Cia et al. in prep. for tables B3 and B4.
Note (2): References as follows:
21 = De Cia et al. (2021Natur.597..206D 2021Natur.597..206D)
22 = Jenkins (2009ApJ...700.1299J 2009ApJ...700.1299J, Cat. J/ApJ/700/1299)
31 = Roman-Duval et al. (2021ApJ...910...95R 2021ApJ...910...95R, Cat. J/ApJ/910/95)
32 = De Cia et al. in prep
41 = Jenkins & Wallerstein (2017ApJ...838...85J 2017ApJ...838...85J)
--------------------------------------------------------------------------------
History:
From electronic version of the journal
References:
Konstantopoulou et al. Paper I 2022A&A...666A..12K 2022A&A...666A..12K, Cat. J/A+A/666/A12
(End) Patricia Vannier [CDS] 23-Apr-2024