J/A+A/666/A12 QSO-DLA and MW stars column densities (Konstantopoulou+, 2022)
Dust depletion of metals from local to distant galaxies.
I. Peculiar nucleosynthesis effects and grain growth in the ISM.
Konstantopoulou C., De Cia A., Krogager J.-K., Ledoux C., Noterdaeme P.,
Fynbo J.P.U., Heintz K.E., Watson D., Andersen A.C., Ramburuth-hurt T.,
Jermann I.
<Astron. Astrophys., 666, A12 (2022)>
=2022A&A...666A..12K 2022A&A...666A..12K (SIMBAD/NED BibCode)
ADC_Keywords: QSOs ; Stars, nearby ; Abundances ; Optical ; Ultraviolet
Keywords: quasars: absorption lines
Abstract:
Large fractions of metals are missing from the observable gas-phase in
the interstellar medium (ISM) because they are incorporated into dust
grains. This phenomenon is called dust depletion. It is important to
study the depletion of metals into dust grains in the ISM to
investigate the origin and evolution of metals and cosmic dust. We
characterize the dust depletion of several metals from the Milky Way
to distant galaxies. We collected measurements of ISM metal column
densities from absorption-line spectroscopy in the literature, and in
addition, we determined Ti and Ni column densities from a sample of 70
damped Lyman-α absorbers (DLAs) toward quasars that were
observed at high spectral resolution with the Very Large Telescope
(VLT) Ultraviolet and Visual Echelle Spectrograph (UVES). We used
relative ISM abundances to estimate the dust depletion of 18 metals
(C, P, O, Cl, Kr, S, Ge, Mg, Si, Cu, Co, Mn, Cr, Ni, Al, Ti, Zn, and
Fe) for different environments (the Milky Way, the Magellanic Clouds,
and DLAs toward quasars and towards gamma-ray bursts). We observed
overall linear relations between the depletion of each metal and the
overall strength of the dust depletion, which we traced with the
observed [Zn/Fe]. The slope of these dust depletion sequences
correlates with the condensation temperature of the various elements,
that is, the more refractory elements show steeper depletion
sequences. In the neutral ISM of the Magellanic Clouds, small
deviations from linearity are observed as an overabundance of the
α-elements Ti, Mg, S, and an underabundance of Mn, including for
metal-rich systems. The Ti, Mg, and Mn deviations completely disappear
when we assume that all systems in our sample of OB stars observed
toward the Magellanic Clouds have an α-element enhancement and
Mn underabundance, regardless of their metallicity. This may imply
that the Magellanic Clouds have recently been enriched in
α-elements, potentially through recent bursts of star formation.
We also observe an S overabundance in all local galaxies, which is an
effect of ionization due to the contribution of their HII regions to
the measured SII column densities. The observed strong correlations of
the depletion sequences of the metals all the way from low-metallicity
quasi-stellar object DLAs to the Milky Way suggest that cosmic dust
has a common origin, regardless of the star formation history, which,
in contrast, varies significantly between these different galaxies.
This supports the importance of grain growth in the ISM as a
significant process of dust production.
Description:
We characterized the dust depletion of several metals in different
environments from the Milky Way, the Magellanic Clouds, and DLAs
toward GRBs and QSOs based on the relative abundances of metals with
different refractory properties (or how easily they incorporate into
dust grains). We collected all the available literature measurements
of metal column densities in these environments, making this a
comprehensive study of relative chemical abundances of metals and for
different environments. We measured new column densities of Ti and Ni
in 70 QSO-DLAs from high-resolution UVES spectra from the sample of De
Cia et al. (2016A&A...596A..97D 2016A&A...596A..97D).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tabled1.dat 167 129 *QSO-DLA column densities
tabled2.dat 126 37 *Milky Way column densities
tabled3.dat 124 24 *Milky Way column densities for elements with
limited coverage
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Note on tabled1.dat, tabled2.dat, tabled3.dat: Revised f-values from
Cashman et al. (2017ApJS..230....8C 2017ApJS..230....8C), Kisielius et al. (2014ApJ...780...76K 2014ApJ...780...76K,
Cat. J/ApJ/780/76; 2015ApJ...804...76K 2015ApJ...804...76K, Cat. J/ApJ/804/76) and
Kurucz (2017, Canadian J. Phys., 95, 825).
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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)
Byte-by-byte Description of file: tabled1.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- QSO QSO name
16- 19 F4.2 --- zabs Absorption redshift
21- 25 F5.2 [cm-2] logN(HI) ?=- HI column density
27- 30 F4.2 [cm-2] e_logN(HI) ?=- HI column density error
32- 36 F5.2 [cm-2] logN(OI) ?=- OI column density
38- 41 F4.2 [cm-2] e_logN(OI) ?=- OI column density error
43- 47 F5.2 [cm-2] logN(MgII) ?=- MgII column density
49- 52 F4.2 [cm-2] e_logN(MgII) ?=- MgII column density error
54- 58 F5.2 [cm-2] logN(SiII) ?=- SiII column density
60- 63 F4.2 [cm-2] e_logN(SiII) ?=- SiII column density error
65- 69 F5.2 [cm-2] logN(SII) ?=- SII column density
71- 74 F4.2 [cm-2] e_logN(SII) ?=- SII column density error
76- 80 F5.2 [cm-2] logN(PII) ?=- PII column density
82- 85 F4.2 [cm-2] e_logN(PII) ?=- PII column density error
87 A1 --- l_logN(TiII) Limit flag on logN(TiII)
88- 92 F5.2 [cm-2] logN(TiII) ?=- TiII column density
94- 97 F4.2 [cm-2] e_logN(TiII) ?=- TiII column density error
99-103 F5.2 [cm-2] logN(CrII) ?=- CrII column density
105-108 F4.2 [cm-2] e_logN(CrII) ?=- CrII column density error
110-114 F5.2 [cm-2] logN(MnII) ?=- MnII column density
116-119 F4.2 [cm-2] e_logN(MnII) ?=- MnII column density error
121-125 F5.2 [cm-2] logN(FeII) ?=- FeII column density
127-130 F4.2 [cm-2] e_logN(FeII) ?=- FeII column density error
132-136 F5.2 [cm-2] logN(CoII) ?=- CoII column density
138-141 F4.2 [cm-2] e_logN(CoII) ?=- CoII column density error
142 A1 --- l_logN(NiII) Limit flag on logN(NiII)
143-147 F5.2 [cm-2] logN(NiII) ?=- NiII column density
149-152 F4.2 [cm-2] e_logN(NiII) ?=- NiII column density error
154-158 F5.2 [cm-2] logN(ZnII) ?=- ZnII column density
160-163 F4.2 [cm-2] e_logN(ZnII) ?=- ZnII column density error
165-167 A3 --- Refs References (1)
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Note (1): References as follows:
* = This work
1 = De Cia et al. (2016A&A...596A..97D 2016A&A...596A..97D)
2 = Berg et al. (2015MNRAS.452.4326B 2015MNRAS.452.4326B, Cat. J/MNRAS/452/4326)
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Byte-by-byte Description of file: tabled2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- Star Star name
14- 18 F5.2 [cm-2] logN(PII) ?=- PII column density
20- 23 F4.2 [cm-2] e_logN(PII) ?=- PII column density error
25- 29 F5.2 [cm-2] logN(MgII) ?=- MgII column density
31- 34 F4.2 [cm-2] e_logN(MgII) ?=- MgII column density error
36- 40 F5.2 [cm-2] logN(SiII) ?=- SiII column density
42- 45 F4.2 [cm-2] e_logN(SiII) ?=- SiII column density error
47- 51 F5.2 [cm-2] logN(SII) ?=- SII column density
53- 56 F4.2 [cm-2] e_logN(SII) ?=- SII column density error
58- 62 F5.2 [cm-2] logN(TiII) ?=- TiII column density
64- 67 F4.2 [cm-2] e_logN(TiII) ?=- TiII column density error
69- 73 F5.2 [cm-2] logN(CrII) ?=- CrII column density
75- 78 F4.2 [cm-2] e_logN(CrII) ?=- CrII column density error
80- 84 F5.2 [cm-2] logN(MnII) ?=- MnII column density
86- 89 F4.2 [cm-2] e_logN(MnII) ?=- MnII column density error
91- 95 F5.2 [cm-2] logN(FeII) ?=- FeII column density
97-100 F4.2 [cm-2] e_logN(FeII) ?=- FeII column density error
102-106 F5.2 [cm-2] logN(NiII) ?=- NiII column density
108-111 F4.2 [cm-2] e_logN(NiII) ?=- NiII column density error
113-117 F5.2 [cm-2] logN(ZnII) ?=- ZnII column density
119-122 F4.2 [cm-2] e_logN(ZnII) ?=- ZnII column density error
124-126 A3 --- Refs References (1)
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Note (1): References as follows:
1 = Jenkins (2009ApJ...700.1299J 2009ApJ...700.1299J, Cat J/ApJ/700/1299)
2 = De Cia et al. (2016A&A...596A..97D 2016A&A...596A..97D)
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Byte-by-byte Description of file: tabled3.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Star Star name
12- 16 F5.2 [cm-2] logN(OI) ?=- OI column density
18- 21 F4.2 [cm-2] e_logN(OI) ?=- OI column density error
23- 27 F5.2 [cm-2] logN(FeII) ?=- FeII column density
29- 32 F4.2 [cm-2] e_logN(FeII) ?=- FeII column density error
34- 38 F5.2 [cm-2] logN(ZnII) ?=- ZnII column density
40- 43 F4.2 [cm-2] e_logN(ZnII) ?=- ZnII column density error
45- 49 F5.2 [cm-2] logN(CoII) ?=- CoII column density
51- 54 F4.2 [cm-2] e_logN(CoII) ?=- CoII column density error
56- 60 F5.2 [cm-2] logN(GeII) ?=- GeII column density
62- 65 F4.2 [cm-2] e_logN(GeII) ?=- GeII column density error
67- 71 F5.2 [cm-2] logN(KrI) ?=- KrI column density
73- 76 F4.2 [cm-2] e_logN(KrI) ?=- KrI column density error
78- 82 F5.2 [cm-2] logN(ClII) ?=- ClII column density
84- 87 F4.2 [cm-2] e_logN(ClII) ?=- ClII column density error
89- 93 F5.2 [cm-2] logN(CuII) ?=- CuII column density
95- 98 F4.2 [cm-2] e_logN(CuII) ?=- CuII column density error
100-104 F5.2 [cm-2] logN(AlII) ?=- AlII column density
106-109 F4.2 [cm-2] e_logN(AlII) ?=- AlII column density error
111-115 F5.2 [cm-2] logN(CII) ?=- CII column density
117-120 F4.2 [cm-2] e_logN(CII) ?=- CII column density error
122-124 A3 --- Refs References (1)
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Note (1): References as follows:
1 = Jenkins (2009ApJ...700.1299J 2009ApJ...700.1299J, Cat. J/ApJ/700/1299)
2 = De Cia et al. (2016A&A...596A..97D 2016A&A...596A..97D)
3 = Phillips et al. (1982MNRAS.200..687P 1982MNRAS.200..687P)
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 17-Feb-2023