J/ApJS/257/63 Interstellar extinction and elemental abundances (Zuo+, 2021)
Interstellar extinction and elemental abundances: individual sight lines.
Zuo W., Li A., Zhao G.
<Astrophys. J. Suppl. Ser., 257, 63 (2021)>
=2021ApJS..257...63Z 2021ApJS..257...63Z
ADC_Keywords: Interstellar medium; Abundances; Extinction
Keywords: Gas-to-dust ratio ; Interstellar dust extinction ;
Interstellar dust ; Cosmic abundances ; Interstellar abundances ;
Solar abundances
Abstract:
While it is well recognized that both the Galactic interstellar
extinction curves and the gas-phase abundances of dust-forming
elements exhibit considerable variations from one sight line to
another, as yet most of the dust extinction modeling efforts have been
directed to the Galactic average extinction curve, which is obtained
by averaging over many clouds of different gas and dust properties.
Therefore, any details concerning the relationship between the dust
properties and the interstellar environments are lost. Here we utilize
the wealth of extinction and elemental abundance data obtained by
space telescopes and explore the dust properties of a large number of
individual sight lines. We model the observed extinction curve of each
sight line and derive the abundances of the major dust-forming
elements (i.e., C, O, Si, Mg, and Fe) required to be tied up in dust
(i.e., dust depletion). We then confront the derived dust depletions
with the observed gas-phase abundances of these elements and
investigate the environmental effects on the dust properties and
elemental depletions. It is found that for the majority of the sight
lines the interstellar oxygen atoms are fully accommodated by gas and
dust and therefore there does not appear to be a "missing oxygen"
problem. For those sight lines with an extinction-to-hydrogen column
density AV/NH≳4.8x10-22mag.cm2.H-1 there are shortages of
C, Si, Mg, and Fe elements for making dust to account for the observed
extinction, even if the interstellar C/H, Si/H, Mg/H, and Fe/H
abundances are assumed to be protosolar abundances augmented by
Galactic chemical evolution.
Description:
We search for in the literature an as complete as possible set of
individual interstellar sight lines for which both the extinction
curves have been observationally determined from the near-IR to the
far-UV and the gas-phase abundances have been measured for at least
one of the dust-forming elements (i.e., C, O, Mg, Si, and Fe). As a
result, we find 81 such sight lines.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 139 81 Extinction parameters for the 81 interstellar
sight lines in our sample
table2.dat 150 81 Hydrogen densities and gas-phase C, O, Mg, Si and
Fe abundances of the 81 interstellar sight lines
in our sample
table3.dat 47 45 Model parameters for fitting the UV/Optical/Near-IR
extinction with a mixture of silicate and
graphite grains
refs.dat 66 34 References
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See also:
J/ApJS/93/211 : IUE survey of H I Lyα absorption. I. (Diplas+ 1994)
J/ApJ/663/320 : IR-through-UV extinction curve (Fitzpatrick+, 2007)
J/ApJ/700/1299 : Gas-phase element depletions in the ISM (Jenkins, 2009)
J/ApJ/711/1236 : Equivalent width of H2 from FUSE (Jensen+, 2010)
J/MNRAS/404/1321 : TiII in Milky way and Magellanic clouds (Welty+, 2010)
J/ApJ/872/55 : OI, GeII, KrI & H abundances from HST UV sp. (Jenkins, 2019)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Star Identifier
12 A1 --- f_Star [12] Flag on Star (1)
14- 17 F4.2 mag Av [0.5/2.8] The V band extinction (2)
19- 22 F4.2 mag e_Av [0.09/0.5] Uncertainty in AV (2)
24- 27 F4.2 mag E(B-V) [0.2/0.8] The (B-V) color excess (2)
29- 32 F4.2 mag e_E(B-V) [0.02/0.2] Uncertainty in E(B-V) (2)
34- 37 F4.2 --- Rv [2/5.9] Total-to-selective extinction ratio (2)
39- 42 F4.2 --- e_Rv [0.1/0.7] Uncertainty in Rv (2)
44- 47 F4.2 mag AU [0.9/3.7]? The U band extinction
49- 52 F4.2 mag AB [0.8/3.4]? The B band extinction
54- 57 F4.2 mag AJ [0.08/0.8]? The J band extinction
59- 62 F4.2 mag AH [0.05/0.5]? The H band extinction
64- 67 F4.2 mag AK [0.06/0.3]? The K band extinction
69- 73 F5.3 --- c1p [0.06/1.9] The c1' extinction parameter (2)
75- 79 F5.3 --- e_c1p [0.02/2.1] Uncertainty in c1' (2)
81- 85 F5.3 --- c2p [0/0.8] The c2' extinction parameter (2)
87- 91 F5.3 --- e_c2p [0.002/0.2] Uncertainty in c2' (2)
93- 97 F5.3 --- c3p [0.2/2.3] The c3' extinction parameter (2)
99-103 F5.3 --- e_c3p [0.04/0.6] Uncertainty in c3' (2)
105-109 F5.3 --- c4p [0.007/0.6] The c4' extinction parameter (2)
111-115 F5.3 --- e_c4p [0.007/0.2] Uncertainty in c4' (2)
117-121 F5.3 cm-1 x0 [4.5/4.7] The x0 extinction parameter (2)
123-127 F5.3 cm-1 e_x0 [0.003/0.05] Uncertainty in x0 (2)
129-133 F5.3 cm-1 gamma [0.6/1.4] The γ extinction parameter (2)
135-139 F5.3 cm-1 e_gamma [0.01/0.1] Uncertainty in gamma (2)
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Note (1): The U, B, J, H, and K extinction data taken from the references
as follows:
1 = Fitzpatrick & Massa (2007, J/ApJ/663/320);
2 = Gordon et al. (2009ApJ...705.1320G 2009ApJ...705.1320G).
Note (2): Data taken from Valencic+ (2004ApJ...616..921V 2004ApJ...616..921V).
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Star Identifier
11- 14 F4.2 10+21/cm2 NH [1/6.92] Total hydrogen column density
16- 20 F5.3 10+21/cm2 e_NH [0.03/3.1] Lower uncertainty in NH
22- 26 F5.3 10+21/cm2 E_NH [0.03/3.1] Upper uncertainty in NH
28- 29 I2 --- r_NH [1/25] Reference code for NH
(see refs.dat file)
31- 34 F4.2 --- f(H2) [0.04/0.93]? Fraction of hydrogen in
molecular form
36- 40 F5.3 10+21/cm2 NHI [0.4/5.9] Atomic hydrogen column density
42- 45 F4.2 10+21/cm2 e_NHI [0/3.1]? Lower uncertainty in NHI
47- 50 F4.2 10+21/cm2 E_NHI [0/3.1]? Upper uncertainty in NHI
52- 53 I2 --- r_NHI [1/79] Reference code for NHI
(see refs.dat file)
55- 59 F5.3 10+21/cm2 NH2 [0.04/3.1]? Molecular hydrogen
column density
61- 65 F5.3 10+21/cm2 e_NH2 [0/0.5]? Lower uncertainty in NH2
67- 71 F5.3 10+21/cm2 E_NH2 [0/0.44]? Upper uncertainty in NH2
73- 74 I2 --- r_NH2 [1/33]? Reference code for NH2
(see refs.dat file)
76- 80 F5.1 ppm [C/H]gas [79/427]? Gas-phase C/H abundance
82- 86 F5.1 ppm e_[C/H]gas [14/104]? Uncertainty in [C/H]
88- 89 I2 --- r_[C/H]gas [11/34]? Reference code for [C/H]
(see refs.dat file)
91- 96 F6.1 ppm [O/H]gas [40/2292]? Gas-phase O/H abundance
98-103 F6.1 ppm e_[O/H]gas [22/1889]? Uncertainty in [O/H]
105-106 I2 --- r_[O/H]gas [1/24]? Reference code for [O/H]
(see refs.dat file)
108-112 F5.2 ppm [Mg/H]gas [1/19]? Gas-phase Mg/H abundance
114-117 F4.2 ppm e_[Mg/H]gas [0.16/8]? Uncertainty in [Mg/H]
119-120 I2 --- r_[Mg/H]gas [1/23]? Reference code for [Mg/H]
(see refs.dat file)
122-126 F5.2 ppm [Si/H]gas [0.06/18]? Gas-phase Si/H abundance
128-133 F6.2 ppm e_[Si/H]gas [0.01/659]? Uncertainty in [Si/H]
135-136 I2 --- r_[Si/H]gas [2/12]? Reference code for [Si/H]
(see refs.dat file)
138-141 F4.2 ppm [Fe/H]gas [0.03/1.8]? Gas-phase Fe/H abundance
143-147 F5.2 ppm e_[Fe/H]gas [0/77]? Uncertainty in [Fe/H]
149-150 I2 --- r_[Fe/H]gas [4/28]? Reference code for [Fe/H]
(see refs.dat file)
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Star Identifier
11- 14 F4.2 --- Av/NH [3.3/8.72] The AV to NH ratio;
in units of 10-22mag.cm2.H-1
16- 19 F4.2 --- alphaS [1.26/3.6] Silicate grain power index
21- 24 F4.2 um acS [0.1/0.3] Silicate grain exponential
cutoff size
26- 29 F4.2 --- alphaC [2.18/4.1] Graphite grain power index
31- 34 F4.2 um acC [0.06/0.6] Graphite grain exponential
cutoff size
36- 40 F5.3 --- chi2 [0.001/0.003] Model χ2
42- 44 I3 ppm [C/H]dust [45/244] Carbon depletion
46- 47 I2 ppm [Si/H]dust [29/85] Silicon depletion
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Ref Reference code
4- 22 A19 --- BibCode Bibcode of the reference
24- 44 A21 --- Auth First author's name(s)
46- 66 A21 --- Comm VizieR catalog reference
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 11-Apr-2022