J/ApJ/674/172 Oxygen abundances of LIRGs and ULIRGs (Rupke+, 2008)
The oxygen abundances of luminous and ultraluminous infrared galaxies.
Rupke D.S.N., Veilleux S., Baker A.J.
<Astrophys. J., 674, 172-193 (2008)>
=2008ApJ...674..172R 2008ApJ...674..172R
ADC_Keywords: Galaxies, IR ; Abundances
Keywords: galaxies: abundances - galaxies: evolution - galaxies: interactions -
galaxies: ISM - galaxies: kinematics and dynamics - infrared: galaxies
Abstract:
Luminous and ultraluminous infrared galaxies (LIRGs and ULIRGs)
dominate the star formation rate budget of the universe at z≳1, yet
no local measurements of their heavy-element abundances exist. We
measure nuclear or near-nuclear oxygen abundances in a sample of 100
star-forming LIRGs and ULIRGs using new, previously published, and
archival spectroscopy of strong emission lines (including [OII]
λλ3726, 3729) in galaxies with redshifts ∼0.1.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 88 100 Sample of Luminous IR galaxies
table2.dat 114 42 New line fluxes
table3.dat 63 100 Abundances
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See also:
II/156 : IRAS Faint Source Catalog, |b|>10, Version 2.0 (Moshir+ 1989)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- Type LIRGs or ULIRGs
8- 22 A15 --- IRAS Galaxy nucleus designation from the IRAS
Faint Source Catalog (Cat. II/156) (1)
25- 47 A23 --- Nuc Nuclear ID (2)
48 A1 --- n_Nuc [a] a: a 2MASS designation exists for this
galaxy, but is attached to another nucleus
50- 55 F6.4 --- z Redshift (3)
57- 61 F5.2 10-7W LIR The 8-1000um infrared luminosity (4)
63- 68 F6.2 mag KsMAG ?=-1.00 Absolute Ks magnitude, compiled and
computed as described in Sect. 4.1
70- 75 F6.2 % fLum Fraction of (unresolved) total infrared
luminosity originating in this nucleus, based
on K-band flux ratios for individual nuclei
77- 80 A4 --- Sample Sample name (5)
82- 88 A7 --- Ref Reference, the first reference is the data
we use in our analysis (6)
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Note (1): Two sources are IRAS sources but not in the FSC, and a
third is not an IRAS source (F1_5=[CDF99] F1-5, Clements et al.,
2001MNRAS.325..665C 2001MNRAS.325..665C). The nucleus is specified if the IRAS flux is
unresolved or spread among two or more nuclei.
Note (2): Designation, in NED nomenclature, which precisely specifies in
sky coordinates the galaxy nucleus from which the IRAS flux and
spectrum originate.
* For 1Jy ULIRGs, the nuclei are already known (Kim et al., 2002,
Cat. J/ApJS/143/277; Veilleux et al. 2002, Cat. J/ApJS/143/315).
* For non-1 Jy ULIRGs and all LIRGs, we specify a unique galaxy nucleus
designation. 2MASS sources are used where possible.
Note (3): Sources are, in order of preference, the SDSS (Rupke et al.,
2005ApJS..160...87R 2005ApJS..160...87R; Kim et al. 1995ApJS...98..129K 1995ApJS...98..129K; Wu et al., 1998,
Cat. J/A+AS/132/181) or NED.
Note (4): The total galaxy luminosity has been multiplied by the factor
in col. KsMAG.
Note (5): Sample from which galaxy is taken as follows:
RBGS = Revised Bright Galaxy Sample
(Sanders et al. 2003, Cat. J/AJ/126/1607)
1 Jy = 1Jy sample (Kim & Sanders 1998ApJS..119...41K 1998ApJS..119...41K),
WGS = Warm Galaxy Sample (Kim et al. 1995ApJS...98..129K 1995ApJS...98..129K)
2 Jy = 2Jy sample (Strauss et al., 1992, Cat. II/174)
FF = FIRST-FSC sample (Stanford et al., 2000 Cat. J/ApJS/131/185)
Note (6): References as follows:
1 = Rupke et al., 2002ApJ...570..588R 2002ApJ...570..588R, 2005ApJS..160...87R 2005ApJS..160...87R
2 = Kim et al., 1995ApJS...98..129K 1995ApJS...98..129K
3 = Wu et al. 1998, Cat. J/A+AS/132/181
4 = SDSS, http://www.sdss.org
5 = Moustakas & Kennicutt, 2006, Cat. J/ApJS/164/81
6 = Liu & Kennicutt, 1995ApJ...450..547L 1995ApJ...450..547L
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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- 6 A6 --- Type LIRGs or ULIRGs
8- 22 A15 --- IRAS Galaxy nucleus designation from the IRAS
Faint Source Catalog
24- 28 F5.2 mag E(B-V) ?=-1.00 Optical extinction, measured from the
Balmer decrement
30- 36 F7.2 0.1nm EWHa Halpha emission-line equivalent width,
uncorrected for underlying absorption
38- 42 F5.2 0.1nm EWHb Hbeta stellar absorption line equivalent width
44- 51 E8.3 mW/m2 F[OII] Observed [OII] λ3726+3729 flux (1)
53- 60 E8.3 mW/m2 FHb Observed Hβ λ4861 flux (2)
62- 69 E8.3 mW/m2 F[OIII] Observed [OIII] λ5007 flux (1)
71- 78 E8.3 mW/m2 F[OI] ?=- Observed [OI] λ6300 flux (1)
80- 87 E8.3 mW/m2 FHa Observed Hα λ6563 flux (1)
89- 96 E8.3 mW/m2 F[NII] Observed [NII] λ6583 flux (1)
98-105 E8.3 mW/m2 F[SII]1 ?=- Observed [SII] λ6716 flux (1)
107-114 E8.3 mW/m2 F[SII]2 ?=- Observed [SII] λ6731 flux (1)
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Note (1): Observed line fluxes, uncorrected for extinction or underlying
stellar absorption. Line flux measurement errors are 5% for strong
lines, and up to 20%-30% in a few individual cases for weak lines
(e.g., [OI], [OIII], and/or [SII]).
Note (2): Hbeta flux had stellar absorption contamination removed
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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- 6 A6 --- Type LIRGs or ULIRGs
8- 22 A15 --- IRAS Galaxy nucleus designation from the IRAS
Faint Source Catalog
24- 27 F4.2 [-] logR23 logarithm of R23
=[F([OII]3726,3729)+F([OIII]4959,5007)]/F(Hb)
29- 33 F5.2 [-] logO23 logarithm of O23
=[F([OIII]4959,5007)+F[OII]3726,3729)
35- 38 F4.2 [-] eps(O)1 ?=- Oxygen abundance from system of
Pilyugin & Thuan 2005ApJ...631..231P 2005ApJ...631..231P (1)
40- 43 F4.2 [-] eps(O)2 ?=- Oxygen abundance from systems of
McGaugh 1991ApJ...380..140M 1991ApJ...380..140M and
Kuzio de Naray et al. 2004MNRAS.355..887D 2004MNRAS.355..887D (1)
45- 48 F4.2 [-] eps(O)3 ?=- Oxygen abundance from system of
Tremonti et al., 2004ApJ...613..898T 2004ApJ...613..898T (1)
50- 53 F4.2 [-] eps(O)4 ?=- Oxygen abundance from system of Charlot &
Longhetti, 2001MNRAS.323..887C 2001MNRAS.323..887C, case F (1)
55- 58 F4.2 [-] eps(O)5 ?=- Oxygen abundance from system of Kewley &
Dopita 2002ApJS..142...35K 2002ApJS..142...35K (1)
60- 63 F4.2 [-] eps(O)6 ?=- Oxygen abundance from system of Charlot &
Longhetti, 2001MNRAS.323..887C 2001MNRAS.323..887C, Case A (1)
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Note (1): See Sect. 3.1 for a description of each system.
The abundances are eps(X) = 12 + log(X/H)
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 09-Apr-2010