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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
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 <z≳0.1. File Summary:
FileName Lrecl Records Explanations
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
See also: II/156 : IRAS Faint Source Catalog, |b|>10, Version 2.0 (Moshir+ 1989) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
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)
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). 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; Kim et al. 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), WGS = Warm Galaxy Sample (Kim et al. 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, 2005ApJS..160...87R 2 = Kim et al., 1995ApJS...98..129K 3 = Wu et al. 1998, Cat. J/A+AS/132/181 4 = SDSS, 5 = Moustakas & Kennicutt, 2006, Cat. J/ApJS/164/81 6 = Liu & Kennicutt, 1995ApJ...450..547L
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
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)
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
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
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 (1) 40- 43 F4.2 [-] eps(O)2 ?=- Oxygen abundance from systems of McGaugh 1991ApJ...380..140M and Kuzio de Naray et al. 2004MNRAS.355..887D (1) 45- 48 F4.2 [-] eps(O)3 ?=- Oxygen abundance from system of Tremonti et al., 2004ApJ...613..898T (1) 50- 53 F4.2 [-] eps(O)4 ?=- Oxygen abundance from system of Charlot & Longhetti, 2001MNRAS.323..887C, case F (1) 55- 58 F4.2 [-] eps(O)5 ?=- Oxygen abundance from system of Kewley & Dopita 2002ApJS..142...35K (1) 60- 63 F4.2 [-] eps(O)6 ?=- Oxygen abundance from system of Charlot & Longhetti, 2001MNRAS.323..887C, Case A (1)
Note (1): See Sect. 3.1 for a description of each system. The abundances are eps(X) = 12 + log(X/H)
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 09-Apr-2010
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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