J/ApJ/704/789 Ultra-luminous infrared galaxies in SDSS-DR6 (Hou+, 2009)
Ultra-luminous infrared galaxies in Sloan Digital Sky Survey Data Release 6. Hou L.G., Wu X.-B., Han J.L. <Astrophys. J., 704, 789-802 (2009)> =2009ApJ...704..789H
ADC_Keywords: Galaxies, IR ; Active gal. nuclei ; Surveys ; Spectroscopy Keywords: galaxies: active - galaxies: formation - galaxies: nuclei - galaxies: starburst - infrared: galaxies Abstract: Ultra-luminous infrared galaxies (ULIRGs) are interesting objects with dramatic properties. Many efforts have been made to understand the physics of their luminous infrared emission and evolutionary stages. However, a large ULIRG sample is still needed to study the properties of their central black holes (BHs), the BH-host galaxy relation, and their evolution. We identified 308 ULIRGs from the Sloan Digital Sky Survey Data Release 6, and classified them into the NL ULIRGs (with only narrow emission lines) and the Type I ULIRGs (with broad emission lines). About 56% of ULIRGs in our total sample show interaction features, and this percentage is 79% for redshift z<0.2. Optical identifications of these ULIRGs show that the active galactic nucleus percentage is at least 49%, and the percentage increases with the infrared luminosity. We found 62 Type I ULIRGs, and estimated their BH masses and velocity dispersions from their optical spectra. Together with known Type I ULIRGs in the literature, a sample of 90 Type I ULIRGs enables us to make a statistical study. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 153 308 The parameters of our ULIRG sample table2.dat 97 62 The parameters of Type I ULIRG sample
See also: II/294 : The SDSS Photometric Catalog, Release 7 (Adelman-McCarthy+, 2009) II/156 : IRAS Faint Source Catalog, |b| > 10, Version 2.0 (Moshir+ 1989) J/ApJS/182/628 : Spitzer quasar and ULIRG evolution study (Veilleux+, 2009) J/MNRAS/375/115 : ULIRGs galaxies in SDSS, 2dF and 6dF (Hwang+, 2007) J/AJ/131/1942 : 2MASS observations of IRAS 1Jy ULIRGs (Chen+, 2006) J/A+A/409/115 : VLA imaging of IRAS 1 Jy ULIRG sample (Nagar+, 2003) J/ApJS/143/315 : IRAS 1Jy sample of ultraluminous galaxies. II. (Veilleux+, 2002) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 11 A11 --- IRAS IRAS identification (Cat. II/156) 13- 17 F5.3 --- z SDSS-DR6 redshift 19- 37 A19 --- SDSS SDSS-DR6 identification (Cat. II/282; superseded by Cat. II/294) 39- 43 F5.2 [Lsun] LFIR Log of far-IR luminosity 45- 50 F6.1 mJy SNVSS ? NVSS 1.4GHz flux density 52- 58 F7.2 mJy SFIRST ? FIRST 1.4GHz flux density 60- 62 A3 --- Class Interaction feature class (1) 64- 66 A3 --- N [Yes/No ] NED identifications? (2) 68- 72 F5.2 aW/m2 fHb ? The Hβ line flux (3) 74- 77 F4.2 aW/m2 e_fHb ? Uncertainty in fHb 79- 83 F5.2 aW/m2 fOIII ? The [OIII](5007) line flux (3) 85- 88 F4.2 aW/m2 e_fOIII ? Uncertainty in fOIII 90- 95 F6.2 aW/m2 fHa ? The Hα line flux (3) 97-100 F4.2 aW/m2 e_fHa ? Uncertainty in fHa 102-106 F5.2 aW/m2 fNII ? The [NII](6583) line flux (3) 108-111 F4.2 aW/m2 e_fNII ? Uncertainty in fNII 113-117 F5.2 aW/m2 fSII ? The [SII](6716+6731) line flux (3) 119-122 F4.2 aW/m2 e_fSII ? Uncertainty in fSII 124-128 F5.2 aW/m2 fOI ? The [OI](6300) line flux (3) 130-133 F4.2 aW/m2 e_fOI ? Uncertainty in fOI 135-153 A19 --- Type Baldwin-Phillips-Terlevich (BPT) diagram galaxy type (Baldwin et al. 1981PASP...93....5B; see Figure 5)
Note (1): ULIRGs are classified into (see Veilleux et al. 2002, Cat. J/ApJS/143/315) the following classes: I = one nucleus but with tail features; II = two identified nuclei and well-developed tidal tails or/and bridges; III = two close or even overlapped nuclei, and their redshifts (almost in all cases, only one source in this system has spectral redshift measurements, and another/others have only SDSS photometric redshift data) are consistent. n = not clear Examples are shown in Figure 3 (see section 2.3). Note (2): Code is: Yes = the redshift or/and the counterpart provided in NED is consistent with ours. No = the redshift is not listed in NED. Note (3): In units of 10-15erg/s/cm2.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 11 A11 --- IRAS IRAS identification (Cat. II/156) 12 A1 --- m_IRAS [w] Multiplicity indicator (F13451+3932 is an interaction system with two bright nuclei) 14- 18 F5.3 --- z Redshift 20- 25 F6.2 10-19W/m2/nm f5100 Continuum flux at 5100 Angstroms (1) 27- 31 F5.2 10-19W/m2/nm E_f5100 Upper limit uncertainty in f5100 33- 37 F5.2 10-19W/m2/nm e_f5100 Lower limit uncertainty in f5100 39- 42 I4 km/s Hb FWHM of broad Hβ component 44- 47 I4 km/s [OIII] FWHM of [OIII](5007) profile 49- 52 I4 km/s NLc FWHM of [OIII] narrow line core 54- 55 I2 km/s E_NLc ? Upper limit uncertainty in NLcore 57- 58 I2 km/s e_NLc ? Lower limit uncertainty in NLcore 60- 62 I3 km/s [SII] ? FWHM of [SII](6716) profile 64- 66 I3 km/s E_[SII] ? Upper limit uncertainty in [SII] 68- 70 I3 km/s e_[SII] ? Lower limit uncertainty in [SII] 72- 77 F6.2 10+7Msun MBH Black hole mass 79- 84 F6.2 10+7Msun e_MBH Uncertainty in MBH 86- 89 F4.2 --- Lb/LE Ratio of bolometric to Eddington luminosities 91- 95 F5.2 [Lsun] logLIR Log of IR luminosity 97 I1 --- q_[OIII] [1/2] Quality of [OIII](5007) FWHM (2)
Note (1): Corrected by use of Fλ(5100Å)rest=(1+z)Fλ((1+z)5100Å)obs, where z is the redshift, and the unit is 10-17erg/s/cm2/Angstrom. Note (2): Quality code is: 1 = fitting result is reliable; 2 = the FWHM can not be well fitted due to the low quality of the spectra or suffer serious absorptions around the emission lines.
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 21-Nov-2011
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