J/ApJS/132/37 Spectroscopy of Southern warm IR galaxies (Kewley+, 2001) ================================================================================ Optical classification of southern warm infrared galaxies. Kewley L.J., Heisler C.A., Dopita M.A., Lumsden S. =2001ApJS..132...37K ================================================================================ ADC_Keywords: Galaxies, IR ; Spectra, infrared Keywords: galaxies: active - galaxies: fundamental parameters - galaxies: ISM - galaxies: starburst - infrared: galaxies - techniques: spectroscopic Abstract: In this paper, we present high-resolution optical spectra and optical classifications from our large sample of 285 warm infrared galaxies 10^8^ 10, Version 2.0 (Moshir+ 1989) Byte-by-byte Description of file: table1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 10 A10 --- IRAS IRAS name 12- 28 A17 --- Name Common name 30- 31 I2 h RAh Right Ascension (B1950) 33- 34 I2 min RAm Right Ascension (B1950) 36- 39 F4.1 s RAs Right Ascension (B1950) 42 A1 --- DE- Declination (B1950) 43- 44 I2 deg DEd Declination (B1950) 46- 47 I2 arcmin DEm Declination (B1950) 49- 50 I2 arcsec DEs Declination (B1950) 52- 56 I5 km/s Vel Recessional velocity 58- 62 F5.1 Mpc Dist Distance 64- 68 F5.2 [solLum] logFIR Log of the Far-IR luminosity in solar units 70- 74 F5.2 [solLum] logIR Log of the IR luminosity in solar units 76- 82 A7 Jy F12 IRAS flux at 12 microns (1) 84- 90 A7 Jy F25 IRAS flux at 25 microns (1) 92- 98 A7 Jy F60 IRAS flux at 60 microns (1) 100-107 A8 Jy F100 IRAS flux at 100 microns (1) -------------------------------------------------------------------------------- Note (1): IRAS Fluxes from Moshir et al. (1990, Cat. ). -------------------------------------------------------------------------------- Byte-by-byte Description of file: table2.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 10 A10 --- IRAS IRAS Name 12- 21 A10 "DD/MM/YYYY" Obs Date observed 23- 25 F3.1 arcsec Seeing ? Atmospheric seeing 27- 84 A58 --- Comm Comments -------------------------------------------------------------------------------- Byte-by-byte Description of file: table3.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 10 A10 --- IRAS IRAS name 12- 16 A5 --- m_IRAS Component in IRAS source 18 A1 --- n_IRAS Note about the flux results (1) 20- 33 A14 --- Name Common name 35- 38 F4.2 [---] Ha/Hb ? Log H{alpha}/H{beta} flux ratio (2) 40- 44 F5.2 [---] OIII/Hb ? Log [OIII](5007{AA})/H{beta} flux ratio 46- 50 F5.2 [---] OI/Ha ? Log [OI](6300{AA})/H{alpha} flux ratio 52- 57 F6.3 [---] NII/Ha Log [NII](6584{AA})/H{alpha} flux ratio 59- 63 F5.2 [---] SII/Ha ? Log [SII](6717,31{AA})/H{alpha} flux ratio 65- 68 F4.2 mag E(B-V) ? The E(B-V) extinction coefficient 70- 73 F4.2 --- SIIRat ? The 6717{AA}/6731{AA} [SII] flux ratio (2) 77- 78 A2 --- l_Ne [<= ] Limit flag on Ne 80- 83 I4 cm-3 Ne ? Mean electron density within 1 kpc (3) 85- 88 I4 km/s HaWidth ? H{alpha} line width -------------------------------------------------------------------------------- Note (1): The note number means the following: 1 = Galaxies which display asymmetries to their line profiles. The fluxes for these galaxies are composed of the sum of two Gaussians; one for the broader asymmetric component and one for the narrow symmetric component. See the Appendix for more details on these galaxies. 2 = Fluxes result from fitting three narrow components to each emission line. See the Appendix for further information about this galaxy. 3 = Fluxes result from fitting a broad H{alpha} component plus two narrow components for each emission line. Note (2): Not reddening-corrected. Note (3): Electron density derived from the SIIRat flux ratio. -------------------------------------------------------------------------------- Byte-by-byte Description of file: table4.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 10 A10 --- IRAS IRAS name 12- 16 A5 --- m_IRAS Component in IRAS source 18- 31 A14 --- Name Common name 33- 37 A5 --- NII Galaxy classification from V087 diagram [NII]/H{alpha} vs [OIII]/H{beta} (1) 39- 43 A5 --- SII Galaxy classification from V087 diagram [SII]/H{alpha} vs [OIII]/H{beta} (1) 45- 49 A5 --- OI Galaxy classification from V087 diagram [OI]/H{alpha} vs [OIII]/H{beta} (1) 51- 61 A11 --- vClass Adopted classification from the V087 method (1) 63- 67 A5 --- tNII Galaxy classification from theoretical diagram [NII]/H{alpha} vs [OIII]/H{beta} (2) 69- 73 A5 --- tSII Galaxy classification from the theoretical [SII]/H{alpha} vs [OIII]/H{beta} diagram (2) 75- 79 A5 --- tOI Galaxy classification from the theoretical [OI]/H{alpha} vs [OIII]/H{beta} diagram (2) 81- 91 A11 --- tClass Adopted classification from the theoretical method (2) 93-131 A39 --- Com Comments (3) -------------------------------------------------------------------------------- Note (1): Classification using the VO87 scheme (Veilleux & Osterbrock, 1987ApJS...63..295V): Galaxies are classed as AGN if they lie above and to the right of the semi-empirical line and have [OIII]/H{beta}>3, LINERS if they lie above and to the right of the semi-empirical line and have [OIII]/H{beta}<3, and starbursts/HII-region like if they lie below and to the left of the semi-empirical line. Objects which lie within 0.1dex of the semi-empirical classification line are given an additional borderline "B"' classification. "AMB" means ambiguous. Note (2): Classification using our theoretical extreme starburst line and extreme mixing line: Galaxies are classed as AGN if they lie above and to the right of the theoretical (extreme starburst) line, HII-region like if they lie below and to the left of the theoretical line. Objects which lie within 0.1dex of the extreme starburst classification line are given an additional borderline ``B'' class. Objects lying below and to the right of our extreme mixing line were classed as LINERs. Objects lying within 0.1dex of the extreme mixing line were given an AGN/L class as they are in between AGN and LINER regions on the diagram. Composite galaxies are indicated with a ``C'' while possible composite galaxies are noted in the comments section. "AMB" means ambiguous. Note (3): Galaxies with broader [OIII] lines than remaining emission lines are shown by an '[OIII] broader' in the comments column. -------------------------------------------------------------------------------- History: * 09-Apr-2001: From electronic version of the journal * 03-Mar-2006: table3.dat, Arp240: IRAS changed from 13370+0105 to 13373+0105 ================================================================================ (End) Greg Schwarz [AAS], Patricia Bauer [CDS] 09-Apr-2001