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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.
   <Astrophys. J. Suppl. Ser. 132, 37 (2001)>
   =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
    108<LIR<1012.5L☉. We have classified these galaxies using
    new theoretical lines on the standard optical diagnostic diagrams. We
    use a theoretical extreme mixing line between the starburst and AGN
    regions to classify LINER galaxies and we define a theoretical
    boundary separating AGNs from starbursts. We find that many galaxies
    previously classified as LINERs appear to lie on a mixing sequence
    between starburst and AGN type galaxies.

File Summary:

       FileName      Lrecl  Records   Explanations

ReadMe            80        .   This file
table1.dat       107      285   Sample parameters
table2.dat        84      283   Log of observations
table3.dat        88      258   Measured flux ratios
table4.dat       131      246   Sample classifications


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- 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. II/156).



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 Hα/Hβ flux ratio (2)
  40- 44  F5.2  [---]   OIII/Hb   ? Log [OIII](5007Å)/Hβ flux ratio
  46- 50  F5.2  [---]   OI/Ha     ? Log [OI](6300Å)/Hα flux ratio
  52- 57  F6.3  [---]   NII/Ha    Log [NII](6584Å)/Hα flux ratio
  59- 63  F5.2  [---]   SII/Ha    ? Log [SII](6717,31Å)/Hα flux ratio
  65- 68  F4.2  mag     E(B-V)    ? The E(B-V) extinction coefficient
  70- 73  F4.2  ---     SIIRat    ? The 6717Å/6731Å [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   ? Hα 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 Hα 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]/Hα vs [OIII]/Hβ (1)
  39- 43  A5    ---    SII      Galaxy classification from V087 diagram
                                [SII]/Hα vs [OIII]/Hβ (1)
  45- 49  A5    ---    OI       Galaxy classification from V087 diagram
                                [OI]/Hα vs [OIII]/Hβ (1)
  51- 61  A11   ---    vClass   Adopted classification from the V087 method (1)
  63- 67  A5    ---    tNII     Galaxy classification from theoretical diagram
                                [NII]/Hα vs [OIII]/Hβ (2)
  69- 73  A5    ---    tSII     Galaxy classification from the theoretical
                                [SII]/Hα vs [OIII]/Hβ diagram (2)
  75- 79  A5    ---    tOI      Galaxy classification from the theoretical
                                [OI]/Hα vs [OIII]/Hβ 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]/Hβ>3, LINERS if they lie
     above and to the right of the semi-empirical line and have
     [OIII]/Hβ<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