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 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:
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FileName Lrecl Records Explanations
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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
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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- 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)
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Note (1): IRAS Fluxes from Moshir et al. (1990, Cat. II/156).
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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- 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
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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- 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
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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.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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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)
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Note (1): Classification using the VO87 scheme (Veilleux & Osterbrock,
1987ApJS...63..295V 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.
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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