J/ApJ/709/884 Role of starburst-AGN composites in LIRG mergers (Yuan+, 2010)
The role of starburst-active galactic nucleus composites in luminous infrared
galaxy mergers: insights from the new optical classification scheme.
Yuan T.-T., Kewley L.J., Sanders D.B.
<Astrophys. J., 709, 884-911 (2010)>
=2010ApJ...709..884Y 2010ApJ...709..884Y
ADC_Keywords: Galaxies, IR ; Morphology ; Active gal. nuclei ; Galaxies, spectra
Keywords: galaxies: active - galaxies: evolution - galaxies: interactions -
galaxies: starburst - infrared: galaxies
Abstract:
We investigate the fraction of starbursts, starburst-active galactic
nucleus (AGN) composites, Seyferts, and low-ionization narrow
emission-line region galaxies (LINERs) as a function of infrared
luminosity (LIR) and merger progress for ∼500 infrared (IR)-selected
galaxies. Using the new optical classifications afforded by the
extremely large data set of the Sloan Digital Sky Survey, we find that
the fraction of LINERs in IR-selected samples is rare (<5%) compared
with other spectral types. The lack of strong IR emission in LINERs is
consistent with recent optical studies suggesting that LINERs contain
AGN with lower accretion rates than in Seyfert galaxies. Most
previously classified IR-luminous LINERs are classified as
starburst-AGN composite galaxies in the new scheme. Starburst-AGN
composites appear to "bridge" the spectral evolution from starburst to
AGN in ULIRGs. The relative strength of the AGN versus starburst
activity shows a significant increase at high IR luminosity. In ULIRGs
(LIR>1012L☉), starburst-AGN composite galaxies dominate at
early-intermediate stages of the merger, and AGN galaxies dominate
during the final merger stages.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 97 118 Spectral classification result for the 1Jy ULIRG
sample (Kim & Sanders, 1998ApJS..119...41K 1998ApJS..119...41K)
table2.dat 97 140 Spectral classification result and morphology
for the IRAS Bright Galaxy Survey (BGS; Veilleux
et al. 1995ApJS...98..171V 1995ApJS...98..171V) sample
table3.dat 97 301 *Spectral classification result and morphology
for the Southern Warm Infrared Galaxies sample
(Kewley et al. 2001, Cat. J/ApJS/132/37)
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Note on table3.dat: We only list the spectral type results for galaxies having
available line ratios with S/N>3σ in all three BPT (Baldwin et al.
1981PASP...93....5B 1981PASP...93....5B) diagrams. The projected radius used for searching
companions is ∼100kpc.
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See also:
J/A+A/508/117 : Spitzer selected starbursts at z∼2 (Fiolet+, 2009)
J/ApJ/686/127 : Starbursts luminosities based on PAH (Weedman+, 2008)
J/AJ/132/321 : Morphology of narrow-line Seyfert 1 galaxies (Deo+, 2006)
J/ApJS/158/139 : Atlas of warm AGN and starbursts (Keel+, 2005)
J/ApJS/143/315 : IRAS 1Jy sample of ultraluminous galaxies. II. (Veilleux+,
2002)
J/ApJS/143/377 : UV-to-FIR magnitudes for 83 starburst galaxies (Wu+, 2002)
J/ApJS/132/37 : Spectroscopy of Southern warm IR galaxies (Kewley+, 2001)
J/ApJ/522/113 : 1Jy IRAS galaxies optical spectroscopy (Veilleux+, 1999)
J/A+AS/130/285 : Sample of starburst nucleus galaxies (Contini+ 1998)
Byte-by-byte Description of file: table[123].dat
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Bytes Format Units Label Explanations
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1 A1 --- f_Name [*] *: ULIRG (not for table 1)
2- 15 A14 --- Name Galaxy name (IRAS for table 1 and 3) (1)
16- 19 A4 --- m_Name Name component
20 A1 --- n_Name [a] Flag on NGC 6621 in table 2 (2)
22- 29 A8 --- OName Other name (not for table 2)
31- 34 A4 --- t[NII] Optical spectral type derived from the
[NII]6583 (6)
36- 38 A3 --- t[SII] Optical Spectral type derived from
[SII]6716,6731 (6)
40- 42 A3 --- t[OI] Optical spectral type derived from
[OI]6300 (6)
44- 47 A4 --- Type Adopted spectral type (6)(4)
49- 51 A3 --- VO87 VO87 spectral type (not for table 3) (6)(5)
53- 55 F3.1 --- D1 ? Empirical linear distance (DAGN) derived
from the [OI]/Hα diagram (7)
57- 59 F3.1 --- D2 ? Empirical linear distance (DAGN) derived
from the [NII]/Hα diagram (7)
61- 66 F6.2 kpc ns ? Projected nuclear separation (not for table 1)
68- 72 A5 --- f_ns Peculiarities (8)
74- 83 A10 --- r_ns Reference(s) (9)
85- 91 A7 --- Class Morphology class (10)
93- 97 F5.2 [Lsun] logL ? log(LIR) in solar units (11)
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Note (1): In table 2, MCG+01-42-088 is a misprint for MCG+01-42-008;
corrected at CDS.
Note (2): a = Line flux of this object given in table A1 ofKim et al.
(1995ApJS...98..129K 1995ApJS...98..129K) has a sign error.
Note (4): Adopted spectral type using the 2-of-3 scheme; single colons
indicate the object does not have the same spectral type in all three
diagrams, i.e., the ambiguous class. Double colon means the
classification does not agree on any of the diagrams, the
classification in those rare cases is highly uncertain.
Note (5): For comparison, we also list the classifications given in
Veilleux et al. (1999, Cat. J/ApJ/522/113) using the traditional VO87
(Veilleux & Osterbrock, 1987ApJS...63..295V 1987ApJS...63..295V) method.
Note (6): Optical spectral types derived in this work from the [NII]6583,
[SII]6716,6731, and [OI]6300 diagrams, respectively. The typical
uncertainty on the emission-line ratios is ∼10%; colons indicate
larger uncertainty of the line ratios of ∼25% for [SII]/Hα and
[OI]/Hα; double colons indicate larger uncertainty of the line
ratios of ∼25% for [OIII]/Hβ (col. t[NII]).
The symbols are:
H = star-forming galaxies,
L = LINERs,
S2 = Seyfert 2 galaxies,
S1 = Seyfert 1 galaxies,
cp = starburst-AGN composite galaxies.
Note (7): See appendix A for a complete definition.
Note (8): Flag as follows:
-1 = single nucleus with tidal features;
-2 = isolated systems
: = lower limit;
m = multiple (more than two) interacting objects;
cl = member of clusters.
Note (9): References used to obtain projected separation or tidal features
as follows:
2MASS = 2MASS images (Ks band);
DSS = DSS images;
tec00 = Tecza et al. (2000ApJ...537..178T 2000ApJ...537..178T)
cb96 = Clements & Baker (1996A&A...314L...5C 1996A&A...314L...5C);
hv95 = Heisler & Vader (1995AJ....110...87H 1995AJ....110...87H);
vva68 = Vorontsov-Velyaminov & Arhipova (1968MCG...C04....0V 1968MCG...C04....0V);
ke01 = Kewley et al. (2001, Cat. J/ApJS/132/37)
Note (10): Morphology class from Veilleux et al. 2002, Cat. J/ApJS/143/315,
as follows:
a = wide binary;
b = close binary;
c = diffuse merger;
d = compact merger;
e = old merger;
tpl = triple mergers;
m = multiple mergers;
iso = isolated.
Note (11): log(LIR/L☉) from Veilleux et al. 1999, Cat. J/ApJ/522/113
in table 1; from Kim et al. 1995ApJS...98..129K 1995ApJS...98..129K in table 2
or from Kewley et al. (2001, Cat. J/ApJS/132/37) in table 3.
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 05-Mar-2012