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
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:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 97 118 Spectral classification result for the 1Jy ULIRG sample (Kim & Sanders, 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) 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)
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) diagrams. The projected radius used for searching companions is ∼100kpc.
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.dat
Bytes Format Units Label Explanations
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 (D_AGN_) derived from the [OI]/Hα diagram (7) 57- 59 F3.1 --- D2 ? Empirical linear distance (D_AGN_) 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(L_IR_) in solar units (11)
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) 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) 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) cb96 = Clements & Baker (1996A&A...314L...5C); hv95 = Heisler & Vader (1995AJ....110...87H); vva68 = Vorontsov-Velyaminov & Arhipova (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 in table 2 or from Kewley et al. (2001, Cat. J/ApJS/132/37) in table 3.
History: From electronic version of the journal
(End) Emmanuelle Perret [CDS] 05-Mar-2012
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