J/ApJ/698/1682 Most luminous dusty galaxies (Weedman+, 2009)
Evolution of the most luminous dusty galaxies.
Weedman D.W., Houck J.R.
<Astrophys. J., 698, 1682-1697 (2009)>
=2009ApJ...698.1682W 2009ApJ...698.1682W
ADC_Keywords: Active gal. nuclei ; Spectra, infrared ; Redshifts
Keywords: galaxies: active - galaxies: distances and redshifts -
galaxies: evolution - galaxies: formation - galaxies: starburst -
infrared: galaxies
Abstract:
A summary of mid-infrared continuum luminosities arising from dust is
given for very luminous galaxies, LIR>1012L☉, with
0.005<z<3.2 containing active galactic nuclei (AGNs), including 115
obscured AGNs and 60 unobscured (type 1) AGNs. All sources have been
observed with the Spitzer Infrared Spectrograph. Obscured AGNs are
defined as having optical depth τ>0.7 in the 9.7um silicate
absorption feature (i.e., half of the continuum is absorbed) and
having equivalent width of the 6.2um polycyclic aromatic hydrocarbon
feature <0.1um (to avoid sources with a significant starburst
component). Unobscured AGNs are defined as those that show silicate in
emission. Luminosity νLν(8um) for the most luminous obscured
AGNs is found to scale as (1+z)2.6 to z=2.8. For unobscured AGNs,
the scaling with redshift is similar, but luminosities
νLν(8um) are approximately three times greater for the most
luminous sources. Using both obscured and unobscured AGNs having total
infrared fluxes from the Infrared Astronomical Satellite, empirical
relations are found between νLν(8um) and LIR.
Description:
In this paper, we assemble data from 20 different Spitzer programs
from the archive to summarize a wide variety of AGNs IRS spectra,
including 115 heavily obscured sources classified by having strong
absorption in the 9.7um silicate feature, and 60 unobscured sources
(type 1 AGN) as classified by silicate emission.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 69 115 Continuum luminosities for obscured AGNs
table2.dat 69 60 Continuum luminosities for Silicate emission AGNs
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See also:
J/ApJ/693/370 : 24um flux-limited sample of galaxies (Weedman+, 2009)
J/MNRAS/395/1695 : Spitzer mid-IR spectroscopy of LIRGs (Hernan-Caballero+,
2009)
J/ApJ/683/114 : IRS spectra of faint IRAS sources (Sargsyan+, 2008)
J/ApJ/658/778 : Spitzer mid-IR spectroscopy of z∼2 ULIRGs (Yan+, 2007)
J/ApJ/671/323 : Spitzer Spectra of a 10mJy galaxy sample (Houck+, 2007)
J/AJ/133/186 : Optical spectroscopy of 77 luminous AGNs and QSOs (Lacy+,
2007)
J/ApJ/642/673 : IR-selected obscured AGN candidates (Polletta+, 2006)
J/ApJ/653/127 : 9.7um silicate features in AGNs (Shi+, 2006)
J/MNRAS/372/741 : SXDF 100µJy catalogue (Simpson+, 2006)
J/AJ/131/2859 : Extragalactic First Look Survey: 24µm data (Fadda+, 2006)
http://www.sdss.org/ : Sloan Digital Sky Survey home page
Byte-by-byte Description of file: table1.dat table2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq Running sequence number
5- 20 A16 --- Name AGN name
21- 22 I2 h RAh Hour of right ascension (J2000)
23- 24 I2 min RAm Minute of right ascension (J2000)
25- 29 F5.2 s RAs Second of right ascension (J2000)
30 A1 --- DE- Sign of the declination (J2000)
31- 32 I2 deg DEd Degree of declination (J2000)
33- 34 I2 arcmin DEm Arcminute of declination (J2000)
35- 38 F4.1 arcsec DEs Arcsecond of declination (J2000)
40- 45 F6.4 --- z Redshift
46 A1 --- r_z [efg] Flag on z (1)
48- 54 F7.2 mJy F8um Observed flux density in continuum at rest
frame 8um (2)
56- 60 F5.2 [10-7W] logL8 Rest-frame luminosity νL_ν(8um) (3)
62- 66 F5.2 [10-7W] logLir ? Infrared luminosity (only for table 2) (4)
68- 69 I2 --- Ref Reference number (5)
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Note (1): Flag as follows:
e = Optical redshift and classification in Lacy et al. (2007,
Cat. J/AJ/133/186)
f = Optical redshift and classification in Simpson et al. (2006,
Cat. J/MNRAS/372/741, <[SMR2006] VLA JHHMMSS+DDMMm> in Simbad)
g = Optical redshift and classification from the SDSS
Note (2): Observed flux density measured from published spectra in references
given, or from our own extractions, as described in Section 2.3.
Typical uncertainties are ±5% for sources with fν(8um)≳5mJy
and ±10% for sources with fν(8um)∼1mJy. Typical uncertainties
are ±5% in table 2. For sources in Schweitzer et al.
(2008ApJ...679..101S 2008ApJ...679..101S, reference 17), fν(8um) is determined by
scaling from published fν(6um) using the average spectra in
Figure 2 of Schweitzer et al. for sources without PAH (characteristic
of the highest luminosity sources), such that
fν(8um)/fν(6um)=1.12.
Note (3): Rest-frame luminosity determined using peak fν(8um) and
luminosity distances DL from E.L. Wright,
http://www.astro.ucla.edu/wright/CosmoCalc.html, for H0=71km/s/Mpc,
ΩM=0.27 and ΩΛ=0.73.
(log[νLν(8um)(L☉)]=log[νLν(8um)(erg/s)]-33.59.)
Note (4): For sources in Schweitzer et al. (2008ApJ...679..101S 2008ApJ...679..101S) (reference 17),
Lir is determined as in Sanders & Mirabel (1996ARA&A..34..749S 1996ARA&A..34..749S) for
sources having measured IRAS flux densities at all IRAS wavelengths;
Lir=2.14x1036DL2[13.5(fν(12um))+5.2(fν(25um))
+2.58(fν(60um))+(f_ν(100um))] for flux densities in mJy
and luminosities in erg/s (L☉=3.83x1033erg/s).
Note (5): Reference for IRS spectrum as follows:
1 = Farrah et al. (2007ApJ...667..149F 2007ApJ...667..149F);
2 = Imanishi et al. (2007ApJS..171...72I 2007ApJS..171...72I);
3 = Sargsyan et al. (2008, Cat. J/ApJ/683/114);
4 = Shi et al. (2006, Cat. J/ApJ/653/127);
5 = Weedman & Houck (2009, Cat. J/ApJ/693/370);
6 = new spectra in Figure 2 [sources 73, 111 from archival program 30447 (G.
Fazio, P.I.), source 90 from archival program 20629 (L. Yan, P.I.),
source 16 from archival program 40539 (G. Helou, P.I), sources 13,20,21,
23,70 from our own new observations, program 50031];
7 = Brand et al. (2008ApJ...680..119B 2008ApJ...680..119B; <[BWD2008] SST24 JHHMMSS.s+DDMMSS> in
Simbad);
8 = Farrah et al. (2009ApJ...696.2044F 2009ApJ...696.2044F; in
Simbad);
9 = Brand et al. (2008ApJ...673..119B 2008ApJ...673..119B; <[BWD2008] SST24 JHHMMSS.s+DDMMSS> in
Simbad);
10 = Houck et al. (2005ApJ...622L.105H 2005ApJ...622L.105H; <[HSW2005] SST24 JHHMMSS.ss+DDMMSS.s>
in Simbad);
11 = Weedman et al. (2006ApJ...638..613W 2006ApJ...638..613W;
<[WLH2006] SST24 JHHMMSS.ss+DDMMSS.s> in Simbad);
12 = Weedman et al. (2006ApJ...653..101W 2006ApJ...653..101W);
13 = Polletta et al. (2008ApJ...675..960P 2008ApJ...675..960P);
14 = Yan et al. (2007, Cat. J/ApJ/658/778;
<[YSF2007] SST24 JHHMMSS.ss+DDMMSS.s> in Simbad); Sajina et
al. (2007ApJ...664..713S 2007ApJ...664..713S);
15 = Martinez-Sansigre et al. (2008ApJ...674..676M 2008ApJ...674..676M);
16 = Hao et al. (2005ApJ...625L..75H 2005ApJ...625L..75H);
17 = Schweitzer et al. (2008ApJ...679..101S 2008ApJ...679..101S);
18 = Markwick-Kemper et al. (2007ApJ...668L.107M 2007ApJ...668L.107M);
19 = new extractions of sources in the FLS and SWIRE Lockman fields having
fν(24um)>5mJy and R>20mag which have optical redshifts and
classifications cited as type 1 AGN in the NED;
20 = new extractions of sources available within Spitzer Legacy Program 40539
(G. Helou, P.I.), a flux limited sample with fν(24um)>5mJy, which
have optical redshifts and classifications as type 1 AGN cited in the NED
or as determined from our examination of SDSS spectra, not including 2
sources also in reference 19.
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 16-Jun-2011