J/ApJS/182/628 Spitzer quasar and ULIRG evolution study (Veilleux+, 2009)
Spitzer quasar and ULIRG evolution study (QUEST).
IV. Comparison of 1 Jy ultraluminous infrared galaxies with Palomar-Green
quasars.
Veilleux S., Rupke D.S.N., Kim D.-C., Genzel R., Sturm E., Lutz D.,
Contursi A., Schweitzer M., Tacconi L.J., Netzer H., Sternberg A.,
Mihos J.C., Baker A.J., Mazzarella J.M., Lord S., Sanders D.B.,
Stockton A., Joseph R.D., Barnes J.E.
<Astrophys. J. Suppl. Ser., 182, 628-666 (2009)>
=2009ApJS..182..628V 2009ApJS..182..628V
ADC_Keywords: Galaxies, IR ; QSOs ; Spectroscopy ; Redshifts
Keywords: galaxies: active - galaxies: interactions - galaxies: Seyfert
galaxies: starburst - infrared: galaxies - quasars: general
Abstract:
We report the results from a comprehensive study of 74 ultraluminous
infrared galaxies (ULIRGs) and 34 Palomar-Green (PG) quasars within
z∼0.3 observed with the Spitzer Infrared Spectrograph (IRS). The
contribution of nuclear activity to the bolometric luminosity in these
systems is quantified using six independent methods that span a range
in wavelength and give consistent results within ~±10%-15% on
average. This agreement suggests that deeply buried active galactic
nuclei (AGNs) invisible to Spitzer IRS but bright in the far-infrared
are not common in this sample. The average derived AGN contribution in
ULIRGs is ∼35%-40%, ranging from ∼15%-35% among "cool"
(f25/f60≤0.2) optically classified HII-like and LINER ULIRGs to
∼50 and ∼75% among warm Seyfert 2 and Seyfert 1 ULIRGs, respectively.
This number exceeds ∼80% in PG QSOs.
Description:
Galaxies from our own program (#3187; P.I. Veilleux) were observed in
the IRS modules SL, SH, and LH, using staring mode. Together, these
modules cover observed wavelengths of 5-35um. The high resolution data
at observed wavelengths of 10-35um (SH and LH modules, with resolution
R∼600) allow sensitive measurements of important atomic and molecular
emission lines.
The ULIRG component of our program focuses on the 1Jy sample, a
complete flux-limited sample of 118 ULIRGs selected at 60um from a
redshift survey of the IRAS faint source catalog (Kim & Sanders,
1998ApJS..119...41K 1998ApJS..119...41K).
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 55 108 Sample (74 ULIRGs and 34 PG quasars)
table2.dat 56 108 Observations
table34.dat 241 108 Emission line fluxes (tables 3 and 4 of paper)
table5.dat 78 108 Continuum measurements
table6.dat 40 74 Fit results: absorption measurements
table7.dat 46 74 Fit results: PAH measurements
table8.dat 54 108 H2 properties
table12.dat 71 108 AGN contributions
table16.dat 122 108 Eddington ratios from photometry and dynamics
--------------------------------------------------------------------------------
See also:
II/156 : IRAS Faint Source Catalog, |b| > 10, Version 2.0 (Moshir+ 1989)
J/ApJS/143/315 : IRAS 1Jy sample of ultralum. galaxies. II. (Veilleux+, 2002)
J/ApJS/143/277 : IRAS 1Jy sample of ultraluminous galaxies. I. (Kim+, 2002)
J/A+A/409/115 : VLA imaging of IRAS 1 Jy ULIRG sample (Nagar+, 2003)
J/AJ/131/1942 : 2MASS observations of IRAS 1Jy ULIRGs (Chen+, 2006)
J/A+A/467/565 : z=1-3 ULIRGs from the Spitzer SWIRE survey (Berta+, 2007)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Type Source type (ULIRG or PG QSO)
9- 22 A14 --- Name Galaxy name (G1)
24- 28 F5.3 --- z Redshift
30- 34 A5 [solLum] logL ? Log bolometric luminosity (1)
36- 39 A4 --- SType Optical spectral type (2)
41- 44 A4 --- IC Interaction class (3)
46 A1 --- l_NS Limit flag on NS
48- 53 F6.2 kpc NS ? Nuclear separation (in mergers)
55 I1 --- r_NS ? Reference for NS (4)
--------------------------------------------------------------------------------
Note (1): For ULIRGs, we assume L(bol)=1.15L(IR).
For PG QSOs, L(bol)=7L(5100Å)+L(IR).
Note (2): From Veilleux et al. (1995ApJS...98..171V 1995ApJS...98..171V, 1999ApJ...522..139V 1999ApJ...522..139V)
and Rupke et al. (2005ApJS..160...87R 2005ApJS..160...87R).
Note (3): From Veilleux et al. (2009, ApJ in press), Veilleux et al.
(2006ApJ...643..707V 2006ApJ...643..707V), or Veilleux et al. (2002, Cat. J/ApJS/143/315)
(in order of preference). Types are QSO, HII, L (liner), S (Seyfert)
or none.
Note (4): References as follows:
1 = Kim et al. (2002, Cat. J/ApJS/143/277);
2 = Veilleux et al. (2006ApJ...643..707V 2006ApJ...643..707V);
3 = Scoville et al. (2000AJ....119..991S 2000AJ....119..991S);
4 = Bahcall et al. (1997ApJ...479..642B 1997ApJ...479..642B);
5 = Sakamoto et al. (1999ApJ...514...68S 1999ApJ...514...68S);
6 = Beswick et al. (2001MNRAS.325..151B 2001MNRAS.325..151B);
7 = Veilleux et al. (2009, ApJ, in press).
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Type Source type (ULIRG or PG QSO)
9- 22 A14 --- Name Galaxy name (G1)
24- 33 A10 --- PID Spitzer proposal ID(s)
35- 38 I4 s SL2 Spitzer/IRS SL2 module exposure time
40- 42 I3 s SL1 Spitzer/IRS SL1 module exposure time
44- 47 I4 s SH ? Spitzer/IRS SH module exposure time
49- 52 I4 s LH ? Spitzer/IRS LH module exposure time
54- 56 I3 s LL ? Spitzer/IRS LL module exposure time
(only when used in the fit)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table34.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Type Source type (ULIRG or PG QSO)
9- 22 A14 --- Name Galaxy name (G1)
24- 31 E8.2 W/cm2 Ne6 ? [NeVI]7.65µm emission line flux
33- 34 I2 % e_Ne6 ? Percent error in Ne6
36 A1 --- l_H2S3 Limit flag on H2S3
37- 44 E8.2 W/cm2 H2S3 ? H2S(3) 9.66µm emission line flux
46- 47 I2 % e_H2S3 ? Percent error in H2S3
49 A1 --- l_S4 Limit flag on S4
50- 57 E8.2 W/cm2 S4 ? [SIV]10.51µm emission line flux
59- 60 I2 % e_S4 ? Percent error in S4
62 A1 --- l_H2S2 Limit flag on H2S2
63- 70 E8.2 W/cm2 H2S2 ? H2S(2) 12.28µm emission line flux
72- 73 I2 % e_H2S2 ? Percent error in H2S2
75 A1 --- l_Hua Limit flag on Hu
76- 83 E8.2 W/cm2 Hua ? Huα (H7-6) 12.37µm emission line flux
85- 86 I2 % e_Hua ? Percent error in Hua
88 A1 --- l_Ne2 Limit flag on Ne2
89- 96 E8.2 W/cm2 Ne2 ? [Ne2]12.81µm emission line flux
98- 99 I2 % e_Ne2 ? Percent error in Ne2
101 A1 --- l_Ne5-14 Limit flag on Ne5
102-109 E8.2 W/cm2 Ne5-14 ? [NeV]14.32µm emission line flux
111-112 I2 % e_Ne5-14 ? Percent error in Ne5
114 A1 --- l_Ne3 Limit flag on Ne3
115-122 E8.2 W/cm2 Ne3 ? [NeIII]15.55µm emission line flux
124-125 I2 % e_Ne3 ? Percent error in in Ne3
127 A1 --- l_H2S1 Limit flag on H2S1
128-135 E8.2 W/cm2 H2S1 ? H2S(1) 17.03µm emission line flux
137-138 I2 % e_H2S1 ? Percent error in in H2S1
140 A1 --- l_Fe2-17 Limit flag on Fe2-17
141-148 E8.2 W/cm2 Fe2-17 ? [FeII]17.94µm emission line flux
150-151 I2 % e_Fe2-17 ? Percent error in Fe2-17
153 A1 --- l_S3-18 Limit flag on S3-18
154-161 E8.2 W/cm2 S3-18 ? [SIII]18.71µm emission line flux
163-164 I2 % e_S3-18 ? Percent error in S3-18
166 A1 --- l_Ne5-24 Limit flag on Ne5
167-174 E8.2 W/cm2 Ne5-24 ? [NeV]24.32µm emission line flux
176-177 I2 % e_Ne5-24 ? Percent error in Ne5
179 A1 --- l_O4 Limit flag on O4
180-187 E8.2 W/cm2 O4 ? [OIV]25.89µm emission line flux
189-190 I2 % e_O4 ? Percent error in O4
192 A1 --- l_Fe2-25 Limit flag on Fe2-25
193-200 E8.2 W/cm2 Fe2-25 ? [FeII]25.99µm emission line flux
202-203 I2 % e_Fe2-25 ? Percent error in Fe2-25
205 A1 --- l_H2S0 Limit flag on H2S0
206-213 E8.2 W/cm2 H2S0 ? H2S(0) 28.22µm emission line flux
215-216 I2 % e_H2S0 ? Percent error in H2S0
218 A1 --- l_S3 Limit flag on S3
219-226 E8.2 W/cm2 S3 ? [SIII]33.48µm emission line flux
228-229 I2 % e_S3 ? Percent error in S3
231 A1 --- l_Si2 Limit flag on Si2
232-239 E8.2 W/cm2 Si2 ? [SiII]34.81µm emission line flux
241 I1 % e_Si2 ? Percent error in Si2
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Type Source type (ULIRG or PG QSO)
9- 22 A14 --- Name Galaxy name (G1)
24- 28 F5.1 mJy R6 ? Rest-frame 6µm continuum flux density (5)
30- 35 F6.1 mJy R15 Rest-frame 15µm continuum flux density (5)
37- 42 F6.1 mJy R20 Rest-frame 20µm continuum flux density (5)
44- 49 F6.1 mJy R25 Rest-frame 25µm continuum flux density (5)
51- 57 F7.1 mJy R30 Rest-frame 30µm continuum flux density (5)
59- 64 F6.1 mJy O12 ? Observed 12µm continuum flux density (6)
66- 71 F6.1 mJy O25 Observed 25µm continuum flux density (6)
73- 78 F6.3 [-] M/FIR ? Log ratio of MIR to FIR luminosities (7)
--------------------------------------------------------------------------------
Note (5): Computed from the IRS spectra using a 3.3% bandpass.
Note (6): Observed-frame rest-frame flux densities computed using step
function approximations to the IRAS 12 and 25µm system response
functions. The flux given is the average fν under the step function.
Note (7): Extincted 5-25µm luminosity minus PAH+silicate emission
(i.e., blackbody only) as a (logarithmic) fraction of the far-infrared
(40-122µm) luminosity. For the PG QSOs, this latter quantity is
available only for the three average spectra divided by L(FIR).
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- Name Galaxy name (G1)
16- 20 F5.2 --- tau Effective peak silicate optical depth (1)
22 A1 --- l_logW1 Limit flag on logW1
24- 28 F5.2 [um] logW1 Log rest-frame H2O+HC (5-7µm)
equivalent width
30- 34 F5.2 [um] logW2 ? Log rest-frame C2H2 (13.7µm)
equivalent width
36- 40 F5.2 [um] logW3 ? Log rest-frame HCN (14µm) equivalent width
--------------------------------------------------------------------------------
Note (1): Computed using the ratio of the total extincted flux to
the total unextincted flux.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- Name Galaxy name (G1)
16 A1 --- l_logW4 Limit flag on logW4
17- 22 F6.2 [um] logW4 Log rest-frame 6µm PAH feature
equivalent width
24 A1 --- l_logW5 Limit flag on logW5
25- 30 F6.2 [um] logW5 Log rest-frame 7µm PAH feature
equivalent width
32 A1 --- l_logR1 Limit flag on logR1
33- 38 F6.2 [-] logR1 Log ratio total PAH to total IR luminosities
40 A1 --- l_logR2 Limit flag on logR2
41- 46 F6.2 [-] logR2 Log ratio total PAH to total FIR luminosities
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table8.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Type Source type (ULIRG or PG QSO)
9- 22 A14 --- Name Galaxy name (G1)
24 A1 --- l_T(4-3) Limit flag on T(4-3)
25- 31 F7.2 K T(4-3) ? Molecular hydrogen excitation temperature
from S(1)/S(2) flux
33- 34 I2 % e_T(4-3) ? Percent error in T(4-3)
36 A1 --- l_T(5-4) Limit flag on T(5-4)
37- 43 F7.2 K T(5-4) ? Molecular hydrogen excitation temperature
from S(2)/S(3) flux
45- 46 I2 % e_T(5-4) ? Percent error in T(5-4)
48- 51 F4.2 [solMass] logMH2 ? Log molecular hydrogen mass (8)
53- 54 I2 % e_logMH2 ? Percent error in logMH2
--------------------------------------------------------------------------------
Note (8): Computed using the partition function from Herbst et al.
(1996AJ....111.2403H 1996AJ....111.2403H), the S(1) flux, and the average of the
(4-3) and (5-4) excitation temperatures.
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Byte-by-byte Description of file: table12.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Type Source type (ULIRG or PG QSO)
9- 22 A14 --- Name Galaxy name (G1)
24 A1 --- l_M1 Limit flag on M1
25- 30 F6.1 % M1 ? Method 1 percent bolometric AGN luminosity (9)
32 A1 --- l_M2 Limit flag on M2
33- 38 F6.1 % M2 ? Method 2 percent bolometric AGN luminosity (9)
40 A1 --- l_M3 Limit flag on M3
41- 46 F6.1 % M3 ? Method 3 percent bolometric AGN luminosity (9)
48 A1 --- l_M4 Limit flag on M4
49- 54 F6.1 % M4 ? Method 4 percent bolometric AGN luminosity (9)
56- 60 F5.1 % M5 Method 5 percent bolometric AGN luminosity (9)
62- 65 F4.1 % M6 ? Method 6 percent bolometric AGN luminosity (9)
67- 71 F5.1 % L(agn) Averaged AGN contribution to the bolometric
luminosity
--------------------------------------------------------------------------------
Note (9): Methods used (see Appendix for more information on the six
individual methods to derive AGN contributions) numbered as:
1 = [OIV]/[NeII];
2 = [NeV]/[NeII];
3 = Weq(PAH 7.7µm);
4 = Laurent et al., 2000A&A...359..887L 2000A&A...359..887L + Armus et al., 2007ApJ...656..148A 2007ApJ...656..148A;
5 = L(MIR)/L(FIR);
6 = f30/f15.
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Byte-by-byte Description of file: table16.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Type Source type (ULIRG or PG QSO)
9- 22 A14 --- Name Galaxy name (G1)
24 A1 --- l_pho1 Limit flag on pho1
25- 30 F6.2 [-] pho1 ? Method 1 log Eddington ratio from photometry (1)
32 A1 --- l_pho2 Limit flag on pho2
33- 38 F6.2 [-] pho2 ? Method 2 log Eddington ratio from photometry (1)
40 A1 --- l_pho3 Limit flag on pho3
41- 46 F6.2 [-] pho3 ? Method 3 log Eddington ratio from photometry (1)
48 A1 --- l_pho4 Limit flag on pho4
49- 54 F6.2 [-] pho4 ? Method 4 log Eddington ratio from photometry (1)
56- 60 F5.2 [-] pho5 ? Method 5 log Eddington ratio from photometry (1)
62- 66 F5.2 [-] pho6 ? Method 6 log Eddington ratio from photometry (1)
68- 72 F5.2 [-] phoA ? Average log Eddington ratio from photometry (1)
74 A1 --- l_dyn1 Limit flag on dyn1
75- 80 F6.2 [-] dyn1 ? Method 1 log Eddington ratio from dynamics (2)
82 A1 --- l_dyn2 Limit flag on dyn2
83- 88 F6.2 [-] dyn2 ? Method 2 log Eddington ratio from dynamics (2)
90 A1 --- l_dyn3 Limit flag on dyn3
91- 96 F6.2 [-] dyn3 ? Method 3 log Eddington ratio from dynamics (2)
98 A1 --- l_dyn4 Limit flag on dyn4
99-104 F6.2 [-] dyn4 ? Method 4 log Eddington ratio from dynamics (2)
106-110 F5.2 [-] dyn5 ? Method 5 log Eddington ratio from dynamics (2)
112-116 F5.2 [-] dyn6 ? Method 6 log Eddington ratio from dynamics (2)
118-122 F5.2 [-] dynA ? Average log Eddington ratio from dynamics (2)
--------------------------------------------------------------------------------
Note (1): "photometric" black hole masses based on measurements of the
H-band luminosity of the spheroidal component in these systems (free
of the central point source) from Veilleux et al. (2002, Cat.
J/ApJS/143/315, 2006ApJ...643..707V 2006ApJ...643..707V, and 2009, ApJ, in press) and
the H-band spheroid luminosity - black hole mass relation of Marconi
& Hunt (2003ApJ...589L..21M 2003ApJ...589L..21M).
Note (2): "dynamical" black hole masses based on the stellar velocity
dispersion of the spheroidal component in these objects from Dasyra et
al. (2006ApJ...638..745D 2006ApJ...638..745D, 2006ApJ...651..835D 2006ApJ...651..835D, 2007ApJ...657..102D 2007ApJ...657..102D)
and the stellar velocity dispersion - black hole mass relation of
Tremaine et al. (2002ApJ...574..740T 2002ApJ...574..740T).
--------------------------------------------------------------------------------
Global notes:
Note (G1): Coordinate-based names beginning with "F" are sources
in the IRAS Faint Source Catalog (Cat. II/156)
History:
From electronic version of the journal
References:
Schweitzer M. Paper I. 2006ApJ...649...79S 2006ApJ...649...79S
Netzer H. Paper II. 2007ApJ...666..806N 2007ApJ...666..806N
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 04-Jan-2010