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. =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" (f_25_/f_60_<=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). File Summary: -------------------------------------------------------------------------------- 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 H_2_ 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 -------------------------------------------------------------------------------- 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(5100{AA})+L(IR). Note (2): From Veilleux et al. (1995ApJS...98..171V, 1999ApJ...522..139V) and Rupke et al. (2005ApJS..160...87R). Note (3): From Veilleux et al. (2009, ApJ in press), Veilleux et al. (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); 3 = Scoville et al. (2000AJ....119..991S); 4 = Bahcall et al. (1997ApJ...479..642B); 5 = Sakamoto et al. (1999ApJ...514...68S); 6 = Beswick et al. (2001MNRAS.325..151B); 7 = Veilleux et al. (2009, ApJ, in press). -------------------------------------------------------------------------------- Byte-by-byte Description of file: table2.dat -------------------------------------------------------------------------------- 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 -------------------------------------------------------------------------------- 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]7.65{mu}m 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 ? H_2_S(3) 9.66{mu}m 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]10.51{mu}m 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 ? H_2_S(2) 12.28{mu}m 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 ? Hu{alpha} (H7-6) 12.37{mu}m 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]12.81{mu}m 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]14.32{mu}m 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]15.55{mu}m 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 ? H_2_S(1) 17.03{mu}m 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]17.94{mu}m 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]18.71{mu}m 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]24.32{mu}m 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]25.89{mu}m 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]25.99{mu}m 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 ? H_2_S(0) 28.22{mu}m 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]33.48{mu}m 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]34.81{mu}m 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 6{mu}m continuum flux density (5) 30- 35 F6.1 mJy R15 Rest-frame 15{mu}m continuum flux density (5) 37- 42 F6.1 mJy R20 Rest-frame 20{mu}m continuum flux density (5) 44- 49 F6.1 mJy R25 Rest-frame 25{mu}m continuum flux density (5) 51- 57 F7.1 mJy R30 Rest-frame 30{mu}m continuum flux density (5) 59- 64 F6.1 mJy O12 ? Observed 12{mu}m continuum flux density (6) 66- 71 F6.1 mJy O25 Observed 25{mu}m 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 25{mu}m system response functions. The flux given is the average f_{nu}_ under the step function. Note (7): Extincted 5-25{mu}m luminosity minus PAH+silicate emission (i.e., blackbody only) as a (logarithmic) fraction of the far-infrared (40-122{mu}m) luminosity. For the PG QSOs, this latter quantity is available only for the three average spectra divided by L(FIR). -------------------------------------------------------------------------------- Byte-by-byte Description of file: table6.dat -------------------------------------------------------------------------------- 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 H_2_O+HC (5-7{mu}m) equivalent width 30- 34 F5.2 [um] logW2 ? Log rest-frame C_2_H_2_ (13.7{mu}m) equivalent width 36- 40 F5.2 [um] logW3 ? Log rest-frame HCN (14{mu}m) 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 -------------------------------------------------------------------------------- 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 6{mu}m PAH feature equivalent width 24 A1 --- l_logW5 Limit flag on logW5 25- 30 F6.2 [um] logW5 Log rest-frame 7{mu}m 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), the S(1) flux, and the average of the (4-3) and (5-4) excitation temperatures. -------------------------------------------------------------------------------- Byte-by-byte Description of file: table12.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_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 = W_eq_(PAH 7.7{mu}m); 4 = Laurent et al., 2000A&A...359..887L + Armus et al., 2007ApJ...656..148A; 5 = L(MIR)/L(FIR); 6 = f30/f15. -------------------------------------------------------------------------------- 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, and 2009, ApJ, in press) and the H-band spheroid luminosity - black hole mass relation of Marconi & Hunt (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...651..835D, 2007ApJ...657..102D) and the stellar velocity dispersion - black hole mass relation of Tremaine et al. (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 Netzer H. Paper II. 2007ApJ...666..806N ================================================================================ (End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 04-Jan-2010