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J/ApJ/669/821  CO Tully-Fisher relation for host galaxies of QSOs (Ho+, 2007)

The CO Tully-Fisher relation and implications for the host galaxies of high-redshift quasars. Ho L.C. <Astrophys. J., 669, 821-829 (2007)> =2007ApJ...669..821H
ADC_Keywords: QSOs ; Active gal. nuclei ; Spectroscopy Keywords: galaxies: bulges - galaxies: ISM - galaxies: kinematics and dynamics - galaxies: nuclei - galaxies: Seyfert - quasars: general Abstract: The integrated line width derived from CO spectroscopy provides a powerful tool to study the internal kinematics of extragalactic objects, including quasars at high redshift, provided that the observed line width can be properly translated to more conventionally used kinematical parameters of galaxies. We show, through the construction of a Ks-band CO Tully-Fisher relation for nearby galaxies spanning a wide range in infrared luminosity, that the CO line width measured at 20% of the peak intensity, when corrected for inclination and other effects, successfully recovers the maximum rotation velocity of the disk. The line width at 50% of the peak intensity performs much more poorly, in large part because CO lines have a wide range of profiles, which are shown to vary systematically with infrared luminosity. We present a practical prescription for converting observed CO line widths into the stellar velocity dispersion of the bulge (σ*) and then apply it to a sample of low-redshift (z≲0.2) and high-redshift (1.4≲z≲6.4) quasars to study their host galaxies. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 57 151 The galaxy sample table2.dat 55 25 The quasar sample
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 15 A15 --- Galaxy Galaxy name 17- 21 F5.1 Mpc Dist Luminosity distance (1) 23- 24 I2 deg Inc ? Inclination angle 25 A1 --- u_Inc Uncertainty flag on Inc (2) 27- 30 I4 km/s W20 CO line width at 20% of peak intensity (3) 32- 34 I3 km/s W50 CO line width at 50% of peak intensity (3) 36- 41 F6.2 mag KsMAG ? Absolute 2MASS Ks band magnitude (4) 43- 47 F5.2 [solLum] logLIR Log of total IR (8-1000 micron) luminosity 49 I1 --- Ref Reference for CO data (5) 51- 57 A7 --- Notes Additional notes (6)
Note (1): Derived from the mean heliocentric velocity listed in Hyperleda ( assuming a Local Group infall velocity of 208km/s toward the Virgo cluster and a Hubble constant of H0=70km/s/Mpc. Note (2): Indicates an especially uncertain inclination because the galaxy morphology is severely disturbed. The inclination angles for the objects from Lavezzi & Dickey (1998AJ....116.2672L) are not listed, but they were applied by these authors to the line widths. Note (3): Corrected for inclination angle and interstellar turbulence following the prescription of Lavezzi & Dickey (1997AJ....114.2437L). Note that these values have not yet been corrected for the velocity-dependent effect discussed by Tutui & Sofue (1999A&A...351..467T; see Eq. 1). Note (4): Not corrected for Galactic or internal extinction. Note (5): Reference for CO data as follows: 1 = Sanders et al. (1991ApJ...370..158S) 2 = Schoniger & Sofue (1994A&A...283...21S) 3 = Lavezzi & Dickey (1998AJ....116.2672L) Note (6): Notes as follows: a = Extreme low-velocity outlier in the Tully-Fisher relation b = IRAS 25micron upper limit c = IRAS 12micron upper limit d = K-band data from Kim et al. (2002, Cat. J/ApJS/143/277) e = inclination angle from McLeod & Rieke (1995ApJ...441...96M) f = inclination angle from Scharwachter et al. (2003A&A...405..959S) g = K-band data from Bushouse & Stanford (1992ApJS...79..213B) h = K-band data from McLeod & Rieke (1995ApJ...441...96M) i = K-band data from Bushouse & Werner (1990ApJ...359...72B)
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 15 A15 --- QSO Quasar name 17- 22 F6.4 --- z Redshift (1) 24- 28 F5.2 [solMass] logMass Black hole mass (2) 30- 32 I3 km/s W20 ?=- CO line width at 20% of peak intensity 34- 36 I3 km/s W50 ?=- CO line width at 50% of peak intensity 38- 40 I3 km/s W20c Corrected CO line width at 20% of peak intensity (3) 42- 44 I3 km/s sig* Sellar velocity dispersion of the bulge derived from W20c and the vm-sigma* relation 46- 50 F5.2 [solLum] logLIR Total Infrared (8-100um)luminosity 52- 53 I2 --- Ref References for CO data (4) 55 A1 --- Notes Notes (5)
Note (1): We adopted the luminosity distances used by Shields et al. (2006ApJ...641..683S), which are based on H0=70km/s/Mpc-1, Ωm=0.3, and ΩΛ=0.7 Note (2): from Shields et al. (2006ApJ...641..683S), except for the following four cases (PG 0052+251, PG 1351+640, PG 1444+407, and PG 0157+001), whose BH masses were derived using eq. (2) from Shields et al., Hβ FWHM from Boroson & Green (1992ApJS...80..109B), and 5100Å continuum luminosities from the spectrophotometry of Neugebauer et al. (1987ApJS...63..615N). Note (3): Corrected for turbulence, an average inclination angle of 45°, the Tutui-Sofue effect, and, in the case of W50, the luminosity dependence on line shape (see Sect. 3) using the IR luminosities. Note (4): References for CO line widths as follows: 1 = Schoeniger & Sofue (1994A&A...283...21S) 2 = Scoville et al. (2003ApJ...585L.105S) 3 = Casoli & Loinard (2001, ASP Conf. Ser. 235, 305) 4 = Evans et al. (2006AJ....132.2398E) 5 = Planesas et al. (1999Sci...286.2493P) 6 = Weiss et al. (2003A&A...409L..41W) 7 = Solomon & Vanden Bout (2005ARA&A..43..677S) 8 = Weiss et al. (2007A&A...467..955W) 9 = Reichers et al. (2006ApJ...650..604R) 10 = Bertoldi et al. (2003A&A...409L..47B) Note (5): Notes as follows: a = I Zw 1 from Table 1; W20c corrected for i=38° b = W20 measured manually from an enlarged version of the published plot; uncertainty ∼100km/s. c = Solomon & Vanden Bout (2005ARA&A..43..677S) quote W50=280km/s from Krips et al. (2004, in The Dense Interstellar Medium in Galaxies, ed. S. Pfalzner et al. (Berlin: Springer), 23), but no line width information is actually given in the latter. Greve et al. (2005MNRAS.359.1165G) attribute W50=440km/s to Planesas et al. (1999Sci...286.2493P) and Krips et al. (2004, in The Dense Interstellar Medium in Galaxies, ed. S. Pfalzner et al. (Berlin: Springer), 23), but it is unclear how this value was deduced. The lensing model of Krips et al. suggests that the double-peaked profile of component "CO-A" arises from the disk of the host galaxy. We thus use the centroid velocities of the two peaks (-160 and +500km/s) as given in Planesas et al. (1999Sci...286.2493P) to infer a full velocity width of 660km/s, which we approximate as W20. d = The W50 value from Weiss et al. (2003A&A...409L..41W) has the smallest error bar; our adopted value differs slightly from the value of 400km/s used by Shields et al. (2006ApJ...641..683S). e = W50 from the average value of 475±17kms obtained using the IRAM Plateau de Bure interferometer, which is better determined than the value from the IRAM 30m. f = W50 differs from the value of 350km/s used by Shields et al. (2006ApJ...641..683S). g = Solomon & Vanden Bout (2005ARA&A..43..677S) quote W50=250km/s from Walter et al. (2003Natur.424..406W), who fit a Gaussian profile to the combined CO(6-5) and CO(7-6) spectra from Bertoldi et al. (2003A&A...409L..47B). The published version of Bertoldi et al.'s paper, however, actually gives W50=279km/s, which we adopt here.
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 27-Jan-2010
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