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 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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 57 151 The galaxy sample
table2.dat 55 25 The quasar sample
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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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)
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Note (1): Derived from the mean heliocentric velocity listed in Hyperleda
(http://leda.univ-lyon1.fr) 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 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 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 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 1991ApJ...370..158S)
2 = Schoniger & Sofue (1994A&A...283...21S 1994A&A...283...21S)
3 = Lavezzi & Dickey (1998AJ....116.2672L 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 1995ApJ...441...96M)
f = inclination angle from Scharwachter et al. (2003A&A...405..959S 2003A&A...405..959S)
g = K-band data from Bushouse & Stanford (1992ApJS...79..213B 1992ApJS...79..213B)
h = K-band data from McLeod & Rieke (1995ApJ...441...96M 1995ApJ...441...96M)
i = K-band data from Bushouse & Werner (1990ApJ...359...72B 1990ApJ...359...72B)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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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)
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Note (1): We adopted the luminosity distances used by Shields et al.
(2006ApJ...641..683S 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 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 1992ApJS...80..109B), and
5100Å continuum luminosities from the spectrophotometry of
Neugebauer et al. (1987ApJS...63..615N 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 1994A&A...283...21S)
2 = Scoville et al. (2003ApJ...585L.105S 2003ApJ...585L.105S)
3 = Casoli & Loinard (2001, ASP Conf. Ser. 235, 305)
4 = Evans et al. (2006AJ....132.2398E 2006AJ....132.2398E)
5 = Planesas et al. (1999Sci...286.2493P 1999Sci...286.2493P)
6 = Weiss et al. (2003A&A...409L..41W 2003A&A...409L..41W)
7 = Solomon & Vanden Bout (2005ARA&A..43..677S 2005ARA&A..43..677S)
8 = Weiss et al. (2007A&A...467..955W 2007A&A...467..955W)
9 = Reichers et al. (2006ApJ...650..604R 2006ApJ...650..604R)
10 = Bertoldi et al. (2003A&A...409L..47B 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 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 2005MNRAS.359.1165G) attribute W50=440km/s to Planesas et
al. (1999Sci...286.2493P 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 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 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 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 2006ApJ...641..683S).
g = Solomon & Vanden Bout (2005ARA&A..43..677S 2005ARA&A..43..677S) quote W50=250km/s
from Walter et al. (2003Natur.424..406W 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 2003A&A...409L..47B). The published version of
Bertoldi et al.'s paper, however, actually gives W50=279km/s,
which we adopt here.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 27-Jan-2010