J/A+A/420/97 Tully-Fisher relation at 0.1<z<1.0 (Boehm+, 2004)
The Tully-Fisher relation at intermediate redshift.
Boehm A., Ziegler B.L., Saglia R.P., Bender R., Fricke K.J., Gabasch A.,
Heidt J., Mehlert D., Noll S., Seitz S.
<Astron. Astrophys. 420, 97 (2004)>
=2004A&A...420...97B 2004A&A...420...97B
ADC_Keywords: Galaxies, photometry ; Rotational velocities ; Redshifts
Keywords: galaxies: spiral - galaxies: evolution -
galaxies: kinematics and dynamics
Abstract:
Using the Very Large Telescope in Multi Object Spectroscopy mode, we
have observed a sample of 113 field spiral galaxies in the FORS Deep
Field (FDF) with redshifts in the range 0.1<z<1.0. The galaxies were
selected based on apparent brightness (R<23) and encompass all late
spectrophotometric types from Sa to Sdm/Im. Spatially resolved
rotation curves have been extracted for 77 galaxies and fitted with
synthetic velocity fields taking into account all observational
effects from inclination and slit misalignment to seeing and slit
width. We also compared different shapes for the intrinsic rotation
curve. To obtain robust values of Vmax, our analysis is focused on
galaxies with rotation curves that extend well into the region of
constant rotation velocity at large radii. If the slope of the local
Tully-Fisher relation (TFR) is held fixed, we find evidence for a
mass-dependent luminosity evolution which is as large as up to 2mag
for the lowest-mass galaxies, but is small or even negligible for the
highest-mass systems in our sample. In effect, the TFR slope is
shallower at z∼0.5 in comparison to the local sample. We argue for a
mass-dependent evolution of the mass-to-light ratio. An additional
population of blue, low-mass spirals does not seem a very appealing
explanation. The flatter tilt we find for the distant TFR is in
contradiction to the predictions of recent semi-analytic simulations.
Description:
Structural parameters, redshifts, spectral types, luminosities and
maximum rotation velocities are presented for a sample of 77 spiral
galaxies in the FORS Deep Field. The galaxies cover the redshift range
0.1<z<1.0 and comprise all spectrophotometric types from Sa to Sdm/Im.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 80 77 Photometric and kinematic data on 77 spirals
in the FORS Deep Field
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See also:
J/A+A/398/49 : UBgRIJKs photometry in the FORS Deep Field (Heidt+, 2003)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- FDF FORS Deep Field photometric catalogue number
(as in Cat. J/A+A/398/49)
6- 7 I2 deg i Disk inclination angle (0 = face-on)
9- 10 I2 deg delta Misalignment angle between disk major axis
and slitlet
12- 15 F4.2 arcsec rd Exponential disk scale length (1)
17- 22 F6.4 --- z Spectroscopic redshift
24- 25 I2 --- TType SED classifier in the de Vaucouleurs scheme
27- 31 F5.2 mag Xmag Total apparent magnitude in filter X (2)
33- 37 F5.2 mag kB K-correction (to rest-frame Johnson B)
39- 42 F4.2 mag AX Galactic absorption (in filter X)
44- 47 F4.2 mag AB Intrinsic absorption in rest-frame B (3)
49- 53 F5.2 mag m-M Distance modulus (4)
55- 60 F6.2 mag BMAG B-band absolute magnitude
62- 65 F4.2 mag e_BMAG Error on B-band absolute magnitude
67- 69 I3 km/s Vmax Intrinsic maximum rotation velocity (5)
71- 73 I3 km/s e_Vmax Error on intrinsic maximum rotation velocity
75- 78 F4.2 mag B-R Rest-frame extinction-corrected B-R color index
80 A1 --- Qual Rotation curve quality (6)
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Note (1): Structural parameters were derived from 2-D surface brightness
profile fitting on ground-based images taking into account the seeing.
According to our simulations, the disk scale length is not a crucial
input parameter for the determination of Vmax in the case of distant
spirals. However, some values of rd may be affected by the limitations
of the ground-based imaging. We therefore recommend not to use these
scale lengths for applications like the Fundamental Plane of spiral
galaxies.
Note (2): Apparent magnitude is given for the filter X which best matches
the rest-frame B-band. For objects with z<0.25, this is the B-band, in
the range 0.25<z<0.55 the g-band was used, for 0.55<z<0.85, the R-band
was used, and at z>0.85 the I-band.
Note (3): Intrinsic absorption is computed following Tully & Fouque
(1985ApJS...58...67T 1985ApJS...58...67T).
Note (4): Adopting the concordance cosmology with Ωλ=0.7,
Ωm=0.3 and H0=70km/s/Mpc.
Note (5): Derived via synthetic velocity fields assuming a linear rise
of the rotation velocity at small galactocentric radii and a flat
rotation curve at large radii ("rise-turnover-flat" shape).
Note (6): Quality flags:
"H" - High quality, symmetric rotation curves with a clearly visible
flat part at large radii. These objects are usable for
Tully-Fisher applications.
"L" - Low quality rotation curves with relatively small spatial
extent and/or asymmetric shapes.
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Acknowledgements: Asmus Boehm
(End) Asmus Boehm [University Observatory Goettingen, Germany] 25-Mar-2004