J/A+A/592/A64 Disk galaxies at 0.1<z<1.0 (Boehm+, 2016)
Disk galaxy scaling relations at intermediate redshifts.
I. The Tully-Fisher and velocity-size relations.
Boehm, A., Ziegler B.L.
<Astron. Astrophys. 592, A64 (2016)>
=2016A&A...592A..64B 2016A&A...592A..64B (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, photometry ; Rotational velocities ; Redshifts
Keywords: galaxies: spiral - galaxies: evolution -
galaxies: kinematics and dynamics - galaxies: structure
Abstract:
Galaxy scaling relations such as the Tully-Fisher relation (between
the maximum rotation velocity Vmax and luminosity) and the
velocity-size relation (between Vmax and the disk scale length) are
powerful tools to quantify the evolution of disk galaxies with cosmic
time. We took spatially resolved slit spectra of 261 field disk
galaxies at redshifts up to z∼1 using the FORS instruments of the ESO
Very Large Telescope. The targets were selected from the FORS Deep
Field and William Herschel Deep Field. Our spectroscopy was
complemented with HST/ACS imaging in the F814W filter. We analyzed the
ionized gas kinematics by extracting rotation curves from the
two-dimensional spectra. Taking into account all geometrical,
observational, and instrumental effects, these rotation curves were
used to derive the intrinsic V_max. Neglecting galaxies with disturbed
kinematics or insufficient spatial rotation curve extent, Vmax was
reliably determined for 124 galaxies covering redshifts 0.05<z<0.97.
This is one of the largest kinematic samples of distant disk galaxies
to date. We compared this data set to the local B-band Tully-Fisher
relation and the local velocity-size relation. The scatter in both
scaling relations is a factor of ∼2 larger at z∼0.5 than at z∼0. The
deviations of individual distant galaxies from the local Tully-Fisher
relation are systematic in the sense that the galaxies are
increasingly overluminous toward higher redshifts, corresponding to an
overluminosity ΔMB=-(1.2±0.5) mag at z=1. This luminosity
evolution at given Vmax is probably driven by younger stellar
populations of distant galaxies with respect to their local
counterparts, potentially combined with modest changes in dark matter
mass fractions. The analysis of the velocity-size relation reveals
that disk galaxies of a given Vmax have grown in size by a factor of
∼1.5 over the past ∼8Gyr, most likely through accretion of cold gas
and/or small satellites. From scrutinizing the combined evolution in
luminosity and size, we find that the galaxies that show the strongest
evolution toward smaller sizes at z∼1 are not those that feature the
strongest evolution in luminosity, and vice versa.
Description:
Redshifts, maximum rotation velocities, (Johnson) B-band absolute
magnitudes and sizes are presented for a sample of 124 disk galaxies
covering redshifts 0.1<z<1.0. The galaxies are selected from the FORS
Deep Field (FDF), see Heidt et al. (2003A&A...398..49H), and the
William Herschel Deep Field (WHDF), see Metcalfe et al.
(2001MNRAS.323..779M 2001MNRAS.323..779M). All given parameters assume a flat cosmology
with H0=70km/s/Mpc, Omegamatter=0.3 and Omegalambda=0.7.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 44 124 Parameters of disk galaxies at 0.1<z<1.0
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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 A1 --- Field [FW] Field name (1)
3- 6 I4 --- ID Galaxy identifier (2)
8- 13 F6.4 --- z Spectroscopic redshift
15- 17 I3 km/s Vmax Intrinsic maximum rotation velocity (3)
19- 21 I3 km/s e_Vmax Error on Vmax
23- 28 F6.2 mag BMAG Johnson B-band absolute magnitude (4)
30- 33 F4.2 mag e_BMAG Error on B-band absolute magnitude
35- 39 F5.2 kpc rd Exponential disk scale length (5)
41- 44 F4.2 kpc e_rd Error on exponential disk scale length
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Note (1): "F" refers to the FDF, "W" to the WHDF.
Note (2): For the FDF, the identifiers are the official IDs also used in the
photometric catalog in Heidt et al. (2003A&A...398..49H, FDF NNNN in Simbad).
The identifiers of the WHDF objects are internal only.
Note (3): Derived via synthetic rotation velocity fields taking into account
all geometrical effects such as disk inclination and all observational
effects such as seeing and influence of slit width. The error on Vmax stems
from the chi-square minimization fit of the synthetic, simulated rotation
curve to the observed rotation curve
Note (4): Computed assuming a mass-dependent intrinsic absorption following
Tully et al. (1998AJ....115.2264T 1998AJ....115.2264T).
Note (5): Derived from two-dimensional surface brightness profile fitting using
the GALFIT package on HST/ACS F814W images. Disk-bulge decomposition for
all but a few galaxies with negligible bulges; for these, only a single
Sersic profile was used for the fits. The error on the disk scale length
is the quadratic sum of the (very small) GALFIT random error and
systematic errors estimated using GALFIT on mock HST/ACS images
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Acknowledgements:
Asmus Boehm, asmus.boehm(at)uibk.ac.at
(End) A. Boehm [IAPP, Univ. Innsbruck, Austria], P. Vannier [CDS] 20-Jun-2016