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TwitterA&A 484, 173-187 (2008)
DOI: 10.1051/0004-6361:20079313
IMAGES
III. The evolution of the near-infrared Tully-Fisher relation over the last 6 Gyr
M. Puech1, 2, H. Flores2, F. Hammer2, Y. Yang2, B. Neichel2, M. Lehnert2, L. Chemin2, N. Nesvadba2, B. Epinat3, P. Amram3, C. Balkowski2, C. Cesarsky1, H. Dannerbauer4, S. di Serego Alighieri5, I. Fuentes-Carrera2, B. Guiderdoni6, A. Kembhavi7, Y. C. Liang8, G. Östlin9, L. Pozzetti10, C. D. Ravikumar11, A. Rawat2, 7, D. Vergani12, J. Vernet1, and H. Wozniak61 ESO, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany
e-mail: mpuech@eso.org
2 GEPI, Observatoire de Paris, CNRS, University Paris Diderot, 5 Place Jules Janssen, 92190 Meudon, France
3 Laboratoire d'Astrophysique de Marseille, Observatoire Astronomique de Marseille-Provence, 2 Place Le Verrier, 13248 Marseille, France
4 MPIA, Königstuhl 17, 69117 Heidelberg, Germany
5 INAF - Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125 Florence, Italy
6 Centre de Recherche Astronomique de Lyon, 9 Avenue Charles André, 69561 Saint-Genis-Laval Cedex, France
7 Inter-University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, Pune 411007, India
8 National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, PR China
9 Stockholm Observatory, AlbaNova University Center, Stockholms Center for Physics, Astronomy and Biotechnology, Roslagstullsbacken 21, 10691 Stockholm, Sweden
10 INAF - Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy
11 Department of Physics, University of Calicut, Kerala 673635, India
12 IASF - INAF, via Bassini 15, 20133 Milano, Italy
Received 21 December 2007 / Accepted 17 March 2008
Abstract
Using the multi-integral field spectrograph GIRAFFE at VLT,
we have derived the K-band Tully-Fisher relation (TFR) at
for a representative sample of 65 galaxies with emission lines
(
). We confirm that the scatter
in the
TFR is caused by galaxies with anomalous
kinematics, and find a positive and strong correlation between the
complexity of the kinematics and the scatter that they contribute to
the TFR. Considering only relaxed-rotating disks, the scatter, and
possibly also the slope, of the TFR, do not appear to evolve with
redshift. We detect an evolution of the K-band TFR zero point
between
and z=0, which, if interpreted as an
evolution of the K-band luminosity of rotating disks, would imply
that a brightening of
mag occurs between
and z=0. Any disagreement with the results of Flores et al. (2006, A&A, 455, 107)
are attributed to both an improvement of the local TFR and the more
detailed accurate measurement of the rotation velocities in the
distant sample. Most of the uncertainty can be explained by the
relatively coarse spatial-resolution of the kinematical data.
Because most rotating disks at are unlikely to experience
further merging events, one may assume that their rotational
velocity, which is taken as a proxy of the total mass, does not
evolve dramatically. If true, our result implies that rotating disks
observed at are rapidly transforming their gas into
stars, to be able to double their stellar masses and be observed on
the TFR at z=0. The rotating disks observed are indeed
emission-line galaxies that are either starbursts or LIRGs, which
implies that they are forming stars at a high rate. Thus, a
significant fraction of the rotating disks are forming the bulk of
their stars within 6 to 8 Gyr, in good agreement with former studies
of the evolution of the mass-metallicity relationship.
Key words: galaxies: evolution -- galaxies: kinematics and dynamics -- galaxies: high-redshift -- galaxies: general -- galaxies: interactions -- galaxies: spiral
© ESO 2008