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IMAGES-III: The evolution of the Near-Infrared Tully-Fisher relation over the last 6 Gyr | | M. Puech
; H. Flores
; F. Hammer
; Y. Yang
; B. Neichel
; M. Lehnert
; L. Chemin
; N. Nesvadba
; B. Epinat
; P. Amram
; C. Balkowski
; C. Cesarsky
; H. Dannerbauer
; S. di Serego Alighieri
; I. Fuentes-Carrera
; B. Guiderdoni
; A. Kembhavi
; Y.C. Liang
; G. Oestlin
; L. Pozzetti
; C.D. Ravikumar
; A. Rawat
; D. Vergani
; J. Vernet
; H. Wozniak
; | | Date: |
20 Mar 2008 | | Abstract: | Using the multi-integral field spectrograph GIRAFFE at VLT, we have derived
the K-band Tully-Fisher relation (TFR) at z~0.6 in a representative sample of
65 galaxies with emission lines (W_(OII) > 15 A). We confirm that the scatter
of the z~0.6 TFR is caused by galaxies with anomalous kinematics, and find a
positive and strong correlation between the complexity of the kinematics and
the scatter contributed to the TFR. Once restricted to relaxed rotating disks,
the TFR seems to not have evolved in scatter, and possibly in slope, while we
detect an evolution of the K-band TFR zero point between z~0.6 and z=0. If
interpreted as an evolution of K-band luminosity in rotating disks, they are
brightening by 0.66+/-0.14 mag from z~0.6 to z=0. Differences with Flores et
al. (2006) are attributed to both the improvement of the local TFR and the more
detailed determination of the rotation velocities in the distant sample. Most
of the uncertainties can be attributed to the influence of the relatively
coarse spatial resolution on the kinematical measurements. Because most
rotating disks at z~0.6 are unlikely to experience further merging events, one
may assume that their rotational velocity (taken as a proxy of the total mass)
would not evolve dramatically. If true, our result means that rotating disks
observed at z~0.6 are transforming rapidly their gas into stars, in order to
roughly double their stellar masses to reach the TFR at z=0. Indeed the
selected rotating disks have emission lines and are either star-bursts or
LIRGs, meaning they are forming stars at high rates. Thus, a significant part
of rotating disks are actively forming the bulk of their stars within 6 to 8
Gyr, in good agreement with former studies on the evolution of the
mass-metallicity relationship. | | Source: | arXiv, 0803.3002 | | Services: | Forum | Review | PDF | Favorites | |
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