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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



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ID: 421497.0, MPI für Astronomie / Publikationen_mpia
IMAGES. III. The evolution of the near-infrared Tully-Fisher relation over the last 6 Gyr
Authors:Puech, M.; Flores, H.; Hammer, F.; Yang, Y.; Neichel, B.; Lehnert, M.; Chemin, L.; Nesvadba, N.; Epinat, B.; Amram, P.; Balkowski, C.; Cesarsky, C.; Dannerbauer, H.; di Serego Alighieri, S.; Fuentes-Carrera, I.; Guiderdoni, B.; Kembhavi, A.; Liang, Y. C.; Östlin, G.; Pozzetti, L.; Ravikumar, C. D.; Rawat, A.; Vergani, D.; Vernet, J.; Wozniak, H.
Language:English
Date of Publication (YYYY-MM-DD):2008
Title of Journal:Astronomy and Astrophysics
Volume:484
Start Page:173
End Page:187
Review Status:Peer-review
Audience:Experts Only
Abstract / Description:Using the multi-integral field spectrograph GIRAFFE at VLT, we have derived the K-band Tully-Fisher relation (TFR) at z Ëœ 0.6 for a representative sample of 65 galaxies with emission lines (W_0(OII)>=15 Å). We confirm that the scatter in the z Ëœ 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 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 z Ëœ 0.6 and z=0, which, if interpreted as an evolution of the K-band luminosity of rotating disks, would imply that a brightening of 0.66 ± 0.14 mag occurs between z Ëœ 0.6 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 zËœ0.6 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 zËœ0.6 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. Intermediate MAss Galaxy Evolution Sequence, ESO programs 174.B-0328(A), 174.B-0328(E).
Free Keywords:galaxies: evolution; galaxies: kinematics and dynamics; galaxies: high-redshift; galaxies: general; galaxies:; interactions; galaxies: spiral
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://adsabs.harvard.edu/abs/2008A%26A...484..173... [ID No:1]
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