Hostname: page-component-cd9895bd7-gvvz8 Total loading time: 0 Render date: 2024-12-25T15:54:57.339Z Has data issue: false hasContentIssue false
  • English
  • Français

The intriguing life of star-forming galaxies in the redshift range 1 ≤ z ≤ 2 using MASSIV

Published online by Cambridge University Press:  17 July 2013

P. Amram ,
C. López-Sanjuan ,
B. Epinat ,
T. Contini ,
D. Vergani ,
L. Tasca ,
O. Le Fèvre ,
B. Garilli ,
C. Divoy  and
J. Queyrel
...Show all authors
P. Amram
Affiliation:
LAM, AMU, CNRS, Marseille (F), email: [email protected]
C. López-Sanjuan
Affiliation:
LAM, AMU, CNRS, Marseille (F), email: [email protected] FEFCA, Teruel (E)
B. Epinat
Affiliation:
LAM, AMU, CNRS, Marseille (F), email: [email protected]
T. Contini
Affiliation:
IRAP, Toulouse (F)
D. Vergani
Affiliation:
INAF, Bologna (I)
L. Tasca
Affiliation:
LAM, AMU, CNRS, Marseille (F), email: [email protected]
O. Le Fèvre
Affiliation:
LAM, AMU, CNRS, Marseille (F), email: [email protected]
B. Garilli
Affiliation:
IASF-INAF, Milano (I)
C. Divoy
Affiliation:
IRAP, Toulouse (F)
J. Queyrel
Affiliation:
IRAP, Toulouse (F)
M. Kissler-Patig
Affiliation:
ESO, Garching b. München (G) GEMINI, Hilo (USA)
J. Moultaka
Affiliation:
IRAP, Toulouse (F)
L. Paioro
Affiliation:
IASF-INAF, Milano (I)
L. Tresse
Affiliation:
LAM, AMU, CNRS, Marseille (F), email: [email protected]
V. Perret
Affiliation:
LAM, AMU, CNRS, Marseille (F), email: [email protected]
F. Bournaud
Affiliation:
CEA, SAp, AIM, Saclay (F).
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

MASSIV (Mass Assembly Survey with SINFONI in VVDS) is an ESO large program which consists of 84 star-forming galaxies, spanning a wide range of stellar masses, observed with the IFU SINFONI on the VLT, in the redshift range 1 ≤ z ≤ 2. To be representative of the normal galaxy population, the sample has been selected from a well-defined, complete and representative parent sample. The kinematics of individual galaxies reveals that 58% of the galaxies are slow rotators, which means that a high fraction of these galaxies should probably be formed through major merger processes which might have produced gaseous thick or spheroidal structures supported by velocity dispersion rather than by rotation. Computations on the major merger rate from close pairs indicate that a typical star-forming galaxy underwent ~0.4 major mergers in the last ~9.5 Gyr, showing that merging is a major process driving mass assembly into the red sequence galaxies. These objects are also intriguing due to the fact that more than one galaxy over four is more metal-rich in its outskirts than in its center.

Keywords

galaxies: evolutiongalaxies: fundamental parametersgalaxies: high-redshiftgalaxies: kinematics and dynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S295: The intriguing life of massive galaxies , August 2012 , pp. 86 - 90
Copyright
Copyright © International Astronomical Union 2013 

References

Buitrago, F., Trujillo, I., Conselice, C. J., & Haeussler, B. 2013, MNRAS, 428, 1460Google Scholar
Contini, T., Garilli, B., Le Fèvre, O., et al. 2012, A&A, 539, 91Google Scholar
de Ravel, L., Le Fèvre, O., Tresse, L., et al. 2009, A&A, 498, 379Google Scholar
Emsellem, E., Cappellari, M., Krajnović, D., et al. 2011, MNRAS, 414, 888Google Scholar
Epinat, B., Tasca, L., Amram, P., et al. 2012, A&A, 539, 92Google Scholar
Le Fèvre, O., Vettolani, G., Garilli, B., et al. 2005, A&A, 439, 845Google Scholar
López-Sanjuan, C., Balcells, M., Pérez-González, P. G., et al. 2009, A&A, 501, 505Google Scholar
López-Sanjuan, C., Le Fèvre, O., de Ravel, L., et al. 2011, A&A, 530, 20Google Scholar
López-Sanjuan, C., Le Fèvre, O., Tasca, L. A. M., et al. 2012, A&A, 553, 78Google Scholar
Queyrel, J., Contini, T., Kissler-Patig, M., et al. 2012, A&A, 539, 93Google Scholar
Vergani, D., Epinat, B., Contini, T., et al. 2012, A&A, 546, 118Google Scholar
Xu, C. K., Zhao, Y., Scoville, N., et al. 2012, ApJ, 747, 85Google Scholar