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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 606660.0, MPI für Astronomie / Publikationen_mpia
Galaxy structure and mode of star formation in the SFR-mass plane from z ~ 2.5 to z ~ 0.1
Authors:Wuyts, S.; Förster Schreiber, N. M.; van der Wel, A.; Magnelli, B.; Guo, Y.; Genzel, R.; Lutz, D.; Aussel, H.; Barro, G.; Berta, S.; Cava, A.; Graciá-Carpio, J.; Hathi, N. P.; Huang, K.-H.; Kocevski, D. D.; Koekemoer, A. M.; Lee, K.-S.; Le Floc'h, E.; McGrath, E. J.; Nordon, R.; Popesso, P.; Pozzi, F.; Riguccini, L.; Rodighiero, G.; Saintonge, A.; Tacconi, L.
Date of Publication (YYYY-MM-DD):2011
Journal Abbrev.:The Astrophysical Journal
Issue / Number:2
Audience:Not Specified
Abstract / Description:We analyze the dependence of galaxy structure (size and Sérsic index) and mode of star formation (ΣSFR and SFRIR/SFRUV) on the position of galaxies in the star formation rate (SFR) versus mass diagram. Our sample comprises roughly 640,000 galaxies at z ~ 0.1, 130,000 galaxies at z ~ 1, and 36,000 galaxies at z ~ 2. Structural measurements for all but the z ~ 0.1 galaxies are based on Hubble Space Telescope imaging, and SFRs are derived using a Herschel-calibrated ladder of SFR indicators. We find that a correlation between the structure and stellar population of galaxies (i.e., a "Hubble sequence") is already in place since at least z ~ 2.5. At all epochs, typical star-forming galaxies on the main sequence are well approximated by exponential disks, while the profiles of quiescent galaxies are better described by de Vaucouleurs profiles. In the upper envelope of the main sequence, the relation between the SFR and Sérsic index reverses, suggesting a rapid buildup of the central mass concentration in these starbursting outliers. We observe quiescent, moderately and highly star-forming systems to co-exist over an order of magnitude or more in stellar mass. At each mass and redshift, galaxies on the main sequence have the largest size. The rate of size growth correlates with specific SFR, and so does ΣSFR at each redshift. A simple model using an empirically determined star formation law and metallicity scaling, in combination with an assumed geometry for dust and stars, is able to relate the observed ΣSFR and SFRIR/SFRUV, provided a more patchy dust geometry is assumed for high-redshift galaxies.
Free Keywords:galaxies: high-redshift; galaxies: stellar content; galaxies: structure
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
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