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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 720079.0, MPI für Astronomie / Publikationen_mpia
Deconstructing the galaxy stellar mass function with UKIDSS and CANDELS: the impact of colour, structure and environment
Authors:Mortlock, A.; Conselice, C. J.; Hartley, W. G.; Duncan, K.; Lani, C.; Ownsworth, J. R.; Almaini, O.; Wel, A. v. d.; Huang, K.-H.; Ashby, M. L. N.; Willner, S. P.; Fontana, A.; Dekel, A.; Koekemoer, A. M.; Ferguson, H. C.; Faber, S. M.; Grogin, N. A.; Kocevski, D. D.
Date of Publication (YYYY-MM-DD):2015
Title of Journal:Monthly Notices of the Royal Astronomical Society
Issue / Number:1
Start Page:2
End Page:24
Audience:Not Specified
Abstract / Description:We combine photometry from the Ultra Deep Survey (UDS), Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) UDS and CANDELS the Great Observatories Origins Deep Survey-South (GOODS-S) surveys to construct the galaxy stellar mass function probing both the low- and high-mass end accurately in the redshift range 0.3 < z < 3. The advantages of using a homogeneous concatenation of these data sets include meaningful measures of environment in the UDS, due to its large area (0.88 deg2), and the high-resolution deep imaging in CANDELS (H160 > 26.0), affording us robust measures of structural parameters. We construct stellar mass functions for the entire sample as parametrized by the Schechter function, and find that there is a decline in the values of φ and of α with higher redshifts, and a nearly constant M* up to z ˜ 3. We divide the galaxy stellar mass function by colour, structure, and environment and explore the links between environmental overdensity, morphology, and the quenching of star formation. We find that a double Schechter function describes galaxies with high Sérsic index (n > 2.5), similar to galaxies which are red or passive. The low-mass end of the n > 2.5 stellar mass function is dominated by blue galaxies, whereas the high-mass end is dominated by red galaxies. This shows that there is a possible link between morphological evolution and star formation quenching in high mass galaxies, which is not seen in lower mass systems. This in turn suggests that there are strong mass-dependent quenching mechanisms. In addition, we find that the number density of high-mass systems is elevated in dense environments, suggesting that an environmental process is building up massive galaxies quicker in over densities than in lower densities.
Free Keywords:galaxies: evolution; galaxies: formation; galaxies: luminosity function; mass function; galaxies: structure
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
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