Article

3D-HST+CANDELS: THE EVOLUTION OF THE GALAXY SIZE-MASS DISTRIBUTION SINCE<i>z</i>= 3

Arjen van der WelMax-Planck Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany; e-mail: [email protected]M. FranxLeiden Observatory, Leiden University, P.O. Box 9513, NL-2300 AA Leiden, The NetherlandsP. G. van DokkumDepartment of Astronomy, Yale University, New Haven, CT 06511, USAR. E. SkeltonSouth African Astronomical Observatory, P.O. Box 9, Observatory 7935, South AfricaI. G. MomchevaDepartment of Astronomy, Yale University, New Haven, CT 06511, USAK. E. WhitakerAstrophysics Science Division, Goddard Space Center, Greenbelt, MD 20771, USAG. B. BrammerSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USAEric F. BellDepartment of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109, USAHans-Walter RixMax-Planck Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany; e-mail: [email protected]S. WuytsMax-Planck Institut für Extraterrestrische Physik, Giessenbachstrasse, D-85748 Garching, GermanyH. C. FergusonUniversité Bourgogne Franche-ComtéB. HoldenUniversity of California Observatories/Lick Observatory, University of California, Santa Cruz, CA 95064, USAG. BarroUniversity of California Observatories/Lick Observatory, University of California, Santa Cruz, CA 95064, USAA. M. KoekemoerSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USAYu-Yen ChangMax-Planck Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany; e-mail: [email protected]E. J. McGrathDepartment of Physics and Astronomy, Colby College, Waterville, ME 0490, USAB. HäusslerCentre for Astrophysics, Science & Technology Research Institute, University of Hertfordshire, Hatfield, Herts AL10 9AB, UKA. DekelRacah Institute of Physics, The Hebrew University, Jerusalem 91904, IsraelP. BehrooziSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USAM. FumagalliLeiden Observatory, Leiden University, P.O. Box 9513, NL-2300 AA Leiden, The NetherlandsJ. LejaDepartment of Astronomy, Yale University, New Haven, CT 06511, USAB. F. LundgrenDepartment of Astronomy, University of Wisconsin, Madison, WI 53706, USAM. V. MasedaMax-Planck Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany; e-mail: [email protected]E. J. NelsonDepartment of Astronomy, Yale University, New Haven, CT 06511, USAD. A. WakeDepartment of Astronomy, University of Wisconsin, Madison, WI 53706, USAS. G. PatelObservatories of the Carnegie Institution of Washington, Pasadena, CA 91101, USAI. LabbéLeiden Observatory, Leiden University, P.O. Box 9513, NL-2300 AA Leiden, The NetherlandsS. M. FaberUniversity of California Observatories/Lick Observatory, University of California, Santa Cruz, CA 95064, USANorman A. GroginSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USAD. D. KocevskiDepartment of Physics and Astronomy, University of Kentucky, Lexington, KY 40506, USA

2014en

ABI

Abstract

Spectroscopic+photometric redshifts, stellar mass estimates, and rest-frame colors from the 3D-HST survey are combined with structural parameter measurements from CANDELS imaging to determine the galaxy size-mass distribution over the redshift range 0 < z < 3. Separating early- and late-type galaxies on the basis of star-formation activity, we confirm that early-type galaxies are on average smaller than late-type galaxies at all redshifts, and we find a significantly different rate of average size evolution at fixed galaxy mass, with fast evolution for the early-type population, R eff(1 + z) -1.48, and moderate evolution for the late-type population, R eff(1 + z)-0.75. The large sample size and dynamic range in both galaxy mass and redshift, in combination with the high fidelity of our measurements due to the extensive use of spectroscopic data, not only fortify previous results but also enable us to probe beyond simple average galaxy size measurements. At all redshifts the slope of the size-mass relation is shallow, , for late-type galaxies with stellar mass >3 × 109 M , and steep, , for early-type galaxies with stellar mass >2 × 1010 M . The intrinsic scatter is ≲0.2 dex for all galaxy types and redshifts. For late-type galaxies, the logarithmic size distribution is not symmetric but is skewed toward small sizes: at all redshifts and masses, a tail of small late-type galaxies exists that overlaps in size with the early-type galaxy population. The number density of massive (∼1011 M ), compact (R eff < 2 kpc) early-type galaxies increases from z = 3 to z = 1.5-2 and then strongly decreases at later cosmic times.

Identifiers

DOI: 10.1088/0004-637x/788/1/28

Citations and references

Cited by 10 references

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