Publication: Structural and Star-forming Relations since z similar to 3: Connecting Compact Star-forming and Quiescent Galaxies
Full text at PDC
Advisors (or tutors)
American Astronomical Society
We study the evolution of the scaling relations that compare the effective density (Sigma(e), r < r(e)) and core density (Sigma(1), r < 1kpc) to the stellar masses of star-forming galaxies (SFGs) and quiescent galaxies. These relations have been fully in place since z similar to 3 and have exhibited almost constant slope and scatter since that time. For SFGs, the zero points in Sigma(e) and Sigma(1) decline by only x 2. This fact plus the narrowness of the relations suggests that galaxies could evolve roughly along the scaling relations. Quiescent galaxies follow different scaling relations that are offset to higher densities at the same mass and redshift. Furthermore, the zero point of their core density has declined by only x 2 since z similar to 3, while the zero point of the effective density declines by x 10. When galaxies quench, they move from the star-forming relations to the quiescent relations. This involves an increase in the core and effective densities, which suggests that SFGs could experience a phase of significant core growth relative to the average evolution along the structural relations. The distribution of massive galaxies relative to the SFR-M. and the quiescent S-M. relations exhibits an L-shape that is independent of redshift. The knee of this relation consists of a subset of "compact" SFGs that are the most likely precursors of quiescent galaxies forming at later times. The compactness selection threshold in Sigma(1). exhibits a small variation from z = 3 to 0.5, Sigma(1) - 0.65(log M* - 10.5)> 9.6 -9.3M(circle dot) kpc(-2), allowing the most efficient identification of compact SFGs and quiescent galaxies at every redshift.
© 2017. The American Astronomical Society. All rights reserved. Support for program number HST-GO-12060 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. G.B. acknowledges support from NSF grant AST-08-08133. P.G.P.-G. acknowledges support from grant AYA2012-31277. This work has made use of the Rainbow Cosmological Surveys Database, which is operated by the Universidad Complutense de Madrid (UCM), partnered with the University of California Observatories at Santa Cruz (UCO/Lick, UCSC). This work was partly supported, by MINECO grant AYA2012-32295. F.L. acknowledges support from NSFC grant 11573017.