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IPM
30
YEARS OLD

“School of Astronomy”

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Paper   IPM / Astronomy / 14689
School of Astronomy
  Title:   Connection Between Stellar Mass Distributions Within Galaxies and Quenching Since z =2
  Author(s): 
1.  moein. MOSLEH
2.  SANDRO. TACCHELLA
3.  ALVIO. RENZINI
4.  C. MARCELLA. A CAROLLO
5.  ALIREZA. MOLAEINEZHAD
6.  MASATO. ONODERA
7.  HABIB. G. KHOSROSHAHI
8.  SIMON. LILLY
  Status:   Published
  Journal: ApJ
  No.:  1
  Vol.:  837
  Year:  2017
  Supported by:  IPM
  Abstract:
We study the history from z �?� 2 to z �?� 0 of the stellar mass assembly of quiescent and star-forming galaxies in a spatially resolved fashion. For this purpose we use multi-wavelength imaging data from the Hubble Space Telescope (HST) over the GOODS fields and the Sloan Digital Sky Survey (SDSS) for the local population. We present the radial stellar mass surface density profiles of galaxies with M�?? > 1010M�??, corrected for mass-to-light ratio (M�??/L) variations, and derive the half-mass radius (Rm), central stellar mass surface density within 1 kpc (Σ1) and surface density at Rm (Σm) for star-forming and quiescent galaxies and study their evolution with redshift. At fixed stellar mass, the half-mass sizes of quiescent galaxies increase from z �?� 2 to z �?� 0 by a factor of �?� 3 �?? 5, whereas the half-mass sizes of star-forming galaxies increase only slightly, by a factor of �?� 2. The central densities Σ1 of quiescent galaxies decline slightly (by a factor of . 1.7) from z �?� 2 to z �?� 0, while for star-forming galaxies Σ1 increases with time, at fixed mass. We show that the central density Σ1 has a tighter correlation with specific star-formation rate (sSFR) than Σm and for all masses and redshifts galaxies with higher central density are more prone to be quenched. Reaching a high central density (Σ1 1010 M�?? kpc2 ) seems to be a prerequisite for the cessation of star formation, though a causal link between high Σ1 and quenching is difficult to prove and their correlation can have a different origin


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