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3D-HST+CANDELS: THE EVOLUTION OF THE GALAXY SIZE–MASS DISTRIBUTION SINCE z = 3

TLDR
In this paper, the galaxy size-mass distribution over the redshift range 0 3 × 10{sup 9} M {sub ☉}, and steep, R{sub eff}∝M{sub ∗}{sup 0.75}, for early-type galaxies with stellar mass > 2 × 10,sup 10} M{sub ǫ, and the intrinsic scattermore is ≲0.2 dex for all galaxy types and redshifts.
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 3 × 10{sup 9} M {sub ☉}, and steep, R{sub eff}∝M{sub ∗}{sup 0.75}, for early-type galaxies with stellar mass >2 × 10{sup 10} M {sub ☉}. The intrinsic scattermore » 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 (∼10{sup 11} M {sub ☉}), compact (R {sub eff} < 2 kpc) early-type galaxies increases from z = 3 to z = 1.5-2 and then strongly decreases at later cosmic times.« less

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Low Gas Fractions Connect Compact Star-Forming Galaxies to their z~2 Quiescent Descendants

TL;DR: In this article, the authors proposed a method to use the NIRCam NIR system to detect the presence of a single photon in the image of the Space Telescope Science Institute (SSI).
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Molecular gas in two companion cluster galaxies at $z=1.2$

TL;DR: In this paper, the authors investigated the effect of cluster environment on the processing of the molecular gas in distant cluster galaxies and found that the two sources contribute equally to the observed CO(2-1) line emission from the two selected galaxies.
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Two channels of supermassive black hole growth as seen on the galaxies mass–size plane

TL;DR: In this article, the authors investigated the variation of black hole masses as a function of their host galaxy stellar mass (Mstar) and half-light radius (Re) and confirmed that the scatter in Mbh within this plane is essentially the same as that in the Mbh - sigma relation, as expected from the negligible scatter reported in the virial mass estimator sigma_v^2=GxMstar/(5xRe).
References
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