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Home » STRUCTURAL EVOLUTION IN MASSIVE GALAXIES AT Z ∼ 2

STRUCTURAL EVOLUTION IN MASSIVE GALAXIES AT Z ∼ 2

(AGENPARL) – GARCHING (GERMANY), dom 18 ottobre 2020 First Author: Tadaki, Ken-ichi
Instruments: ALMA_Band_7, ALMA_Bands
ProgramIDs: 2012.1.00245.S, 2012.1.00983.S, 2013.1.00205.S, 2013.1.00566.S, 2013.1.00884.S, 2015.1.00242.S, 2016.1.01079.S, 2017.1.01027.S
BibCode: 2020ApJ…901…74T

We present 0″2 resolution Atacama Large Millimeter/submillimeter Array (ALMA) observations at 870 μm in a stellar mass-selected sample of 85 massive ( ${M}_{star }gt {10}^{11},{M}_{odot }$ <!– –> ) star-forming galaxies (SFGs) at $z=1.9mbox{–}2.6$ <!– –> in the CANDELS/3D-Hubble Space Telescope fields of UDS and GOODS-S. We measure the effective radius of the rest-frame far-infrared (FIR) emission for 62 massive SFGs. They are distributed over wide ranges of FIR size from ${R}_{{rm{e}},mathrm{FIR}}=0.4,mathrm{kpc}$ <!– –> to ${R}_{{rm{e}},mathrm{FIR}}=6,mathrm{kpc}$ <!– –> . The effective radius of the FIR emission is smaller by a factor of ${2.3}_{-1.0}^{+1.9}$ <!– –> than the effective radius of the optical emission and is smaller by a factor of ${1.9}_{-1.0}^{+1.9}$ <!– –> than the half-mass radius. Taking into account potential extended components, the FIR size would change only by ∼10%. By combining the spatial distributions of the FIR and optical emission, we investigate how galaxies change the effective radius of the optical emission and the stellar mass within a radius of 1 kpc, ${M}_{1mathrm{kpc}}$ <!– –> . The compact starburst puts most of the massive SFGs on the mass-size relation for quiescent galaxies (QGs) at z ∼ 2 within 300 Myr if the current star formation activity and its spatial distribution are maintained. We also find that within 300 Myr, ∼38% of massive SFGs can reach the central mass of ${M}_{1mathrm{kpc}}={10}^{10.5},{M}_{odot }$ <!– –> , which is around the boundary between massive SFGs and QGs. These results suggest an outside-in transformation scenario in which a dense core is formed at the center of a more extended disk, likely via dissipative in-disk inflows. Synchronized observations at ALMA 870 μm and James Webb Space Telescope 3-4 μm will explicitly verify this scenario.

Fonte/Source: http://feedproxy.google.com/~r/ESOtelbibPapers/~3/UOzrS0VdViw/detail.php

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