Stellar and Molecular Gas Rotation in a Recently-Quenched Massive Galaxy
  at z~0.7
  The process by which massive galaxies transition from blue, star-forming
disks into red, quiescent galaxies remains one of the most poorly-understood
aspects of galaxy evolution. In this investigation, we attempt to gain a better
understanding of how star formation is quenched by focusing on a massive
post-starburst galaxy at z = 0.747. The target has a high stellar mass and a
molecular gas fraction of ~30% -- unusually high for its low star formation
rate. We look for indicators of star formation suppression mechanisms in the
stellar kinematics and age distribution of the galaxy obtained from spatially
resolved Gemini Integral-Field spectra and in the gas kinematics obtained from
ALMA. We find evidence of significant rotation in the stars, but we do not
detect a stellar age gradient within 5 kpc. The molecular gas is aligned with
the stellar component, and we see no evidence of strong gas outflows. Our
target may represent the product of a merger-induced starburst or of
morphological quenching; however, our results are not completely consistent
with any of the prominent quenching models.
