@article{0ab8b02a63f84951a74449ac1f1198ce,
title = "Stellar and Molecular Gas Rotation in a Recently Quenched Massive Galaxy at z ∼ 0.7",
abstract = "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 (SFR). 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 the Atacama Large Millimeter/submillimeter Array (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.",
keywords = "galaxies: evolution, galaxies: formation, galaxies: kinematics and dynamics",
author = "Qiana Hunt and Rachel Bezanson and Greene, {Jenny E.} and Spilker, {Justin S.} and Suess, {Katherine A.} and Mariska Kriek and Desika Narayanan and Robert Feldmann and {Van Der Wel}, Arjen and Petchara Pattarakijwanich",
note = "Funding Information: This paper is based on observations obtained at the Gemini Observatory, acquired through the Gemini Observatory Archive under Program ID GN-2016A-FT-6 and processed using the Gemini IRAF package, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnolog{\'i}a e Innovaci{\'o}n Productiva (Argentina), and Minist{\'e}rio da Ci{\^e}ncia, Tecnologia e Inova{\c c}{\~a}o (Brazil). Funding Information: D.N. was funded in part by NSF AST-1715206 and HST AR-15043.0001. Funding Information: This paper makes use of the following ALMA data: ADS/ JAO.ALMA#2016.1.00126.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship Program under grant No. DGE 1106400. Publisher Copyright: {\textcopyright} 2018. The American Astronomical Society. All rights reserved..",
year = "2018",
month = jun,
day = "20",
doi = "10.3847/2041-8213/aaca9a",
language = "English (US)",
volume = "860",
journal = "Astrophysical Journal Letters",
issn = "2041-8205",
publisher = "IOP Publishing Ltd.",
number = "2",
}