Journal article
On the Gas Content, Star Formation Efficiency, and Environmental Quenching of Massive Galaxies in Protoclusters at z approximate to 2.0-2.5
The Astrophysical journal, Vol.887(2), 183
12/20/2019
DOI: 10.3847/1538-4357/ab5302
Abstract
We present ALMA Band 6 (nu = 233 GHz,lambda = 1.3 mm) continuum observations toward 68 "normal" star-forming galaxies within two Coma-like progenitor structures at z = 2.10 and 2.47, from which ISM masses are derived, providing the largest census of molecular gas mass in overdense environments at these redshifts. Our sample comprises galaxies with a stellar mass range of 1 x 10(9)M(circle dot)-4 x 10(11) M-circle dot with a mean M* approximate to 6 x 10(10)M(circle dot). Combining these measurements with multiwavelength observations and spectral energy distribution modeling, we characterize the gas mass fraction and the star formation efficiency, and infer the impact of the environment on galaxies' evolution. Most of our detected galaxies (greater than or similar to 70%) have star formation efficiencies and gas fractions similar to those found for coeval field galaxies and in agreement with the field scaling relations. However, we do find that the protoclusters contain an increased fraction of massive, gas-poor galaxies, with low gas fractions (f(gas) less than or similar to 6%-10%) and red rest-frame ultraviolet/optical colors typical of post-starburst and passive galaxies. The relatively high abundance of passive galaxies suggests an accelerated evolution of massive galaxies in protocluster environments. The large fraction of quenched galaxies in these overdense structures also implies that environmental quenching takes place during the early phases of cluster assembly, even before virialization. From our data, we derive a quenching efficiency of epsilon(q) approximate to 0.45 and an upper limit on the quenching timescale of tau(q) < 1 Gyr.
Details
- Title: Subtitle
- On the Gas Content, Star Formation Efficiency, and Environmental Quenching of Massive Galaxies in Protoclusters at z approximate to 2.0-2.5
- Creators
- J. A. Zavala - The University of Texas at AustinC. M. Casey - The University of Texas at AustinN. Scoville - California Institute of TechnologyJ. B. Champagne - The University of Texas at AustinY. Chiang - Johns Hopkins UniversityH. Dannerbauer - Instituto de Astrofísica de CanariasP. Drew - The University of Texas at AustinH. Fu - University of IowaJ. Spilker - The University of Texas at AustinL. Spitler - Macquarie UniversityK. V. Tran - Mitchell InstituteE. Treister - Pontificia Universidad Católica de ChileS. Toft - University of Copenhagen
- Resource Type
- Journal article
- Publication Details
- The Astrophysical journal, Vol.887(2), 183
- DOI
- 10.3847/1538-4357/ab5302
- ISSN
- 0004-637X
- eISSN
- 1538-4357
- Publisher
- IOP Publishing Ltd
- Number of pages
- 15
- Grant note
- AST-1714528; AST1814034 / NSF; National Science Foundation (NSF) 648179 / European Research Council (ERC) Consolidator Grant funding scheme (project ConTExt) Danish National Research Foundation; Danmarks Grundforskningsfond 1160999 / FONDECYT; Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT); CONICYT FONDECYT PFB-06/2007; AFB170002 / Basal-CATA; Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT); CONICYT PIA/BASAL FEDER (European Regional Development Funds) PIA ACT172033 / CONICYT; Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT) RYC-2014-15686; AYA2017-84061-P / Spanish Ministry of Science, Innovation and Universities (MICIU) under the 2014 Ramon y Cajal program University of Texas at Austin College of Natural Sciences
- Language
- English
- Date published
- 12/20/2019
- Academic Unit
- Physics and Astronomy
- Record Identifier
- 9984428763902771
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