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dc.rights.licensePublished 2021 June 8 • © 2021. The American Astronomical Society. All rights reserved.-
dc.contributor.authorGuo, Y.-
dc.contributor.authorCarleton, T.-
dc.contributor.authorBell, E. F.-
dc.contributor.authorChen, Z.-
dc.contributor.authorDekel, A.-
dc.contributor.authorFaber, S. M.-
dc.contributor.authorGiavalisco, M.-
dc.contributor.authorKocevski, D. D.-
dc.contributor.authorKoekemoer, A. M.-
dc.contributor.authorKoo, D. C.-
dc.contributor.authorKurczynski, P.-
dc.contributor.authorLee, S. K.-
dc.contributor.authorLiu, F. S.-
dc.contributor.authorPapovich, C.-
dc.contributor.authorPérez González, G.-
dc.date.accessioned2022-02-15T14:26:43Z-
dc.date.available2022-02-15T14:26:43Z-
dc.date.issued2021-06-08-
dc.identifier.citationThe Astrophysical Journal 914(1): 7(2021)es
dc.identifier.issn0004-637X-
dc.identifier.otherhttps://iopscience.iop.org/article/10.3847/1538-4357/abf115-
dc.identifier.urihttp://hdl.handle.net/20.500.12666/612-
dc.description.abstractWe use the Cosmic Assembly Deep Near-infrared Extragalactic Legacy Survey data to study the relationship between quenching and the stellar mass surface density within the central radius of 1 kpc (Σ1) of low-mass galaxies (stellar mass M* ≲ 109.5 M⊙) at 0.5 ≤ z < 1.5. Our sample is mass complete down to ∼109 M⊙ at 0.5 ≤ z < 1.0. We compare the mean Σ1 of star-forming galaxies (SFGs) and quenched galaxies (QGs) at the same redshift and M*. We find that low-mass QGs have a higher Σ1 than low-mass SFGs, similar to galaxies above 1010 M⊙. The difference of Σ1 between QGs and SFGs increases slightly with M* at M* ≲ 1010 M⊙ and decreases with M* at M* ≳ 1010 M⊙. The turnover mass is consistent with the mass where quenching mechanisms transition from internal to environmental quenching. At 0.5 ≤ z < 1.0, we find that Σ1 of galaxies increases by about 0.25 dex in the green valley (i.e., the transition region from star forming to fully quenched), regardless of their M*. Using the observed specific star formation rate gradient in the literature as a constraint, we estimate that the quenching timescale (i.e., time spent in the transition) of low-mass galaxies is a few (∼4) Gyr at 0.5 ≤ z < 1.0. The mechanisms responsible for quenching need to gradually quench star formation in an outside-in way, i.e., preferentially ceasing star formation in outskirts of galaxies while maintaining their central star formation to increase Σ1. An interesting and intriguing result is the similarity of the growth of Σ1 in the green valley between low-mass and massive galaxies, which suggests that the role of internal processes in quenching low-mass galaxies is a question worthy of further investigation.es
dc.description.sponsorshipThe authors thank the anonymous referee for providing valuable comments, which improved the manuscript. Support for Program numbers HST-AR-13891, HST-AR-15025, and HST-GO-12060 were provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. Members of the CANDELS team at UCSC acknowledge support from NASA HST grant GO-12060.10-A and from NSF grants AST-0808133 and AST-1615730. S.L. acknowledges the support from the National Research Foundation of Korea (NRF) grant (2020R1I1A1A01060310) funded by the Korean government (MSIP).es
dc.language.isoenges
dc.publisherIOP Science Publishinges
dc.rightsAttribution-NonCommercial-NoDerivatives 4.0 Internationales
dc.rights.urihttps://creativecommons.org/licenses/by-nc-nd/4.0/-
dc.subjectGalaxy formationes
dc.subjectGalaxy evolutiones
dc.subjectGalaxy quenchinges
dc.subjectGalaxy structurees
dc.subjectGalaxy physicses
dc.subjectDwarf galaxieses
dc.subjectQuenched galaxieses
dc.subjectGalaxy environmentses
dc.subjectExtragalactic astronomyes
dc.titleImplications of Increased Central Mass Surface Densities for the Quenching of Low-mass Galaxieses
dc.typeinfo:eu-repo/semantics/articlees
dc.contributor.orcidGuo, Y. [0000-0003-2775-2002]-
dc.contributor.orcidCarleton, T. [0000-0001-6650-2853]-
dc.contributor.orcidBell, E. F. [0000-0002-5564-9873]-
dc.contributor.orcidChen, Z. [0000-0002-2326-0476]-
dc.contributor.orcidDekel, A. [0000-0003-4174-0374]-
dc.contributor.orcidFabel, S. M. [0000-0003-4996-214X]-
dc.contributor.orcidGiavalisco, M. [0000-0002-7831-8751]-
dc.contributor.orcidKocevski, D. D. [0000-0002-8360-3880]-
dc.contributor.orcidKoekemoer, A. M. [0000-0002-6610-2048]-
dc.contributor.orcidKoo, D. C. [0000-0003-3385-6799]-
dc.contributor.orcidKurczynski, P. [0000-0002-8816-5146]-
dc.contributor.orcidLee, S. K. [0000-0001-5342-8906]-
dc.contributor.orcidLiu, F. S. [0000-0002-1064-1544]-
dc.contributor.orcidPapovich, C. [0000-0001-7503-8482]-
dc.contributor.orcidPérez González, P. G. [0000-0003-4528-5639]-
dc.identifier.doi10.3847/1538-4357/abf115-
dc.identifier.e-issn1538-4357-
dc.contributor.funderNational Science Foundation (NSF)-
dc.contributor.funderNational Aeronautics and Space Administration (NASA)-
dc.contributor.funderNational Research Foundation of Korea (NRF)-
dc.description.peerreviewedPeerreviewes
dc.identifier.funderhttp://dx.doi.org/10.13039/100000001-
dc.identifier.funderhttp://dx.doi.org/10.13039/100000104-
dc.identifier.funderhttp://dx.doi.org/10.13039/501100003725-
dc.type.hasVersioninfo:eu-repo/semantics/publishedVersion-
dc.rights.accessRightsinfo:eu-repo/semantics/openAccess-
dc.type.coarhttp://purl.org/coar/resource_type/c_6501-
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