Show simple item record

dc.contributor.advisorRudnick, Gregory H
dc.contributor.authorLee-Brown, Donald
dc.date.accessioned2017-05-15T03:08:07Z
dc.date.available2017-05-15T03:08:07Z
dc.date.issued2016-12-31
dc.date.submitted2016
dc.identifier.otherhttp://dissertations.umi.com/ku:15003
dc.identifier.urihttp://hdl.handle.net/1808/24174
dc.description.abstractUnderstanding how galaxies stop forming stars is a principle pursuit of extragalactic astrophysics. Here, I present a study of the relation between galaxy stellar age and mass in the $z=1.62$ protocluster IRC 0218. After separating star forming and quiescent galaxies on the basis of their $UVJ$ colors, we find that at stellar masses $M_* \ge 10^{10.8} M_{\odot}$, the quiescent fraction in IRC 0218 is $f_Q=1.0^{+0.00}_{-0.36}$, approximately $2-3 \times$ higher than the field value. At lower masses, $f_Q$ is consistent with the field. Using galaxy $D_{n}(4000)$ values as measures of stellar age, we find no relation between age and mass. This may indicate that the mass dependence of $f_Q$ was imprinted early in IRC 0218's history. Alternatively, the lack of a relation may be due to mass redistribution through gasless merging. Ultimately, our results place constraints on the mechanism(s) responsible for quenching in dense environments at $z\ge 1.5$.
dc.format.extent49 pages
dc.language.isoen
dc.publisherUniversity of Kansas
dc.rightsCopyright held by the author.
dc.subjectAstronomy
dc.subjectAstrophysics
dc.subjectGalaxies
dc.subjectGalaxy Clusters
dc.subjectGalaxy Evolution
dc.titleThe Ages of Passive Galaxies in a z=1.62 Protocluster
dc.typeThesis
dc.contributor.cmtememberAnthony-Twarog, Barbara J
dc.contributor.cmtememberHawley, Steven A
dc.thesis.degreeDisciplinePhysics & Astronomy
dc.thesis.degreeLevelM.S.
dc.identifier.orcid
dc.rights.accessrightsopenAccess


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record