Massive passive galaxies at z ~ 1.6

Show simple item record

dc.contributor.advisor Sawicki, Marcin, 1969-
dc.creator Arcila-Osejo, Liz Maria
dc.date.accessioned 2018-05-31T14:38:08Z
dc.date.available 2018-05-31T14:38:08Z
dc.date.issued 2018
dc.identifier.other QB857.5 E96 A728 2018
dc.identifier.uri http://library2.smu.ca/handle/01/27532
dc.description xii, 215 leaves : coloured illustrations ; 29 cm
dc.description Includes abstract and appendices.
dc.description Includes bibliographical references (leaves 200-215).
dc.description.abstract We build a K-selected catalog of z&nbsp;&sim; 1.6 gzKs galaxies in the Deep and Wide fields of the Canada-France-Hawaii Legacy Survey, with a final effective area of 27.6 deg<sup>2</sup>. This catalog allows us to recover a representative sample of rare massive passive galaxies (log (M<sub>*</sub>/M<sub>☉</sub>) &gt;&nbsp;11.14) and very rare ultra-massive passive galaxies&nbsp;(log (M<sub>*</sub>/M<sub>☉</sub>) &gt; 11.49). The latter is an important population of galaxies, with significant build-up of stellar mass when the universe was only&nbsp;&sim; 4 Gyr old. This sample of ultra-massive passive galaxies (or UMPEGs) allows us to constrain the bright end of the stellar mass function. Once corrected for Eddington Bias, we find that passive galaxies at this redshift are well described by a Schechter function, as expected in a mass quenching scenario (Peng et al. 2010). Next, we find a lack of massive companions (star-forming or passive) to these UMPEGs and only a handful of lower mass (50% or less the mass of the UMPEG) companions. Using a simple dynamical friction estimate, we find that through merging these companions can at most contribute a&nbsp;&sim; 25% mass growth of these galaxies from z&nbsp;&sim;&nbsp;1.6 to z&nbsp;&sim; 1. Finally, we recover regions with an over-density of massive passive galaxies as sample environments for proto-clusters with an evolved population. These proto-clusters have an under-density of bright star-forming galaxies, hinting at them being proto-clusters where quenching is largely done.
dc.description.provenance Submitted by Greg Hilliard (greg.hilliard@smu.ca) on 2018-05-31T14:38:08Z No. of bitstreams: 1 Arcila-Osejo_Liz_PHD_2018.pdf: 11168140 bytes, checksum: 06eddc61d20a8f8258ff562325cafeae (MD5) en
dc.description.provenance Made available in DSpace on 2018-05-31T14:38:08Z (GMT). No. of bitstreams: 1 Arcila-Osejo_Liz_PHD_2018.pdf: 11168140 bytes, checksum: 06eddc61d20a8f8258ff562325cafeae (MD5) Previous issue date: 2018-03-29 en
dc.language.iso en en_CA
dc.publisher Halifax, N.S. : Saint Mary's University
dc.subject.lcc QB857.5.E96
dc.subject.lcsh Galaxies -- Evolution
dc.subject.lcsh Galaxies -- Formation
dc.title Massive passive galaxies at z ~ 1.6 en_CA
dc.type Text en_CA
thesis.degree.name Doctor of Philosophy in Astronomy
thesis.degree.level Masters
thesis.degree.discipline Astronomy and Physics
thesis.degree.grantor Saint Mary's University (Halifax, N.S.)
 Find Full text

Files in this item

 
 

This item appears in the following Collection(s)

Show simple item record

Search DSpace


Browse

My Account