The Morphology-Density Relation of Galaxies at z~1.6

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dc.contributor.advisorMuzzin, Adam
dc.contributor.authorBrown, Westley Andrew Louise
dc.date.accessioned2024-07-18T21:21:16Z
dc.date.available2024-07-18T21:21:16Z
dc.date.copyright2024-01-29
dc.date.issued2024-07-18
dc.date.updated2024-07-18T21:21:16Z
dc.degree.disciplinePhysics And Astronomy
dc.degree.levelMaster's
dc.degree.nameMSc - Master of Science
dc.description.abstractThe relationship between galaxy morphology and environment has been well-studied in the local universe and at low redshift, showing that galaxies in dense clusters tend to be elliptical and bulge-like while galaxies in low-density fields tend to be spiral and disk-like. However, this relationship is less understood at higher redshifts, and the few studies at high-z rely on samples with incomplete redshift measurements and poorly constrained stellar masses. We explore the morphology-density relation at z~1.6, the tail end of cosmic noon, using a sample of 3 SpARCS clusters and 2 fields from 3D-HST/CANDELS. Using Sersic index as a proxy for galaxy morphology, we find that the morphology-density relation is already in place in clusters at this epoch. Additionally, we find a significant difference in the relationship between galaxy morphology and stellar mass in clusters compared to field environments. This suggests that the morphology-density relation may be driven by mass-dependent environmental processes.
dc.identifier.urihttps://hdl.handle.net/10315/42152
dc.languageen
dc.rightsAuthor owns copyright, except where explicitly noted. Please contact the author directly with licensing requests.
dc.subjectAstrophysics
dc.subject.keywordsGalaxies
dc.subject.keywordsGalaxy evolution
dc.subject.keywordsGalaxy morphology
dc.subject.keywordsGalaxy clusters
dc.subject.keywordsHigh redshift
dc.subject.keywordsGrism spectroscopy
dc.subject.keywordsStellar mass
dc.titleThe Morphology-Density Relation of Galaxies at z~1.6
dc.typeElectronic Thesis or Dissertation

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