{"id":{"repo_id":"york","oai_identifier":"oai:yorkspace.library.yorku.ca:10315/42152"},"canonical_url":"https://search.dev.ndltd.org/etd/york/oai:yorkspace.library.yorku.ca:10315/42152","repository":{"repo_id":"york","name":"York University","base_url":"https://yorkspace.library.yorku.ca/oai/request"},"display":{"title":"The Morphology-Density Relation of Galaxies at z~1.6","abstract":"The 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.","abstract_html":"The 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.","abstract_has_math":false,"creators":["Brown, Westley Andrew Louise"],"institution":null,"degree_name":null,"degree_level":null,"degree_discipline":null,"degree_department":null,"school":null,"contributors":[],"advisors":["Muzzin, Adam"],"committee_chairs":[],"committee_members":[],"year":2024,"date_issued":"2024-07-18","date_published":"2024-07-18","updated_at":"2026-07-24T06:33:34Z","subjects":["Astrophysics"],"languages":["en"],"rights":["Author owns copyright, except where explicitly noted. Please contact the author directly with licensing requests."],"rights_urls":[],"identifier_entries":[]},"links":{"outbound_url":"https://hdl.handle.net/10315/42152","outbound_label":"Handle","outbound_source":"dc:identifier.uri"},"metadata_groups":[{"id":"people","label":"People","entries":[{"key":"dc:contributor.advisor","label":"Advisor","values":["Muzzin, Adam"]},{"key":"dc:creator","label":"Author","values":["Brown, Westley Andrew Louise"]}]},{"id":"academic_context","label":"Academic Context","entries":[{"key":"dc:date.accessioned","label":"Dc Date Accessioned","values":["2024-07-18T21:21:16Z"]},{"key":"dc:date.available","label":"Dc Date Available","values":["2024-07-18T21:21:16Z"]},{"key":"dc:date.issued","label":"Date","values":["2024-07-18"]},{"key":"dc:type","label":"Dc Type","values":["Electronic Thesis or Dissertation"]}]},{"id":"subjects_keywords","label":"Subjects and Keywords","entries":[{"key":"dc:subject","label":"Dc Subject","values":["Astrophysics"]}]},{"id":"language_rights","label":"Language and Rights","entries":[{"key":"dc:language","label":"Dc Language","values":["en"]},{"key":"dc:rights","label":"Dc Rights","values":["Author owns copyright, except where explicitly noted. Please contact the author directly with licensing requests."]}]},{"id":"identifiers","label":"Identifiers","entries":[{"key":"dc:identifier.uri","label":"Identifier URI","values":["https://hdl.handle.net/10315/42152"]}]},{"id":"additional","label":"Additional Metadata","entries":[{"key":"dc:description.abstract","label":"Abstract","values":["The 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."]},{"key":"dc:title","label":"Title","values":["The Morphology-Density Relation of Galaxies at z~1.6"]}]}],"canonical_facts":{"dc:contributor.advisor":["Muzzin, Adam"],"dc:creator":["Brown, Westley Andrew Louise"],"dc:date.accessioned":["2024-07-18T21:21:16Z"],"dc:date.available":["2024-07-18T21:21:16Z"],"dc:date.issued":["2024-07-18"],"dc:description.abstract":["The 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.uri":["https://hdl.handle.net/10315/42152"],"dc:language":["en"],"dc:rights":["Author owns copyright, except where explicitly noted. Please contact the author directly with licensing requests."],"dc:subject":["Astrophysics"],"dc:title":["The Morphology-Density Relation of Galaxies at z~1.6"],"dc:type":["Electronic Thesis or Dissertation"]},"updated_at":"2026-07-24T06:33:34Z"}