{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:UYOPHJBQTCTOLFOQV2VOHJYNC4","short_pith_number":"pith:UYOPHJBQ","schema_version":"1.0","canonical_sha256":"a61cf3a43098a6e595d0aeaae3a70d1733cf3004df3570fb695997ebd5227a31","source":{"kind":"arxiv","id":"1411.6355","version":1},"attestation_state":"computed","paper":{"title":"Galaxy And Mass Assembly (GAMA): mass-size relations of z$<$0.1 galaxies subdivided by S\\'ersic index, colour and morphology","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Aaron S.G. Robotham, Alister W. Graham, Amanda J. Moffett, \\'Angel R. L\\'opez-S\\'anchez, Boris H\\\"aussler, Christopher J. Conselice, Edward N. Taylor, Iraklis S. Konstantopoulos, Ivan K. Baldry, Jon Loveday, Joss Bland-Hawthorn, Lee S. Kelvin, Luke J.M. Davies, Mehmet Alpaslan, Michelle E. Cluver, Peder Norberg, Rebecca Lange, Sarah Brough, Simon P. Driver, Stephen K. Andrews, Stephen M. Wilkins, Steven Bamford, Steven Phillipps","submitted_at":"2014-11-24T06:23:20Z","abstract_excerpt":"We use data from the Galaxy And Mass Assembly (GAMA) survey in the redshift range 0.01$<$z$<$0.1 (8399 galaxies in $g$ to $K_s$ bands) to derive the stellar mass $-$ half-light radius relations for various divisions of 'early' and 'late'-type samples. We find the choice of division between early and late (i.e., colour, shape, morphology) is not particularly critical, however, the adopted mass limits and sample selections (i.e., the careful rejection of outliers and use of robust fitting methods) are important. In particular we note that for samples extending to low stellar mass limits ($<10^{1"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"1411.6355","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2014-11-24T06:23:20Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"3f3cd5d521d4b836b4efa88c3e1c9bbfcf9fec9dac2f26c74e345a3527182aab","abstract_canon_sha256":"5cfa34b24b78cc7d0f3502dc87adb7a65a4a2dc65e9e956a7cded133cf5c4a40"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:09:37.143455Z","signature_b64":"5xusRYYiafTQmfWUuOYCei5X8L+18ZifpJPZ5lmpsWVJnethZceXtKOEXaGoABQY42JdrVLKNdXRv6eRs/WqDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"a61cf3a43098a6e595d0aeaae3a70d1733cf3004df3570fb695997ebd5227a31","last_reissued_at":"2026-05-18T01:09:37.143017Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:09:37.143017Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Galaxy And Mass Assembly (GAMA): mass-size relations of z$<$0.1 galaxies subdivided by S\\'ersic index, colour and morphology","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.GA","authors_text":"Aaron S.G. Robotham, Alister W. Graham, Amanda J. Moffett, \\'Angel R. L\\'opez-S\\'anchez, Boris H\\\"aussler, Christopher J. Conselice, Edward N. Taylor, Iraklis S. Konstantopoulos, Ivan K. Baldry, Jon Loveday, Joss Bland-Hawthorn, Lee S. Kelvin, Luke J.M. Davies, Mehmet Alpaslan, Michelle E. Cluver, Peder Norberg, Rebecca Lange, Sarah Brough, Simon P. Driver, Stephen K. Andrews, Stephen M. Wilkins, Steven Bamford, Steven Phillipps","submitted_at":"2014-11-24T06:23:20Z","abstract_excerpt":"We use data from the Galaxy And Mass Assembly (GAMA) survey in the redshift range 0.01$<$z$<$0.1 (8399 galaxies in $g$ to $K_s$ bands) to derive the stellar mass $-$ half-light radius relations for various divisions of 'early' and 'late'-type samples. We find the choice of division between early and late (i.e., colour, shape, morphology) is not particularly critical, however, the adopted mass limits and sample selections (i.e., the careful rejection of outliers and use of robust fitting methods) are important. In particular we note that for samples extending to low stellar mass limits ($<10^{1"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1411.6355","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"},"aliases":[{"alias_kind":"arxiv","alias_value":"1411.6355","created_at":"2026-05-18T01:09:37.143087+00:00"},{"alias_kind":"arxiv_version","alias_value":"1411.6355v1","created_at":"2026-05-18T01:09:37.143087+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1411.6355","created_at":"2026-05-18T01:09:37.143087+00:00"},{"alias_kind":"pith_short_12","alias_value":"UYOPHJBQTCTO","created_at":"2026-05-18T12:28:52.271510+00:00"},{"alias_kind":"pith_short_16","alias_value":"UYOPHJBQTCTOLFOQ","created_at":"2026-05-18T12:28:52.271510+00:00"},{"alias_kind":"pith_short_8","alias_value":"UYOPHJBQ","created_at":"2026-05-18T12:28:52.271510+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2605.15327","citing_title":"Witnessing the rapid growth of disk galaxies over cosmic time using JWST and HST","ref_index":146,"is_internal_anchor":true},{"citing_arxiv_id":"2605.08353","citing_title":"Empirical estimates of how massive galaxies can be in {\\Lambda}CDM","ref_index":186,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/UYOPHJBQTCTOLFOQV2VOHJYNC4","json":"https://pith.science/pith/UYOPHJBQTCTOLFOQV2VOHJYNC4.json","graph_json":"https://pith.science/api/pith-number/UYOPHJBQTCTOLFOQV2VOHJYNC4/graph.json","events_json":"https://pith.science/api/pith-number/UYOPHJBQTCTOLFOQV2VOHJYNC4/events.json","paper":"https://pith.science/paper/UYOPHJBQ"},"agent_actions":{"view_html":"https://pith.science/pith/UYOPHJBQTCTOLFOQV2VOHJYNC4","download_json":"https://pith.science/pith/UYOPHJBQTCTOLFOQV2VOHJYNC4.json","view_paper":"https://pith.science/paper/UYOPHJBQ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1411.6355&json=true","fetch_graph":"https://pith.science/api/pith-number/UYOPHJBQTCTOLFOQV2VOHJYNC4/graph.json","fetch_events":"https://pith.science/api/pith-number/UYOPHJBQTCTOLFOQV2VOHJYNC4/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/UYOPHJBQTCTOLFOQV2VOHJYNC4/action/timestamp_anchor","attest_storage":"https://pith.science/pith/UYOPHJBQTCTOLFOQV2VOHJYNC4/action/storage_attestation","attest_author":"https://pith.science/pith/UYOPHJBQTCTOLFOQV2VOHJYNC4/action/author_attestation","sign_citation":"https://pith.science/pith/UYOPHJBQTCTOLFOQV2VOHJYNC4/action/citation_signature","submit_replication":"https://pith.science/pith/UYOPHJBQTCTOLFOQV2VOHJYNC4/action/replication_record"}},"created_at":"2026-05-18T01:09:37.143087+00:00","updated_at":"2026-05-18T01:09:37.143087+00:00"}