{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:YX3MZ75YQ6EYSRFMWLI52VSVER","short_pith_number":"pith:YX3MZ75Y","schema_version":"1.0","canonical_sha256":"c5f6ccffb887898944acb2d1dd5655245dcce76e478976553c2d588a1d7a83a0","source":{"kind":"arxiv","id":"1107.0317","version":2},"attestation_state":"computed","paper":{"title":"Galaxy Structure and Mode of Star Formation in the SFR-Mass Plane from z ~ 2.5 to z ~ 0.1","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Amelie Saintonge, Antonio Cava, Anton M. Koekemoer, Arjen van der Wel, Benjamin Magnelli, Dale D. Kocevski, Dieter Lutz, Elizabeth J. McGrath, Emeric Le Floc'h, Francesca Pozzi, Giulia Rodighiero, Guillermo Barro, Herve Aussel, Javier Gracia-Carpio, Kuang-Han Huang, Kyoung-Soo Lee, Laurie Riguccini, Linda Tacconi, Natascha M. Forster Schreiber, Nimish P. Hathi, Paola Popesso, Raanan Nordon, Reinhard Genzel, Stefano Berta, Stijn Wuyts, Yicheng Guo","submitted_at":"2011-07-01T20:00:02Z","abstract_excerpt":"We analyze the dependence of galaxy structure (size and Sersic index) and mode of star formation (\\Sigma_SFR and SFR_IR/SFR_UV) on the position of galaxies in the SFR versus Mass diagram. Our sample comprises roughly 640000 galaxies at z~0.1, 130000 galaxies at z~1, and 36000 galaxies at z~2. Structural measurements for all but the z~0.1 galaxies were based on HST imaging, and SFRs are derived using a Herschel-calibrated ladder of SFR indicators. We find that a correlation between the structure and stellar population of galaxies (i.e., a 'Hubble sequence') is already in place since at least z~"},"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":"1107.0317","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2011-07-01T20:00:02Z","cross_cats_sorted":[],"title_canon_sha256":"92cd642b6ddf49772aab1d3855c833dc86bc7313dd070fe004e8d7094216090e","abstract_canon_sha256":"53a078fb16cf8f108c7f61a90130a8f06504b57e1829ab3885628a2314d9d323"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:01:25.704345Z","signature_b64":"6hdcccUA4VZko7mMqBJitI+KNKUpGgbLgk7M24Tna0yiTOW2OKCkVUm2LR2ABfpZ1EwnMGCZ2nNSTUhmVzlFBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c5f6ccffb887898944acb2d1dd5655245dcce76e478976553c2d588a1d7a83a0","last_reissued_at":"2026-05-18T02:01:25.703918Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:01:25.703918Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Galaxy Structure and Mode of Star Formation in the SFR-Mass Plane from z ~ 2.5 to z ~ 0.1","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Amelie Saintonge, Antonio Cava, Anton M. Koekemoer, Arjen van der Wel, Benjamin Magnelli, Dale D. Kocevski, Dieter Lutz, Elizabeth J. McGrath, Emeric Le Floc'h, Francesca Pozzi, Giulia Rodighiero, Guillermo Barro, Herve Aussel, Javier Gracia-Carpio, Kuang-Han Huang, Kyoung-Soo Lee, Laurie Riguccini, Linda Tacconi, Natascha M. Forster Schreiber, Nimish P. Hathi, Paola Popesso, Raanan Nordon, Reinhard Genzel, Stefano Berta, Stijn Wuyts, Yicheng Guo","submitted_at":"2011-07-01T20:00:02Z","abstract_excerpt":"We analyze the dependence of galaxy structure (size and Sersic index) and mode of star formation (\\Sigma_SFR and SFR_IR/SFR_UV) on the position of galaxies in the SFR versus Mass diagram. Our sample comprises roughly 640000 galaxies at z~0.1, 130000 galaxies at z~1, and 36000 galaxies at z~2. Structural measurements for all but the z~0.1 galaxies were based on HST imaging, and SFRs are derived using a Herschel-calibrated ladder of SFR indicators. We find that a correlation between the structure and stellar population of galaxies (i.e., a 'Hubble sequence') is already in place since at least z~"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1107.0317","kind":"arxiv","version":2},"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":"1107.0317","created_at":"2026-05-18T02:01:25.703986+00:00"},{"alias_kind":"arxiv_version","alias_value":"1107.0317v2","created_at":"2026-05-18T02:01:25.703986+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1107.0317","created_at":"2026-05-18T02:01:25.703986+00:00"},{"alias_kind":"pith_short_12","alias_value":"YX3MZ75YQ6EY","created_at":"2026-05-18T12:26:47.523578+00:00"},{"alias_kind":"pith_short_16","alias_value":"YX3MZ75YQ6EYSRFM","created_at":"2026-05-18T12:26:47.523578+00:00"},{"alias_kind":"pith_short_8","alias_value":"YX3MZ75Y","created_at":"2026-05-18T12:26:47.523578+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2605.19661","citing_title":"COSMOS-Web: Star formation along the early Hubble sequence and the evolution of dust over the redshift range 0<z<12","ref_index":101,"is_internal_anchor":true},{"citing_arxiv_id":"2605.20590","citing_title":"Spider-Webb: enhanced star formation in low-mass galaxies within the Spiderweb protocluster revealed by JWST Pa$\\beta$ narrow-band imaging","ref_index":33,"is_internal_anchor":true},{"citing_arxiv_id":"2605.19661","citing_title":"COSMOS-Web: Star formation along the early Hubble sequence and the evolution of dust over the redshift range 0<z<12","ref_index":101,"is_internal_anchor":true},{"citing_arxiv_id":"2605.08353","citing_title":"Empirical estimates of how massive galaxies can be in {\\Lambda}CDM","ref_index":207,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/YX3MZ75YQ6EYSRFMWLI52VSVER","json":"https://pith.science/pith/YX3MZ75YQ6EYSRFMWLI52VSVER.json","graph_json":"https://pith.science/api/pith-number/YX3MZ75YQ6EYSRFMWLI52VSVER/graph.json","events_json":"https://pith.science/api/pith-number/YX3MZ75YQ6EYSRFMWLI52VSVER/events.json","paper":"https://pith.science/paper/YX3MZ75Y"},"agent_actions":{"view_html":"https://pith.science/pith/YX3MZ75YQ6EYSRFMWLI52VSVER","download_json":"https://pith.science/pith/YX3MZ75YQ6EYSRFMWLI52VSVER.json","view_paper":"https://pith.science/paper/YX3MZ75Y","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1107.0317&json=true","fetch_graph":"https://pith.science/api/pith-number/YX3MZ75YQ6EYSRFMWLI52VSVER/graph.json","fetch_events":"https://pith.science/api/pith-number/YX3MZ75YQ6EYSRFMWLI52VSVER/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/YX3MZ75YQ6EYSRFMWLI52VSVER/action/timestamp_anchor","attest_storage":"https://pith.science/pith/YX3MZ75YQ6EYSRFMWLI52VSVER/action/storage_attestation","attest_author":"https://pith.science/pith/YX3MZ75YQ6EYSRFMWLI52VSVER/action/author_attestation","sign_citation":"https://pith.science/pith/YX3MZ75YQ6EYSRFMWLI52VSVER/action/citation_signature","submit_replication":"https://pith.science/pith/YX3MZ75YQ6EYSRFMWLI52VSVER/action/replication_record"}},"created_at":"2026-05-18T02:01:25.703986+00:00","updated_at":"2026-05-18T02:01:25.703986+00:00"}