{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:LTJVVS23DT6Q2EJU5NJRVDGE62","short_pith_number":"pith:LTJVVS23","schema_version":"1.0","canonical_sha256":"5cd35acb5b1cfd0d1134eb531a8cc4f692c522b027f1132205dbd0cef699e5af","source":{"kind":"arxiv","id":"1108.3911","version":1},"attestation_state":"computed","paper":{"title":"Herschel-ATLAS Galaxy Counts and High Redshift Luminosity Functions: The Formation of Massive Early Type Galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Bressan, A. Cava, A. Cooray, A. Dariush, A. Lapi, D.G. Bonfield, D. Herranz, D.J.B. Smith, D.L. Clements, E. Ibar, E. Pascale, E. Rigby, G. de Zotti, G. Rodighiero, J. Fritz, J. Gonzalez-Nuevo, J. Wardlow, L. Danese, L. Dunne, L. Fan, M. Baes, M.J. Jarvis, M.J. Michalowski, M. Lopez-Caniego, M. Massardi, M. Negrello, M. Pohlen, P. Temi, P. van der Werf, R. Auld, R. Hopwood, R. Ivison, S. Buttiglione, S. Dye, S. Eales, S. Kaviraj, S. Maddox, S. Serjeant","submitted_at":"2011-08-19T07:45:35Z","abstract_excerpt":"Exploiting the Herschel-ATLAS Science Demonstration Phase (SDP) survey data, we have determined the luminosity functions (LFs) at rest-frame wavelengths of 100 and 250 micron and at several redshifts z>1, for bright sub-mm galaxies with star formation rates (SFR) >100 M_sun/yr. We find that the evolution of the comoving LF is strong up to z~2.5, and slows down at higher redshifts. From the LFs and the information on halo masses inferred from clustering analysis, we derived an average relation between SFR and halo mass (and its scatter). We also infer that the timescale of the main episode of d"},"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":"1108.3911","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2011-08-19T07:45:35Z","cross_cats_sorted":[],"title_canon_sha256":"53b2e3365b219708b08d6fa1e80124905571ae8d4ad8704bf47e60e0aad49d5c","abstract_canon_sha256":"67bf68542a1741cf913284c0c439523b304186357bb916ec6c2bbd638871074b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:00:50.575750Z","signature_b64":"O6E0POF/ygFBQbO0tcFVNN5YCDSGJ6+/C9tPL5XZUA7KimC7oIRfoaGitGy6cf3nHzDN4OmkH/bXeIh9f30mAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"5cd35acb5b1cfd0d1134eb531a8cc4f692c522b027f1132205dbd0cef699e5af","last_reissued_at":"2026-05-18T02:00:50.575030Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:00:50.575030Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Herschel-ATLAS Galaxy Counts and High Redshift Luminosity Functions: The Formation of Massive Early Type Galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Bressan, A. Cava, A. Cooray, A. Dariush, A. Lapi, D.G. Bonfield, D. Herranz, D.J.B. Smith, D.L. Clements, E. Ibar, E. Pascale, E. Rigby, G. de Zotti, G. Rodighiero, J. Fritz, J. Gonzalez-Nuevo, J. Wardlow, L. Danese, L. Dunne, L. Fan, M. Baes, M.J. Jarvis, M.J. Michalowski, M. Lopez-Caniego, M. Massardi, M. Negrello, M. Pohlen, P. Temi, P. van der Werf, R. Auld, R. Hopwood, R. Ivison, S. Buttiglione, S. Dye, S. Eales, S. Kaviraj, S. Maddox, S. Serjeant","submitted_at":"2011-08-19T07:45:35Z","abstract_excerpt":"Exploiting the Herschel-ATLAS Science Demonstration Phase (SDP) survey data, we have determined the luminosity functions (LFs) at rest-frame wavelengths of 100 and 250 micron and at several redshifts z>1, for bright sub-mm galaxies with star formation rates (SFR) >100 M_sun/yr. We find that the evolution of the comoving LF is strong up to z~2.5, and slows down at higher redshifts. From the LFs and the information on halo masses inferred from clustering analysis, we derived an average relation between SFR and halo mass (and its scatter). We also infer that the timescale of the main episode of d"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1108.3911","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":"1108.3911","created_at":"2026-05-18T02:00:50.575143+00:00"},{"alias_kind":"arxiv_version","alias_value":"1108.3911v1","created_at":"2026-05-18T02:00:50.575143+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1108.3911","created_at":"2026-05-18T02:00:50.575143+00:00"},{"alias_kind":"pith_short_12","alias_value":"LTJVVS23DT6Q","created_at":"2026-05-18T12:26:34.985390+00:00"},{"alias_kind":"pith_short_16","alias_value":"LTJVVS23DT6Q2EJU","created_at":"2026-05-18T12:26:34.985390+00:00"},{"alias_kind":"pith_short_8","alias_value":"LTJVVS23","created_at":"2026-05-18T12:26:34.985390+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/LTJVVS23DT6Q2EJU5NJRVDGE62","json":"https://pith.science/pith/LTJVVS23DT6Q2EJU5NJRVDGE62.json","graph_json":"https://pith.science/api/pith-number/LTJVVS23DT6Q2EJU5NJRVDGE62/graph.json","events_json":"https://pith.science/api/pith-number/LTJVVS23DT6Q2EJU5NJRVDGE62/events.json","paper":"https://pith.science/paper/LTJVVS23"},"agent_actions":{"view_html":"https://pith.science/pith/LTJVVS23DT6Q2EJU5NJRVDGE62","download_json":"https://pith.science/pith/LTJVVS23DT6Q2EJU5NJRVDGE62.json","view_paper":"https://pith.science/paper/LTJVVS23","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1108.3911&json=true","fetch_graph":"https://pith.science/api/pith-number/LTJVVS23DT6Q2EJU5NJRVDGE62/graph.json","fetch_events":"https://pith.science/api/pith-number/LTJVVS23DT6Q2EJU5NJRVDGE62/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/LTJVVS23DT6Q2EJU5NJRVDGE62/action/timestamp_anchor","attest_storage":"https://pith.science/pith/LTJVVS23DT6Q2EJU5NJRVDGE62/action/storage_attestation","attest_author":"https://pith.science/pith/LTJVVS23DT6Q2EJU5NJRVDGE62/action/author_attestation","sign_citation":"https://pith.science/pith/LTJVVS23DT6Q2EJU5NJRVDGE62/action/citation_signature","submit_replication":"https://pith.science/pith/LTJVVS23DT6Q2EJU5NJRVDGE62/action/replication_record"}},"created_at":"2026-05-18T02:00:50.575143+00:00","updated_at":"2026-05-18T02:00:50.575143+00:00"}