{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:KW5RLKEOANU7BNWN7ZKXFE63JA","short_pith_number":"pith:KW5RLKEO","schema_version":"1.0","canonical_sha256":"55bb15a88e0369f0b6cdfe557293db4805c776dc26510ae92c6a7f161f0ecce1","source":{"kind":"arxiv","id":"1604.06802","version":2},"attestation_state":"computed","paper":{"title":"The FMOS-COSMOS survey of star-forming galaxies at z~1.6. IV: Excitation state and chemical enrichment of the interstellar medium","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. Puglisi, A. Renzini, C. Maier, D. Kashino, D. Masters, D. Sanders, E. Daddi, F. Civano, F. Valentino, G. Rodighiero, H. J. Zahid, J. Chu, J. D. Silverman, J. S. Kartaltepe, L. J. Kewley, M. Kajisawa, M. Onodera, N. Arimoto, N. Sugiyama, O. Ilbert, O. Le Fevre, S. Juneau, T. Miyaji, T. Nagao, Y. Taniguchi","submitted_at":"2016-04-22T20:00:02Z","abstract_excerpt":"We investigate the physical conditions of ionized gas in high-z star-forming galaxies using diagnostic diagrams based on the rest-frame optical emission lines. The sample consists of 701 galaxies with an Ha detection at $1.4\\lesssim z\\lesssim1.7$, from the FMOS-COSMOS survey, that represent the normal star-forming population over the stellar mass range $10^{9.6} \\lesssim M_\\ast/M_\\odot \\lesssim 10^{11.6}$ with those at $M_\\ast>10^{11}~M_\\odot$ being well sampled. We confirm an offset of the average location of star-forming galaxies in the BPT diagram ([OIII]/Hb vs. [NII]/Ha), primarily towards"},"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":"1604.06802","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2016-04-22T20:00:02Z","cross_cats_sorted":[],"title_canon_sha256":"2c3a7ceada661cdfa50988f306da0310d5703ba1a3423b778ece8c4be88e59dd","abstract_canon_sha256":"85e212a8c352731ba11bf6535ed5351feb63ff16fcadd22c7d0f164dd42c2821"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:52:17.365818Z","signature_b64":"/Y2EXRBnm/8Opg+mOecI5ZH4Esq/bJ0wgNMPiDjvZP4pTm8o/TZnNzNJeIe2AuRJj7ck2fpBu965osxdq7jaBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"55bb15a88e0369f0b6cdfe557293db4805c776dc26510ae92c6a7f161f0ecce1","last_reissued_at":"2026-05-18T00:52:17.365221Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:52:17.365221Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The FMOS-COSMOS survey of star-forming galaxies at z~1.6. IV: Excitation state and chemical enrichment of the interstellar medium","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. Puglisi, A. Renzini, C. Maier, D. Kashino, D. Masters, D. Sanders, E. Daddi, F. Civano, F. Valentino, G. Rodighiero, H. J. Zahid, J. Chu, J. D. Silverman, J. S. Kartaltepe, L. J. Kewley, M. Kajisawa, M. Onodera, N. Arimoto, N. Sugiyama, O. Ilbert, O. Le Fevre, S. Juneau, T. Miyaji, T. Nagao, Y. Taniguchi","submitted_at":"2016-04-22T20:00:02Z","abstract_excerpt":"We investigate the physical conditions of ionized gas in high-z star-forming galaxies using diagnostic diagrams based on the rest-frame optical emission lines. The sample consists of 701 galaxies with an Ha detection at $1.4\\lesssim z\\lesssim1.7$, from the FMOS-COSMOS survey, that represent the normal star-forming population over the stellar mass range $10^{9.6} \\lesssim M_\\ast/M_\\odot \\lesssim 10^{11.6}$ with those at $M_\\ast>10^{11}~M_\\odot$ being well sampled. We confirm an offset of the average location of star-forming galaxies in the BPT diagram ([OIII]/Hb vs. [NII]/Ha), primarily towards"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1604.06802","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":"1604.06802","created_at":"2026-05-18T00:52:17.365336+00:00"},{"alias_kind":"arxiv_version","alias_value":"1604.06802v2","created_at":"2026-05-18T00:52:17.365336+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1604.06802","created_at":"2026-05-18T00:52:17.365336+00:00"},{"alias_kind":"pith_short_12","alias_value":"KW5RLKEOANU7","created_at":"2026-05-18T12:30:29.479603+00:00"},{"alias_kind":"pith_short_16","alias_value":"KW5RLKEOANU7BNWN","created_at":"2026-05-18T12:30:29.479603+00:00"},{"alias_kind":"pith_short_8","alias_value":"KW5RLKEO","created_at":"2026-05-18T12:30:29.479603+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/KW5RLKEOANU7BNWN7ZKXFE63JA","json":"https://pith.science/pith/KW5RLKEOANU7BNWN7ZKXFE63JA.json","graph_json":"https://pith.science/api/pith-number/KW5RLKEOANU7BNWN7ZKXFE63JA/graph.json","events_json":"https://pith.science/api/pith-number/KW5RLKEOANU7BNWN7ZKXFE63JA/events.json","paper":"https://pith.science/paper/KW5RLKEO"},"agent_actions":{"view_html":"https://pith.science/pith/KW5RLKEOANU7BNWN7ZKXFE63JA","download_json":"https://pith.science/pith/KW5RLKEOANU7BNWN7ZKXFE63JA.json","view_paper":"https://pith.science/paper/KW5RLKEO","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1604.06802&json=true","fetch_graph":"https://pith.science/api/pith-number/KW5RLKEOANU7BNWN7ZKXFE63JA/graph.json","fetch_events":"https://pith.science/api/pith-number/KW5RLKEOANU7BNWN7ZKXFE63JA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/KW5RLKEOANU7BNWN7ZKXFE63JA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/KW5RLKEOANU7BNWN7ZKXFE63JA/action/storage_attestation","attest_author":"https://pith.science/pith/KW5RLKEOANU7BNWN7ZKXFE63JA/action/author_attestation","sign_citation":"https://pith.science/pith/KW5RLKEOANU7BNWN7ZKXFE63JA/action/citation_signature","submit_replication":"https://pith.science/pith/KW5RLKEOANU7BNWN7ZKXFE63JA/action/replication_record"}},"created_at":"2026-05-18T00:52:17.365336+00:00","updated_at":"2026-05-18T00:52:17.365336+00:00"}