{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:W325FIGIJDVTG6YP33NE4FX3IW","short_pith_number":"pith:W325FIGI","schema_version":"1.0","canonical_sha256":"b6f5d2a0c848eb337b0fdeda4e16fb45aa5e54d3c3181887965634e72715dfbe","source":{"kind":"arxiv","id":"1907.07933","version":1},"attestation_state":"computed","paper":{"title":"Recalibration of [O II] $\\lambda 3727$ as a Star Formation Rate Estimator for Active and Inactive Galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Luis C. Ho, Ming-Yang Zhuang","submitted_at":"2019-07-18T09:11:41Z","abstract_excerpt":"We investigate the use of the [O II] $\\lambda3727$ emission line as a star formation rate (SFR) estimator using Sloan Digital Sky Spectra for nearly 100,000 star-forming galaxies and 5,500 galaxies with narrow-line active galactic nuclei. Consistent with previous work, we find that the [O II]/H$\\alpha$ ratio in star-forming galaxies depends strongly on gas-phase metallicity. Using metallicities derived from the [N II] $\\lambda 6584$/[O II] $\\lambda 3727$ method, we refine a metallicity-dependent SFR estimator based on [O II] that is calibrated within a scatter of 0.056 dex against the more com"},"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":"1907.07933","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2019-07-18T09:11:41Z","cross_cats_sorted":[],"title_canon_sha256":"481e5ba2e72b360dff411d5d8164d3858bca5280d12e3acb5595fd45ec185c9f","abstract_canon_sha256":"7422c9d1adaa1e5dc543ae3c1d06f609ac2159e89c1a3547c13616c3fe8324b6"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:03:49.869616Z","signature_b64":"5KpBBi4ElNk3GWCMxYuhHq1F4OEbBueEs6BRABsisKiUYWkw0GS7whLvb8+kzEhTKQEw9Q1HxC/LR3JJ/Ms8CA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b6f5d2a0c848eb337b0fdeda4e16fb45aa5e54d3c3181887965634e72715dfbe","last_reissued_at":"2026-07-05T00:03:49.869266Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:03:49.869266Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Recalibration of [O II] $\\lambda 3727$ as a Star Formation Rate Estimator for Active and Inactive Galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Luis C. Ho, Ming-Yang Zhuang","submitted_at":"2019-07-18T09:11:41Z","abstract_excerpt":"We investigate the use of the [O II] $\\lambda3727$ emission line as a star formation rate (SFR) estimator using Sloan Digital Sky Spectra for nearly 100,000 star-forming galaxies and 5,500 galaxies with narrow-line active galactic nuclei. Consistent with previous work, we find that the [O II]/H$\\alpha$ ratio in star-forming galaxies depends strongly on gas-phase metallicity. Using metallicities derived from the [N II] $\\lambda 6584$/[O II] $\\lambda 3727$ method, we refine a metallicity-dependent SFR estimator based on [O II] that is calibrated within a scatter of 0.056 dex against the more com"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1907.07933","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/1907.07933/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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":"1907.07933","created_at":"2026-07-05T00:03:49.869321+00:00"},{"alias_kind":"arxiv_version","alias_value":"1907.07933v1","created_at":"2026-07-05T00:03:49.869321+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1907.07933","created_at":"2026-07-05T00:03:49.869321+00:00"},{"alias_kind":"pith_short_12","alias_value":"W325FIGIJDVT","created_at":"2026-07-05T00:03:49.869321+00:00"},{"alias_kind":"pith_short_16","alias_value":"W325FIGIJDVTG6YP","created_at":"2026-07-05T00:03:49.869321+00:00"},{"alias_kind":"pith_short_8","alias_value":"W325FIGI","created_at":"2026-07-05T00:03:49.869321+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.08749","citing_title":"Deep Spectroscopic Follow-Up of Maisie's Galaxy -- A Typical Galaxy in the Early Universe","ref_index":15,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/W325FIGIJDVTG6YP33NE4FX3IW","json":"https://pith.science/pith/W325FIGIJDVTG6YP33NE4FX3IW.json","graph_json":"https://pith.science/api/pith-number/W325FIGIJDVTG6YP33NE4FX3IW/graph.json","events_json":"https://pith.science/api/pith-number/W325FIGIJDVTG6YP33NE4FX3IW/events.json","paper":"https://pith.science/paper/W325FIGI"},"agent_actions":{"view_html":"https://pith.science/pith/W325FIGIJDVTG6YP33NE4FX3IW","download_json":"https://pith.science/pith/W325FIGIJDVTG6YP33NE4FX3IW.json","view_paper":"https://pith.science/paper/W325FIGI","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1907.07933&json=true","fetch_graph":"https://pith.science/api/pith-number/W325FIGIJDVTG6YP33NE4FX3IW/graph.json","fetch_events":"https://pith.science/api/pith-number/W325FIGIJDVTG6YP33NE4FX3IW/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/W325FIGIJDVTG6YP33NE4FX3IW/action/timestamp_anchor","attest_storage":"https://pith.science/pith/W325FIGIJDVTG6YP33NE4FX3IW/action/storage_attestation","attest_author":"https://pith.science/pith/W325FIGIJDVTG6YP33NE4FX3IW/action/author_attestation","sign_citation":"https://pith.science/pith/W325FIGIJDVTG6YP33NE4FX3IW/action/citation_signature","submit_replication":"https://pith.science/pith/W325FIGIJDVTG6YP33NE4FX3IW/action/replication_record"}},"created_at":"2026-07-05T00:03:49.869321+00:00","updated_at":"2026-07-05T00:03:49.869321+00:00"}