{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:OCMRPSLM4S5CXKLEYPJSIOCVHB","short_pith_number":"pith:OCMRPSLM","schema_version":"1.0","canonical_sha256":"709917c96ce4ba2ba964c3d3243855387f586475eb96e3c6b502b9c968b3614a","source":{"kind":"arxiv","id":"1607.08036","version":1},"attestation_state":"computed","paper":{"title":"Lighting the dark molecular gas: H$_{2}$ as a direct tracer","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Aditya Togi, J. D. T. Smith","submitted_at":"2016-07-27T11:09:46Z","abstract_excerpt":"Robust knowledge of molecular gas mass is critical for understanding star formation in galaxies. The H$_{2}$ molecule does not emit efficiently in the cold interstellar medium, hence the molecular gas content of galaxies is typically inferred using indirect tracers. At low metallicity and in other extreme environments, these tracers can be subject to substantial biases. We present a new method of estimating total molecular gas mass in galaxies directly from pure mid-infrared rotational H$_{2}$ emission. By assuming a power-law distribution of H$_{2}$ rotational temperatures, we can accurately "},"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":"1607.08036","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2016-07-27T11:09:46Z","cross_cats_sorted":[],"title_canon_sha256":"0f1133beef2670881064565ca91cbd83b85a1219363342cf19bad5bc3297fbef","abstract_canon_sha256":"8331d6d6e460f073d3aca33db19d5c9904776064362e9fb59e37936734bf3625"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:02:37.603190Z","signature_b64":"VWtTeKRPJ9xxgNjYY4LWv1f6SrJyn/UtwrBzifML84idGH3JEJB4GbQr6MeETh8l0GNmOjDaoOJgFucxZIwrCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"709917c96ce4ba2ba964c3d3243855387f586475eb96e3c6b502b9c968b3614a","last_reissued_at":"2026-05-18T01:02:37.602491Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:02:37.602491Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Lighting the dark molecular gas: H$_{2}$ as a direct tracer","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Aditya Togi, J. D. T. Smith","submitted_at":"2016-07-27T11:09:46Z","abstract_excerpt":"Robust knowledge of molecular gas mass is critical for understanding star formation in galaxies. The H$_{2}$ molecule does not emit efficiently in the cold interstellar medium, hence the molecular gas content of galaxies is typically inferred using indirect tracers. At low metallicity and in other extreme environments, these tracers can be subject to substantial biases. We present a new method of estimating total molecular gas mass in galaxies directly from pure mid-infrared rotational H$_{2}$ emission. By assuming a power-law distribution of H$_{2}$ rotational temperatures, we can accurately "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1607.08036","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":"1607.08036","created_at":"2026-05-18T01:02:37.602612+00:00"},{"alias_kind":"arxiv_version","alias_value":"1607.08036v1","created_at":"2026-05-18T01:02:37.602612+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1607.08036","created_at":"2026-05-18T01:02:37.602612+00:00"},{"alias_kind":"pith_short_12","alias_value":"OCMRPSLM4S5C","created_at":"2026-05-18T12:30:36.002864+00:00"},{"alias_kind":"pith_short_16","alias_value":"OCMRPSLM4S5CXKLE","created_at":"2026-05-18T12:30:36.002864+00:00"},{"alias_kind":"pith_short_8","alias_value":"OCMRPSLM","created_at":"2026-05-18T12:30:36.002864+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.25856","citing_title":"JWST resolves jet-driven H2 and ionized outflows in radio galaxy 3C305","ref_index":81,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OCMRPSLM4S5CXKLEYPJSIOCVHB","json":"https://pith.science/pith/OCMRPSLM4S5CXKLEYPJSIOCVHB.json","graph_json":"https://pith.science/api/pith-number/OCMRPSLM4S5CXKLEYPJSIOCVHB/graph.json","events_json":"https://pith.science/api/pith-number/OCMRPSLM4S5CXKLEYPJSIOCVHB/events.json","paper":"https://pith.science/paper/OCMRPSLM"},"agent_actions":{"view_html":"https://pith.science/pith/OCMRPSLM4S5CXKLEYPJSIOCVHB","download_json":"https://pith.science/pith/OCMRPSLM4S5CXKLEYPJSIOCVHB.json","view_paper":"https://pith.science/paper/OCMRPSLM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1607.08036&json=true","fetch_graph":"https://pith.science/api/pith-number/OCMRPSLM4S5CXKLEYPJSIOCVHB/graph.json","fetch_events":"https://pith.science/api/pith-number/OCMRPSLM4S5CXKLEYPJSIOCVHB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OCMRPSLM4S5CXKLEYPJSIOCVHB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OCMRPSLM4S5CXKLEYPJSIOCVHB/action/storage_attestation","attest_author":"https://pith.science/pith/OCMRPSLM4S5CXKLEYPJSIOCVHB/action/author_attestation","sign_citation":"https://pith.science/pith/OCMRPSLM4S5CXKLEYPJSIOCVHB/action/citation_signature","submit_replication":"https://pith.science/pith/OCMRPSLM4S5CXKLEYPJSIOCVHB/action/replication_record"}},"created_at":"2026-05-18T01:02:37.602612+00:00","updated_at":"2026-05-18T01:02:37.602612+00:00"}