{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2002:H2STNHRJFMQ45KMY2ZBR7EEWOX","short_pith_number":"pith:H2STNHRJ","schema_version":"1.0","canonical_sha256":"3ea5369e292b21cea998d6431f909675f2decfe8e28127ff412329b666f37578","source":{"kind":"arxiv","id":"astro-ph/0207105","version":3},"attestation_state":"computed","paper":{"title":"The Millennium Arecibo 21-CM Absorption Line Survey. II. Properties of the Warm and Cold Neutral Media","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Carl Heiles, T.H. Troland","submitted_at":"2002-07-04T02:26:00Z","abstract_excerpt":"We use the Gaussian-fit results of Paper I to investigate the properties of interstellar HI in the Solar neighborhood. The Warm and Cold Neutral Media (WNM and CNM) are physically distinct components. The CNM spin temperature histogram peaks at about 40 K. About 60% of all HI is WNM. At z=0, we derive a volume filling fraction of about 0.50 for the WNM; this value is very rough. The upper-limit WNM temperatures determined from line width range upward from about 500 K; a minimum of about 48% of the WNM lies in the thermally unstable region 500 to 5000 K. The WNM is a prominent constituent of th"},"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":"astro-ph/0207105","kind":"arxiv","version":3},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2002-07-04T02:26:00Z","cross_cats_sorted":[],"title_canon_sha256":"f12116ed4f6a618752af4ce06f9a19692d0f5b96273e031585a8b903cd63982d","abstract_canon_sha256":"0e10e0e65dec61d896c72d4a2684be5bfa25ca04e33b2fa06a6199ffaa7df86d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:25:11.791903Z","signature_b64":"jqPGeoZv4icdkzw/kgO0Tbr5AaGXrtqJACMqYaIwKDQBgk+qIZcwewPG4DoJJqk1L6mkuhIU0g+rl1iHr5BNCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3ea5369e292b21cea998d6431f909675f2decfe8e28127ff412329b666f37578","last_reissued_at":"2026-07-04T17:25:11.791465Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:25:11.791465Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Millennium Arecibo 21-CM Absorption Line Survey. II. Properties of the Warm and Cold Neutral Media","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Carl Heiles, T.H. Troland","submitted_at":"2002-07-04T02:26:00Z","abstract_excerpt":"We use the Gaussian-fit results of Paper I to investigate the properties of interstellar HI in the Solar neighborhood. The Warm and Cold Neutral Media (WNM and CNM) are physically distinct components. The CNM spin temperature histogram peaks at about 40 K. About 60% of all HI is WNM. At z=0, we derive a volume filling fraction of about 0.50 for the WNM; this value is very rough. The upper-limit WNM temperatures determined from line width range upward from about 500 K; a minimum of about 48% of the WNM lies in the thermally unstable region 500 to 5000 K. The WNM is a prominent constituent of th"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0207105","kind":"arxiv","version":3},"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/astro-ph/0207105/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":"astro-ph/0207105","created_at":"2026-07-04T17:25:11.791530+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0207105v3","created_at":"2026-07-04T17:25:11.791530+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0207105","created_at":"2026-07-04T17:25:11.791530+00:00"},{"alias_kind":"pith_short_12","alias_value":"H2STNHRJFMQ4","created_at":"2026-07-04T17:25:11.791530+00:00"},{"alias_kind":"pith_short_16","alias_value":"H2STNHRJFMQ45KMY","created_at":"2026-07-04T17:25:11.791530+00:00"},{"alias_kind":"pith_short_8","alias_value":"H2STNHRJ","created_at":"2026-07-04T17:25:11.791530+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":6,"internal_anchor_count":5,"sample":[{"citing_arxiv_id":"2606.06108","citing_title":"Grain-size evolution and rapid dust growth in high-redshift galaxies","ref_index":118,"is_internal_anchor":true},{"citing_arxiv_id":"2606.25158","citing_title":"Early phases of star formation with SKAO: synchrotron emission from dense starless cores in molecular clouds","ref_index":292,"is_internal_anchor":true},{"citing_arxiv_id":"2606.25077","citing_title":"Small-scale Magnetic Fields in the Milky Way and Nearby Galaxies","ref_index":92,"is_internal_anchor":true},{"citing_arxiv_id":"2605.22225","citing_title":"Silicate cosmic dust grain collisions in the interstellar medium: A molecular dynamics study","ref_index":133,"is_internal_anchor":true},{"citing_arxiv_id":"2605.17024","citing_title":"The ${}^{13}\\mathrm{CO}(2{-}1)/^{12}\\mathrm{CO}(2{-}1)$ Line Ratio from 100 Molecular Clouds in the Large Magellanic Cloud","ref_index":153,"is_internal_anchor":true},{"citing_arxiv_id":"2604.08775","citing_title":"Colloquium: Radio astronomy with the Arecibo 305-m telescope: In contemporaneous context","ref_index":82,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/H2STNHRJFMQ45KMY2ZBR7EEWOX","json":"https://pith.science/pith/H2STNHRJFMQ45KMY2ZBR7EEWOX.json","graph_json":"https://pith.science/api/pith-number/H2STNHRJFMQ45KMY2ZBR7EEWOX/graph.json","events_json":"https://pith.science/api/pith-number/H2STNHRJFMQ45KMY2ZBR7EEWOX/events.json","paper":"https://pith.science/paper/H2STNHRJ"},"agent_actions":{"view_html":"https://pith.science/pith/H2STNHRJFMQ45KMY2ZBR7EEWOX","download_json":"https://pith.science/pith/H2STNHRJFMQ45KMY2ZBR7EEWOX.json","view_paper":"https://pith.science/paper/H2STNHRJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0207105&json=true","fetch_graph":"https://pith.science/api/pith-number/H2STNHRJFMQ45KMY2ZBR7EEWOX/graph.json","fetch_events":"https://pith.science/api/pith-number/H2STNHRJFMQ45KMY2ZBR7EEWOX/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/H2STNHRJFMQ45KMY2ZBR7EEWOX/action/timestamp_anchor","attest_storage":"https://pith.science/pith/H2STNHRJFMQ45KMY2ZBR7EEWOX/action/storage_attestation","attest_author":"https://pith.science/pith/H2STNHRJFMQ45KMY2ZBR7EEWOX/action/author_attestation","sign_citation":"https://pith.science/pith/H2STNHRJFMQ45KMY2ZBR7EEWOX/action/citation_signature","submit_replication":"https://pith.science/pith/H2STNHRJFMQ45KMY2ZBR7EEWOX/action/replication_record"}},"created_at":"2026-07-04T17:25:11.791530+00:00","updated_at":"2026-07-04T17:25:11.791530+00:00"}