{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:VRHCY3HIDQNKIKRLJ5DF3TRSCJ","short_pith_number":"pith:VRHCY3HI","schema_version":"1.0","canonical_sha256":"ac4e2c6ce81c1aa42a2b4f465dce3212634ed633fa3bd2447a43b51783e2882b","source":{"kind":"arxiv","id":"1903.11940","version":1},"attestation_state":"computed","paper":{"title":"A Novel Statistical Method for Measuring the Temperature-Density Relation in the IGM Using the $b$-$N_{\\text{HI}}$ Distribution of Absorbers in the Ly$\\alpha$ Forest","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Hector Hiss, Jos\\'e O\\~norbe, Joseph F. Hennawi, Michael Walther","submitted_at":"2019-03-28T13:14:30Z","abstract_excerpt":"We present a new method for determining the thermal state of the intergalactic medium based on Voigt profile decomposition of the Ly$\\alpha$ forest. The distribution of Doppler parameter and column density ($b$-$N_{\\text{HI}}$ distribution) is sensitive to the temperature density relation $T=T_0 (\\rho/\\rho_0)^{\\gamma-1}$, and previous work has inferred $T_0$ and $\\gamma$ by fitting its low-$b$ cutoff. This approach discards the majority of available data, and is susceptible to systematics related to cutoff determination. We present a method that exploits all information encoded in the $b$-$N_{"},"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":"1903.11940","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2019-03-28T13:14:30Z","cross_cats_sorted":[],"title_canon_sha256":"7f6bac73a35ad74832c360bf64a0c19d6b938db2383c523ff4360aed6d2e3adc","abstract_canon_sha256":"8467ef025b9fb3d3cb6a532ae423989fb14dabb69260caa399d27ec53f915306"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:46:18.044931Z","signature_b64":"9FLFtF8QZacz0c2haZ4fSi052hA247eWRLpXOP1MaITPh5MwD0kkmSafM1/N8dMkzCs5yeGQLmnTqiB9GuAkCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ac4e2c6ce81c1aa42a2b4f465dce3212634ed633fa3bd2447a43b51783e2882b","last_reissued_at":"2026-05-17T23:46:18.044155Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:46:18.044155Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A Novel Statistical Method for Measuring the Temperature-Density Relation in the IGM Using the $b$-$N_{\\text{HI}}$ Distribution of Absorbers in the Ly$\\alpha$ Forest","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Hector Hiss, Jos\\'e O\\~norbe, Joseph F. Hennawi, Michael Walther","submitted_at":"2019-03-28T13:14:30Z","abstract_excerpt":"We present a new method for determining the thermal state of the intergalactic medium based on Voigt profile decomposition of the Ly$\\alpha$ forest. The distribution of Doppler parameter and column density ($b$-$N_{\\text{HI}}$ distribution) is sensitive to the temperature density relation $T=T_0 (\\rho/\\rho_0)^{\\gamma-1}$, and previous work has inferred $T_0$ and $\\gamma$ by fitting its low-$b$ cutoff. This approach discards the majority of available data, and is susceptible to systematics related to cutoff determination. We present a method that exploits all information encoded in the $b$-$N_{"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1903.11940","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"},"aliases":[{"alias_kind":"arxiv","alias_value":"1903.11940","created_at":"2026-05-17T23:46:18.044284+00:00"},{"alias_kind":"arxiv_version","alias_value":"1903.11940v1","created_at":"2026-05-17T23:46:18.044284+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1903.11940","created_at":"2026-05-17T23:46:18.044284+00:00"},{"alias_kind":"pith_short_12","alias_value":"VRHCY3HIDQNK","created_at":"2026-05-18T12:33:30.264802+00:00"},{"alias_kind":"pith_short_16","alias_value":"VRHCY3HIDQNKIKRL","created_at":"2026-05-18T12:33:30.264802+00:00"},{"alias_kind":"pith_short_8","alias_value":"VRHCY3HI","created_at":"2026-05-18T12:33:30.264802+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.22489","citing_title":"Machine Learning Techniques for Astrophysics and Cosmology: Lyman-$\\alpha$ forest","ref_index":282,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/VRHCY3HIDQNKIKRLJ5DF3TRSCJ","json":"https://pith.science/pith/VRHCY3HIDQNKIKRLJ5DF3TRSCJ.json","graph_json":"https://pith.science/api/pith-number/VRHCY3HIDQNKIKRLJ5DF3TRSCJ/graph.json","events_json":"https://pith.science/api/pith-number/VRHCY3HIDQNKIKRLJ5DF3TRSCJ/events.json","paper":"https://pith.science/paper/VRHCY3HI"},"agent_actions":{"view_html":"https://pith.science/pith/VRHCY3HIDQNKIKRLJ5DF3TRSCJ","download_json":"https://pith.science/pith/VRHCY3HIDQNKIKRLJ5DF3TRSCJ.json","view_paper":"https://pith.science/paper/VRHCY3HI","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1903.11940&json=true","fetch_graph":"https://pith.science/api/pith-number/VRHCY3HIDQNKIKRLJ5DF3TRSCJ/graph.json","fetch_events":"https://pith.science/api/pith-number/VRHCY3HIDQNKIKRLJ5DF3TRSCJ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/VRHCY3HIDQNKIKRLJ5DF3TRSCJ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/VRHCY3HIDQNKIKRLJ5DF3TRSCJ/action/storage_attestation","attest_author":"https://pith.science/pith/VRHCY3HIDQNKIKRLJ5DF3TRSCJ/action/author_attestation","sign_citation":"https://pith.science/pith/VRHCY3HIDQNKIKRLJ5DF3TRSCJ/action/citation_signature","submit_replication":"https://pith.science/pith/VRHCY3HIDQNKIKRLJ5DF3TRSCJ/action/replication_record"}},"created_at":"2026-05-17T23:46:18.044284+00:00","updated_at":"2026-05-17T23:46:18.044284+00:00"}