{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:4NNW7W52ESSPBYTNUGXXISUFHA","short_pith_number":"pith:4NNW7W52","schema_version":"1.0","canonical_sha256":"e35b6fdbba24a4f0e26da1af744a8538223bea0f000342491102b93a85e3da83","source":{"kind":"arxiv","id":"2503.14348","version":1},"attestation_state":"computed","paper":{"title":"The H$\\alpha$ sky in three dimensions","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Catherine Zucker, Dhanesh Krishnarao, Gordian Edenhofer, Kenneth Wood, Lewis McCallum, L. Matthew Haffner, Robert Benjamin","submitted_at":"2025-03-18T15:26:18Z","abstract_excerpt":"We combine parallax distances to nearby O stars with parsec-scale resolution three-dimensional dust maps of the local region of the Milky Way (within 1.25 kpc of the Sun) to simulate the transfer of Lyman continuum photons through the interstellar medium. Assuming a fixed gas-to-dust ratio, we determine the density of ionized gas, electron temperature, and H$\\alpha$ emissivity throughout the local Milky Way. There is good morphological agreement between the predicted and observed H$\\alpha$ all-sky map of the Wisconsin H$\\alpha$ Mapper. We find that our simulation underproduces the observed H$\\"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"2503.14348","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2025-03-18T15:26:18Z","cross_cats_sorted":[],"title_canon_sha256":"b8f8a58191deba4745b0c8cfc325405bdef7d5483c817c919aaf1f3b763648eb","abstract_canon_sha256":"203e6fcef6b1a4086297341e3f83de1bb16d788ae8a2b21f2ea3605ca3a0b757"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:34:00.572037Z","signature_b64":"eEc4TMQBpPus1Rgd31RTw5K6nDbNv1ul89oDvceXbnd+ybzgzDZcIJph3f7Ee8z//twEp4XRGXQWvBpLmZ9JAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e35b6fdbba24a4f0e26da1af744a8538223bea0f000342491102b93a85e3da83","last_reissued_at":"2026-07-05T10:34:00.571569Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:34:00.571569Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The H$\\alpha$ sky in three dimensions","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Catherine Zucker, Dhanesh Krishnarao, Gordian Edenhofer, Kenneth Wood, Lewis McCallum, L. Matthew Haffner, Robert Benjamin","submitted_at":"2025-03-18T15:26:18Z","abstract_excerpt":"We combine parallax distances to nearby O stars with parsec-scale resolution three-dimensional dust maps of the local region of the Milky Way (within 1.25 kpc of the Sun) to simulate the transfer of Lyman continuum photons through the interstellar medium. Assuming a fixed gas-to-dust ratio, we determine the density of ionized gas, electron temperature, and H$\\alpha$ emissivity throughout the local Milky Way. There is good morphological agreement between the predicted and observed H$\\alpha$ all-sky map of the Wisconsin H$\\alpha$ Mapper. We find that our simulation underproduces the observed H$\\"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2503.14348","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/2503.14348/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":"2503.14348","created_at":"2026-07-05T10:34:00.571634+00:00"},{"alias_kind":"arxiv_version","alias_value":"2503.14348v1","created_at":"2026-07-05T10:34:00.571634+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2503.14348","created_at":"2026-07-05T10:34:00.571634+00:00"},{"alias_kind":"pith_short_12","alias_value":"4NNW7W52ESSP","created_at":"2026-07-05T10:34:00.571634+00:00"},{"alias_kind":"pith_short_16","alias_value":"4NNW7W52ESSPBYTN","created_at":"2026-07-05T10:34:00.571634+00:00"},{"alias_kind":"pith_short_8","alias_value":"4NNW7W52","created_at":"2026-07-05T10:34:00.571634+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.07451","citing_title":"Milky Way Atlas: A radial-velocity-resolved, three-dimensional map of H I within 1.25 kpc","ref_index":46,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/4NNW7W52ESSPBYTNUGXXISUFHA","json":"https://pith.science/pith/4NNW7W52ESSPBYTNUGXXISUFHA.json","graph_json":"https://pith.science/api/pith-number/4NNW7W52ESSPBYTNUGXXISUFHA/graph.json","events_json":"https://pith.science/api/pith-number/4NNW7W52ESSPBYTNUGXXISUFHA/events.json","paper":"https://pith.science/paper/4NNW7W52"},"agent_actions":{"view_html":"https://pith.science/pith/4NNW7W52ESSPBYTNUGXXISUFHA","download_json":"https://pith.science/pith/4NNW7W52ESSPBYTNUGXXISUFHA.json","view_paper":"https://pith.science/paper/4NNW7W52","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2503.14348&json=true","fetch_graph":"https://pith.science/api/pith-number/4NNW7W52ESSPBYTNUGXXISUFHA/graph.json","fetch_events":"https://pith.science/api/pith-number/4NNW7W52ESSPBYTNUGXXISUFHA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/4NNW7W52ESSPBYTNUGXXISUFHA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/4NNW7W52ESSPBYTNUGXXISUFHA/action/storage_attestation","attest_author":"https://pith.science/pith/4NNW7W52ESSPBYTNUGXXISUFHA/action/author_attestation","sign_citation":"https://pith.science/pith/4NNW7W52ESSPBYTNUGXXISUFHA/action/citation_signature","submit_replication":"https://pith.science/pith/4NNW7W52ESSPBYTNUGXXISUFHA/action/replication_record"}},"created_at":"2026-07-05T10:34:00.571634+00:00","updated_at":"2026-07-05T10:34:00.571634+00:00"}