{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:VR3NWKFNOPBCHYO5777QW2LQXY","short_pith_number":"pith:VR3NWKFN","schema_version":"1.0","canonical_sha256":"ac76db28ad73c223e1ddffff0b6970be0ff5957288ebfcd9d6a1f7fa5a6f10ca","source":{"kind":"arxiv","id":"2410.07967","version":1},"attestation_state":"computed","paper":{"title":"Determining the Magnetic Field in the Galactic Plane from New Arecibo Pulsar Faraday Rotation Measurements","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Alice P. Curtin, Joanna M. Rankin, Joel M. Weisberg","submitted_at":"2024-10-10T14:27:13Z","abstract_excerpt":"We develop a new method for studying the Galactic magnetic field along the spiral arms using pulsar Faraday rotation measures (RMs). Our new technique accounts for the dot-product nature of Faraday rotation and also splits the associated path integral into segments corresponding to particular zones along the LOS. We apply this geometrically-corrected, arm-by-arm technique to the low-latitude portion of a recently published set of Arecibo Faraday RMs for 313 pulsars along with previously obtained RMs in the same regions. We find disparities $>1\\sigma$ between the magnitude of the field above an"},"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":"2410.07967","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.GA","submitted_at":"2024-10-10T14:27:13Z","cross_cats_sorted":[],"title_canon_sha256":"452702b5b009b32549701f47aecd3be6599d936f58a3d1eb3d945fcb5083ca59","abstract_canon_sha256":"cafa12f5ff9c6266a1b892252067d230ad8d1d424d6272d809b6f91302206d15"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T09:18:46.796321Z","signature_b64":"tsDISbwJPEHpXZ5d+iR9Kmk9XlR6leOnpAZ0co4dBTGR1G9r3v8R1UNdzLKtEiSMwU34dA75C2vj24Ngl/c+AA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ac76db28ad73c223e1ddffff0b6970be0ff5957288ebfcd9d6a1f7fa5a6f10ca","last_reissued_at":"2026-07-05T09:18:46.795335Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T09:18:46.795335Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Determining the Magnetic Field in the Galactic Plane from New Arecibo Pulsar Faraday Rotation Measurements","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Alice P. Curtin, Joanna M. Rankin, Joel M. Weisberg","submitted_at":"2024-10-10T14:27:13Z","abstract_excerpt":"We develop a new method for studying the Galactic magnetic field along the spiral arms using pulsar Faraday rotation measures (RMs). Our new technique accounts for the dot-product nature of Faraday rotation and also splits the associated path integral into segments corresponding to particular zones along the LOS. We apply this geometrically-corrected, arm-by-arm technique to the low-latitude portion of a recently published set of Arecibo Faraday RMs for 313 pulsars along with previously obtained RMs in the same regions. We find disparities $>1\\sigma$ between the magnitude of the field above an"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2410.07967","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/2410.07967/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":"2410.07967","created_at":"2026-07-05T09:18:46.795787+00:00"},{"alias_kind":"arxiv_version","alias_value":"2410.07967v1","created_at":"2026-07-05T09:18:46.795787+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2410.07967","created_at":"2026-07-05T09:18:46.795787+00:00"},{"alias_kind":"pith_short_12","alias_value":"VR3NWKFNOPBC","created_at":"2026-07-05T09:18:46.795787+00:00"},{"alias_kind":"pith_short_16","alias_value":"VR3NWKFNOPBCHYO5","created_at":"2026-07-05T09:18:46.795787+00:00"},{"alias_kind":"pith_short_8","alias_value":"VR3NWKFN","created_at":"2026-07-05T09:18:46.795787+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.03314","citing_title":"Exploring the Magnetic Field Structure of the Milky Way with Pulsars in the SKA Era","ref_index":8,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/VR3NWKFNOPBCHYO5777QW2LQXY","json":"https://pith.science/pith/VR3NWKFNOPBCHYO5777QW2LQXY.json","graph_json":"https://pith.science/api/pith-number/VR3NWKFNOPBCHYO5777QW2LQXY/graph.json","events_json":"https://pith.science/api/pith-number/VR3NWKFNOPBCHYO5777QW2LQXY/events.json","paper":"https://pith.science/paper/VR3NWKFN"},"agent_actions":{"view_html":"https://pith.science/pith/VR3NWKFNOPBCHYO5777QW2LQXY","download_json":"https://pith.science/pith/VR3NWKFNOPBCHYO5777QW2LQXY.json","view_paper":"https://pith.science/paper/VR3NWKFN","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2410.07967&json=true","fetch_graph":"https://pith.science/api/pith-number/VR3NWKFNOPBCHYO5777QW2LQXY/graph.json","fetch_events":"https://pith.science/api/pith-number/VR3NWKFNOPBCHYO5777QW2LQXY/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/VR3NWKFNOPBCHYO5777QW2LQXY/action/timestamp_anchor","attest_storage":"https://pith.science/pith/VR3NWKFNOPBCHYO5777QW2LQXY/action/storage_attestation","attest_author":"https://pith.science/pith/VR3NWKFNOPBCHYO5777QW2LQXY/action/author_attestation","sign_citation":"https://pith.science/pith/VR3NWKFNOPBCHYO5777QW2LQXY/action/citation_signature","submit_replication":"https://pith.science/pith/VR3NWKFNOPBCHYO5777QW2LQXY/action/replication_record"}},"created_at":"2026-07-05T09:18:46.795787+00:00","updated_at":"2026-07-05T09:18:46.795787+00:00"}