{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:GWDBLR4NS3B3KNK6PT77A7H37F","short_pith_number":"pith:GWDBLR4N","schema_version":"1.0","canonical_sha256":"358615c78d96c3b5355e7cfff07cfbf9515bcb8bb5e142479861c8c576e31c50","source":{"kind":"arxiv","id":"1602.01873","version":1},"attestation_state":"computed","paper":{"title":"Dispersion of Magnetic Fields in Molecular Clouds. IV - Analysis of Interferometry Data","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Charles L. H. Hull, John E. Vaillancourt, Martin Houde, Richard L. Plambeck, Roger H. Hildebrand","submitted_at":"2016-02-04T22:45:02Z","abstract_excerpt":"We expand on the dispersion analysis of polarimetry maps toward applications to interferometry data. We show how the filtering of low-spatial frequencies can be accounted for within the idealized Gaussian turbulence model, initially introduced for single-dish data analysis, to recover reliable estimates for correlation lengths of magnetized turbulence, as well as magnetic field strengths (plane-of-the-sky component) using the Davis-Chandrasekhar-Fermi method. We apply our updated technique to TADPOL/CARMA data obtained on W3(OH), W3 Main, and DR21(OH). For W3(OH) our analysis yields a turbulen"},"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":"1602.01873","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2016-02-04T22:45:02Z","cross_cats_sorted":[],"title_canon_sha256":"19e7ddad27d893c3596c4eeaa08d12562e6e6d0121d59221ee77e6d845e48f49","abstract_canon_sha256":"43416d84d65d37dba06f83f8b07007b74e14f823b70eba882bbc318eeef5ca9c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:18:37.610944Z","signature_b64":"qdhQRgYWYjmA40iwp9qVLAWmNkVtpFIuAB1MiNEsQSPH9ux6h0zHwHpHf40oTPHpHNYAUXxESc3Rfrfq6cvjDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"358615c78d96c3b5355e7cfff07cfbf9515bcb8bb5e142479861c8c576e31c50","last_reissued_at":"2026-05-18T01:18:37.610426Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:18:37.610426Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Dispersion of Magnetic Fields in Molecular Clouds. IV - Analysis of Interferometry Data","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"Charles L. H. Hull, John E. Vaillancourt, Martin Houde, Richard L. Plambeck, Roger H. Hildebrand","submitted_at":"2016-02-04T22:45:02Z","abstract_excerpt":"We expand on the dispersion analysis of polarimetry maps toward applications to interferometry data. We show how the filtering of low-spatial frequencies can be accounted for within the idealized Gaussian turbulence model, initially introduced for single-dish data analysis, to recover reliable estimates for correlation lengths of magnetized turbulence, as well as magnetic field strengths (plane-of-the-sky component) using the Davis-Chandrasekhar-Fermi method. We apply our updated technique to TADPOL/CARMA data obtained on W3(OH), W3 Main, and DR21(OH). For W3(OH) our analysis yields a turbulen"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1602.01873","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":"1602.01873","created_at":"2026-05-18T01:18:37.610510+00:00"},{"alias_kind":"arxiv_version","alias_value":"1602.01873v1","created_at":"2026-05-18T01:18:37.610510+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1602.01873","created_at":"2026-05-18T01:18:37.610510+00:00"},{"alias_kind":"pith_short_12","alias_value":"GWDBLR4NS3B3","created_at":"2026-05-18T12:30:19.053100+00:00"},{"alias_kind":"pith_short_16","alias_value":"GWDBLR4NS3B3KNK6","created_at":"2026-05-18T12:30:19.053100+00:00"},{"alias_kind":"pith_short_8","alias_value":"GWDBLR4N","created_at":"2026-05-18T12:30:19.053100+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.02149","citing_title":"The magnetic field of the Milky Way: an observational perspective","ref_index":163,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/GWDBLR4NS3B3KNK6PT77A7H37F","json":"https://pith.science/pith/GWDBLR4NS3B3KNK6PT77A7H37F.json","graph_json":"https://pith.science/api/pith-number/GWDBLR4NS3B3KNK6PT77A7H37F/graph.json","events_json":"https://pith.science/api/pith-number/GWDBLR4NS3B3KNK6PT77A7H37F/events.json","paper":"https://pith.science/paper/GWDBLR4N"},"agent_actions":{"view_html":"https://pith.science/pith/GWDBLR4NS3B3KNK6PT77A7H37F","download_json":"https://pith.science/pith/GWDBLR4NS3B3KNK6PT77A7H37F.json","view_paper":"https://pith.science/paper/GWDBLR4N","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1602.01873&json=true","fetch_graph":"https://pith.science/api/pith-number/GWDBLR4NS3B3KNK6PT77A7H37F/graph.json","fetch_events":"https://pith.science/api/pith-number/GWDBLR4NS3B3KNK6PT77A7H37F/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/GWDBLR4NS3B3KNK6PT77A7H37F/action/timestamp_anchor","attest_storage":"https://pith.science/pith/GWDBLR4NS3B3KNK6PT77A7H37F/action/storage_attestation","attest_author":"https://pith.science/pith/GWDBLR4NS3B3KNK6PT77A7H37F/action/author_attestation","sign_citation":"https://pith.science/pith/GWDBLR4NS3B3KNK6PT77A7H37F/action/citation_signature","submit_replication":"https://pith.science/pith/GWDBLR4NS3B3KNK6PT77A7H37F/action/replication_record"}},"created_at":"2026-05-18T01:18:37.610510+00:00","updated_at":"2026-05-18T01:18:37.610510+00:00"}