{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2003:7HJZJ3WX3GYYLWXQEW6QEC2KY5","short_pith_number":"pith:7HJZJ3WX","schema_version":"1.0","canonical_sha256":"f9d394eed7d9b185daf025bd020b4ac75519f6098805b75f3106e5455089e206","source":{"kind":"arxiv","id":"astro-ph/0305604","version":2},"attestation_state":"computed","paper":{"title":"SCUBA Polarization Measurements of the Magnetic Field Strengths in the L183, L1544, and L43 Prestellar Cores","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"D. J. Nutter, D. Ward-Thompson, J. M. Kirk, R. M. Crutcher","submitted_at":"2003-05-30T18:12:58Z","abstract_excerpt":"We have mapped linearly polarized dust emission from L183 with the JCMT SCUBA polarimeter and have analyzed these and our previously published data for the prestellar cores L183, L1544, and L43 in order to estimate magnetic field strengths in the plane of the sky, $B_{pos}$. The analysis used the Chandrasekhar-Fermi technique, which relates the dispersion in polarization position angles to $B_{pos}$. We have used these estimates of the field strengths (neglecting the unmeasured line-of-sight component) to find the mass-to-magnetic flux ratios $\\lambda$ (in units of the critical ratio for magne"},"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/0305604","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2003-05-30T18:12:58Z","cross_cats_sorted":[],"title_canon_sha256":"03e4c84e24064a4a62684d39636389a46ab64c6d737dd321d768e8d72763e991","abstract_canon_sha256":"d398495acdc31aab3652ae4575feba8b613adf71bcbd63341837c05146703128"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:37:13.703974Z","signature_b64":"Sa2gJ6MwY7PX68Rf2ZLnnhn17r2U1Utc+dtAqUqKAgCDF+MQHMLptgRZ8R9ui0Y9R3SEyF6rQaf5VX7UygvACg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"f9d394eed7d9b185daf025bd020b4ac75519f6098805b75f3106e5455089e206","last_reissued_at":"2026-07-04T16:37:13.703498Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:37:13.703498Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"SCUBA Polarization Measurements of the Magnetic Field Strengths in the L183, L1544, and L43 Prestellar Cores","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"D. J. Nutter, D. Ward-Thompson, J. M. Kirk, R. M. Crutcher","submitted_at":"2003-05-30T18:12:58Z","abstract_excerpt":"We have mapped linearly polarized dust emission from L183 with the JCMT SCUBA polarimeter and have analyzed these and our previously published data for the prestellar cores L183, L1544, and L43 in order to estimate magnetic field strengths in the plane of the sky, $B_{pos}$. The analysis used the Chandrasekhar-Fermi technique, which relates the dispersion in polarization position angles to $B_{pos}$. We have used these estimates of the field strengths (neglecting the unmeasured line-of-sight component) to find the mass-to-magnetic flux ratios $\\lambda$ (in units of the critical ratio for magne"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0305604","kind":"arxiv","version":2},"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/0305604/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/0305604","created_at":"2026-07-04T16:37:13.703584+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0305604v2","created_at":"2026-07-04T16:37:13.703584+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0305604","created_at":"2026-07-04T16:37:13.703584+00:00"},{"alias_kind":"pith_short_12","alias_value":"7HJZJ3WX3GYY","created_at":"2026-07-04T16:37:13.703584+00:00"},{"alias_kind":"pith_short_16","alias_value":"7HJZJ3WX3GYYLWXQ","created_at":"2026-07-04T16:37:13.703584+00:00"},{"alias_kind":"pith_short_8","alias_value":"7HJZJ3WX","created_at":"2026-07-04T16:37:13.703584+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2606.13123","citing_title":"Grain alignment and dust evolution physics with polarisation (GRADE-POL). II. On the physical basis of Serkowski and super-Serkowski polarisation spectra","ref_index":102,"is_internal_anchor":true},{"citing_arxiv_id":"2606.22090","citing_title":"Measuring Magnetic Field Strengths in Galactic Star-forming Regions via the Zeeman Effect with the SKA","ref_index":51,"is_internal_anchor":true},{"citing_arxiv_id":"2606.23802","citing_title":"Characterising magnetic fields at the onset of star cluster formation: From giant molecular clouds to infrared dark clumps","ref_index":75,"is_internal_anchor":true},{"citing_arxiv_id":"2605.17708","citing_title":"BISTRO Survey: Gravity-Dominated and Magnetically Regulated Star Formation in M17 SW","ref_index":59,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/7HJZJ3WX3GYYLWXQEW6QEC2KY5","json":"https://pith.science/pith/7HJZJ3WX3GYYLWXQEW6QEC2KY5.json","graph_json":"https://pith.science/api/pith-number/7HJZJ3WX3GYYLWXQEW6QEC2KY5/graph.json","events_json":"https://pith.science/api/pith-number/7HJZJ3WX3GYYLWXQEW6QEC2KY5/events.json","paper":"https://pith.science/paper/7HJZJ3WX"},"agent_actions":{"view_html":"https://pith.science/pith/7HJZJ3WX3GYYLWXQEW6QEC2KY5","download_json":"https://pith.science/pith/7HJZJ3WX3GYYLWXQEW6QEC2KY5.json","view_paper":"https://pith.science/paper/7HJZJ3WX","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0305604&json=true","fetch_graph":"https://pith.science/api/pith-number/7HJZJ3WX3GYYLWXQEW6QEC2KY5/graph.json","fetch_events":"https://pith.science/api/pith-number/7HJZJ3WX3GYYLWXQEW6QEC2KY5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/7HJZJ3WX3GYYLWXQEW6QEC2KY5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/7HJZJ3WX3GYYLWXQEW6QEC2KY5/action/storage_attestation","attest_author":"https://pith.science/pith/7HJZJ3WX3GYYLWXQEW6QEC2KY5/action/author_attestation","sign_citation":"https://pith.science/pith/7HJZJ3WX3GYYLWXQEW6QEC2KY5/action/citation_signature","submit_replication":"https://pith.science/pith/7HJZJ3WX3GYYLWXQEW6QEC2KY5/action/replication_record"}},"created_at":"2026-07-04T16:37:13.703584+00:00","updated_at":"2026-07-04T16:37:13.703584+00:00"}