{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2001:LG4OZJBAVPW6JP6F63OV552HKO","short_pith_number":"pith:LG4OZJBA","schema_version":"1.0","canonical_sha256":"59b8eca420abede4bfc5f6dd5ef74753a70b1cc444fb0adeabb10db6dd2898d7","source":{"kind":"arxiv","id":"astro-ph/0103286","version":1},"attestation_state":"computed","paper":{"title":"Magnetic Field Diagnostics Based on Far-Infrared Polarimetry: Tests Using Numerical Simulations","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"E. G. Zweibel, F. Heitsch, M.L. Norman, M.-M. Mac Low, P.S. Li","submitted_at":"2001-03-18T15:35:46Z","abstract_excerpt":"The dynamical state of star-forming molecular clouds cannot be understood without determining the structure and strength of their magnetic fields. Measurements of polarized far-infrared radiation from thermally aligned dust grains are used to map the orientation of the field and estimate its strength, but the accuracy of the results has remained in doubt. In order to assess the reliability of this method, we apply it to simulated far-infrared polarization maps derived from three-dimensional simulations of supersonic magnetohydrodynamical turbulence, and compare the estimated values to the know"},"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/0103286","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2001-03-18T15:35:46Z","cross_cats_sorted":[],"title_canon_sha256":"66979a40ad42d220e583d051b9a0818f39b26296a2067b002258dafaf0fea88a","abstract_canon_sha256":"e3f963052bfdf6d60f08cf5a9480e15f866f623ffa82e07d4476e8ecc61c9282"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:22:53.465045Z","signature_b64":"dy9QDnl9kgtH1xy5fnABxXF9j2H2cDsL4Mjhb7zB9BSMsydhdabQIdx1/o5HpBXse6zP3mV591IOqw24qbfuAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"59b8eca420abede4bfc5f6dd5ef74753a70b1cc444fb0adeabb10db6dd2898d7","last_reissued_at":"2026-07-04T16:22:53.464602Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:22:53.464602Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Magnetic Field Diagnostics Based on Far-Infrared Polarimetry: Tests Using Numerical Simulations","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"E. G. Zweibel, F. Heitsch, M.L. Norman, M.-M. Mac Low, P.S. Li","submitted_at":"2001-03-18T15:35:46Z","abstract_excerpt":"The dynamical state of star-forming molecular clouds cannot be understood without determining the structure and strength of their magnetic fields. Measurements of polarized far-infrared radiation from thermally aligned dust grains are used to map the orientation of the field and estimate its strength, but the accuracy of the results has remained in doubt. In order to assess the reliability of this method, we apply it to simulated far-infrared polarization maps derived from three-dimensional simulations of supersonic magnetohydrodynamical turbulence, and compare the estimated values to the know"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0103286","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/astro-ph/0103286/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/0103286","created_at":"2026-07-04T16:22:53.464676+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0103286v1","created_at":"2026-07-04T16:22:53.464676+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0103286","created_at":"2026-07-04T16:22:53.464676+00:00"},{"alias_kind":"pith_short_12","alias_value":"LG4OZJBAVPW6","created_at":"2026-07-04T16:22:53.464676+00:00"},{"alias_kind":"pith_short_16","alias_value":"LG4OZJBAVPW6JP6F","created_at":"2026-07-04T16:22:53.464676+00:00"},{"alias_kind":"pith_short_8","alias_value":"LG4OZJBA","created_at":"2026-07-04T16:22:53.464676+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2606.02149","citing_title":"The magnetic field of the Milky Way: an observational perspective","ref_index":152,"is_internal_anchor":true},{"citing_arxiv_id":"2606.25077","citing_title":"Small-scale Magnetic Fields in the Milky Way and Nearby Galaxies","ref_index":50,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/LG4OZJBAVPW6JP6F63OV552HKO","json":"https://pith.science/pith/LG4OZJBAVPW6JP6F63OV552HKO.json","graph_json":"https://pith.science/api/pith-number/LG4OZJBAVPW6JP6F63OV552HKO/graph.json","events_json":"https://pith.science/api/pith-number/LG4OZJBAVPW6JP6F63OV552HKO/events.json","paper":"https://pith.science/paper/LG4OZJBA"},"agent_actions":{"view_html":"https://pith.science/pith/LG4OZJBAVPW6JP6F63OV552HKO","download_json":"https://pith.science/pith/LG4OZJBAVPW6JP6F63OV552HKO.json","view_paper":"https://pith.science/paper/LG4OZJBA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0103286&json=true","fetch_graph":"https://pith.science/api/pith-number/LG4OZJBAVPW6JP6F63OV552HKO/graph.json","fetch_events":"https://pith.science/api/pith-number/LG4OZJBAVPW6JP6F63OV552HKO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/LG4OZJBAVPW6JP6F63OV552HKO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/LG4OZJBAVPW6JP6F63OV552HKO/action/storage_attestation","attest_author":"https://pith.science/pith/LG4OZJBAVPW6JP6F63OV552HKO/action/author_attestation","sign_citation":"https://pith.science/pith/LG4OZJBAVPW6JP6F63OV552HKO/action/citation_signature","submit_replication":"https://pith.science/pith/LG4OZJBAVPW6JP6F63OV552HKO/action/replication_record"}},"created_at":"2026-07-04T16:22:53.464676+00:00","updated_at":"2026-07-04T16:22:53.464676+00:00"}