{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:W4IE6YL5Y5QCCMWZYLM6FNNN7Y","short_pith_number":"pith:W4IE6YL5","schema_version":"1.0","canonical_sha256":"b7104f617dc7602132d9c2d9e2b5adfe34cbdca0f5c20e8c83c090ddabe66aed","source":{"kind":"arxiv","id":"2005.12921","version":2},"attestation_state":"computed","paper":{"title":"Outflows, cores and magnetic field orientations in W43-MM1 as seen by ALMA","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"C. Arce-Tord, C. L. H. Hull, F. Louvet, F. Motte, G. Garay, L. Bronfman, P. C. Cortes, P. Didelon, T. Nony, V. J. M. Le Gouellec","submitted_at":"2020-05-26T18:00:01Z","abstract_excerpt":"It has been proposed that the magnetic field, pervasive in the ISM, plays an important role in the process of massive star formation. To better understand its impact at the pre and protostellar stages, high-angular resolution observations of polarized dust emission toward a large sample of massive dense cores are needed. To this end, we used the Atacama Large Millimeter Array in Band 6 (1.3 mm) in full polarization mode to map the polarized emission from dust grains at a physical scale of $\\sim$2700 au in the massive protocluster W43-MM1. We used these data to measure the orientation of the ma"},"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":"2005.12921","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2020-05-26T18:00:01Z","cross_cats_sorted":[],"title_canon_sha256":"83088caf74eb13110d65d0620cd4343cf464e57f5caf866042774c6786166dda","abstract_canon_sha256":"8fbf1ea09362c19aef861a268f124f9aec266c1b8caa0b685108f78cd379950c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T01:38:37.532852Z","signature_b64":"d4HYomjRN7yjsFbOoXjRL+JGd6P/O2mg1DMc6NAFZpV6HCfrtDpKy7D5VMttBZ4smVXfmIkdo9dOqSQqDCoHCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b7104f617dc7602132d9c2d9e2b5adfe34cbdca0f5c20e8c83c090ddabe66aed","last_reissued_at":"2026-07-05T01:38:37.532404Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T01:38:37.532404Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Outflows, cores and magnetic field orientations in W43-MM1 as seen by ALMA","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"C. Arce-Tord, C. L. H. Hull, F. Louvet, F. Motte, G. Garay, L. Bronfman, P. C. Cortes, P. Didelon, T. Nony, V. J. M. Le Gouellec","submitted_at":"2020-05-26T18:00:01Z","abstract_excerpt":"It has been proposed that the magnetic field, pervasive in the ISM, plays an important role in the process of massive star formation. To better understand its impact at the pre and protostellar stages, high-angular resolution observations of polarized dust emission toward a large sample of massive dense cores are needed. To this end, we used the Atacama Large Millimeter Array in Band 6 (1.3 mm) in full polarization mode to map the polarized emission from dust grains at a physical scale of $\\sim$2700 au in the massive protocluster W43-MM1. We used these data to measure the orientation of the ma"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2005.12921","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/2005.12921/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":"2005.12921","created_at":"2026-07-05T01:38:37.532471+00:00"},{"alias_kind":"arxiv_version","alias_value":"2005.12921v2","created_at":"2026-07-05T01:38:37.532471+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2005.12921","created_at":"2026-07-05T01:38:37.532471+00:00"},{"alias_kind":"pith_short_12","alias_value":"W4IE6YL5Y5QC","created_at":"2026-07-05T01:38:37.532471+00:00"},{"alias_kind":"pith_short_16","alias_value":"W4IE6YL5Y5QCCMWZ","created_at":"2026-07-05T01:38:37.532471+00:00"},{"alias_kind":"pith_short_8","alias_value":"W4IE6YL5","created_at":"2026-07-05T01:38:37.532471+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.10029","citing_title":"Challenges in probing turbulent and magnetic support in cores: the W43-MM1 protocluster case study","ref_index":154,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/W4IE6YL5Y5QCCMWZYLM6FNNN7Y","json":"https://pith.science/pith/W4IE6YL5Y5QCCMWZYLM6FNNN7Y.json","graph_json":"https://pith.science/api/pith-number/W4IE6YL5Y5QCCMWZYLM6FNNN7Y/graph.json","events_json":"https://pith.science/api/pith-number/W4IE6YL5Y5QCCMWZYLM6FNNN7Y/events.json","paper":"https://pith.science/paper/W4IE6YL5"},"agent_actions":{"view_html":"https://pith.science/pith/W4IE6YL5Y5QCCMWZYLM6FNNN7Y","download_json":"https://pith.science/pith/W4IE6YL5Y5QCCMWZYLM6FNNN7Y.json","view_paper":"https://pith.science/paper/W4IE6YL5","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2005.12921&json=true","fetch_graph":"https://pith.science/api/pith-number/W4IE6YL5Y5QCCMWZYLM6FNNN7Y/graph.json","fetch_events":"https://pith.science/api/pith-number/W4IE6YL5Y5QCCMWZYLM6FNNN7Y/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/W4IE6YL5Y5QCCMWZYLM6FNNN7Y/action/timestamp_anchor","attest_storage":"https://pith.science/pith/W4IE6YL5Y5QCCMWZYLM6FNNN7Y/action/storage_attestation","attest_author":"https://pith.science/pith/W4IE6YL5Y5QCCMWZYLM6FNNN7Y/action/author_attestation","sign_citation":"https://pith.science/pith/W4IE6YL5Y5QCCMWZYLM6FNNN7Y/action/citation_signature","submit_replication":"https://pith.science/pith/W4IE6YL5Y5QCCMWZYLM6FNNN7Y/action/replication_record"}},"created_at":"2026-07-05T01:38:37.532471+00:00","updated_at":"2026-07-05T01:38:37.532471+00:00"}