{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:LK76NKZJSPBG4P56WDDNVXVQBB","short_pith_number":"pith:LK76NKZJ","schema_version":"1.0","canonical_sha256":"5abfe6ab2993c26e3fbeb0c6dadeb00845a93d585e91401de52de705bcae5a87","source":{"kind":"arxiv","id":"1302.0143","version":2},"attestation_state":"computed","paper":{"title":"Comparing Polarised Synchrotron and Thermal Dust Emission in the Galactic Plane","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. J. Banday, A. W. Strong, C. Combet, E. Falgarone, E. Orlando, J. F. Mac\\'ias-P\\'erez, K. M. Ferri\\`ere, L. Fauvet, T. R. Jaffe","submitted_at":"2013-02-01T11:14:08Z","abstract_excerpt":"As the next step toward an improved large scale Galactic magnetic field model, we present a simple comparison of polarised synchrotron and thermal dust emission on the Galactic plane. We find that the field configuration in our previous model that reproduces the polarised synchrotron is not compatible with the WMAP 94 GHz polarised emission data. In particular, the high degree of dust polarisation in the outer Galaxy (90deg < l < 270deg) implies that the fields in the dust-emitting regions are more ordered than the average of synchrotron-emitting regions. This new dust information allows us to"},"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":"1302.0143","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2013-02-01T11:14:08Z","cross_cats_sorted":[],"title_canon_sha256":"4bbdc1de6c83aa6581eaf43fcef2377b02e6ed3b317ff00023fc256dcdb59fc7","abstract_canon_sha256":"2e8b9f41bb085e167e3c97f0f936506ee84472f3f1222850445332c63767d9cd"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:23:02.347758Z","signature_b64":"U6uemotUHs+9XlbigxmYtjXVXef/wxpHutNJRIw9dbyIUx6Dr5bnU0uuvR6w7Mr0lXN8KRL43tJGwxFdrZmLCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"5abfe6ab2993c26e3fbeb0c6dadeb00845a93d585e91401de52de705bcae5a87","last_reissued_at":"2026-05-18T00:23:02.347225Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:23:02.347225Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Comparing Polarised Synchrotron and Thermal Dust Emission in the Galactic Plane","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"A. J. Banday, A. W. Strong, C. Combet, E. Falgarone, E. Orlando, J. F. Mac\\'ias-P\\'erez, K. M. Ferri\\`ere, L. Fauvet, T. R. Jaffe","submitted_at":"2013-02-01T11:14:08Z","abstract_excerpt":"As the next step toward an improved large scale Galactic magnetic field model, we present a simple comparison of polarised synchrotron and thermal dust emission on the Galactic plane. We find that the field configuration in our previous model that reproduces the polarised synchrotron is not compatible with the WMAP 94 GHz polarised emission data. In particular, the high degree of dust polarisation in the outer Galaxy (90deg < l < 270deg) implies that the fields in the dust-emitting regions are more ordered than the average of synchrotron-emitting regions. This new dust information allows us to"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1302.0143","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":""},"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":"1302.0143","created_at":"2026-05-18T00:23:02.347310+00:00"},{"alias_kind":"arxiv_version","alias_value":"1302.0143v2","created_at":"2026-05-18T00:23:02.347310+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1302.0143","created_at":"2026-05-18T00:23:02.347310+00:00"},{"alias_kind":"pith_short_12","alias_value":"LK76NKZJSPBG","created_at":"2026-05-18T12:27:51.066281+00:00"},{"alias_kind":"pith_short_16","alias_value":"LK76NKZJSPBG4P56","created_at":"2026-05-18T12:27:51.066281+00:00"},{"alias_kind":"pith_short_8","alias_value":"LK76NKZJ","created_at":"2026-05-18T12:27:51.066281+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":175,"is_internal_anchor":true},{"citing_arxiv_id":"2601.19386","citing_title":"Constraints on Primordial Black Holes from Galactic Diffuse Synchrotron Emissions","ref_index":153,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/LK76NKZJSPBG4P56WDDNVXVQBB","json":"https://pith.science/pith/LK76NKZJSPBG4P56WDDNVXVQBB.json","graph_json":"https://pith.science/api/pith-number/LK76NKZJSPBG4P56WDDNVXVQBB/graph.json","events_json":"https://pith.science/api/pith-number/LK76NKZJSPBG4P56WDDNVXVQBB/events.json","paper":"https://pith.science/paper/LK76NKZJ"},"agent_actions":{"view_html":"https://pith.science/pith/LK76NKZJSPBG4P56WDDNVXVQBB","download_json":"https://pith.science/pith/LK76NKZJSPBG4P56WDDNVXVQBB.json","view_paper":"https://pith.science/paper/LK76NKZJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1302.0143&json=true","fetch_graph":"https://pith.science/api/pith-number/LK76NKZJSPBG4P56WDDNVXVQBB/graph.json","fetch_events":"https://pith.science/api/pith-number/LK76NKZJSPBG4P56WDDNVXVQBB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/LK76NKZJSPBG4P56WDDNVXVQBB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/LK76NKZJSPBG4P56WDDNVXVQBB/action/storage_attestation","attest_author":"https://pith.science/pith/LK76NKZJSPBG4P56WDDNVXVQBB/action/author_attestation","sign_citation":"https://pith.science/pith/LK76NKZJSPBG4P56WDDNVXVQBB/action/citation_signature","submit_replication":"https://pith.science/pith/LK76NKZJSPBG4P56WDDNVXVQBB/action/replication_record"}},"created_at":"2026-05-18T00:23:02.347310+00:00","updated_at":"2026-05-18T00:23:02.347310+00:00"}