{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:RD5Z7MQ4OKJOXQ3OPA43VO7LES","short_pith_number":"pith:RD5Z7MQ4","schema_version":"1.0","canonical_sha256":"88fb9fb21c7292ebc36e7839babbeb249db34f18407819d34ce5885cb318cddf","source":{"kind":"arxiv","id":"1805.01242","version":1},"attestation_state":"computed","paper":{"title":"A Model for Anisotropic Interstellar Scattering and its Application to Sgr A*","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Dimitrios Psaltis, Geoff Bower, Lia Medeiros, Lindy Blackburn, Michael Johnson, Ramesh Narayan","submitted_at":"2018-05-03T11:56:47Z","abstract_excerpt":"Scattering in the ionized interstellar medium is commonly observed to be anisotropic, with theories of magnetohydrodynamic (MHD) turbulence explaining the anisotropy through a preferred magnetic field direction throughout the scattering regions. In particular, the line of sight to the Galactic Center supermassive black hole, Sgr A*, exhibits strong and anisotropic scattering, which dominates its observed size at wavelengths of a few millimeters and longer. Therefore, inferences of the intrinsic structure of \\sgra\\ at these wavelengths are sensitive to the assumed scattering model. In addition,"},"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":"1805.01242","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2018-05-03T11:56:47Z","cross_cats_sorted":[],"title_canon_sha256":"826e5e64bfc45ee2794f7d5f7e948e928789c0a5e801572d1004def3011da4fd","abstract_canon_sha256":"54ceca116075ef5f10f863a94528aeea3e3ccf9e8cb52ed0434e5f3c61419f54"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:16:52.090219Z","signature_b64":"QW+DfFZi+IXbV4ab/jWS8UnIpxvYmeU1LnoLhC6iYujB5zqLnkOcXoEVG07QU41NMV8dDp1mojm0iJf+WngrBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"88fb9fb21c7292ebc36e7839babbeb249db34f18407819d34ce5885cb318cddf","last_reissued_at":"2026-05-18T00:16:52.089525Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:16:52.089525Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A Model for Anisotropic Interstellar Scattering and its Application to Sgr A*","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Dimitrios Psaltis, Geoff Bower, Lia Medeiros, Lindy Blackburn, Michael Johnson, Ramesh Narayan","submitted_at":"2018-05-03T11:56:47Z","abstract_excerpt":"Scattering in the ionized interstellar medium is commonly observed to be anisotropic, with theories of magnetohydrodynamic (MHD) turbulence explaining the anisotropy through a preferred magnetic field direction throughout the scattering regions. In particular, the line of sight to the Galactic Center supermassive black hole, Sgr A*, exhibits strong and anisotropic scattering, which dominates its observed size at wavelengths of a few millimeters and longer. Therefore, inferences of the intrinsic structure of \\sgra\\ at these wavelengths are sensitive to the assumed scattering model. In addition,"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1805.01242","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":"1805.01242","created_at":"2026-05-18T00:16:52.089655+00:00"},{"alias_kind":"arxiv_version","alias_value":"1805.01242v1","created_at":"2026-05-18T00:16:52.089655+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1805.01242","created_at":"2026-05-18T00:16:52.089655+00:00"},{"alias_kind":"pith_short_12","alias_value":"RD5Z7MQ4OKJO","created_at":"2026-05-18T12:32:50.500415+00:00"},{"alias_kind":"pith_short_16","alias_value":"RD5Z7MQ4OKJOXQ3O","created_at":"2026-05-18T12:32:50.500415+00:00"},{"alias_kind":"pith_short_8","alias_value":"RD5Z7MQ4","created_at":"2026-05-18T12:32:50.500415+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"1906.11239","citing_title":"First M87 Event Horizon Telescope Results. II. Array and Instrumentation","ref_index":91,"is_internal_anchor":true},{"citing_arxiv_id":"2604.22638","citing_title":"Variability of Sagittarius A* at 3 GHz on minute-scale with MeerKAT","ref_index":1,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/RD5Z7MQ4OKJOXQ3OPA43VO7LES","json":"https://pith.science/pith/RD5Z7MQ4OKJOXQ3OPA43VO7LES.json","graph_json":"https://pith.science/api/pith-number/RD5Z7MQ4OKJOXQ3OPA43VO7LES/graph.json","events_json":"https://pith.science/api/pith-number/RD5Z7MQ4OKJOXQ3OPA43VO7LES/events.json","paper":"https://pith.science/paper/RD5Z7MQ4"},"agent_actions":{"view_html":"https://pith.science/pith/RD5Z7MQ4OKJOXQ3OPA43VO7LES","download_json":"https://pith.science/pith/RD5Z7MQ4OKJOXQ3OPA43VO7LES.json","view_paper":"https://pith.science/paper/RD5Z7MQ4","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1805.01242&json=true","fetch_graph":"https://pith.science/api/pith-number/RD5Z7MQ4OKJOXQ3OPA43VO7LES/graph.json","fetch_events":"https://pith.science/api/pith-number/RD5Z7MQ4OKJOXQ3OPA43VO7LES/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/RD5Z7MQ4OKJOXQ3OPA43VO7LES/action/timestamp_anchor","attest_storage":"https://pith.science/pith/RD5Z7MQ4OKJOXQ3OPA43VO7LES/action/storage_attestation","attest_author":"https://pith.science/pith/RD5Z7MQ4OKJOXQ3OPA43VO7LES/action/author_attestation","sign_citation":"https://pith.science/pith/RD5Z7MQ4OKJOXQ3OPA43VO7LES/action/citation_signature","submit_replication":"https://pith.science/pith/RD5Z7MQ4OKJOXQ3OPA43VO7LES/action/replication_record"}},"created_at":"2026-05-18T00:16:52.089655+00:00","updated_at":"2026-05-18T00:16:52.089655+00:00"}