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In hemisphere comparison method, we find the dipole direction is $(l = 37 \\pm 40^{\\circ}, b = 33 \\pm 16^{\\circ})$ with the maximum anisotropy level of $\\delta=0.136 {}^{+0.009}_{-0.005}$. From the dipole fitting method, we find that the magnitude of anisotropy is $A = (3.7 {}^{+2.5}_{-3.7}) \\times 10^{-4}$, and the direction of the dipole $(l = 329^{\\circ}{}^{+ 101^{\\circ}}_{-28^{\\circ}"},"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":"1805.09195","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2018-05-23T14:34:40Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"bfb5a0a994e40f718a2ce3e8a0fa55dd09351fd2086c84e58eee1b00b88f0f43","abstract_canon_sha256":"c9f8c19aa61500c2b54f6ecfeb6350e631d4f43fe62876c906b31ba134ead674"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:11:30.097390Z","signature_b64":"5+AnkGgPksPidJqDI9pDWhX0Bq2s95GNfEHMHa73l7xV77UCOs44wxGh78JkqRu9aN3LCksoNrai/GMDT5xUAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"52d990bde99f583fde9a3830ac59be6e66bdb9936a132827dc99d0ef8f749e24","last_reissued_at":"2026-05-18T00:11:30.096798Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:11:30.096798Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Testing the anisotropy of cosmic acceleration from Pantheon supernovae sample","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.CO","authors_text":"F. 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From the dipole fitting method, we find that the magnitude of anisotropy is $A = (3.7 {}^{+2.5}_{-3.7}) \\times 10^{-4}$, and the direction of the dipole $(l = 329^{\\circ}{}^{+ 101^{\\circ}}_{-28^{\\circ}"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1805.09195","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":"1805.09195","created_at":"2026-05-18T00:11:30.096893+00:00"},{"alias_kind":"arxiv_version","alias_value":"1805.09195v2","created_at":"2026-05-18T00:11:30.096893+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1805.09195","created_at":"2026-05-18T00:11:30.096893+00:00"},{"alias_kind":"pith_short_12","alias_value":"KLMZBPPJT5MD","created_at":"2026-05-18T12:32:33.847187+00:00"},{"alias_kind":"pith_short_16","alias_value":"KLMZBPPJT5MD7XU2","created_at":"2026-05-18T12:32:33.847187+00:00"},{"alias_kind":"pith_short_8","alias_value":"KLMZBPPJ","created_at":"2026-05-18T12:32:33.847187+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2602.11093","citing_title":"New constraints on cosmic anisotropy from galaxy clusters using an improved dipole fitting method","ref_index":128,"is_internal_anchor":true},{"citing_arxiv_id":"2604.04408","citing_title":"Probing cosmic anisotropy with galaxy clusters and supernovae","ref_index":56,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/KLMZBPPJT5MD7XU2HAYKYWN6NZ","json":"https://pith.science/pith/KLMZBPPJT5MD7XU2HAYKYWN6NZ.json","graph_json":"https://pith.science/api/pith-number/KLMZBPPJT5MD7XU2HAYKYWN6NZ/graph.json","events_json":"https://pith.science/api/pith-number/KLMZBPPJT5MD7XU2HAYKYWN6NZ/events.json","paper":"https://pith.science/paper/KLMZBPPJ"},"agent_actions":{"view_html":"https://pith.science/pith/KLMZBPPJT5MD7XU2HAYKYWN6NZ","download_json":"https://pith.science/pith/KLMZBPPJT5MD7XU2HAYKYWN6NZ.json","view_paper":"https://pith.science/paper/KLMZBPPJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1805.09195&json=true","fetch_graph":"https://pith.science/api/pith-number/KLMZBPPJT5MD7XU2HAYKYWN6NZ/graph.json","fetch_events":"https://pith.science/api/pith-number/KLMZBPPJT5MD7XU2HAYKYWN6NZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/KLMZBPPJT5MD7XU2HAYKYWN6NZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/KLMZBPPJT5MD7XU2HAYKYWN6NZ/action/storage_attestation","attest_author":"https://pith.science/pith/KLMZBPPJT5MD7XU2HAYKYWN6NZ/action/author_attestation","sign_citation":"https://pith.science/pith/KLMZBPPJT5MD7XU2HAYKYWN6NZ/action/citation_signature","submit_replication":"https://pith.science/pith/KLMZBPPJT5MD7XU2HAYKYWN6NZ/action/replication_record"}},"created_at":"2026-05-18T00:11:30.096893+00:00","updated_at":"2026-05-18T00:11:30.096893+00:00"}