{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:XRCG336GD72QMWNWVNOBTGDPHL","short_pith_number":"pith:XRCG336G","schema_version":"1.0","canonical_sha256":"bc446defc61ff50659b6ab5c19986f3ade69cfc223f6d83272f83c6dd702ae55","source":{"kind":"arxiv","id":"1712.03444","version":2},"attestation_state":"computed","paper":{"title":"The dipole anisotropy of AllWISE galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"J. Colin, M. Rameez, R. Mohayaee, S. Sarkar","submitted_at":"2017-12-09T21:59:54Z","abstract_excerpt":"We determine the dipole in the WISE galaxy catalogue. After reducing star contamination to <0.1% by rejecting sources with high apparent motion and those close to the Galactic plane, we eliminate low redshift sources to suppress the non-kinematic, clustering dipole. We remove sources within {\\pm}5{\\deg} of the super-galactic plane, as well as those within 1'' of 2MRS sources at redshift z < 0.03. We enforce cuts on the source angular extent to preferentially select distant ones. As we progress along these steps, the dipole converges in direction to within 5{\\deg} of the CMB dipole and its magn"},"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":"1712.03444","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2017-12-09T21:59:54Z","cross_cats_sorted":[],"title_canon_sha256":"b8f056cb2ee99695c49f344eb79cdf06300fac265c35a80e23ba94975cc8dfb0","abstract_canon_sha256":"61481648e95b0481731d367e57e199711a55be1fd3452a9d459be04a3edc01fc"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:17:23.990946Z","signature_b64":"yHRuYMfWpNkOohz2mLytrUfAeIuqb4LhuXYoXmhn4/Dmdk3pVmyW7shhgEO0nhBGhbg7gkRtbfYL4l4AWF4mAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"bc446defc61ff50659b6ab5c19986f3ade69cfc223f6d83272f83c6dd702ae55","last_reissued_at":"2026-05-18T00:17:23.990173Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:17:23.990173Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The dipole anisotropy of AllWISE galaxies","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"J. Colin, M. Rameez, R. Mohayaee, S. Sarkar","submitted_at":"2017-12-09T21:59:54Z","abstract_excerpt":"We determine the dipole in the WISE galaxy catalogue. After reducing star contamination to <0.1% by rejecting sources with high apparent motion and those close to the Galactic plane, we eliminate low redshift sources to suppress the non-kinematic, clustering dipole. We remove sources within {\\pm}5{\\deg} of the super-galactic plane, as well as those within 1'' of 2MRS sources at redshift z < 0.03. We enforce cuts on the source angular extent to preferentially select distant ones. As we progress along these steps, the dipole converges in direction to within 5{\\deg} of the CMB dipole and its magn"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1712.03444","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":"1712.03444","created_at":"2026-05-18T00:17:23.990331+00:00"},{"alias_kind":"arxiv_version","alias_value":"1712.03444v2","created_at":"2026-05-18T00:17:23.990331+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1712.03444","created_at":"2026-05-18T00:17:23.990331+00:00"},{"alias_kind":"pith_short_12","alias_value":"XRCG336GD72Q","created_at":"2026-05-18T12:31:56.362134+00:00"},{"alias_kind":"pith_short_16","alias_value":"XRCG336GD72QMWNW","created_at":"2026-05-18T12:31:56.362134+00:00"},{"alias_kind":"pith_short_8","alias_value":"XRCG336G","created_at":"2026-05-18T12:31:56.362134+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"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":97,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XRCG336GD72QMWNWVNOBTGDPHL","json":"https://pith.science/pith/XRCG336GD72QMWNWVNOBTGDPHL.json","graph_json":"https://pith.science/api/pith-number/XRCG336GD72QMWNWVNOBTGDPHL/graph.json","events_json":"https://pith.science/api/pith-number/XRCG336GD72QMWNWVNOBTGDPHL/events.json","paper":"https://pith.science/paper/XRCG336G"},"agent_actions":{"view_html":"https://pith.science/pith/XRCG336GD72QMWNWVNOBTGDPHL","download_json":"https://pith.science/pith/XRCG336GD72QMWNWVNOBTGDPHL.json","view_paper":"https://pith.science/paper/XRCG336G","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1712.03444&json=true","fetch_graph":"https://pith.science/api/pith-number/XRCG336GD72QMWNWVNOBTGDPHL/graph.json","fetch_events":"https://pith.science/api/pith-number/XRCG336GD72QMWNWVNOBTGDPHL/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XRCG336GD72QMWNWVNOBTGDPHL/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XRCG336GD72QMWNWVNOBTGDPHL/action/storage_attestation","attest_author":"https://pith.science/pith/XRCG336GD72QMWNWVNOBTGDPHL/action/author_attestation","sign_citation":"https://pith.science/pith/XRCG336GD72QMWNWVNOBTGDPHL/action/citation_signature","submit_replication":"https://pith.science/pith/XRCG336GD72QMWNWVNOBTGDPHL/action/replication_record"}},"created_at":"2026-05-18T00:17:23.990331+00:00","updated_at":"2026-05-18T00:17:23.990331+00:00"}