{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:EOUFO25ZPPRXNNHPRRNMRBVYDN","short_pith_number":"pith:EOUFO25Z","schema_version":"1.0","canonical_sha256":"23a8576bb97be376b4ef8c5ac886b81b6ae88f92db868c5450239a0862dfb03d","source":{"kind":"arxiv","id":"2004.03305","version":1},"attestation_state":"computed","paper":{"title":"Probing cosmic isotropy with a new X-ray galaxy cluster sample through the $L_{\\text{X}}-T$ scaling relation","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"F. Pacaud, G. Schellenberger, K. Migkas, L. Lovisari, M. E. Ramos-Ceja, T. H. Reiprich","submitted_at":"2020-04-07T12:19:26Z","abstract_excerpt":"The isotropy of the late Universe is an assumption greatly used in astronomy. However, many studies have recently reported deviations from isotropy with a definitive conclusion yet to be made. New, independent methods to robustly test the cosmic isotropy are of crucial importance. In this work, we investigate the directional behavior of the X-ray luminosity-temperature ($L_X-T$) relation of galaxy clusters. A tight correlation exists between the luminosity and temperature of the X-ray-emitting intracluster medium. While the measured luminosity depends on the underlying cosmology, the temperatu"},"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":"2004.03305","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2020-04-07T12:19:26Z","cross_cats_sorted":[],"title_canon_sha256":"112cbfdc2a1fe73f547523b7dde836d05a0ea64d765a5258a3f51699f9df5056","abstract_canon_sha256":"9d5bf61506b89c472ed71b15ba6d43d14265a66dc839bc6c268393940c9e81c8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:53:54.222158Z","signature_b64":"HTxRv1EEYZo2sQbL2S/rcL3CSlQgXO+3fWQvIvMhWC5JrCn98gSx77iUbxydQ8/9bAT2jrzFO4pU3kihX64ICQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"23a8576bb97be376b4ef8c5ac886b81b6ae88f92db868c5450239a0862dfb03d","last_reissued_at":"2026-07-05T00:53:54.221693Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:53:54.221693Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Probing cosmic isotropy with a new X-ray galaxy cluster sample through the $L_{\\text{X}}-T$ scaling relation","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"F. Pacaud, G. Schellenberger, K. Migkas, L. Lovisari, M. E. Ramos-Ceja, T. H. Reiprich","submitted_at":"2020-04-07T12:19:26Z","abstract_excerpt":"The isotropy of the late Universe is an assumption greatly used in astronomy. However, many studies have recently reported deviations from isotropy with a definitive conclusion yet to be made. New, independent methods to robustly test the cosmic isotropy are of crucial importance. In this work, we investigate the directional behavior of the X-ray luminosity-temperature ($L_X-T$) relation of galaxy clusters. A tight correlation exists between the luminosity and temperature of the X-ray-emitting intracluster medium. While the measured luminosity depends on the underlying cosmology, the temperatu"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2004.03305","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2004.03305/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":"2004.03305","created_at":"2026-07-05T00:53:54.221746+00:00"},{"alias_kind":"arxiv_version","alias_value":"2004.03305v1","created_at":"2026-07-05T00:53:54.221746+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2004.03305","created_at":"2026-07-05T00:53:54.221746+00:00"},{"alias_kind":"pith_short_12","alias_value":"EOUFO25ZPPRX","created_at":"2026-07-05T00:53:54.221746+00:00"},{"alias_kind":"pith_short_16","alias_value":"EOUFO25ZPPRXNNHP","created_at":"2026-07-05T00:53:54.221746+00:00"},{"alias_kind":"pith_short_8","alias_value":"EOUFO25Z","created_at":"2026-07-05T00:53:54.221746+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.07821","citing_title":"Multipolar structure of the local expansion rate from incomplete sky data","ref_index":65,"is_internal_anchor":true},{"citing_arxiv_id":"2512.02526","citing_title":"Updates on dipolar anisotropy in local measurements of the Hubble constant from Cosmicflows-4","ref_index":50,"is_internal_anchor":false},{"citing_arxiv_id":"2602.11093","citing_title":"New constraints on cosmic anisotropy from galaxy clusters using an improved dipole fitting method","ref_index":71,"is_internal_anchor":false},{"citing_arxiv_id":"2103.01183","citing_title":"In the Realm of the Hubble tension $-$ a Review of Solutions","ref_index":33,"is_internal_anchor":false},{"citing_arxiv_id":"2604.04408","citing_title":"Probing cosmic anisotropy with galaxy clusters and supernovae","ref_index":66,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/EOUFO25ZPPRXNNHPRRNMRBVYDN","json":"https://pith.science/pith/EOUFO25ZPPRXNNHPRRNMRBVYDN.json","graph_json":"https://pith.science/api/pith-number/EOUFO25ZPPRXNNHPRRNMRBVYDN/graph.json","events_json":"https://pith.science/api/pith-number/EOUFO25ZPPRXNNHPRRNMRBVYDN/events.json","paper":"https://pith.science/paper/EOUFO25Z"},"agent_actions":{"view_html":"https://pith.science/pith/EOUFO25ZPPRXNNHPRRNMRBVYDN","download_json":"https://pith.science/pith/EOUFO25ZPPRXNNHPRRNMRBVYDN.json","view_paper":"https://pith.science/paper/EOUFO25Z","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2004.03305&json=true","fetch_graph":"https://pith.science/api/pith-number/EOUFO25ZPPRXNNHPRRNMRBVYDN/graph.json","fetch_events":"https://pith.science/api/pith-number/EOUFO25ZPPRXNNHPRRNMRBVYDN/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/EOUFO25ZPPRXNNHPRRNMRBVYDN/action/timestamp_anchor","attest_storage":"https://pith.science/pith/EOUFO25ZPPRXNNHPRRNMRBVYDN/action/storage_attestation","attest_author":"https://pith.science/pith/EOUFO25ZPPRXNNHPRRNMRBVYDN/action/author_attestation","sign_citation":"https://pith.science/pith/EOUFO25ZPPRXNNHPRRNMRBVYDN/action/citation_signature","submit_replication":"https://pith.science/pith/EOUFO25ZPPRXNNHPRRNMRBVYDN/action/replication_record"}},"created_at":"2026-07-05T00:53:54.221746+00:00","updated_at":"2026-07-05T00:53:54.221746+00:00"}