{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:CQBWROQ3NAJN4RIEH3XRZEEJQ5","short_pith_number":"pith:CQBWROQ3","schema_version":"1.0","canonical_sha256":"140368ba1b6812de45043eef1c908987467ce88ad32246ee97c45a6da478e036","source":{"kind":"arxiv","id":"1812.06981","version":2},"attestation_state":"computed","paper":{"title":"Observable tests of self-interacting dark matter in galaxy clusters: BCG wobbles in a constant density core","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ex"],"primary_cat":"astro-ph.CO","authors_text":"Andrew Robertson, David Harvey, Ian G. McCarthy, Richard Massey","submitted_at":"2018-12-17T19:00:01Z","abstract_excerpt":"Models of Cold Dark Matter predict that the distribution of dark matter in galaxy clusters should be cuspy, centrally concentrated. Constant density cores would be strong evidence for beyond-CDM physics, such as Self-Interacting Dark Matter (SIDM). An observable consequence would be oscillations of the Brightest Cluster Galaxy (BCG) in otherwise relaxed galaxy clusters. Offset BCGs have indeed been observed - but only interpreted via a simplified, analytic model of oscillations. We compare these observations to the BAHAMAS-SIDM suite of cosmological simulations, which include SIDM and a fully "},"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":"1812.06981","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2018-12-17T19:00:01Z","cross_cats_sorted":["hep-ex"],"title_canon_sha256":"01ce8d60bf29ed2c27c26e878d38e0acbb15c71849dd5e64ba6afaa367d85b09","abstract_canon_sha256":"bcaa1e4fe7cc1914bfb20b8e46dd9661af07087d2fc63238fb3c7fcd37a37a86"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:04:26.794272Z","signature_b64":"2kRSRHsV0zwX7BbeubkacnpDrnESkN7/9jgmSasMRtXhhACYA2z4xTMLO1oSpGDHssY6tKlZHLxnP41FyWvsDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"140368ba1b6812de45043eef1c908987467ce88ad32246ee97c45a6da478e036","last_reissued_at":"2026-07-05T00:04:26.793753Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:04:26.793753Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Observable tests of self-interacting dark matter in galaxy clusters: BCG wobbles in a constant density core","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ex"],"primary_cat":"astro-ph.CO","authors_text":"Andrew Robertson, David Harvey, Ian G. McCarthy, Richard Massey","submitted_at":"2018-12-17T19:00:01Z","abstract_excerpt":"Models of Cold Dark Matter predict that the distribution of dark matter in galaxy clusters should be cuspy, centrally concentrated. Constant density cores would be strong evidence for beyond-CDM physics, such as Self-Interacting Dark Matter (SIDM). An observable consequence would be oscillations of the Brightest Cluster Galaxy (BCG) in otherwise relaxed galaxy clusters. Offset BCGs have indeed been observed - but only interpreted via a simplified, analytic model of oscillations. We compare these observations to the BAHAMAS-SIDM suite of cosmological simulations, which include SIDM and a fully "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1812.06981","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/1812.06981/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":"1812.06981","created_at":"2026-07-05T00:04:26.793818+00:00"},{"alias_kind":"arxiv_version","alias_value":"1812.06981v2","created_at":"2026-07-05T00:04:26.793818+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1812.06981","created_at":"2026-07-05T00:04:26.793818+00:00"},{"alias_kind":"pith_short_12","alias_value":"CQBWROQ3NAJN","created_at":"2026-07-05T00:04:26.793818+00:00"},{"alias_kind":"pith_short_16","alias_value":"CQBWROQ3NAJN4RIE","created_at":"2026-07-05T00:04:26.793818+00:00"},{"alias_kind":"pith_short_8","alias_value":"CQBWROQ3","created_at":"2026-07-05T00:04:26.793818+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.07406","citing_title":"Dark Neutrons as Dark Matter: Collisions in Halos and Direct Detection from Dark CP Violation","ref_index":60,"is_internal_anchor":true},{"citing_arxiv_id":"2605.27513","citing_title":"Constraints on a Light Leptophilic Scalar from Dark-Sector Couplings","ref_index":74,"is_internal_anchor":false},{"citing_arxiv_id":"2605.22685","citing_title":"Dwarf Galaxy Constraints on Interacting Fermionic Dark Matter","ref_index":57,"is_internal_anchor":false},{"citing_arxiv_id":"2602.02678","citing_title":"Axion-Like Electrophilic Portal for Pion Dark Matter","ref_index":85,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/CQBWROQ3NAJN4RIEH3XRZEEJQ5","json":"https://pith.science/pith/CQBWROQ3NAJN4RIEH3XRZEEJQ5.json","graph_json":"https://pith.science/api/pith-number/CQBWROQ3NAJN4RIEH3XRZEEJQ5/graph.json","events_json":"https://pith.science/api/pith-number/CQBWROQ3NAJN4RIEH3XRZEEJQ5/events.json","paper":"https://pith.science/paper/CQBWROQ3"},"agent_actions":{"view_html":"https://pith.science/pith/CQBWROQ3NAJN4RIEH3XRZEEJQ5","download_json":"https://pith.science/pith/CQBWROQ3NAJN4RIEH3XRZEEJQ5.json","view_paper":"https://pith.science/paper/CQBWROQ3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1812.06981&json=true","fetch_graph":"https://pith.science/api/pith-number/CQBWROQ3NAJN4RIEH3XRZEEJQ5/graph.json","fetch_events":"https://pith.science/api/pith-number/CQBWROQ3NAJN4RIEH3XRZEEJQ5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/CQBWROQ3NAJN4RIEH3XRZEEJQ5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/CQBWROQ3NAJN4RIEH3XRZEEJQ5/action/storage_attestation","attest_author":"https://pith.science/pith/CQBWROQ3NAJN4RIEH3XRZEEJQ5/action/author_attestation","sign_citation":"https://pith.science/pith/CQBWROQ3NAJN4RIEH3XRZEEJQ5/action/citation_signature","submit_replication":"https://pith.science/pith/CQBWROQ3NAJN4RIEH3XRZEEJQ5/action/replication_record"}},"created_at":"2026-07-05T00:04:26.793818+00:00","updated_at":"2026-07-05T00:04:26.793818+00:00"}