{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:7ZCYNDOQ6XHUZSLHWSSIL5ZPKO","short_pith_number":"pith:7ZCYNDOQ","schema_version":"1.0","canonical_sha256":"fe45868dd0f5cf4cc967b4a485f72f5389a72558a2a9324560d3b89ece48be7b","source":{"kind":"arxiv","id":"2507.01820","version":1},"attestation_state":"computed","paper":{"title":"The Cosmological analysis of X-ray cluster surveys VII. Bypassing scaling relations with Lagrangian Deep Learning and Simulation-based inference","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Fran\\c{c}ois Lanusse, Marguerite Pierre, Nicolas Cerardi, Xavier Corap","submitted_at":"2025-07-02T15:36:12Z","abstract_excerpt":"Galaxy clusters, the pinnacle of structure formation in our universe, are a powerful cosmological probe. Several approaches have been proposed to express cluster number counts, but all these methods rely on empirical explicit scaling relations that link observed properties to the total cluster mass. These scaling relations are over-parametrised, inducing some degeneracy with cosmology. Moreover, they do not provide a direct handle on the numerous non-gravitational phenomena that affect the physics of the intra-cluster medium. We present a proof-of-concept to model cluster number counts, that b"},"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":"2507.01820","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.CO","submitted_at":"2025-07-02T15:36:12Z","cross_cats_sorted":[],"title_canon_sha256":"c330c97048cb200d9a0094f06cfed2a52bfa36f66b843dfe932033698e6cab58","abstract_canon_sha256":"70a0abc5d0706f81eac9f02b01095f67e74599a379224eed9fbfadecaa110989"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T12:07:39.283741Z","signature_b64":"WC9zwj35Kt8LDjYyLt8rQqMImAi/cklXeWyBv0vmeiq3FtBVtB7pKC9dLw2Nm6TBVTmOgM3pOxBCamNqgmbFBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"fe45868dd0f5cf4cc967b4a485f72f5389a72558a2a9324560d3b89ece48be7b","last_reissued_at":"2026-07-05T12:07:39.283201Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T12:07:39.283201Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Cosmological analysis of X-ray cluster surveys VII. Bypassing scaling relations with Lagrangian Deep Learning and Simulation-based inference","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Fran\\c{c}ois Lanusse, Marguerite Pierre, Nicolas Cerardi, Xavier Corap","submitted_at":"2025-07-02T15:36:12Z","abstract_excerpt":"Galaxy clusters, the pinnacle of structure formation in our universe, are a powerful cosmological probe. Several approaches have been proposed to express cluster number counts, but all these methods rely on empirical explicit scaling relations that link observed properties to the total cluster mass. These scaling relations are over-parametrised, inducing some degeneracy with cosmology. Moreover, they do not provide a direct handle on the numerous non-gravitational phenomena that affect the physics of the intra-cluster medium. We present a proof-of-concept to model cluster number counts, that b"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2507.01820","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/2507.01820/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":"2507.01820","created_at":"2026-07-05T12:07:39.283259+00:00"},{"alias_kind":"arxiv_version","alias_value":"2507.01820v1","created_at":"2026-07-05T12:07:39.283259+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2507.01820","created_at":"2026-07-05T12:07:39.283259+00:00"},{"alias_kind":"pith_short_12","alias_value":"7ZCYNDOQ6XHU","created_at":"2026-07-05T12:07:39.283259+00:00"},{"alias_kind":"pith_short_16","alias_value":"7ZCYNDOQ6XHUZSLH","created_at":"2026-07-05T12:07:39.283259+00:00"},{"alias_kind":"pith_short_8","alias_value":"7ZCYNDOQ","created_at":"2026-07-05T12:07:39.283259+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.30459","citing_title":"Cosmology-dependent covariance in galaxy cluster number counts: consequences for parameter inference","ref_index":34,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/7ZCYNDOQ6XHUZSLHWSSIL5ZPKO","json":"https://pith.science/pith/7ZCYNDOQ6XHUZSLHWSSIL5ZPKO.json","graph_json":"https://pith.science/api/pith-number/7ZCYNDOQ6XHUZSLHWSSIL5ZPKO/graph.json","events_json":"https://pith.science/api/pith-number/7ZCYNDOQ6XHUZSLHWSSIL5ZPKO/events.json","paper":"https://pith.science/paper/7ZCYNDOQ"},"agent_actions":{"view_html":"https://pith.science/pith/7ZCYNDOQ6XHUZSLHWSSIL5ZPKO","download_json":"https://pith.science/pith/7ZCYNDOQ6XHUZSLHWSSIL5ZPKO.json","view_paper":"https://pith.science/paper/7ZCYNDOQ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2507.01820&json=true","fetch_graph":"https://pith.science/api/pith-number/7ZCYNDOQ6XHUZSLHWSSIL5ZPKO/graph.json","fetch_events":"https://pith.science/api/pith-number/7ZCYNDOQ6XHUZSLHWSSIL5ZPKO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/7ZCYNDOQ6XHUZSLHWSSIL5ZPKO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/7ZCYNDOQ6XHUZSLHWSSIL5ZPKO/action/storage_attestation","attest_author":"https://pith.science/pith/7ZCYNDOQ6XHUZSLHWSSIL5ZPKO/action/author_attestation","sign_citation":"https://pith.science/pith/7ZCYNDOQ6XHUZSLHWSSIL5ZPKO/action/citation_signature","submit_replication":"https://pith.science/pith/7ZCYNDOQ6XHUZSLHWSSIL5ZPKO/action/replication_record"}},"created_at":"2026-07-05T12:07:39.283259+00:00","updated_at":"2026-07-05T12:07:39.283259+00:00"}