{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:FYNVPZOTD362GL4M5ZNDFRD5JY","short_pith_number":"pith:FYNVPZOT","schema_version":"1.0","canonical_sha256":"2e1b57e5d31efda32f8cee5a32c47d4e3596eb2c23155ada5557086d35638b85","source":{"kind":"arxiv","id":"2309.02920","version":2},"attestation_state":"computed","paper":{"title":"Determining the Baryon Impact on the Matter Power Spectrum with Galaxy Clusters","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Aurel Schneider, Giovanni Arico', Laila Linke, Sebastian Grandis","submitted_at":"2023-09-06T11:32:06Z","abstract_excerpt":"The redistribution of baryonic matter in massive halos through processes like active galactic nuclei feedback and star formation leads to a suppression of the matter power spectrum on small scales. This redistribution can be measured empirically via the gas and stellar mass fractions in galaxy clusters, and leaves imprints on their electron density profiles. We constrain two semi-analytical baryon correction models with a compilation of recent Bayesian population studies of galaxy groups and clusters sampling a mass range above $\\sim 3 \\times 10^{13}$ $M_\\odot$, and with cluster gas density pr"},"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":"2309.02920","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.CO","submitted_at":"2023-09-06T11:32:06Z","cross_cats_sorted":[],"title_canon_sha256":"2da9d23a619b350bac7d23cf9036867b1b29a50e177bf24482231c8de04151d4","abstract_canon_sha256":"98b91a1953d2ce1c332a04bfb513183bb90f4d033affcd47ba2fc6d1f614d075"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T07:55:24.137890Z","signature_b64":"OimyZp3AYGSWcEw1qajWiIgduHEh1YWQ7tIkaZFXhCe26YaVPC+6CgJVSvROq3DxZh8m0CmJFnfO7ZOpwdz3Cw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2e1b57e5d31efda32f8cee5a32c47d4e3596eb2c23155ada5557086d35638b85","last_reissued_at":"2026-07-05T07:55:24.137505Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T07:55:24.137505Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Determining the Baryon Impact on the Matter Power Spectrum with Galaxy Clusters","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Aurel Schneider, Giovanni Arico', Laila Linke, Sebastian Grandis","submitted_at":"2023-09-06T11:32:06Z","abstract_excerpt":"The redistribution of baryonic matter in massive halos through processes like active galactic nuclei feedback and star formation leads to a suppression of the matter power spectrum on small scales. This redistribution can be measured empirically via the gas and stellar mass fractions in galaxy clusters, and leaves imprints on their electron density profiles. We constrain two semi-analytical baryon correction models with a compilation of recent Bayesian population studies of galaxy groups and clusters sampling a mass range above $\\sim 3 \\times 10^{13}$ $M_\\odot$, and with cluster gas density pr"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2309.02920","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/2309.02920/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":"2309.02920","created_at":"2026-07-05T07:55:24.137564+00:00"},{"alias_kind":"arxiv_version","alias_value":"2309.02920v2","created_at":"2026-07-05T07:55:24.137564+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2309.02920","created_at":"2026-07-05T07:55:24.137564+00:00"},{"alias_kind":"pith_short_12","alias_value":"FYNVPZOTD362","created_at":"2026-07-05T07:55:24.137564+00:00"},{"alias_kind":"pith_short_16","alias_value":"FYNVPZOTD362GL4M","created_at":"2026-07-05T07:55:24.137564+00:00"},{"alias_kind":"pith_short_8","alias_value":"FYNVPZOT","created_at":"2026-07-05T07:55:24.137564+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.00818","citing_title":"$4\\times3$ Point Correlation Functions in Galaxy Surveys: Impact of Baryonic Feedback","ref_index":45,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/FYNVPZOTD362GL4M5ZNDFRD5JY","json":"https://pith.science/pith/FYNVPZOTD362GL4M5ZNDFRD5JY.json","graph_json":"https://pith.science/api/pith-number/FYNVPZOTD362GL4M5ZNDFRD5JY/graph.json","events_json":"https://pith.science/api/pith-number/FYNVPZOTD362GL4M5ZNDFRD5JY/events.json","paper":"https://pith.science/paper/FYNVPZOT"},"agent_actions":{"view_html":"https://pith.science/pith/FYNVPZOTD362GL4M5ZNDFRD5JY","download_json":"https://pith.science/pith/FYNVPZOTD362GL4M5ZNDFRD5JY.json","view_paper":"https://pith.science/paper/FYNVPZOT","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2309.02920&json=true","fetch_graph":"https://pith.science/api/pith-number/FYNVPZOTD362GL4M5ZNDFRD5JY/graph.json","fetch_events":"https://pith.science/api/pith-number/FYNVPZOTD362GL4M5ZNDFRD5JY/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/FYNVPZOTD362GL4M5ZNDFRD5JY/action/timestamp_anchor","attest_storage":"https://pith.science/pith/FYNVPZOTD362GL4M5ZNDFRD5JY/action/storage_attestation","attest_author":"https://pith.science/pith/FYNVPZOTD362GL4M5ZNDFRD5JY/action/author_attestation","sign_citation":"https://pith.science/pith/FYNVPZOTD362GL4M5ZNDFRD5JY/action/citation_signature","submit_replication":"https://pith.science/pith/FYNVPZOTD362GL4M5ZNDFRD5JY/action/replication_record"}},"created_at":"2026-07-05T07:55:24.137564+00:00","updated_at":"2026-07-05T07:55:24.137564+00:00"}