{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:RVU2UFLEEUZO2OXK6LOIRMQ5TG","short_pith_number":"pith:RVU2UFLE","schema_version":"1.0","canonical_sha256":"8d69aa15642532ed3aeaf2dc88b21d99898ec855ff91e2a9c080ae1e76ba378d","source":{"kind":"arxiv","id":"2505.08275","version":2},"attestation_state":"computed","paper":{"title":"Statistics of Gas Density, Velocity, and Magnetic Fields in Cool-Core Galaxy Clusters","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.GA","authors_text":"Alex Lazarian, G. Brunetti, John A. ZuHone, Yue Hu","submitted_at":"2025-05-13T06:40:11Z","abstract_excerpt":"Understanding turbulence within the Intracluster Medium (ICM) of galaxy clusters is pivotal for comprehending their evolution and dynamics. Employing 3D magnetohydrodynamic (MHD) simulations of galaxy cluster mergers, we examine the statistical properties of gas density, magnetic fields, and velocity, particularly emphasizing the central regions spanning 400 kpc. The simulations are designed to resemble massive cool-core clusters such as Perseus, while varying the initial plasma $\\beta$ values (100, 200, and 500). Our findings indicate that while the statistical histogram distributions of gas "},"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":"2505.08275","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2025-05-13T06:40:11Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"d2e4ea8b3efd8ae179453222b1fce97ff7ccfbf1a8ce09f712b481f577f2b488","abstract_canon_sha256":"ec03de5db3a1c5ebba0dae025563917d10dc5a6df95db29ef8f67bdf49b90b64"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T11:44:48.470070Z","signature_b64":"81ZwfOmPjnXNziv5SAHGjuRvk7zMk6Lf+VYurB4NtUDTG5XWWH3EVezCeqzm4CeplrNoD9ORlRoSQRVZ2nnKDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"8d69aa15642532ed3aeaf2dc88b21d99898ec855ff91e2a9c080ae1e76ba378d","last_reissued_at":"2026-07-05T11:44:48.469621Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T11:44:48.469621Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Statistics of Gas Density, Velocity, and Magnetic Fields in Cool-Core Galaxy Clusters","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.GA","authors_text":"Alex Lazarian, G. Brunetti, John A. ZuHone, Yue Hu","submitted_at":"2025-05-13T06:40:11Z","abstract_excerpt":"Understanding turbulence within the Intracluster Medium (ICM) of galaxy clusters is pivotal for comprehending their evolution and dynamics. Employing 3D magnetohydrodynamic (MHD) simulations of galaxy cluster mergers, we examine the statistical properties of gas density, magnetic fields, and velocity, particularly emphasizing the central regions spanning 400 kpc. The simulations are designed to resemble massive cool-core clusters such as Perseus, while varying the initial plasma $\\beta$ values (100, 200, and 500). Our findings indicate that while the statistical histogram distributions of gas "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2505.08275","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/2505.08275/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":"2505.08275","created_at":"2026-07-05T11:44:48.469679+00:00"},{"alias_kind":"arxiv_version","alias_value":"2505.08275v2","created_at":"2026-07-05T11:44:48.469679+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2505.08275","created_at":"2026-07-05T11:44:48.469679+00:00"},{"alias_kind":"pith_short_12","alias_value":"RVU2UFLEEUZO","created_at":"2026-07-05T11:44:48.469679+00:00"},{"alias_kind":"pith_short_16","alias_value":"RVU2UFLEEUZO2OXK","created_at":"2026-07-05T11:44:48.469679+00:00"},{"alias_kind":"pith_short_8","alias_value":"RVU2UFLE","created_at":"2026-07-05T11:44:48.469679+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/RVU2UFLEEUZO2OXK6LOIRMQ5TG","json":"https://pith.science/pith/RVU2UFLEEUZO2OXK6LOIRMQ5TG.json","graph_json":"https://pith.science/api/pith-number/RVU2UFLEEUZO2OXK6LOIRMQ5TG/graph.json","events_json":"https://pith.science/api/pith-number/RVU2UFLEEUZO2OXK6LOIRMQ5TG/events.json","paper":"https://pith.science/paper/RVU2UFLE"},"agent_actions":{"view_html":"https://pith.science/pith/RVU2UFLEEUZO2OXK6LOIRMQ5TG","download_json":"https://pith.science/pith/RVU2UFLEEUZO2OXK6LOIRMQ5TG.json","view_paper":"https://pith.science/paper/RVU2UFLE","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2505.08275&json=true","fetch_graph":"https://pith.science/api/pith-number/RVU2UFLEEUZO2OXK6LOIRMQ5TG/graph.json","fetch_events":"https://pith.science/api/pith-number/RVU2UFLEEUZO2OXK6LOIRMQ5TG/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/RVU2UFLEEUZO2OXK6LOIRMQ5TG/action/timestamp_anchor","attest_storage":"https://pith.science/pith/RVU2UFLEEUZO2OXK6LOIRMQ5TG/action/storage_attestation","attest_author":"https://pith.science/pith/RVU2UFLEEUZO2OXK6LOIRMQ5TG/action/author_attestation","sign_citation":"https://pith.science/pith/RVU2UFLEEUZO2OXK6LOIRMQ5TG/action/citation_signature","submit_replication":"https://pith.science/pith/RVU2UFLEEUZO2OXK6LOIRMQ5TG/action/replication_record"}},"created_at":"2026-07-05T11:44:48.469679+00:00","updated_at":"2026-07-05T11:44:48.469679+00:00"}