{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2004:MGAV7RNAXSNB4QDWJ7XGINBOLB","short_pith_number":"pith:MGAV7RNA","schema_version":"1.0","canonical_sha256":"61815fc5a0bc9a1e40764fee64342e584552091e8a6fc4d733a1dfca7af927b4","source":{"kind":"arxiv","id":"astro-ph/0404132","version":2},"attestation_state":"computed","paper":{"title":"Probing Turbulence in the Coma Galaxy Cluster","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Finoguenov, F. Miniati, H. Boehringer, P. Schuecker, U.G. Briel","submitted_at":"2004-04-06T14:25:51Z","abstract_excerpt":"Spatially-resolved gas pressure maps of the Coma galaxy cluster are obtained from a mosaic of XMM-Newton observations in the scale range between a resolution of 20 kpc and an extent of 2.8 Mpc. A Fourier analysis of the data reveals the presence of a scale-invariant pressure fluctuation spectrum in the range between 40 and 90 kpc and is found to be well described by a projected Kolmogorov/Oboukhov-type turbulence spectrum. Deprojection and integration of the spectrum yields the lower limit of $\\sim 10$ percent of the total intracluster medium pressure in turbulent form. The results also provid"},"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":"astro-ph/0404132","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2004-04-06T14:25:51Z","cross_cats_sorted":[],"title_canon_sha256":"3f633a5a6166e426aff833e6efa861335652d44fa467dd7f88aae36f6ea8fcdf","abstract_canon_sha256":"80561338d7b9e5268661a9051eca3745da5bb9b09eeba33b1c297995865e6b42"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:43:32.075882Z","signature_b64":"IZMdEc1aXWlMdg9BCnUSutT7Bo27+hV2x/f9MpIMlbpx9ZdingHLx+lIrly3th7dRF6N+395WxXq8yWb0vXEAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"61815fc5a0bc9a1e40764fee64342e584552091e8a6fc4d733a1dfca7af927b4","last_reissued_at":"2026-07-04T16:43:32.075475Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:43:32.075475Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Probing Turbulence in the Coma Galaxy Cluster","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"A. Finoguenov, F. Miniati, H. Boehringer, P. Schuecker, U.G. Briel","submitted_at":"2004-04-06T14:25:51Z","abstract_excerpt":"Spatially-resolved gas pressure maps of the Coma galaxy cluster are obtained from a mosaic of XMM-Newton observations in the scale range between a resolution of 20 kpc and an extent of 2.8 Mpc. A Fourier analysis of the data reveals the presence of a scale-invariant pressure fluctuation spectrum in the range between 40 and 90 kpc and is found to be well described by a projected Kolmogorov/Oboukhov-type turbulence spectrum. Deprojection and integration of the spectrum yields the lower limit of $\\sim 10$ percent of the total intracluster medium pressure in turbulent form. The results also provid"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0404132","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/astro-ph/0404132/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":"astro-ph/0404132","created_at":"2026-07-04T16:43:32.075535+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0404132v2","created_at":"2026-07-04T16:43:32.075535+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0404132","created_at":"2026-07-04T16:43:32.075535+00:00"},{"alias_kind":"pith_short_12","alias_value":"MGAV7RNAXSNB","created_at":"2026-07-04T16:43:32.075535+00:00"},{"alias_kind":"pith_short_16","alias_value":"MGAV7RNAXSNB4QDW","created_at":"2026-07-04T16:43:32.075535+00:00"},{"alias_kind":"pith_short_8","alias_value":"MGAV7RNA","created_at":"2026-07-04T16:43:32.075535+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.06346","citing_title":"Unravelling Turbulence and Magnetic Fields in Galaxy Clusters with SKA and XRISM","ref_index":68,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MGAV7RNAXSNB4QDWJ7XGINBOLB","json":"https://pith.science/pith/MGAV7RNAXSNB4QDWJ7XGINBOLB.json","graph_json":"https://pith.science/api/pith-number/MGAV7RNAXSNB4QDWJ7XGINBOLB/graph.json","events_json":"https://pith.science/api/pith-number/MGAV7RNAXSNB4QDWJ7XGINBOLB/events.json","paper":"https://pith.science/paper/MGAV7RNA"},"agent_actions":{"view_html":"https://pith.science/pith/MGAV7RNAXSNB4QDWJ7XGINBOLB","download_json":"https://pith.science/pith/MGAV7RNAXSNB4QDWJ7XGINBOLB.json","view_paper":"https://pith.science/paper/MGAV7RNA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0404132&json=true","fetch_graph":"https://pith.science/api/pith-number/MGAV7RNAXSNB4QDWJ7XGINBOLB/graph.json","fetch_events":"https://pith.science/api/pith-number/MGAV7RNAXSNB4QDWJ7XGINBOLB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MGAV7RNAXSNB4QDWJ7XGINBOLB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MGAV7RNAXSNB4QDWJ7XGINBOLB/action/storage_attestation","attest_author":"https://pith.science/pith/MGAV7RNAXSNB4QDWJ7XGINBOLB/action/author_attestation","sign_citation":"https://pith.science/pith/MGAV7RNAXSNB4QDWJ7XGINBOLB/action/citation_signature","submit_replication":"https://pith.science/pith/MGAV7RNAXSNB4QDWJ7XGINBOLB/action/replication_record"}},"created_at":"2026-07-04T16:43:32.075535+00:00","updated_at":"2026-07-04T16:43:32.075535+00:00"}