{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:FOMVYHHEZQQL6VPRHNO2NKU7BG","short_pith_number":"pith:FOMVYHHE","schema_version":"1.0","canonical_sha256":"2b995c1ce4cc20bf55f13b5da6aa9f0994fa3f4075a1db4eccd42654ab82f1d0","source":{"kind":"arxiv","id":"1111.4337","version":2},"attestation_state":"computed","paper":{"title":"An XMM-Newton spatially-resolved study of metal abundance evolution in distant galaxy clusters","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Alessandro Baldi, Fabio Gastaldello, Italo Balestra, Paolo Tozzi, Silvano Molendi, Stefano Ettori","submitted_at":"2011-11-18T11:27:10Z","abstract_excerpt":"We present an XMM-Newton analysis of the X-ray spectra of 39 clusters of galaxies at 0.4<z<1.4, covering a temperature range of 1.5<=kT<=11 keV. We performed a spatially resolved spectral analysis to study how the abundance evolves with redshift not only through a single emission measure performed on the whole cluster but also spatially resolving the cluster emission. We do not observe a statistically significant (>2sigma) abundance evolution with redshift. The most significant deviation from no evolution (90% c.l.) is observed in the emission from the whole cluster (r<0.6r500), that could be "},"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":"1111.4337","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2011-11-18T11:27:10Z","cross_cats_sorted":[],"title_canon_sha256":"2e2adc93aaffc8ec2fcf43354b907ded65218053be59f8ae7551b2830f154ae1","abstract_canon_sha256":"fbb461d627f1e9c772cc2a5bf834d77996d84de8b57b7e1e7b72c58ee3cac845"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:59:29.353116Z","signature_b64":"zVg4r6Hl+N8bLAp9grdRHuxgZg4IaqLh5+2eAP8jByk7510yIZJlIyt8FGH5fnRywX7X+bNwc2b25TfVguugAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2b995c1ce4cc20bf55f13b5da6aa9f0994fa3f4075a1db4eccd42654ab82f1d0","last_reissued_at":"2026-05-18T01:59:29.352519Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:59:29.352519Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"An XMM-Newton spatially-resolved study of metal abundance evolution in distant galaxy clusters","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Alessandro Baldi, Fabio Gastaldello, Italo Balestra, Paolo Tozzi, Silvano Molendi, Stefano Ettori","submitted_at":"2011-11-18T11:27:10Z","abstract_excerpt":"We present an XMM-Newton analysis of the X-ray spectra of 39 clusters of galaxies at 0.4<z<1.4, covering a temperature range of 1.5<=kT<=11 keV. We performed a spatially resolved spectral analysis to study how the abundance evolves with redshift not only through a single emission measure performed on the whole cluster but also spatially resolving the cluster emission. We do not observe a statistically significant (>2sigma) abundance evolution with redshift. The most significant deviation from no evolution (90% c.l.) is observed in the emission from the whole cluster (r<0.6r500), that could be "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1111.4337","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":""},"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":"1111.4337","created_at":"2026-05-18T01:59:29.352611+00:00"},{"alias_kind":"arxiv_version","alias_value":"1111.4337v2","created_at":"2026-05-18T01:59:29.352611+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1111.4337","created_at":"2026-05-18T01:59:29.352611+00:00"},{"alias_kind":"pith_short_12","alias_value":"FOMVYHHEZQQL","created_at":"2026-05-18T12:26:28.662955+00:00"},{"alias_kind":"pith_short_16","alias_value":"FOMVYHHEZQQL6VPR","created_at":"2026-05-18T12:26:28.662955+00:00"},{"alias_kind":"pith_short_8","alias_value":"FOMVYHHE","created_at":"2026-05-18T12:26:28.662955+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.25746","citing_title":"Exploring the physics of ram pressure stripping with radio continuum observations in the SKA era","ref_index":45,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/FOMVYHHEZQQL6VPRHNO2NKU7BG","json":"https://pith.science/pith/FOMVYHHEZQQL6VPRHNO2NKU7BG.json","graph_json":"https://pith.science/api/pith-number/FOMVYHHEZQQL6VPRHNO2NKU7BG/graph.json","events_json":"https://pith.science/api/pith-number/FOMVYHHEZQQL6VPRHNO2NKU7BG/events.json","paper":"https://pith.science/paper/FOMVYHHE"},"agent_actions":{"view_html":"https://pith.science/pith/FOMVYHHEZQQL6VPRHNO2NKU7BG","download_json":"https://pith.science/pith/FOMVYHHEZQQL6VPRHNO2NKU7BG.json","view_paper":"https://pith.science/paper/FOMVYHHE","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1111.4337&json=true","fetch_graph":"https://pith.science/api/pith-number/FOMVYHHEZQQL6VPRHNO2NKU7BG/graph.json","fetch_events":"https://pith.science/api/pith-number/FOMVYHHEZQQL6VPRHNO2NKU7BG/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/FOMVYHHEZQQL6VPRHNO2NKU7BG/action/timestamp_anchor","attest_storage":"https://pith.science/pith/FOMVYHHEZQQL6VPRHNO2NKU7BG/action/storage_attestation","attest_author":"https://pith.science/pith/FOMVYHHEZQQL6VPRHNO2NKU7BG/action/author_attestation","sign_citation":"https://pith.science/pith/FOMVYHHEZQQL6VPRHNO2NKU7BG/action/citation_signature","submit_replication":"https://pith.science/pith/FOMVYHHEZQQL6VPRHNO2NKU7BG/action/replication_record"}},"created_at":"2026-05-18T01:59:29.352611+00:00","updated_at":"2026-05-18T01:59:29.352611+00:00"}