{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:YASBHWVQFZE5DLSQLYDMQN52GO","short_pith_number":"pith:YASBHWVQ","schema_version":"1.0","canonical_sha256":"c02413dab02e49d1ae505e06c837ba33b3901775463902932e1d4d9c64b893d4","source":{"kind":"arxiv","id":"2403.18648","version":2},"attestation_state":"computed","paper":{"title":"Can the splashback radius be an observable boundary of galaxy clusters?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Jenny G. Sorce, Nabila Aghanim, Stefano Ettori, Th\\'eo Lebeau","submitted_at":"2024-03-27T14:56:39Z","abstract_excerpt":"The splashback radius was proposed as a physically motivated boundary of clusters as it sets the limit between the infalling and the orbitally dominated regions. However, galaxy clusters are complex objects connected to filaments of the cosmic web from which they accrete matter that disturbs them and modifies their morphology. In this context, estimating the splashback radius and the cluster boundary becomes challenging. In this work, we use a constrained hydrodynamical simulation of the Virgo cluster's replica embedded in its large-scale structure to investigate the impact of its local enviro"},"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":"2403.18648","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2024-03-27T14:56:39Z","cross_cats_sorted":[],"title_canon_sha256":"130e52dd9c42a78049a0e940b8efb52889f4c1237516ac013d39703f4dafca1f","abstract_canon_sha256":"594d47d9f441f0a1913f33de2215d08af890b927f7605ec7b8c3d0abac86adea"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T09:01:31.627743Z","signature_b64":"buPu4GclV0m9XMdCenTvjVHLHQlKg23mKqjIT3FV/ENviu+rFWMlWUMkygXKcf9ngZGV9oE8vGt9mOEu/wCJDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c02413dab02e49d1ae505e06c837ba33b3901775463902932e1d4d9c64b893d4","last_reissued_at":"2026-07-05T09:01:31.627306Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T09:01:31.627306Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Can the splashback radius be an observable boundary of galaxy clusters?","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Jenny G. Sorce, Nabila Aghanim, Stefano Ettori, Th\\'eo Lebeau","submitted_at":"2024-03-27T14:56:39Z","abstract_excerpt":"The splashback radius was proposed as a physically motivated boundary of clusters as it sets the limit between the infalling and the orbitally dominated regions. However, galaxy clusters are complex objects connected to filaments of the cosmic web from which they accrete matter that disturbs them and modifies their morphology. In this context, estimating the splashback radius and the cluster boundary becomes challenging. In this work, we use a constrained hydrodynamical simulation of the Virgo cluster's replica embedded in its large-scale structure to investigate the impact of its local enviro"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2403.18648","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/2403.18648/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":"2403.18648","created_at":"2026-07-05T09:01:31.627372+00:00"},{"alias_kind":"arxiv_version","alias_value":"2403.18648v2","created_at":"2026-07-05T09:01:31.627372+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2403.18648","created_at":"2026-07-05T09:01:31.627372+00:00"},{"alias_kind":"pith_short_12","alias_value":"YASBHWVQFZE5","created_at":"2026-07-05T09:01:31.627372+00:00"},{"alias_kind":"pith_short_16","alias_value":"YASBHWVQFZE5DLSQ","created_at":"2026-07-05T09:01:31.627372+00:00"},{"alias_kind":"pith_short_8","alias_value":"YASBHWVQ","created_at":"2026-07-05T09:01:31.627372+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2608.06619","citing_title":"Average soft X-ray surface brightness profile of massive galaxy clusters in Magneticum simulations","ref_index":32,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/YASBHWVQFZE5DLSQLYDMQN52GO","json":"https://pith.science/pith/YASBHWVQFZE5DLSQLYDMQN52GO.json","graph_json":"https://pith.science/api/pith-number/YASBHWVQFZE5DLSQLYDMQN52GO/graph.json","events_json":"https://pith.science/api/pith-number/YASBHWVQFZE5DLSQLYDMQN52GO/events.json","paper":"https://pith.science/paper/YASBHWVQ"},"agent_actions":{"view_html":"https://pith.science/pith/YASBHWVQFZE5DLSQLYDMQN52GO","download_json":"https://pith.science/pith/YASBHWVQFZE5DLSQLYDMQN52GO.json","view_paper":"https://pith.science/paper/YASBHWVQ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2403.18648&json=true","fetch_graph":"https://pith.science/api/pith-number/YASBHWVQFZE5DLSQLYDMQN52GO/graph.json","fetch_events":"https://pith.science/api/pith-number/YASBHWVQFZE5DLSQLYDMQN52GO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/YASBHWVQFZE5DLSQLYDMQN52GO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/YASBHWVQFZE5DLSQLYDMQN52GO/action/storage_attestation","attest_author":"https://pith.science/pith/YASBHWVQFZE5DLSQLYDMQN52GO/action/author_attestation","sign_citation":"https://pith.science/pith/YASBHWVQFZE5DLSQLYDMQN52GO/action/citation_signature","submit_replication":"https://pith.science/pith/YASBHWVQFZE5DLSQLYDMQN52GO/action/replication_record"}},"created_at":"2026-07-05T09:01:31.627372+00:00","updated_at":"2026-07-05T09:01:31.627372+00:00"}