{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2010:YEQQWXUMK4K7E5JRJ2HALHCNJB","short_pith_number":"pith:YEQQWXUM","schema_version":"1.0","canonical_sha256":"c1210b5e8c5715f275314e8e059c4d4852f32f6aea4934efb912840c73272803","source":{"kind":"arxiv","id":"1011.3302","version":1},"attestation_state":"computed","paper":{"title":"The Cool-Core Bias in X-ray Galaxy Cluster Samples I: Method And Application To HIFLUGCS","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","astro-ph.IM"],"primary_cat":"astro-ph.CO","authors_text":"D. Eckert, S. Molendi, S. Paltani","submitted_at":"2010-11-15T07:12:44Z","abstract_excerpt":"When selecting flux-limited cluster samples, the detection efficiency of X-ray instruments is not the same for centrally-peaked and flat objects, which introduces a bias in flux-limited cluster samples. We quantify this effect in the case of a well-known cluster sample, HIFLUGCS. We simulate a population of X-ray clusters with various surface-brightness profiles, and use the instrumental characteristics of the ROSAT All-Sky Survey (RASS) to select flux-limited samples similar to the HIFLUGCS sample and predict the expected bias. For comparison, we also estimate observationally the bias in the "},"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":"1011.3302","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2010-11-15T07:12:44Z","cross_cats_sorted":["astro-ph.HE","astro-ph.IM"],"title_canon_sha256":"5a2d12b1ea8cb80c5152a0a3c2e6a3d1b724c192f6e24bea820801dde806874b","abstract_canon_sha256":"2181bcbbcfc8cfd48eb4dc039d2261a62e1d1269aee11dcc550b528c6c718bea"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:04:47.668203Z","signature_b64":"pOoiQ9qSa2Igi5e7XaBPUeNE5wN4qKZxzk8QREdVUOKAx8YIr3/q3hdo1VFObgc9GR8uT7DQg+P1tdDqlB03Dg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c1210b5e8c5715f275314e8e059c4d4852f32f6aea4934efb912840c73272803","last_reissued_at":"2026-05-18T02:04:47.667599Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:04:47.667599Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Cool-Core Bias in X-ray Galaxy Cluster Samples I: Method And Application To HIFLUGCS","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE","astro-ph.IM"],"primary_cat":"astro-ph.CO","authors_text":"D. Eckert, S. Molendi, S. Paltani","submitted_at":"2010-11-15T07:12:44Z","abstract_excerpt":"When selecting flux-limited cluster samples, the detection efficiency of X-ray instruments is not the same for centrally-peaked and flat objects, which introduces a bias in flux-limited cluster samples. We quantify this effect in the case of a well-known cluster sample, HIFLUGCS. We simulate a population of X-ray clusters with various surface-brightness profiles, and use the instrumental characteristics of the ROSAT All-Sky Survey (RASS) to select flux-limited samples similar to the HIFLUGCS sample and predict the expected bias. For comparison, we also estimate observationally the bias in the "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1011.3302","kind":"arxiv","version":1},"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":"1011.3302","created_at":"2026-05-18T02:04:47.667704+00:00"},{"alias_kind":"arxiv_version","alias_value":"1011.3302v1","created_at":"2026-05-18T02:04:47.667704+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1011.3302","created_at":"2026-05-18T02:04:47.667704+00:00"},{"alias_kind":"pith_short_12","alias_value":"YEQQWXUMK4K7","created_at":"2026-05-18T12:26:17.028572+00:00"},{"alias_kind":"pith_short_16","alias_value":"YEQQWXUMK4K7E5JR","created_at":"2026-05-18T12:26:17.028572+00:00"},{"alias_kind":"pith_short_8","alias_value":"YEQQWXUM","created_at":"2026-05-18T12:26:17.028572+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2605.16483","citing_title":"The limits of feedback from active galactic nuclei","ref_index":26,"is_internal_anchor":true},{"citing_arxiv_id":"2605.15264","citing_title":"Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. II. Mass Mapping and Overdensity Characterization","ref_index":183,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/YEQQWXUMK4K7E5JRJ2HALHCNJB","json":"https://pith.science/pith/YEQQWXUMK4K7E5JRJ2HALHCNJB.json","graph_json":"https://pith.science/api/pith-number/YEQQWXUMK4K7E5JRJ2HALHCNJB/graph.json","events_json":"https://pith.science/api/pith-number/YEQQWXUMK4K7E5JRJ2HALHCNJB/events.json","paper":"https://pith.science/paper/YEQQWXUM"},"agent_actions":{"view_html":"https://pith.science/pith/YEQQWXUMK4K7E5JRJ2HALHCNJB","download_json":"https://pith.science/pith/YEQQWXUMK4K7E5JRJ2HALHCNJB.json","view_paper":"https://pith.science/paper/YEQQWXUM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1011.3302&json=true","fetch_graph":"https://pith.science/api/pith-number/YEQQWXUMK4K7E5JRJ2HALHCNJB/graph.json","fetch_events":"https://pith.science/api/pith-number/YEQQWXUMK4K7E5JRJ2HALHCNJB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/YEQQWXUMK4K7E5JRJ2HALHCNJB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/YEQQWXUMK4K7E5JRJ2HALHCNJB/action/storage_attestation","attest_author":"https://pith.science/pith/YEQQWXUMK4K7E5JRJ2HALHCNJB/action/author_attestation","sign_citation":"https://pith.science/pith/YEQQWXUMK4K7E5JRJ2HALHCNJB/action/citation_signature","submit_replication":"https://pith.science/pith/YEQQWXUMK4K7E5JRJ2HALHCNJB/action/replication_record"}},"created_at":"2026-05-18T02:04:47.667704+00:00","updated_at":"2026-05-18T02:04:47.667704+00:00"}