{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2001:EEGMWZX3DQ2OXRPAXNVZAJBZ6E","short_pith_number":"pith:EEGMWZX3","schema_version":"1.0","canonical_sha256":"210ccb66fb1c34ebc5e0bb6b902439f124328a75bb03e6580e67631c308be6d4","source":{"kind":"arxiv","id":"astro-ph/0105396","version":2},"attestation_state":"computed","paper":{"title":"Constraints on Omega_m, Omega_L, and Sigma_8, from Galaxy Cluster Redshift Distributions","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Gilbert Holder, Joseph Mohr, Zoltan Haiman","submitted_at":"2001-05-22T22:14:38Z","abstract_excerpt":"We show that the counts of galaxy clusters in future deep cluster surveys can place strong constraints on the matter density, Omega_m, the vacuum energy density, Omega_L, and the normalization of the matter power spectrum, sigma_8. Degeneracies between these parameters are different from those in studies of either high--redshift type Ia Supernovae (SNe), or cosmic microwave background (CMB) anisotropies. Using a mass threshold for cluster detection expected to be typical for upcoming SZE surveys, we find that constraints on Omega_m and sigma_8 at the level of roughly 5% or better can be expect"},"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/0105396","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2001-05-22T22:14:38Z","cross_cats_sorted":[],"title_canon_sha256":"f5059cdc3cb9f33276f7924eba738faf5fdb52226ddda3eb4f6601e34a18e489","abstract_canon_sha256":"974212a9a123a5309e610eed66a4b814956cdc49ba79fe8eac032064850b3fd0"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:23:01.315801Z","signature_b64":"UlBqYgOtuh67kNobZ68PiHU67PqgCC194D2xsHzYZmSc0VpMPCK++RO0lF34rF1Wqjku4OCTGHBAtJgR4/8XDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"210ccb66fb1c34ebc5e0bb6b902439f124328a75bb03e6580e67631c308be6d4","last_reissued_at":"2026-05-18T04:23:01.315178Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:23:01.315178Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Constraints on Omega_m, Omega_L, and Sigma_8, from Galaxy Cluster Redshift Distributions","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Gilbert Holder, Joseph Mohr, Zoltan Haiman","submitted_at":"2001-05-22T22:14:38Z","abstract_excerpt":"We show that the counts of galaxy clusters in future deep cluster surveys can place strong constraints on the matter density, Omega_m, the vacuum energy density, Omega_L, and the normalization of the matter power spectrum, sigma_8. Degeneracies between these parameters are different from those in studies of either high--redshift type Ia Supernovae (SNe), or cosmic microwave background (CMB) anisotropies. Using a mass threshold for cluster detection expected to be typical for upcoming SZE surveys, we find that constraints on Omega_m and sigma_8 at the level of roughly 5% or better can be expect"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0105396","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":"astro-ph/0105396","created_at":"2026-05-18T04:23:01.315286+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0105396v2","created_at":"2026-05-18T04:23:01.315286+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0105396","created_at":"2026-05-18T04:23:01.315286+00:00"},{"alias_kind":"pith_short_12","alias_value":"EEGMWZX3DQ2O","created_at":"2026-05-18T12:25:50.254431+00:00"},{"alias_kind":"pith_short_16","alias_value":"EEGMWZX3DQ2OXRPA","created_at":"2026-05-18T12:25:50.254431+00:00"},{"alias_kind":"pith_short_8","alias_value":"EEGMWZX3","created_at":"2026-05-18T12:25:50.254431+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2510.00753","citing_title":"Impact of projection-induced optical selection bias on the weak lensing mass calibration of galaxy clusters","ref_index":3,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/EEGMWZX3DQ2OXRPAXNVZAJBZ6E","json":"https://pith.science/pith/EEGMWZX3DQ2OXRPAXNVZAJBZ6E.json","graph_json":"https://pith.science/api/pith-number/EEGMWZX3DQ2OXRPAXNVZAJBZ6E/graph.json","events_json":"https://pith.science/api/pith-number/EEGMWZX3DQ2OXRPAXNVZAJBZ6E/events.json","paper":"https://pith.science/paper/EEGMWZX3"},"agent_actions":{"view_html":"https://pith.science/pith/EEGMWZX3DQ2OXRPAXNVZAJBZ6E","download_json":"https://pith.science/pith/EEGMWZX3DQ2OXRPAXNVZAJBZ6E.json","view_paper":"https://pith.science/paper/EEGMWZX3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0105396&json=true","fetch_graph":"https://pith.science/api/pith-number/EEGMWZX3DQ2OXRPAXNVZAJBZ6E/graph.json","fetch_events":"https://pith.science/api/pith-number/EEGMWZX3DQ2OXRPAXNVZAJBZ6E/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/EEGMWZX3DQ2OXRPAXNVZAJBZ6E/action/timestamp_anchor","attest_storage":"https://pith.science/pith/EEGMWZX3DQ2OXRPAXNVZAJBZ6E/action/storage_attestation","attest_author":"https://pith.science/pith/EEGMWZX3DQ2OXRPAXNVZAJBZ6E/action/author_attestation","sign_citation":"https://pith.science/pith/EEGMWZX3DQ2OXRPAXNVZAJBZ6E/action/citation_signature","submit_replication":"https://pith.science/pith/EEGMWZX3DQ2OXRPAXNVZAJBZ6E/action/replication_record"}},"created_at":"2026-05-18T04:23:01.315286+00:00","updated_at":"2026-05-18T04:23:01.315286+00:00"}