{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:S65QSAQDDJK56VNSO2QI6U6N5Z","short_pith_number":"pith:S65QSAQD","schema_version":"1.0","canonical_sha256":"97bb0902031a55df55b276a08f53cdee559d353d633489448a78a1e371478cba","source":{"kind":"arxiv","id":"1204.4725","version":1},"attestation_state":"computed","paper":{"title":"The 6dF Galaxy Survey: z \\approx 0 measurement of the growth rate and sigma_8","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Chris Blake, D. Heath Jones, Florian Beutler, Fred Watson, Gregory B. Poole, Lachlan Campbell, Lister Staveley-Smith, Matthew Colless, Quentin Parker, Will Saunders","submitted_at":"2012-04-20T20:00:03Z","abstract_excerpt":"We present a detailed analysis of redshift-space distortions in the two-point correlation function of the 6dF Galaxy Survey (6dFGS). The K-band selected sub-sample which we employ in this study contains 81971 galaxies distributed over 17000deg^2 with an effective redshift z = 0.067. By modelling the 2D galaxy correlation function, xi(r_p,pi), we measure the parameter combination f(z)sigma_8(z) = 0.423 +/- 0.055. Alternatively, by assuming standard gravity we can break the degeneracy between sigma_8 and the galaxy bias parameter, b. Combining our data with the Hubble constant prior from Riess e"},"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":"1204.4725","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2012-04-20T20:00:03Z","cross_cats_sorted":[],"title_canon_sha256":"4b764e2c95e229698af3d812bcd6b1c89c26c81ceb7db5fa46f9b6060338ac3d","abstract_canon_sha256":"4032636fc215e66a1fd2f7cf2b83bd8d94a909f91aa96e31bb5e2557096cd53d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:57:47.958801Z","signature_b64":"QcnZ9Wq897WPN6aDjaac90hihkwpNjRgKVYRHLkegkYw2pq62W6h3zkN8LGEiZVntF3roYlwGFPNdmr9vxn8Aw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"97bb0902031a55df55b276a08f53cdee559d353d633489448a78a1e371478cba","last_reissued_at":"2026-05-18T01:57:47.958286Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:57:47.958286Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The 6dF Galaxy Survey: z \\approx 0 measurement of the growth rate and sigma_8","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Chris Blake, D. Heath Jones, Florian Beutler, Fred Watson, Gregory B. Poole, Lachlan Campbell, Lister Staveley-Smith, Matthew Colless, Quentin Parker, Will Saunders","submitted_at":"2012-04-20T20:00:03Z","abstract_excerpt":"We present a detailed analysis of redshift-space distortions in the two-point correlation function of the 6dF Galaxy Survey (6dFGS). The K-band selected sub-sample which we employ in this study contains 81971 galaxies distributed over 17000deg^2 with an effective redshift z = 0.067. By modelling the 2D galaxy correlation function, xi(r_p,pi), we measure the parameter combination f(z)sigma_8(z) = 0.423 +/- 0.055. Alternatively, by assuming standard gravity we can break the degeneracy between sigma_8 and the galaxy bias parameter, b. Combining our data with the Hubble constant prior from Riess e"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1204.4725","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":"1204.4725","created_at":"2026-05-18T01:57:47.958364+00:00"},{"alias_kind":"arxiv_version","alias_value":"1204.4725v1","created_at":"2026-05-18T01:57:47.958364+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1204.4725","created_at":"2026-05-18T01:57:47.958364+00:00"},{"alias_kind":"pith_short_12","alias_value":"S65QSAQDDJK5","created_at":"2026-05-18T12:27:20.899486+00:00"},{"alias_kind":"pith_short_16","alias_value":"S65QSAQDDJK56VNS","created_at":"2026-05-18T12:27:20.899486+00:00"},{"alias_kind":"pith_short_8","alias_value":"S65QSAQD","created_at":"2026-05-18T12:27:20.899486+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"2605.23367","citing_title":"Cosmological constraints from neighbor-density-weighted marked correlation functions","ref_index":10,"is_internal_anchor":true},{"citing_arxiv_id":"2411.07970","citing_title":"MUltiplexed Survey Telescope (MUST) Science White Paper I: Overview of Large-Scale Structure Cosmology in the Era of Stage-V Spectroscopic Surveys","ref_index":299,"is_internal_anchor":true},{"citing_arxiv_id":"2504.20478","citing_title":"Tomographic Alcock-Paczynski Test with Marked Correlation Functions","ref_index":7,"is_internal_anchor":true},{"citing_arxiv_id":"1807.06209","citing_title":"Planck 2018 results. VI. Cosmological parameters","ref_index":48,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/S65QSAQDDJK56VNSO2QI6U6N5Z","json":"https://pith.science/pith/S65QSAQDDJK56VNSO2QI6U6N5Z.json","graph_json":"https://pith.science/api/pith-number/S65QSAQDDJK56VNSO2QI6U6N5Z/graph.json","events_json":"https://pith.science/api/pith-number/S65QSAQDDJK56VNSO2QI6U6N5Z/events.json","paper":"https://pith.science/paper/S65QSAQD"},"agent_actions":{"view_html":"https://pith.science/pith/S65QSAQDDJK56VNSO2QI6U6N5Z","download_json":"https://pith.science/pith/S65QSAQDDJK56VNSO2QI6U6N5Z.json","view_paper":"https://pith.science/paper/S65QSAQD","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1204.4725&json=true","fetch_graph":"https://pith.science/api/pith-number/S65QSAQDDJK56VNSO2QI6U6N5Z/graph.json","fetch_events":"https://pith.science/api/pith-number/S65QSAQDDJK56VNSO2QI6U6N5Z/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/S65QSAQDDJK56VNSO2QI6U6N5Z/action/timestamp_anchor","attest_storage":"https://pith.science/pith/S65QSAQDDJK56VNSO2QI6U6N5Z/action/storage_attestation","attest_author":"https://pith.science/pith/S65QSAQDDJK56VNSO2QI6U6N5Z/action/author_attestation","sign_citation":"https://pith.science/pith/S65QSAQDDJK56VNSO2QI6U6N5Z/action/citation_signature","submit_replication":"https://pith.science/pith/S65QSAQDDJK56VNSO2QI6U6N5Z/action/replication_record"}},"created_at":"2026-05-18T01:57:47.958364+00:00","updated_at":"2026-05-18T01:57:47.958364+00:00"}