{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:RG34PTXSQV4DPE6E3DJ7PH3IVW","short_pith_number":"pith:RG34PTXS","schema_version":"1.0","canonical_sha256":"89b7c7cef285783793c4d8d3f79f68ad801343870337bc142d94a92b8b096d62","source":{"kind":"arxiv","id":"1303.4486","version":2},"attestation_state":"computed","paper":{"title":"The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements and the strong power of normalized growth rate on constraining dark energy","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Antonio J. Cuesta, Ariel G. Sanchez, Chia-Hsun Chuang, Daniel J. Eisenstein, Daniel Thomas, David H. Weinberg, David J Schlegel, Donald P. Schneider, Eyal Kazin, Florian Beutler, Francisco Prada, Joel R. Brownstein, Jon Brinkmann, Marc Manera, Nikhil Padmanabhan, Xiaoying Xu","submitted_at":"2013-03-19T04:57:18Z","abstract_excerpt":"We present measurements of the anisotropic galaxy clustering from the Data Release 9 (DR9) CMASS sample of the SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS). We analyze the broad-range shape of the monopole and quadrupole correlation functions to obtain constraints, at the effective redshift $z=0.57$ of the sample, on the Hubble expansion rate $H(z)$, the angular-diameter distance $D_A(z)$, the normalized growth rate $f(z)\\sigma_8(z)$, the physical matter density $\\Omega_m h^2$, and the biased amplitude of matter fluctuation b\\sigma_8(z). We obtain {$H(0.57)$, $D_A(0.57)$, $f(0.57)\\s"},"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":"1303.4486","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2013-03-19T04:57:18Z","cross_cats_sorted":[],"title_canon_sha256":"9f254ef06619606a68032dcb4014fe4c579f4c23191fe9cfa89c49119f757ad4","abstract_canon_sha256":"b8adae5f6f92c4534b2a454d353ef8073b36a44be0acfe6c32f936e4d511b1c6"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:38:32.231676Z","signature_b64":"sDTywsYJZKumDBsboHNbNZ9nak9iAYbR7GQycBdDwIH0RPC8u8qQuus+b/+zID0vwWzvvtuRLPy3+bgPEd+/Bg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"89b7c7cef285783793c4d8d3f79f68ad801343870337bc142d94a92b8b096d62","last_reissued_at":"2026-05-18T00:38:32.231236Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:38:32.231236Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements and the strong power of normalized growth rate on constraining dark energy","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Antonio J. Cuesta, Ariel G. Sanchez, Chia-Hsun Chuang, Daniel J. Eisenstein, Daniel Thomas, David H. Weinberg, David J Schlegel, Donald P. Schneider, Eyal Kazin, Florian Beutler, Francisco Prada, Joel R. Brownstein, Jon Brinkmann, Marc Manera, Nikhil Padmanabhan, Xiaoying Xu","submitted_at":"2013-03-19T04:57:18Z","abstract_excerpt":"We present measurements of the anisotropic galaxy clustering from the Data Release 9 (DR9) CMASS sample of the SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS). We analyze the broad-range shape of the monopole and quadrupole correlation functions to obtain constraints, at the effective redshift $z=0.57$ of the sample, on the Hubble expansion rate $H(z)$, the angular-diameter distance $D_A(z)$, the normalized growth rate $f(z)\\sigma_8(z)$, the physical matter density $\\Omega_m h^2$, and the biased amplitude of matter fluctuation b\\sigma_8(z). We obtain {$H(0.57)$, $D_A(0.57)$, $f(0.57)\\s"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1303.4486","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":"1303.4486","created_at":"2026-05-18T00:38:32.231298+00:00"},{"alias_kind":"arxiv_version","alias_value":"1303.4486v2","created_at":"2026-05-18T00:38:32.231298+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1303.4486","created_at":"2026-05-18T00:38:32.231298+00:00"},{"alias_kind":"pith_short_12","alias_value":"RG34PTXSQV4D","created_at":"2026-05-18T12:27:57.521954+00:00"},{"alias_kind":"pith_short_16","alias_value":"RG34PTXSQV4DPE6E","created_at":"2026-05-18T12:27:57.521954+00:00"},{"alias_kind":"pith_short_8","alias_value":"RG34PTXS","created_at":"2026-05-18T12:27:57.521954+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.23793","citing_title":"From Big Bang Nucleosynthesis to Late-Time Acceleration in $f(Q,L_m)$ Gravity","ref_index":79,"is_internal_anchor":false},{"citing_arxiv_id":"2604.22450","citing_title":"Exploring Cosmic Evolution in R\\'enyi Entropic Cosmology with Constraints from DESI DR2 BAO and GW Data","ref_index":61,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/RG34PTXSQV4DPE6E3DJ7PH3IVW","json":"https://pith.science/pith/RG34PTXSQV4DPE6E3DJ7PH3IVW.json","graph_json":"https://pith.science/api/pith-number/RG34PTXSQV4DPE6E3DJ7PH3IVW/graph.json","events_json":"https://pith.science/api/pith-number/RG34PTXSQV4DPE6E3DJ7PH3IVW/events.json","paper":"https://pith.science/paper/RG34PTXS"},"agent_actions":{"view_html":"https://pith.science/pith/RG34PTXSQV4DPE6E3DJ7PH3IVW","download_json":"https://pith.science/pith/RG34PTXSQV4DPE6E3DJ7PH3IVW.json","view_paper":"https://pith.science/paper/RG34PTXS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1303.4486&json=true","fetch_graph":"https://pith.science/api/pith-number/RG34PTXSQV4DPE6E3DJ7PH3IVW/graph.json","fetch_events":"https://pith.science/api/pith-number/RG34PTXSQV4DPE6E3DJ7PH3IVW/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/RG34PTXSQV4DPE6E3DJ7PH3IVW/action/timestamp_anchor","attest_storage":"https://pith.science/pith/RG34PTXSQV4DPE6E3DJ7PH3IVW/action/storage_attestation","attest_author":"https://pith.science/pith/RG34PTXSQV4DPE6E3DJ7PH3IVW/action/author_attestation","sign_citation":"https://pith.science/pith/RG34PTXSQV4DPE6E3DJ7PH3IVW/action/citation_signature","submit_replication":"https://pith.science/pith/RG34PTXSQV4DPE6E3DJ7PH3IVW/action/replication_record"}},"created_at":"2026-05-18T00:38:32.231298+00:00","updated_at":"2026-05-18T00:38:32.231298+00:00"}