{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:GRICVZSA4IKAR4TGI5BNLKUFCZ","short_pith_number":"pith:GRICVZSA","schema_version":"1.0","canonical_sha256":"34502ae640e21408f2664742d5aa85166d8de48530e741bfc038c05432cce9a2","source":{"kind":"arxiv","id":"2308.08593","version":2},"attestation_state":"computed","paper":{"title":"Fast computation of the non-Gaussian covariance of redshift-space galaxy power spectrum multipoles","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Yosuke Kobayashi","submitted_at":"2023-08-16T18:00:01Z","abstract_excerpt":"The non-Gaussian part of the covariance matrix of the galaxy power spectrum involves the connected four-point correlation in Fourier space, i.e. trispectrum. This paper introduces a fast method to compute the non-Gaussian part of the covariance matrix of the galaxy power spectrum multipoles in redshift space at tree-level standard perturbation theory. For the tree-level galaxy trispectrum, the angular integral between two wavevectors can be evaluated analytically by employing an FFTLog. The new implementation computes the non-Gaussian covariance of the power spectrum monopole, quadrupole, hexa"},"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":"2308.08593","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.CO","submitted_at":"2023-08-16T18:00:01Z","cross_cats_sorted":[],"title_canon_sha256":"7d43c5f118a75685a867e3ff1b1b747dc80ea67c4c26cf745ed871a1d63597f3","abstract_canon_sha256":"ed326ddbfa4d8a7ff24dc9981e9a5cf4a7f09830b37218d3cf662fc296c07455"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T07:09:00.888069Z","signature_b64":"G3gnlUUkO2S0CUJNsodk2/QwpOCaCbH1a3evrn8AQeP4GJyA3C7EsVVh9ZXbiXXZlFokZ57mwKHm2TJ+L6/xAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"34502ae640e21408f2664742d5aa85166d8de48530e741bfc038c05432cce9a2","last_reissued_at":"2026-07-05T07:09:00.887638Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T07:09:00.887638Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Fast computation of the non-Gaussian covariance of redshift-space galaxy power spectrum multipoles","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Yosuke Kobayashi","submitted_at":"2023-08-16T18:00:01Z","abstract_excerpt":"The non-Gaussian part of the covariance matrix of the galaxy power spectrum involves the connected four-point correlation in Fourier space, i.e. trispectrum. This paper introduces a fast method to compute the non-Gaussian part of the covariance matrix of the galaxy power spectrum multipoles in redshift space at tree-level standard perturbation theory. For the tree-level galaxy trispectrum, the angular integral between two wavevectors can be evaluated analytically by employing an FFTLog. The new implementation computes the non-Gaussian covariance of the power spectrum monopole, quadrupole, hexa"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2308.08593","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/2308.08593/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":"2308.08593","created_at":"2026-07-05T07:09:00.887693+00:00"},{"alias_kind":"arxiv_version","alias_value":"2308.08593v2","created_at":"2026-07-05T07:09:00.887693+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2308.08593","created_at":"2026-07-05T07:09:00.887693+00:00"},{"alias_kind":"pith_short_12","alias_value":"GRICVZSA4IKA","created_at":"2026-07-05T07:09:00.887693+00:00"},{"alias_kind":"pith_short_16","alias_value":"GRICVZSA4IKAR4TG","created_at":"2026-07-05T07:09:00.887693+00:00"},{"alias_kind":"pith_short_8","alias_value":"GRICVZSA","created_at":"2026-07-05T07:09:00.887693+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.24852","citing_title":"The 3D clustering of Lyman Alpha Emitters measured with DESI","ref_index":83,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/GRICVZSA4IKAR4TGI5BNLKUFCZ","json":"https://pith.science/pith/GRICVZSA4IKAR4TGI5BNLKUFCZ.json","graph_json":"https://pith.science/api/pith-number/GRICVZSA4IKAR4TGI5BNLKUFCZ/graph.json","events_json":"https://pith.science/api/pith-number/GRICVZSA4IKAR4TGI5BNLKUFCZ/events.json","paper":"https://pith.science/paper/GRICVZSA"},"agent_actions":{"view_html":"https://pith.science/pith/GRICVZSA4IKAR4TGI5BNLKUFCZ","download_json":"https://pith.science/pith/GRICVZSA4IKAR4TGI5BNLKUFCZ.json","view_paper":"https://pith.science/paper/GRICVZSA","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2308.08593&json=true","fetch_graph":"https://pith.science/api/pith-number/GRICVZSA4IKAR4TGI5BNLKUFCZ/graph.json","fetch_events":"https://pith.science/api/pith-number/GRICVZSA4IKAR4TGI5BNLKUFCZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/GRICVZSA4IKAR4TGI5BNLKUFCZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/GRICVZSA4IKAR4TGI5BNLKUFCZ/action/storage_attestation","attest_author":"https://pith.science/pith/GRICVZSA4IKAR4TGI5BNLKUFCZ/action/author_attestation","sign_citation":"https://pith.science/pith/GRICVZSA4IKAR4TGI5BNLKUFCZ/action/citation_signature","submit_replication":"https://pith.science/pith/GRICVZSA4IKAR4TGI5BNLKUFCZ/action/replication_record"}},"created_at":"2026-07-05T07:09:00.887693+00:00","updated_at":"2026-07-05T07:09:00.887693+00:00"}