{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:MILKCXF7RLZRPUL2TQ2ZKUJ7PR","short_pith_number":"pith:MILKCXF7","schema_version":"1.0","canonical_sha256":"6216a15cbf8af317d17a9c3595513f7c7239fb318003821ebaeb94213b0d18a6","source":{"kind":"arxiv","id":"2208.02791","version":2},"attestation_state":"computed","paper":{"title":"Fast computation of non-linear power spectrum in cosmologies with massive neutrinos","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.CO","authors_text":"Alejandro Aviles, Hern\\'an E. Noriega, Mariana Vargas-Maga\\~na, Sebastien Fromenteau","submitted_at":"2022-08-04T17:44:23Z","abstract_excerpt":"We compute 1-loop corrections to the redshift space galaxy power spectrum in cosmologies containing additional scales, and hence kernels different from Einstein-de Sitter (EdS). Specifically, our method is tailored for cosmologies in the presence of massive neutrinos and some modified gravity models; in this article we concentrate on the former case. The perturbative kernels have contributions that we notice appear either from the logarithmic growth factor $f(k,t)$, which is scale-dependent because of the neutrino free-streaming, or from the failure of the commonly used approximation $f^2=\\Ome"},"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":"2208.02791","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.CO","submitted_at":"2022-08-04T17:44:23Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"2257d45eb00960224b778210856c29365db7acc8660ff39bfb357389c6c2f5e5","abstract_canon_sha256":"307bc2377c345597d616b967db97630f440437dd24f757cb0370c48a0dc5c07e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:17:27.853411Z","signature_b64":"yd2tFnhNbuwizIpiCGzGp9OYZRJfILlCVL+x9Kcchcd0SUPsErXdAneCeGtvX8hdUBNfXG8i3WUCIjTdq3ZXCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6216a15cbf8af317d17a9c3595513f7c7239fb318003821ebaeb94213b0d18a6","last_reissued_at":"2026-07-05T05:17:27.852905Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:17:27.852905Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Fast computation of non-linear power spectrum in cosmologies with massive neutrinos","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.CO","authors_text":"Alejandro Aviles, Hern\\'an E. Noriega, Mariana Vargas-Maga\\~na, Sebastien Fromenteau","submitted_at":"2022-08-04T17:44:23Z","abstract_excerpt":"We compute 1-loop corrections to the redshift space galaxy power spectrum in cosmologies containing additional scales, and hence kernels different from Einstein-de Sitter (EdS). Specifically, our method is tailored for cosmologies in the presence of massive neutrinos and some modified gravity models; in this article we concentrate on the former case. The perturbative kernels have contributions that we notice appear either from the logarithmic growth factor $f(k,t)$, which is scale-dependent because of the neutrino free-streaming, or from the failure of the commonly used approximation $f^2=\\Ome"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2208.02791","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/2208.02791/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":"2208.02791","created_at":"2026-07-05T05:17:27.852961+00:00"},{"alias_kind":"arxiv_version","alias_value":"2208.02791v2","created_at":"2026-07-05T05:17:27.852961+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2208.02791","created_at":"2026-07-05T05:17:27.852961+00:00"},{"alias_kind":"pith_short_12","alias_value":"MILKCXF7RLZR","created_at":"2026-07-05T05:17:27.852961+00:00"},{"alias_kind":"pith_short_16","alias_value":"MILKCXF7RLZRPUL2","created_at":"2026-07-05T05:17:27.852961+00:00"},{"alias_kind":"pith_short_8","alias_value":"MILKCXF7","created_at":"2026-07-05T05:17:27.852961+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":9,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.05114","citing_title":"Effective Field Theory of Large Scale Structure and Newtonian Motion Gauges","ref_index":81,"is_internal_anchor":false},{"citing_arxiv_id":"2508.19106","citing_title":"Tracing Signatures of Modified Gravity in Redshift-Space Galaxy Bispectrum Multipoles: Prospects for Euclid","ref_index":116,"is_internal_anchor":false},{"citing_arxiv_id":"2411.12021","citing_title":"DESI 2024 V: Full-Shape Galaxy Clustering from Galaxies and Quasars","ref_index":138,"is_internal_anchor":false},{"citing_arxiv_id":"2511.20757","citing_title":"Reanalyzing DESI DR1: 2. Constraints on Dark Energy, Spatial Curvature, and Neutrino Masses","ref_index":120,"is_internal_anchor":false},{"citing_arxiv_id":"2411.12022","citing_title":"DESI 2024 VII: Cosmological Constraints from the Full-Shape Modeling of Clustering Measurements","ref_index":126,"is_internal_anchor":false},{"citing_arxiv_id":"2604.26915","citing_title":"Testing Scale-Dependent Modified Gravity with DESI DR1","ref_index":64,"is_internal_anchor":false},{"citing_arxiv_id":"2605.05114","citing_title":"Effective Field Theory of Large Scale Structure and Newtonian Motion Gauges","ref_index":73,"is_internal_anchor":false},{"citing_arxiv_id":"2604.08895","citing_title":"FolpsD: combining EFT and phenomenological approaches for joint power spectrum and bispectrum analyses","ref_index":59,"is_internal_anchor":false},{"citing_arxiv_id":"2604.14504","citing_title":"Forecasting neutrino mass constraints from the Nancy Grace Roman Space Telescope","ref_index":23,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MILKCXF7RLZRPUL2TQ2ZKUJ7PR","json":"https://pith.science/pith/MILKCXF7RLZRPUL2TQ2ZKUJ7PR.json","graph_json":"https://pith.science/api/pith-number/MILKCXF7RLZRPUL2TQ2ZKUJ7PR/graph.json","events_json":"https://pith.science/api/pith-number/MILKCXF7RLZRPUL2TQ2ZKUJ7PR/events.json","paper":"https://pith.science/paper/MILKCXF7"},"agent_actions":{"view_html":"https://pith.science/pith/MILKCXF7RLZRPUL2TQ2ZKUJ7PR","download_json":"https://pith.science/pith/MILKCXF7RLZRPUL2TQ2ZKUJ7PR.json","view_paper":"https://pith.science/paper/MILKCXF7","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2208.02791&json=true","fetch_graph":"https://pith.science/api/pith-number/MILKCXF7RLZRPUL2TQ2ZKUJ7PR/graph.json","fetch_events":"https://pith.science/api/pith-number/MILKCXF7RLZRPUL2TQ2ZKUJ7PR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MILKCXF7RLZRPUL2TQ2ZKUJ7PR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MILKCXF7RLZRPUL2TQ2ZKUJ7PR/action/storage_attestation","attest_author":"https://pith.science/pith/MILKCXF7RLZRPUL2TQ2ZKUJ7PR/action/author_attestation","sign_citation":"https://pith.science/pith/MILKCXF7RLZRPUL2TQ2ZKUJ7PR/action/citation_signature","submit_replication":"https://pith.science/pith/MILKCXF7RLZRPUL2TQ2ZKUJ7PR/action/replication_record"}},"created_at":"2026-07-05T05:17:27.852961+00:00","updated_at":"2026-07-05T05:17:27.852961+00:00"}