{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:TGQ53HVZCYYA4SLK74FJJULDTN","short_pith_number":"pith:TGQ53HVZ","schema_version":"1.0","canonical_sha256":"99a1dd9eb916300e496aff0a94d1639b45b05e7d501e62fbf7e3a40deabd8796","source":{"kind":"arxiv","id":"1606.02520","version":2},"attestation_state":"computed","paper":{"title":"A Perturbative Approach to the Redshift Space Power Spectrum: Beyond the Standard Model","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Benjamin Bose, Kazuya Koyama","submitted_at":"2016-06-08T11:54:09Z","abstract_excerpt":"We develop a code to produce the power spectrum in redshift space based on standard perturbation theory (SPT) at 1-loop order. The code can be applied to a wide range of modified gravity and dark energy models using a recently proposed numerical method by A.Taruya. This includes Horndeski's theory with a general potential, which accommodates both chameleon and Vainshtein screening mechanisms and provides a non-linear extension of the effective theory of dark energy up to third order. Focus is on a recent non-linear model of the redshift space power spectrum which has been shown to model the an"},"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":"1606.02520","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2016-06-08T11:54:09Z","cross_cats_sorted":[],"title_canon_sha256":"6366889c3e10b134a820e6594fe194172674b46841d561b0265f4a80b8e99f28","abstract_canon_sha256":"1241da8b8b0823025a27260d7a2060ab84a049419b2343693c042c572424002b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:07:16.178375Z","signature_b64":"Jhk1niKvqArRajuCXrmHNlIgt7ReThVb4F2+xgiJ/ZioNx62uxnMfbUO5Rre80SfnW/opW3PezQUHccN0G0bBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"99a1dd9eb916300e496aff0a94d1639b45b05e7d501e62fbf7e3a40deabd8796","last_reissued_at":"2026-05-18T01:07:16.177793Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:07:16.177793Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A Perturbative Approach to the Redshift Space Power Spectrum: Beyond the Standard Model","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Benjamin Bose, Kazuya Koyama","submitted_at":"2016-06-08T11:54:09Z","abstract_excerpt":"We develop a code to produce the power spectrum in redshift space based on standard perturbation theory (SPT) at 1-loop order. The code can be applied to a wide range of modified gravity and dark energy models using a recently proposed numerical method by A.Taruya. This includes Horndeski's theory with a general potential, which accommodates both chameleon and Vainshtein screening mechanisms and provides a non-linear extension of the effective theory of dark energy up to third order. Focus is on a recent non-linear model of the redshift space power spectrum which has been shown to model the an"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1606.02520","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":"1606.02520","created_at":"2026-05-18T01:07:16.177883+00:00"},{"alias_kind":"arxiv_version","alias_value":"1606.02520v2","created_at":"2026-05-18T01:07:16.177883+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1606.02520","created_at":"2026-05-18T01:07:16.177883+00:00"},{"alias_kind":"pith_short_12","alias_value":"TGQ53HVZCYYA","created_at":"2026-05-18T12:30:44.179134+00:00"},{"alias_kind":"pith_short_16","alias_value":"TGQ53HVZCYYA4SLK","created_at":"2026-05-18T12:30:44.179134+00:00"},{"alias_kind":"pith_short_8","alias_value":"TGQ53HVZ","created_at":"2026-05-18T12:30:44.179134+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.26915","citing_title":"Testing Scale-Dependent Modified Gravity with DESI DR1","ref_index":22,"is_internal_anchor":false},{"citing_arxiv_id":"2605.04154","citing_title":"A Master Equation for Screening in Luminal Horndeski Gravity","ref_index":97,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/TGQ53HVZCYYA4SLK74FJJULDTN","json":"https://pith.science/pith/TGQ53HVZCYYA4SLK74FJJULDTN.json","graph_json":"https://pith.science/api/pith-number/TGQ53HVZCYYA4SLK74FJJULDTN/graph.json","events_json":"https://pith.science/api/pith-number/TGQ53HVZCYYA4SLK74FJJULDTN/events.json","paper":"https://pith.science/paper/TGQ53HVZ"},"agent_actions":{"view_html":"https://pith.science/pith/TGQ53HVZCYYA4SLK74FJJULDTN","download_json":"https://pith.science/pith/TGQ53HVZCYYA4SLK74FJJULDTN.json","view_paper":"https://pith.science/paper/TGQ53HVZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1606.02520&json=true","fetch_graph":"https://pith.science/api/pith-number/TGQ53HVZCYYA4SLK74FJJULDTN/graph.json","fetch_events":"https://pith.science/api/pith-number/TGQ53HVZCYYA4SLK74FJJULDTN/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/TGQ53HVZCYYA4SLK74FJJULDTN/action/timestamp_anchor","attest_storage":"https://pith.science/pith/TGQ53HVZCYYA4SLK74FJJULDTN/action/storage_attestation","attest_author":"https://pith.science/pith/TGQ53HVZCYYA4SLK74FJJULDTN/action/author_attestation","sign_citation":"https://pith.science/pith/TGQ53HVZCYYA4SLK74FJJULDTN/action/citation_signature","submit_replication":"https://pith.science/pith/TGQ53HVZCYYA4SLK74FJJULDTN/action/replication_record"}},"created_at":"2026-05-18T01:07:16.177883+00:00","updated_at":"2026-05-18T01:07:16.177883+00:00"}