{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:Y7OFTSPIWI2E4MV5QIXDKQU6TR","short_pith_number":"pith:Y7OFTSPI","schema_version":"1.0","canonical_sha256":"c7dc59c9e8b2344e32bd822e35429e9c5c19d2bf7b5602113c2280bcc3f24a8e","source":{"kind":"arxiv","id":"1207.0839","version":2},"attestation_state":"computed","paper":{"title":"Distribution function approach to redshift space distortions. Part IV: perturbation theory applied to dark matter","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Patrick McDonald, Teppei Okumura, Tobias Baldauf, Uro\\v{s} Seljak, Zvonimir Vlah","submitted_at":"2012-07-03T21:22:37Z","abstract_excerpt":"We develop a perturbative approach to redshift space distortions (RSD) using the phase space distribution function approach and apply it to the dark matter redshift space power spectrum and its moments. RSD can be written as a sum over density weighted velocity moments correlators, with the lowest order being density, momentum density and stress energy density. We use standard and extended perturbation theory (PT) to determine their auto and cross correlators, comparing them to N-body simulations. We show which of the terms can be modeled well with the standard PT and which need additional ter"},"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":"1207.0839","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2012-07-03T21:22:37Z","cross_cats_sorted":[],"title_canon_sha256":"bdf63ebf6833c7533377e6778de2dfe480f93c65fc2e026d71dc780f2addce00","abstract_canon_sha256":"041a997572fc894bad3a0cb74dfdc930da963ee404516b3af9478daad2e480c5"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:56:35.137459Z","signature_b64":"BmkRZm7ZE5Sm0X9Hg+dPzqgIsQkJ/hYGqDCWIAW2kw8xn8X7dAtem6ln+GaQ6n5dPjYu/okfhXJ0BNDCE7I8BQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c7dc59c9e8b2344e32bd822e35429e9c5c19d2bf7b5602113c2280bcc3f24a8e","last_reissued_at":"2026-05-18T01:56:35.137061Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:56:35.137061Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Distribution function approach to redshift space distortions. Part IV: perturbation theory applied to dark matter","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Patrick McDonald, Teppei Okumura, Tobias Baldauf, Uro\\v{s} Seljak, Zvonimir Vlah","submitted_at":"2012-07-03T21:22:37Z","abstract_excerpt":"We develop a perturbative approach to redshift space distortions (RSD) using the phase space distribution function approach and apply it to the dark matter redshift space power spectrum and its moments. RSD can be written as a sum over density weighted velocity moments correlators, with the lowest order being density, momentum density and stress energy density. We use standard and extended perturbation theory (PT) to determine their auto and cross correlators, comparing them to N-body simulations. We show which of the terms can be modeled well with the standard PT and which need additional ter"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1207.0839","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":"1207.0839","created_at":"2026-05-18T01:56:35.137118+00:00"},{"alias_kind":"arxiv_version","alias_value":"1207.0839v2","created_at":"2026-05-18T01:56:35.137118+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1207.0839","created_at":"2026-05-18T01:56:35.137118+00:00"},{"alias_kind":"pith_short_12","alias_value":"Y7OFTSPIWI2E","created_at":"2026-05-18T12:27:27.928770+00:00"},{"alias_kind":"pith_short_16","alias_value":"Y7OFTSPIWI2E4MV5","created_at":"2026-05-18T12:27:27.928770+00:00"},{"alias_kind":"pith_short_8","alias_value":"Y7OFTSPI","created_at":"2026-05-18T12:27:27.928770+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"1611.00036","citing_title":"The DESI Experiment Part I: Science,Targeting, and Survey Design","ref_index":58,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/Y7OFTSPIWI2E4MV5QIXDKQU6TR","json":"https://pith.science/pith/Y7OFTSPIWI2E4MV5QIXDKQU6TR.json","graph_json":"https://pith.science/api/pith-number/Y7OFTSPIWI2E4MV5QIXDKQU6TR/graph.json","events_json":"https://pith.science/api/pith-number/Y7OFTSPIWI2E4MV5QIXDKQU6TR/events.json","paper":"https://pith.science/paper/Y7OFTSPI"},"agent_actions":{"view_html":"https://pith.science/pith/Y7OFTSPIWI2E4MV5QIXDKQU6TR","download_json":"https://pith.science/pith/Y7OFTSPIWI2E4MV5QIXDKQU6TR.json","view_paper":"https://pith.science/paper/Y7OFTSPI","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1207.0839&json=true","fetch_graph":"https://pith.science/api/pith-number/Y7OFTSPIWI2E4MV5QIXDKQU6TR/graph.json","fetch_events":"https://pith.science/api/pith-number/Y7OFTSPIWI2E4MV5QIXDKQU6TR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/Y7OFTSPIWI2E4MV5QIXDKQU6TR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/Y7OFTSPIWI2E4MV5QIXDKQU6TR/action/storage_attestation","attest_author":"https://pith.science/pith/Y7OFTSPIWI2E4MV5QIXDKQU6TR/action/author_attestation","sign_citation":"https://pith.science/pith/Y7OFTSPIWI2E4MV5QIXDKQU6TR/action/citation_signature","submit_replication":"https://pith.science/pith/Y7OFTSPIWI2E4MV5QIXDKQU6TR/action/replication_record"}},"created_at":"2026-05-18T01:56:35.137118+00:00","updated_at":"2026-05-18T01:56:35.137118+00:00"}