{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:C7BAK75ZBLTDBXV7OBJ6R5HKQR","short_pith_number":"pith:C7BAK75Z","schema_version":"1.0","canonical_sha256":"17c2057fb90ae630debf7053e8f4ea845c80853be18184464d856ffae7232906","source":{"kind":"arxiv","id":"1503.05920","version":3},"attestation_state":"computed","paper":{"title":"Matter power spectrum and the challenge of percent accuracy","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Aurel Schneider, Darren S. Reed, Doug Potter, Frazer R. Pearce, Joachim Stadel, Julian Onions, Robert E. Smith, Romain Teyssier, Roman Scoccimarro, Volker Springel","submitted_at":"2015-03-19T20:00:23Z","abstract_excerpt":"Future galaxy surveys require one percent precision in the theoretical knowledge of the power spectrum over a large range including very nonlinear scales. While this level of accuracy is easily obtained in the linear regime with perturbation theory, it represents a serious challenge for small scales where numerical simulations are required. In this paper we quantify the precision of present-day $N$-body methods, identifying main potential error sources from the set-up of initial conditions to the measurement of the final power spectrum. We directly compare three widely used $N$-body codes, Ram"},"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":"1503.05920","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2015-03-19T20:00:23Z","cross_cats_sorted":[],"title_canon_sha256":"f2ba81c1bab276c913f34b94cfee35e7f51ea9946b0e4719084f182d2cd17879","abstract_canon_sha256":"37f799c8da7c29f094ba8c4a589db8068f4c9dbc705a3c00414cf0a2bb2f00e4"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:15:46.965078Z","signature_b64":"EpuLuYJ0iwf1b1Ah09ocWsG7Ou+Z1WwhD5L5m3gsXNzqoOqQQ+a5+siJmWfoRsp3qKbzwEcIf4UoyDmaScrzCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"17c2057fb90ae630debf7053e8f4ea845c80853be18184464d856ffae7232906","last_reissued_at":"2026-05-18T01:15:46.964393Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:15:46.964393Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Matter power spectrum and the challenge of percent accuracy","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Aurel Schneider, Darren S. Reed, Doug Potter, Frazer R. Pearce, Joachim Stadel, Julian Onions, Robert E. Smith, Romain Teyssier, Roman Scoccimarro, Volker Springel","submitted_at":"2015-03-19T20:00:23Z","abstract_excerpt":"Future galaxy surveys require one percent precision in the theoretical knowledge of the power spectrum over a large range including very nonlinear scales. While this level of accuracy is easily obtained in the linear regime with perturbation theory, it represents a serious challenge for small scales where numerical simulations are required. In this paper we quantify the precision of present-day $N$-body methods, identifying main potential error sources from the set-up of initial conditions to the measurement of the final power spectrum. We directly compare three widely used $N$-body codes, Ram"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1503.05920","kind":"arxiv","version":3},"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":"1503.05920","created_at":"2026-05-18T01:15:46.964505+00:00"},{"alias_kind":"arxiv_version","alias_value":"1503.05920v3","created_at":"2026-05-18T01:15:46.964505+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1503.05920","created_at":"2026-05-18T01:15:46.964505+00:00"},{"alias_kind":"pith_short_12","alias_value":"C7BAK75ZBLTD","created_at":"2026-05-18T12:29:14.074870+00:00"},{"alias_kind":"pith_short_16","alias_value":"C7BAK75ZBLTDBXV7","created_at":"2026-05-18T12:29:14.074870+00:00"},{"alias_kind":"pith_short_8","alias_value":"C7BAK75Z","created_at":"2026-05-18T12:29:14.074870+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2510.14888","citing_title":"Modeling nonlinear scales for dynamical dark energy cosmologies with COLA","ref_index":79,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/C7BAK75ZBLTDBXV7OBJ6R5HKQR","json":"https://pith.science/pith/C7BAK75ZBLTDBXV7OBJ6R5HKQR.json","graph_json":"https://pith.science/api/pith-number/C7BAK75ZBLTDBXV7OBJ6R5HKQR/graph.json","events_json":"https://pith.science/api/pith-number/C7BAK75ZBLTDBXV7OBJ6R5HKQR/events.json","paper":"https://pith.science/paper/C7BAK75Z"},"agent_actions":{"view_html":"https://pith.science/pith/C7BAK75ZBLTDBXV7OBJ6R5HKQR","download_json":"https://pith.science/pith/C7BAK75ZBLTDBXV7OBJ6R5HKQR.json","view_paper":"https://pith.science/paper/C7BAK75Z","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1503.05920&json=true","fetch_graph":"https://pith.science/api/pith-number/C7BAK75ZBLTDBXV7OBJ6R5HKQR/graph.json","fetch_events":"https://pith.science/api/pith-number/C7BAK75ZBLTDBXV7OBJ6R5HKQR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/C7BAK75ZBLTDBXV7OBJ6R5HKQR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/C7BAK75ZBLTDBXV7OBJ6R5HKQR/action/storage_attestation","attest_author":"https://pith.science/pith/C7BAK75ZBLTDBXV7OBJ6R5HKQR/action/author_attestation","sign_citation":"https://pith.science/pith/C7BAK75ZBLTDBXV7OBJ6R5HKQR/action/citation_signature","submit_replication":"https://pith.science/pith/C7BAK75ZBLTDBXV7OBJ6R5HKQR/action/replication_record"}},"created_at":"2026-05-18T01:15:46.964505+00:00","updated_at":"2026-05-18T01:15:46.964505+00:00"}