{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:XFC3YUVIOY2XBRYAJNBK7T4ZHI","short_pith_number":"pith:XFC3YUVI","schema_version":"1.0","canonical_sha256":"b945bc52a8763570c7004b42afcf993a23ad0de23719b33ee96de785d0582704","source":{"kind":"arxiv","id":"1104.2934","version":2},"attestation_state":"computed","paper":{"title":"The Cosmic Linear Anisotropy Solving System (CLASS) III: Comparision with CAMB for LambdaCDM","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Julien Lesgourgues","submitted_at":"2011-04-14T22:09:26Z","abstract_excerpt":"By confronting the two independent Boltzmann codes CLASS and CAMB, we establish that for concordance cosmology and for a given recombination history, lensed CMB and matter power spectra can be computed by current codes with an accuracy of 0.01%. We list a few tiny changes in CAMB which are necessary in order to reach such a level. Using the common limit of the two codes as a set of reference spectra, we derive precision settings corresponding to fixed levels of error in the computation of a CMB likelihood. We find that for a given precision level, CLASS is about 2.5 times faster than CAMB for "},"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":"1104.2934","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2011-04-14T22:09:26Z","cross_cats_sorted":[],"title_canon_sha256":"ed81ee14af5c2564033e55d7da71548a507581178faa3438e01e9ec7530f4d85","abstract_canon_sha256":"20bf0609cf1e43ef2246c49e5e18aa112e84ee921243b8c0369b0e47afd6d5a9"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:22:09.029753Z","signature_b64":"ghw/cPZGC8UiblKiDp5cGukqvBEXNkxf6PzJpkJHVbfYE0jb5w6UEXV4gZUHEQbdgwtas+xDFJAEWs95iBZdDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b945bc52a8763570c7004b42afcf993a23ad0de23719b33ee96de785d0582704","last_reissued_at":"2026-05-18T02:22:09.029254Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:22:09.029254Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Cosmic Linear Anisotropy Solving System (CLASS) III: Comparision with CAMB for LambdaCDM","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Julien Lesgourgues","submitted_at":"2011-04-14T22:09:26Z","abstract_excerpt":"By confronting the two independent Boltzmann codes CLASS and CAMB, we establish that for concordance cosmology and for a given recombination history, lensed CMB and matter power spectra can be computed by current codes with an accuracy of 0.01%. We list a few tiny changes in CAMB which are necessary in order to reach such a level. Using the common limit of the two codes as a set of reference spectra, we derive precision settings corresponding to fixed levels of error in the computation of a CMB likelihood. We find that for a given precision level, CLASS is about 2.5 times faster than CAMB for "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1104.2934","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":"1104.2934","created_at":"2026-05-18T02:22:09.029334+00:00"},{"alias_kind":"arxiv_version","alias_value":"1104.2934v2","created_at":"2026-05-18T02:22:09.029334+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1104.2934","created_at":"2026-05-18T02:22:09.029334+00:00"},{"alias_kind":"pith_short_12","alias_value":"XFC3YUVIOY2X","created_at":"2026-05-18T12:26:44.992195+00:00"},{"alias_kind":"pith_short_16","alias_value":"XFC3YUVIOY2XBRYA","created_at":"2026-05-18T12:26:44.992195+00:00"},{"alias_kind":"pith_short_8","alias_value":"XFC3YUVI","created_at":"2026-05-18T12:26:44.992195+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":7,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"2510.13752","citing_title":"Effects of primordial magnetic fields on 21 cm multifrequency angular power spectra","ref_index":26,"is_internal_anchor":true},{"citing_arxiv_id":"2304.05202","citing_title":"The Atacama Cosmology Telescope: A Measurement of the DR6 CMB Lensing Power Spectrum and its Implications for Structure Growth","ref_index":53,"is_internal_anchor":true},{"citing_arxiv_id":"2601.19812","citing_title":"An essential building block for cosmological zoom-in perturbation theory","ref_index":56,"is_internal_anchor":true},{"citing_arxiv_id":"1104.2933","citing_title":"The Cosmic Linear Anisotropy Solving System (CLASS) II: Approximation schemes","ref_index":8,"is_internal_anchor":false},{"citing_arxiv_id":"2604.03167","citing_title":"Mapping the redshift drift at various redshifts through cosmography","ref_index":74,"is_internal_anchor":false},{"citing_arxiv_id":"2605.05323","citing_title":"Primordial Magnetic Fields at Cosmic Dawn: 21-cm Forecasts with HERA and SKA","ref_index":58,"is_internal_anchor":false},{"citing_arxiv_id":"2604.05095","citing_title":"A generic $\\omega_b$ tension in early-time solutions to the Hubble tension","ref_index":47,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XFC3YUVIOY2XBRYAJNBK7T4ZHI","json":"https://pith.science/pith/XFC3YUVIOY2XBRYAJNBK7T4ZHI.json","graph_json":"https://pith.science/api/pith-number/XFC3YUVIOY2XBRYAJNBK7T4ZHI/graph.json","events_json":"https://pith.science/api/pith-number/XFC3YUVIOY2XBRYAJNBK7T4ZHI/events.json","paper":"https://pith.science/paper/XFC3YUVI"},"agent_actions":{"view_html":"https://pith.science/pith/XFC3YUVIOY2XBRYAJNBK7T4ZHI","download_json":"https://pith.science/pith/XFC3YUVIOY2XBRYAJNBK7T4ZHI.json","view_paper":"https://pith.science/paper/XFC3YUVI","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1104.2934&json=true","fetch_graph":"https://pith.science/api/pith-number/XFC3YUVIOY2XBRYAJNBK7T4ZHI/graph.json","fetch_events":"https://pith.science/api/pith-number/XFC3YUVIOY2XBRYAJNBK7T4ZHI/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XFC3YUVIOY2XBRYAJNBK7T4ZHI/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XFC3YUVIOY2XBRYAJNBK7T4ZHI/action/storage_attestation","attest_author":"https://pith.science/pith/XFC3YUVIOY2XBRYAJNBK7T4ZHI/action/author_attestation","sign_citation":"https://pith.science/pith/XFC3YUVIOY2XBRYAJNBK7T4ZHI/action/citation_signature","submit_replication":"https://pith.science/pith/XFC3YUVIOY2XBRYAJNBK7T4ZHI/action/replication_record"}},"created_at":"2026-05-18T02:22:09.029334+00:00","updated_at":"2026-05-18T02:22:09.029334+00:00"}