{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:WHCYJEUVWE2QN77GN7RKNIRP6U","short_pith_number":"pith:WHCYJEUV","schema_version":"1.0","canonical_sha256":"b1c5849295b13506ffe66fe2a6a22ff5364e64d5b08677cb5018b7c73fb2b8af","source":{"kind":"arxiv","id":"2008.09123","version":2},"attestation_state":"computed","paper":{"title":"Cosmological perturbations for two cold fluids in $\\Lambda$CDM","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Cora Uhlemann, Cornelius Rampf, Oliver Hahn","submitted_at":"2020-08-20T18:00:01Z","abstract_excerpt":"The cosmic large-scale structure of our Universe is comprised of baryons and cold dark matter (CDM). Yet it is customary to treat these two components as a combined single-matter fluid with vanishing pressure, which is justified only for sufficiently large scales and late times. Here we go beyond the single-fluid approximation and develop the perturbation theory for two gravitationally coupled fluids while still assuming vanishing pressure. We mostly focus on perturbative expansions in powers of $D$ (or $D_+$), the linear structure growth of matter in a $\\Lambda$CDM Universe with cosmological "},"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":"2008.09123","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2020-08-20T18:00:01Z","cross_cats_sorted":[],"title_canon_sha256":"ffdfbf57ad72d22bdd68e12ba14456ed8876f1b3fc63c948113de39b883dc5ec","abstract_canon_sha256":"0aabdcecb8ddbfec69b17567ae6b740c8d77e38cdcd7daf6dc3a0a94f81a7ccf"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T01:56:43.685804Z","signature_b64":"AzUgot323/gs4B7TgWcFfBA1Fkajgz4CMTew4sANsDltiCsbvjSzChP6TBdh3MSJGKZeRrrD0Ds3lZqq4lT3Dw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b1c5849295b13506ffe66fe2a6a22ff5364e64d5b08677cb5018b7c73fb2b8af","last_reissued_at":"2026-07-05T01:56:43.685394Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T01:56:43.685394Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Cosmological perturbations for two cold fluids in $\\Lambda$CDM","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Cora Uhlemann, Cornelius Rampf, Oliver Hahn","submitted_at":"2020-08-20T18:00:01Z","abstract_excerpt":"The cosmic large-scale structure of our Universe is comprised of baryons and cold dark matter (CDM). Yet it is customary to treat these two components as a combined single-matter fluid with vanishing pressure, which is justified only for sufficiently large scales and late times. Here we go beyond the single-fluid approximation and develop the perturbation theory for two gravitationally coupled fluids while still assuming vanishing pressure. We mostly focus on perturbative expansions in powers of $D$ (or $D_+$), the linear structure growth of matter in a $\\Lambda$CDM Universe with cosmological "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2008.09123","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/2008.09123/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":"2008.09123","created_at":"2026-07-05T01:56:43.685452+00:00"},{"alias_kind":"arxiv_version","alias_value":"2008.09123v2","created_at":"2026-07-05T01:56:43.685452+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2008.09123","created_at":"2026-07-05T01:56:43.685452+00:00"},{"alias_kind":"pith_short_12","alias_value":"WHCYJEUVWE2Q","created_at":"2026-07-05T01:56:43.685452+00:00"},{"alias_kind":"pith_short_16","alias_value":"WHCYJEUVWE2QN77G","created_at":"2026-07-05T01:56:43.685452+00:00"},{"alias_kind":"pith_short_8","alias_value":"WHCYJEUV","created_at":"2026-07-05T01:56:43.685452+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2603.25999","citing_title":"Cosmological constraints on the big bang quantum cosmology model","ref_index":1,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/WHCYJEUVWE2QN77GN7RKNIRP6U","json":"https://pith.science/pith/WHCYJEUVWE2QN77GN7RKNIRP6U.json","graph_json":"https://pith.science/api/pith-number/WHCYJEUVWE2QN77GN7RKNIRP6U/graph.json","events_json":"https://pith.science/api/pith-number/WHCYJEUVWE2QN77GN7RKNIRP6U/events.json","paper":"https://pith.science/paper/WHCYJEUV"},"agent_actions":{"view_html":"https://pith.science/pith/WHCYJEUVWE2QN77GN7RKNIRP6U","download_json":"https://pith.science/pith/WHCYJEUVWE2QN77GN7RKNIRP6U.json","view_paper":"https://pith.science/paper/WHCYJEUV","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2008.09123&json=true","fetch_graph":"https://pith.science/api/pith-number/WHCYJEUVWE2QN77GN7RKNIRP6U/graph.json","fetch_events":"https://pith.science/api/pith-number/WHCYJEUVWE2QN77GN7RKNIRP6U/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/WHCYJEUVWE2QN77GN7RKNIRP6U/action/timestamp_anchor","attest_storage":"https://pith.science/pith/WHCYJEUVWE2QN77GN7RKNIRP6U/action/storage_attestation","attest_author":"https://pith.science/pith/WHCYJEUVWE2QN77GN7RKNIRP6U/action/author_attestation","sign_citation":"https://pith.science/pith/WHCYJEUVWE2QN77GN7RKNIRP6U/action/citation_signature","submit_replication":"https://pith.science/pith/WHCYJEUVWE2QN77GN7RKNIRP6U/action/replication_record"}},"created_at":"2026-07-05T01:56:43.685452+00:00","updated_at":"2026-07-05T01:56:43.685452+00:00"}