{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:BRVYI2JGY6FAIZOFOLXBACUR4O","short_pith_number":"pith:BRVYI2JG","schema_version":"1.0","canonical_sha256":"0c6b846926c78a0465c572ee100a91e3a65040df095d51e8bfd1d56ad5eb1a42","source":{"kind":"arxiv","id":"1912.06621","version":3},"attestation_state":"computed","paper":{"title":"Primordial non-Gaussianity without tails -- how to measure fNL with the bulk of the density PDF","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Cora Uhlemann, Francisco Villaescusa-Navarro, Marc Manera, Oliver Friedrich, Takahiro Nishimichi, Tobias Baldauf","submitted_at":"2019-12-13T17:33:43Z","abstract_excerpt":"We investigate the possibility to detect primordial non-Gaussianity by analysing the bulk of the probability distribution function (PDF) of late-time cosmic density fluctuations. For this purpose we devise a new method to predict the impact of general non-Gaussian initial conditions on the late-time density PDF. At redshift $z=1$ and for a smoothing scale of 30Mpc/$h$ our predictions agree with the high-resolution Quijote N-body simulations to $\\sim 0.2\\%$ precision. This is within cosmic variance of a $\\sim 100(\\mathrm{Gpc}/h)^3$ survey volume. When restricting to this 30Mpc/$h$ smoothing sca"},"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":"1912.06621","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2019-12-13T17:33:43Z","cross_cats_sorted":[],"title_canon_sha256":"1ff0d73567e3846b6a4ed1e2e3e7fb774c50511bb2e021b6dfe9ed05d0ad2a90","abstract_canon_sha256":"4e7630fa3fdd8090400c744b627a13d55b7915882e5e5d994a3325b708c49137"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T03:01:51.573669Z","signature_b64":"Bg5UckSivKrcYAld65C3b1iJ/x9JGVG1zdI07g/CrWkxjDoVupbPsdPuBt0EZLOIyrZ2UcWP5yJjnE5jZrFsAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"0c6b846926c78a0465c572ee100a91e3a65040df095d51e8bfd1d56ad5eb1a42","last_reissued_at":"2026-07-05T03:01:51.573287Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T03:01:51.573287Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Primordial non-Gaussianity without tails -- how to measure fNL with the bulk of the density PDF","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Cora Uhlemann, Francisco Villaescusa-Navarro, Marc Manera, Oliver Friedrich, Takahiro Nishimichi, Tobias Baldauf","submitted_at":"2019-12-13T17:33:43Z","abstract_excerpt":"We investigate the possibility to detect primordial non-Gaussianity by analysing the bulk of the probability distribution function (PDF) of late-time cosmic density fluctuations. For this purpose we devise a new method to predict the impact of general non-Gaussian initial conditions on the late-time density PDF. At redshift $z=1$ and for a smoothing scale of 30Mpc/$h$ our predictions agree with the high-resolution Quijote N-body simulations to $\\sim 0.2\\%$ precision. This is within cosmic variance of a $\\sim 100(\\mathrm{Gpc}/h)^3$ survey volume. When restricting to this 30Mpc/$h$ smoothing sca"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1912.06621","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/1912.06621/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":"1912.06621","created_at":"2026-07-05T03:01:51.573351+00:00"},{"alias_kind":"arxiv_version","alias_value":"1912.06621v3","created_at":"2026-07-05T03:01:51.573351+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1912.06621","created_at":"2026-07-05T03:01:51.573351+00:00"},{"alias_kind":"pith_short_12","alias_value":"BRVYI2JGY6FA","created_at":"2026-07-05T03:01:51.573351+00:00"},{"alias_kind":"pith_short_16","alias_value":"BRVYI2JGY6FAIZOF","created_at":"2026-07-05T03:01:51.573351+00:00"},{"alias_kind":"pith_short_8","alias_value":"BRVYI2JG","created_at":"2026-07-05T03:01:51.573351+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2607.08593","citing_title":"Beyond {\\Lambda}CDM with the SKA Observatory -- II: Unveiling the Secrets of the Early Universe","ref_index":24,"is_internal_anchor":true},{"citing_arxiv_id":"2607.06526","citing_title":"One with HI: Modelling HI Intensity Mapping one-point statistics including systematics","ref_index":19,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/BRVYI2JGY6FAIZOFOLXBACUR4O","json":"https://pith.science/pith/BRVYI2JGY6FAIZOFOLXBACUR4O.json","graph_json":"https://pith.science/api/pith-number/BRVYI2JGY6FAIZOFOLXBACUR4O/graph.json","events_json":"https://pith.science/api/pith-number/BRVYI2JGY6FAIZOFOLXBACUR4O/events.json","paper":"https://pith.science/paper/BRVYI2JG"},"agent_actions":{"view_html":"https://pith.science/pith/BRVYI2JGY6FAIZOFOLXBACUR4O","download_json":"https://pith.science/pith/BRVYI2JGY6FAIZOFOLXBACUR4O.json","view_paper":"https://pith.science/paper/BRVYI2JG","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1912.06621&json=true","fetch_graph":"https://pith.science/api/pith-number/BRVYI2JGY6FAIZOFOLXBACUR4O/graph.json","fetch_events":"https://pith.science/api/pith-number/BRVYI2JGY6FAIZOFOLXBACUR4O/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/BRVYI2JGY6FAIZOFOLXBACUR4O/action/timestamp_anchor","attest_storage":"https://pith.science/pith/BRVYI2JGY6FAIZOFOLXBACUR4O/action/storage_attestation","attest_author":"https://pith.science/pith/BRVYI2JGY6FAIZOFOLXBACUR4O/action/author_attestation","sign_citation":"https://pith.science/pith/BRVYI2JGY6FAIZOFOLXBACUR4O/action/citation_signature","submit_replication":"https://pith.science/pith/BRVYI2JGY6FAIZOFOLXBACUR4O/action/replication_record"}},"created_at":"2026-07-05T03:01:51.573351+00:00","updated_at":"2026-07-05T03:01:51.573351+00:00"}