{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:VM6VT3AVH3ABIGDMYVKRSOX7WR","short_pith_number":"pith:VM6VT3AV","schema_version":"1.0","canonical_sha256":"ab3d59ec153ec014186cc555193affb44cb69f9ef8f0f2f08d51357c44c6f470","source":{"kind":"arxiv","id":"2211.07565","version":2},"attestation_state":"computed","paper":{"title":"Quijote-PNG: Quasi-maximum likelihood estimation of Primordial Non-Gaussianity in the non-linear halo density field","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Benjamin D. Wandelt, Dionysios Karagiannis, Drew Jamieson, Francisco Villaescusa-Navarro, Gabriel Jung, Licia Verde, Marco Baldi, Michele Liguori, William R Coulton","submitted_at":"2022-11-14T17:34:46Z","abstract_excerpt":"We study primordial non-Gaussian signatures in the redshift-space halo field on non-linear scales, using a quasi-maximum likelihood estimator based on optimally compressed power spectrum and modal bispectrum statistics. We train and validate the estimator on a suite of halo catalogues constructed from the Quijote-PNG N-body simulations, which we release to accompany this paper. We verify its unbiasedness and near optimality, for the three main types of primordial non-Gaussianity (PNG): local, equilateral, and orthogonal. We compare the modal bispectrum expansion with a $k$-binning approach, sh"},"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":"2211.07565","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2022-11-14T17:34:46Z","cross_cats_sorted":[],"title_canon_sha256":"2eeb9460ef5b887e30fd267440d4b73a55f522496aaf0d5025b586952a1761cf","abstract_canon_sha256":"223a30ddf78d77791caa28727e3ad6d3542b76c30b77d23eeb65159fc60c04ad"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T06:11:17.833799Z","signature_b64":"Bb4ar/UeVOLrtADIgC32eoCcyVl7NyIoEj+WHJFo8Hpe2mIB8wzh7EQq9xFZqKU7GEyAJWiqIDeGGKC+uqXlAQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ab3d59ec153ec014186cc555193affb44cb69f9ef8f0f2f08d51357c44c6f470","last_reissued_at":"2026-07-05T06:11:17.833361Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T06:11:17.833361Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Quijote-PNG: Quasi-maximum likelihood estimation of Primordial Non-Gaussianity in the non-linear halo density field","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Benjamin D. Wandelt, Dionysios Karagiannis, Drew Jamieson, Francisco Villaescusa-Navarro, Gabriel Jung, Licia Verde, Marco Baldi, Michele Liguori, William R Coulton","submitted_at":"2022-11-14T17:34:46Z","abstract_excerpt":"We study primordial non-Gaussian signatures in the redshift-space halo field on non-linear scales, using a quasi-maximum likelihood estimator based on optimally compressed power spectrum and modal bispectrum statistics. We train and validate the estimator on a suite of halo catalogues constructed from the Quijote-PNG N-body simulations, which we release to accompany this paper. We verify its unbiasedness and near optimality, for the three main types of primordial non-Gaussianity (PNG): local, equilateral, and orthogonal. We compare the modal bispectrum expansion with a $k$-binning approach, sh"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2211.07565","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/2211.07565/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":"2211.07565","created_at":"2026-07-05T06:11:17.833423+00:00"},{"alias_kind":"arxiv_version","alias_value":"2211.07565v2","created_at":"2026-07-05T06:11:17.833423+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2211.07565","created_at":"2026-07-05T06:11:17.833423+00:00"},{"alias_kind":"pith_short_12","alias_value":"VM6VT3AVH3AB","created_at":"2026-07-05T06:11:17.833423+00:00"},{"alias_kind":"pith_short_16","alias_value":"VM6VT3AVH3ABIGDM","created_at":"2026-07-05T06:11:17.833423+00:00"},{"alias_kind":"pith_short_8","alias_value":"VM6VT3AV","created_at":"2026-07-05T06:11:17.833423+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.03259","citing_title":"Cosmology with HI Intensity Mapping","ref_index":200,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/VM6VT3AVH3ABIGDMYVKRSOX7WR","json":"https://pith.science/pith/VM6VT3AVH3ABIGDMYVKRSOX7WR.json","graph_json":"https://pith.science/api/pith-number/VM6VT3AVH3ABIGDMYVKRSOX7WR/graph.json","events_json":"https://pith.science/api/pith-number/VM6VT3AVH3ABIGDMYVKRSOX7WR/events.json","paper":"https://pith.science/paper/VM6VT3AV"},"agent_actions":{"view_html":"https://pith.science/pith/VM6VT3AVH3ABIGDMYVKRSOX7WR","download_json":"https://pith.science/pith/VM6VT3AVH3ABIGDMYVKRSOX7WR.json","view_paper":"https://pith.science/paper/VM6VT3AV","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2211.07565&json=true","fetch_graph":"https://pith.science/api/pith-number/VM6VT3AVH3ABIGDMYVKRSOX7WR/graph.json","fetch_events":"https://pith.science/api/pith-number/VM6VT3AVH3ABIGDMYVKRSOX7WR/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/VM6VT3AVH3ABIGDMYVKRSOX7WR/action/timestamp_anchor","attest_storage":"https://pith.science/pith/VM6VT3AVH3ABIGDMYVKRSOX7WR/action/storage_attestation","attest_author":"https://pith.science/pith/VM6VT3AVH3ABIGDMYVKRSOX7WR/action/author_attestation","sign_citation":"https://pith.science/pith/VM6VT3AVH3ABIGDMYVKRSOX7WR/action/citation_signature","submit_replication":"https://pith.science/pith/VM6VT3AVH3ABIGDMYVKRSOX7WR/action/replication_record"}},"created_at":"2026-07-05T06:11:17.833423+00:00","updated_at":"2026-07-05T06:11:17.833423+00:00"}