{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:FK7CU7MG45GX5Q5RTC2OLDQMXK","short_pith_number":"pith:FK7CU7MG","schema_version":"1.0","canonical_sha256":"2abe2a7d86e74d7ec3b198b4e58e0cbaa8ef2e122a6b142e078441ea27c6f409","source":{"kind":"arxiv","id":"1802.07622","version":2},"attestation_state":"computed","paper":{"title":"Cubic Halo Bias in Eulerian and Lagrangian Space","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Muntazir Mehdi Abidi, Tobias Baldauf","submitted_at":"2018-02-21T15:51:25Z","abstract_excerpt":"Predictions of the next-to-leading order, i.e. one-loop, halo power spectra depend on local and non-local bias parameters up to cubic order. The linear bias parameter can be estimated from the large scale limit of the halo-matter power spectrum, and the second order bias parameters from the large scale, tree-level, bispectrum. Cubic operators would naturally be quantified using the tree-level trispectrum. As the latter is computationally expensive, we extent the quadratic field method proposed in Schmittfull et al. 2014 to cubic fields in order to estimate cubic bias parameters. We cross-corre"},"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":"1802.07622","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2018-02-21T15:51:25Z","cross_cats_sorted":[],"title_canon_sha256":"4f1771cd9780f8dcd4966a92e30c59c23e23a5d8f862c6bc1f1c6f25b5284b98","abstract_canon_sha256":"eee63cd0ecf1e498d4b718617e1ea3274d0dc34eeeb2e4a57c5d38925a84a440"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:09:16.063588Z","signature_b64":"zNYN3UKKUC8yV+IOHQBf9xVDlBB02xKofHDykkoJXcRTzunwZFOe01A0oAPMosSrdboxgYPvVdieFEAb0H/ZBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2abe2a7d86e74d7ec3b198b4e58e0cbaa8ef2e122a6b142e078441ea27c6f409","last_reissued_at":"2026-05-18T00:09:16.062913Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:09:16.062913Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Cubic Halo Bias in Eulerian and Lagrangian Space","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Muntazir Mehdi Abidi, Tobias Baldauf","submitted_at":"2018-02-21T15:51:25Z","abstract_excerpt":"Predictions of the next-to-leading order, i.e. one-loop, halo power spectra depend on local and non-local bias parameters up to cubic order. The linear bias parameter can be estimated from the large scale limit of the halo-matter power spectrum, and the second order bias parameters from the large scale, tree-level, bispectrum. Cubic operators would naturally be quantified using the tree-level trispectrum. As the latter is computationally expensive, we extent the quadratic field method proposed in Schmittfull et al. 2014 to cubic fields in order to estimate cubic bias parameters. We cross-corre"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1802.07622","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":"1802.07622","created_at":"2026-05-18T00:09:16.063019+00:00"},{"alias_kind":"arxiv_version","alias_value":"1802.07622v2","created_at":"2026-05-18T00:09:16.063019+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1802.07622","created_at":"2026-05-18T00:09:16.063019+00:00"},{"alias_kind":"pith_short_12","alias_value":"FK7CU7MG45GX","created_at":"2026-05-18T12:32:22.470017+00:00"},{"alias_kind":"pith_short_16","alias_value":"FK7CU7MG45GX5Q5R","created_at":"2026-05-18T12:32:22.470017+00:00"},{"alias_kind":"pith_short_8","alias_value":"FK7CU7MG","created_at":"2026-05-18T12:32:22.470017+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.06021","citing_title":"Testing parity with composite-field spectra of BOSS and DESI luminous red galaxies","ref_index":52,"is_internal_anchor":false},{"citing_arxiv_id":"2604.14504","citing_title":"Forecasting neutrino mass constraints from the Nancy Grace Roman Space Telescope","ref_index":95,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/FK7CU7MG45GX5Q5RTC2OLDQMXK","json":"https://pith.science/pith/FK7CU7MG45GX5Q5RTC2OLDQMXK.json","graph_json":"https://pith.science/api/pith-number/FK7CU7MG45GX5Q5RTC2OLDQMXK/graph.json","events_json":"https://pith.science/api/pith-number/FK7CU7MG45GX5Q5RTC2OLDQMXK/events.json","paper":"https://pith.science/paper/FK7CU7MG"},"agent_actions":{"view_html":"https://pith.science/pith/FK7CU7MG45GX5Q5RTC2OLDQMXK","download_json":"https://pith.science/pith/FK7CU7MG45GX5Q5RTC2OLDQMXK.json","view_paper":"https://pith.science/paper/FK7CU7MG","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1802.07622&json=true","fetch_graph":"https://pith.science/api/pith-number/FK7CU7MG45GX5Q5RTC2OLDQMXK/graph.json","fetch_events":"https://pith.science/api/pith-number/FK7CU7MG45GX5Q5RTC2OLDQMXK/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/FK7CU7MG45GX5Q5RTC2OLDQMXK/action/timestamp_anchor","attest_storage":"https://pith.science/pith/FK7CU7MG45GX5Q5RTC2OLDQMXK/action/storage_attestation","attest_author":"https://pith.science/pith/FK7CU7MG45GX5Q5RTC2OLDQMXK/action/author_attestation","sign_citation":"https://pith.science/pith/FK7CU7MG45GX5Q5RTC2OLDQMXK/action/citation_signature","submit_replication":"https://pith.science/pith/FK7CU7MG45GX5Q5RTC2OLDQMXK/action/replication_record"}},"created_at":"2026-05-18T00:09:16.063019+00:00","updated_at":"2026-05-18T00:09:16.063019+00:00"}