{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2010:TDGGTRQBZ3HGHPUVAKTPUVIOVV","short_pith_number":"pith:TDGGTRQB","schema_version":"1.0","canonical_sha256":"98cc69c601cece63be9502a6fa550ead402d5182d4d87ff2e574337f7b54ee2c","source":{"kind":"arxiv","id":"1005.1203","version":2},"attestation_state":"computed","paper":{"title":"An Improved Calculation of the Non-Gaussian Halo Mass Function","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Aseem Paranjape, Guido D'Amico, Jorge Nore\\~na, Marcello Musso","submitted_at":"2010-05-07T13:25:30Z","abstract_excerpt":"The abundance of collapsed objects in the universe, or halo mass function, is an important theoretical tool in studying the effects of primordially generated non-Gaussianities on the large scale structure. The non-Gaussian mass function has been calculated by several authors in different ways, typically by exploiting the smallness of certain parameters which naturally appear in the calculation, to set up a perturbative expansion. We improve upon the existing results for the mass function by combining path integral methods and saddle point techniques (which have been separately applied in previ"},"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":"1005.1203","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2010-05-07T13:25:30Z","cross_cats_sorted":["hep-ph"],"title_canon_sha256":"10486d2f062e9b497fe01e7f5d1c754488ffc9d0e819c272e99f74ffa43c81a2","abstract_canon_sha256":"dbbc3c7a89e6998e355fc590f2873ae81597c54fa9831d4a1d3025cd91ca3f99"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:24:08.725385Z","signature_b64":"Y20IwkVlSBjEc72eC8Z07tKJPhBDIrnuJBtEub4Ab7hGaEmZAAA9wubcDQ4t49nlgdc1+tkeHiFyBh1JZBvgCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"98cc69c601cece63be9502a6fa550ead402d5182d4d87ff2e574337f7b54ee2c","last_reissued_at":"2026-05-18T02:24:08.724620Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:24:08.724620Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"An Improved Calculation of the Non-Gaussian Halo Mass Function","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Aseem Paranjape, Guido D'Amico, Jorge Nore\\~na, Marcello Musso","submitted_at":"2010-05-07T13:25:30Z","abstract_excerpt":"The abundance of collapsed objects in the universe, or halo mass function, is an important theoretical tool in studying the effects of primordially generated non-Gaussianities on the large scale structure. The non-Gaussian mass function has been calculated by several authors in different ways, typically by exploiting the smallness of certain parameters which naturally appear in the calculation, to set up a perturbative expansion. We improve upon the existing results for the mass function by combining path integral methods and saddle point techniques (which have been separately applied in previ"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1005.1203","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":"1005.1203","created_at":"2026-05-18T02:24:08.724721+00:00"},{"alias_kind":"arxiv_version","alias_value":"1005.1203v2","created_at":"2026-05-18T02:24:08.724721+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1005.1203","created_at":"2026-05-18T02:24:08.724721+00:00"},{"alias_kind":"pith_short_12","alias_value":"TDGGTRQBZ3HG","created_at":"2026-05-18T12:26:13.927090+00:00"},{"alias_kind":"pith_short_16","alias_value":"TDGGTRQBZ3HGHPUV","created_at":"2026-05-18T12:26:13.927090+00:00"},{"alias_kind":"pith_short_8","alias_value":"TDGGTRQB","created_at":"2026-05-18T12:26:13.927090+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2607.05505","citing_title":"The dark matter halo mass function in the $\\Lambda\\mathrm{CDM}$ cosmology at all times and over all scales -- from planetary to galaxy cluster masses","ref_index":124,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/TDGGTRQBZ3HGHPUVAKTPUVIOVV","json":"https://pith.science/pith/TDGGTRQBZ3HGHPUVAKTPUVIOVV.json","graph_json":"https://pith.science/api/pith-number/TDGGTRQBZ3HGHPUVAKTPUVIOVV/graph.json","events_json":"https://pith.science/api/pith-number/TDGGTRQBZ3HGHPUVAKTPUVIOVV/events.json","paper":"https://pith.science/paper/TDGGTRQB"},"agent_actions":{"view_html":"https://pith.science/pith/TDGGTRQBZ3HGHPUVAKTPUVIOVV","download_json":"https://pith.science/pith/TDGGTRQBZ3HGHPUVAKTPUVIOVV.json","view_paper":"https://pith.science/paper/TDGGTRQB","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1005.1203&json=true","fetch_graph":"https://pith.science/api/pith-number/TDGGTRQBZ3HGHPUVAKTPUVIOVV/graph.json","fetch_events":"https://pith.science/api/pith-number/TDGGTRQBZ3HGHPUVAKTPUVIOVV/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/TDGGTRQBZ3HGHPUVAKTPUVIOVV/action/timestamp_anchor","attest_storage":"https://pith.science/pith/TDGGTRQBZ3HGHPUVAKTPUVIOVV/action/storage_attestation","attest_author":"https://pith.science/pith/TDGGTRQBZ3HGHPUVAKTPUVIOVV/action/author_attestation","sign_citation":"https://pith.science/pith/TDGGTRQBZ3HGHPUVAKTPUVIOVV/action/citation_signature","submit_replication":"https://pith.science/pith/TDGGTRQBZ3HGHPUVAKTPUVIOVV/action/replication_record"}},"created_at":"2026-05-18T02:24:08.724721+00:00","updated_at":"2026-05-18T02:24:08.724721+00:00"}