{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:G2PUR3OPVTJRIIQMFGZR6JM5C5","short_pith_number":"pith:G2PUR3OP","schema_version":"1.0","canonical_sha256":"369f48edcfacd314220c29b31f259d17701d0a3c78880ec739c0898491d6bab2","source":{"kind":"arxiv","id":"1405.7023","version":4},"attestation_state":"computed","paper":{"title":"Calculating the mass spectrum of primordial black holes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"gr-qc","authors_text":"Christian T. Byrnes, Misao Sasaki, Sam Young","submitted_at":"2014-05-27T19:23:15Z","abstract_excerpt":"We reinspect the calculation for the mass fraction of primordial black holes (PBHs) which are formed from primordial perturbations, finding that performing the calculation using the comoving curvature perturbation $\\mathcal{R}_{c}$ in the standard way vastly overestimates the number of PBHs, by many orders of magnitude. This is because PBHs form shortly after horizon entry, meaning modes significantly larger than the PBH are unobservable and should not affect whether a PBH forms or not - this important effect is not taken into account by smoothing the distribution in the standard fashion. We d"},"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":"1405.7023","kind":"arxiv","version":4},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2014-05-27T19:23:15Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"2f3103b0cfddfd6d5adf08b2d0282d07df80ce2064a8ace9057b9accd2458e78","abstract_canon_sha256":"7b0a6d52803a6077df7b02d7ae2b2c6b61cdfdefc60c1d8dca92bcd17e05e924"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:25:40.361687Z","signature_b64":"tFRnAx6CGZmLw2l+HMuMgJQ+7DAtRSSsCEq7iu1XvBSAbjRnXCmhk27y+C1hDoKs/QZGLT+MPYpz0aH/Lh2JBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"369f48edcfacd314220c29b31f259d17701d0a3c78880ec739c0898491d6bab2","last_reissued_at":"2026-05-18T02:25:40.361256Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:25:40.361256Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Calculating the mass spectrum of primordial black holes","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"gr-qc","authors_text":"Christian T. Byrnes, Misao Sasaki, Sam Young","submitted_at":"2014-05-27T19:23:15Z","abstract_excerpt":"We reinspect the calculation for the mass fraction of primordial black holes (PBHs) which are formed from primordial perturbations, finding that performing the calculation using the comoving curvature perturbation $\\mathcal{R}_{c}$ in the standard way vastly overestimates the number of PBHs, by many orders of magnitude. This is because PBHs form shortly after horizon entry, meaning modes significantly larger than the PBH are unobservable and should not affect whether a PBH forms or not - this important effect is not taken into account by smoothing the distribution in the standard fashion. We d"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1405.7023","kind":"arxiv","version":4},"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":"1405.7023","created_at":"2026-05-18T02:25:40.361328+00:00"},{"alias_kind":"arxiv_version","alias_value":"1405.7023v4","created_at":"2026-05-18T02:25:40.361328+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1405.7023","created_at":"2026-05-18T02:25:40.361328+00:00"},{"alias_kind":"pith_short_12","alias_value":"G2PUR3OPVTJR","created_at":"2026-05-18T12:28:28.263976+00:00"},{"alias_kind":"pith_short_16","alias_value":"G2PUR3OPVTJRIIQM","created_at":"2026-05-18T12:28:28.263976+00:00"},{"alias_kind":"pith_short_8","alias_value":"G2PUR3OP","created_at":"2026-05-18T12:28:28.263976+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"2605.22789","citing_title":"Primordial black holes in excursion set theory: Formation probabilities, mass functions, and window functions","ref_index":43,"is_internal_anchor":true},{"citing_arxiv_id":"2505.16820","citing_title":"Isotropy, anisotropies and non-Gaussianity in the scalar-induced gravitational-wave background: diagrammatic approach for primordial non-Gaussianity up to arbitrary order","ref_index":241,"is_internal_anchor":true},{"citing_arxiv_id":"2605.21477","citing_title":"Opening the Window of Ultra-Light PBHs by Exorcising the Poltergeist","ref_index":57,"is_internal_anchor":true},{"citing_arxiv_id":"2604.27496","citing_title":"Primordial black hole dark matter from axion inflation","ref_index":55,"is_internal_anchor":false},{"citing_arxiv_id":"2604.26005","citing_title":"Asteroid-mass Primordial Black Holes as Dark Matter from Supersymmetry","ref_index":104,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/G2PUR3OPVTJRIIQMFGZR6JM5C5","json":"https://pith.science/pith/G2PUR3OPVTJRIIQMFGZR6JM5C5.json","graph_json":"https://pith.science/api/pith-number/G2PUR3OPVTJRIIQMFGZR6JM5C5/graph.json","events_json":"https://pith.science/api/pith-number/G2PUR3OPVTJRIIQMFGZR6JM5C5/events.json","paper":"https://pith.science/paper/G2PUR3OP"},"agent_actions":{"view_html":"https://pith.science/pith/G2PUR3OPVTJRIIQMFGZR6JM5C5","download_json":"https://pith.science/pith/G2PUR3OPVTJRIIQMFGZR6JM5C5.json","view_paper":"https://pith.science/paper/G2PUR3OP","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1405.7023&json=true","fetch_graph":"https://pith.science/api/pith-number/G2PUR3OPVTJRIIQMFGZR6JM5C5/graph.json","fetch_events":"https://pith.science/api/pith-number/G2PUR3OPVTJRIIQMFGZR6JM5C5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/G2PUR3OPVTJRIIQMFGZR6JM5C5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/G2PUR3OPVTJRIIQMFGZR6JM5C5/action/storage_attestation","attest_author":"https://pith.science/pith/G2PUR3OPVTJRIIQMFGZR6JM5C5/action/author_attestation","sign_citation":"https://pith.science/pith/G2PUR3OPVTJRIIQMFGZR6JM5C5/action/citation_signature","submit_replication":"https://pith.science/pith/G2PUR3OPVTJRIIQMFGZR6JM5C5/action/replication_record"}},"created_at":"2026-05-18T02:25:40.361328+00:00","updated_at":"2026-05-18T02:25:40.361328+00:00"}