{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:5EF2BXNWS2UH2BDKK7OXMAQ52S","short_pith_number":"pith:5EF2BXNW","schema_version":"1.0","canonical_sha256":"e90ba0ddb696a87d046a57dd76021dd4be373d05f7d196e83f4446179eb310e2","source":{"kind":"arxiv","id":"2506.13858","version":1},"attestation_state":"computed","paper":{"title":"Not-quite-primordial black holes","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Neal Weiner, Priyamvada Natarajan, Soubhik Kumar, Wenzer Qin","submitted_at":"2025-06-16T18:00:00Z","abstract_excerpt":"We propose a new mechanism for the formation of seeds of supermassive black holes at early cosmic epochs. Enhanced density fluctuations with amplitudes that are not large enough to form primordial black holes post-inflation can still lead to collapsed dark matter halos at very early times. For halos forming prior to $1+z \\approx 200$, the Cosmic Microwave Background (CMB) is energetic enough to suppress the formation of molecular hydrogen, hence preventing cooling and fragmentation, as a consequence of which baryons falling into the potential well of the halo may undergo \"direct collapse\" into"},"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":"2506.13858","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.CO","submitted_at":"2025-06-16T18:00:00Z","cross_cats_sorted":["astro-ph.GA","hep-ph"],"title_canon_sha256":"b76d6acbfb99328b9bc6f891d8f649ef2c5805bddaac63ebec892ee84882f074","abstract_canon_sha256":"06d5ec305b9e54a460977eb5f66b434c71233135e085bd130f515c2230e51d22"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T11:26:52.824963Z","signature_b64":"s5VwzIZa8Jhzj48ncq8VoqVDiQdlpsCdRWL2c/2OxK0CogUxJ9ixP78gwx3jYKkF6b0wC84U3/p1d6VxIg/jDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e90ba0ddb696a87d046a57dd76021dd4be373d05f7d196e83f4446179eb310e2","last_reissued_at":"2026-07-05T11:26:52.824495Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T11:26:52.824495Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Not-quite-primordial black holes","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Neal Weiner, Priyamvada Natarajan, Soubhik Kumar, Wenzer Qin","submitted_at":"2025-06-16T18:00:00Z","abstract_excerpt":"We propose a new mechanism for the formation of seeds of supermassive black holes at early cosmic epochs. Enhanced density fluctuations with amplitudes that are not large enough to form primordial black holes post-inflation can still lead to collapsed dark matter halos at very early times. For halos forming prior to $1+z \\approx 200$, the Cosmic Microwave Background (CMB) is energetic enough to suppress the formation of molecular hydrogen, hence preventing cooling and fragmentation, as a consequence of which baryons falling into the potential well of the halo may undergo \"direct collapse\" into"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2506.13858","kind":"arxiv","version":1},"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/2506.13858/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":"2506.13858","created_at":"2026-07-05T11:26:52.824545+00:00"},{"alias_kind":"arxiv_version","alias_value":"2506.13858v1","created_at":"2026-07-05T11:26:52.824545+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2506.13858","created_at":"2026-07-05T11:26:52.824545+00:00"},{"alias_kind":"pith_short_12","alias_value":"5EF2BXNWS2UH","created_at":"2026-07-05T11:26:52.824545+00:00"},{"alias_kind":"pith_short_16","alias_value":"5EF2BXNWS2UH2BDK","created_at":"2026-07-05T11:26:52.824545+00:00"},{"alias_kind":"pith_short_8","alias_value":"5EF2BXNW","created_at":"2026-07-05T11:26:52.824545+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":7,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.25014","citing_title":"Probing Confining Dark Sectors with Cosmological Perturbations","ref_index":66,"is_internal_anchor":false},{"citing_arxiv_id":"2606.07357","citing_title":"Origin of monolithic high-z galaxies and UV luminosity of mergering high-z galaxies in the cosmological model with non-standard spectrum of density perturbations","ref_index":30,"is_internal_anchor":false},{"citing_arxiv_id":"2605.22161","citing_title":"Blue-tilted Runnings and the JWST Early Galaxy Tension","ref_index":49,"is_internal_anchor":false},{"citing_arxiv_id":"2605.22161","citing_title":"Blue-tilted Runnings and the JWST Early Galaxy Tension","ref_index":43,"is_internal_anchor":false},{"citing_arxiv_id":"2509.25325","citing_title":"Direct Collapse Black Hole Candidates from Decaying Dark Matter","ref_index":39,"is_internal_anchor":false},{"citing_arxiv_id":"2601.02321","citing_title":"Axions explain the formation of supermassive black holes at cosmic dawn","ref_index":10,"is_internal_anchor":false},{"citing_arxiv_id":"2604.01684","citing_title":"Smoluchowski Coagulation Equation and the Evolution of Primordial Black Hole Clusters","ref_index":138,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/5EF2BXNWS2UH2BDKK7OXMAQ52S","json":"https://pith.science/pith/5EF2BXNWS2UH2BDKK7OXMAQ52S.json","graph_json":"https://pith.science/api/pith-number/5EF2BXNWS2UH2BDKK7OXMAQ52S/graph.json","events_json":"https://pith.science/api/pith-number/5EF2BXNWS2UH2BDKK7OXMAQ52S/events.json","paper":"https://pith.science/paper/5EF2BXNW"},"agent_actions":{"view_html":"https://pith.science/pith/5EF2BXNWS2UH2BDKK7OXMAQ52S","download_json":"https://pith.science/pith/5EF2BXNWS2UH2BDKK7OXMAQ52S.json","view_paper":"https://pith.science/paper/5EF2BXNW","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2506.13858&json=true","fetch_graph":"https://pith.science/api/pith-number/5EF2BXNWS2UH2BDKK7OXMAQ52S/graph.json","fetch_events":"https://pith.science/api/pith-number/5EF2BXNWS2UH2BDKK7OXMAQ52S/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/5EF2BXNWS2UH2BDKK7OXMAQ52S/action/timestamp_anchor","attest_storage":"https://pith.science/pith/5EF2BXNWS2UH2BDKK7OXMAQ52S/action/storage_attestation","attest_author":"https://pith.science/pith/5EF2BXNWS2UH2BDKK7OXMAQ52S/action/author_attestation","sign_citation":"https://pith.science/pith/5EF2BXNWS2UH2BDKK7OXMAQ52S/action/citation_signature","submit_replication":"https://pith.science/pith/5EF2BXNWS2UH2BDKK7OXMAQ52S/action/replication_record"}},"created_at":"2026-07-05T11:26:52.824545+00:00","updated_at":"2026-07-05T11:26:52.824545+00:00"}