{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2014:L3UDQBELE7AAWECN6D5YAMP7RT","short_pith_number":"pith:L3UDQBEL","schema_version":"1.0","canonical_sha256":"5ee838048b27c00b104df0fb8031ff8cc9c60d1370cd37b1215a93246be46e3a","source":{"kind":"arxiv","id":"1405.4858","version":3},"attestation_state":"computed","paper":{"title":"Spherical collapse in $\\nu \\Lambda CDM$","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Marilena Loverde","submitted_at":"2014-05-19T20:00:04Z","abstract_excerpt":"The abundance of massive dark matter halos hosting galaxy clusters provides an important test of the masses of relic neutrino species. The dominant effect of neutrino mass is to lower the typical amplitude of density perturbations that eventually form halos, but for neutrino masses $> 0.4eV$ the threshold for halo formation can be changed significantly as well. We study the spherical collapse model for halo formation in cosmologies with neutrino masses in the range $m_{\\nu i} =0.05eV$- $1eV$ and find that halo formation is differently sensitive to $\\Omega_\\nu$ and $m_\\nu$. That is, different n"},"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":"1405.4858","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2014-05-19T20:00:04Z","cross_cats_sorted":[],"title_canon_sha256":"1c5d4804ff5dbd8b53ef1c3f18a3394b68630bca62b81d6370b27173e9a1a13f","abstract_canon_sha256":"d81f4ebad05a2b21f617861c9bd2ef66e7d53b0726c01a5d24c2f80dd89c276e"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:38:59.380099Z","signature_b64":"gZVn8Er/pEiI2XzxyvybF7VNmpub2CqMJ0WVeGtrBoirLO4ine7hJ8UaBanUCRFe40Pi6PL6H1rfMr0VCgbRCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"5ee838048b27c00b104df0fb8031ff8cc9c60d1370cd37b1215a93246be46e3a","last_reissued_at":"2026-05-18T02:38:59.379616Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:38:59.379616Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Spherical collapse in $\\nu \\Lambda CDM$","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Marilena Loverde","submitted_at":"2014-05-19T20:00:04Z","abstract_excerpt":"The abundance of massive dark matter halos hosting galaxy clusters provides an important test of the masses of relic neutrino species. The dominant effect of neutrino mass is to lower the typical amplitude of density perturbations that eventually form halos, but for neutrino masses $> 0.4eV$ the threshold for halo formation can be changed significantly as well. We study the spherical collapse model for halo formation in cosmologies with neutrino masses in the range $m_{\\nu i} =0.05eV$- $1eV$ and find that halo formation is differently sensitive to $\\Omega_\\nu$ and $m_\\nu$. That is, different n"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1405.4858","kind":"arxiv","version":3},"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":"1405.4858","created_at":"2026-05-18T02:38:59.379697+00:00"},{"alias_kind":"arxiv_version","alias_value":"1405.4858v3","created_at":"2026-05-18T02:38:59.379697+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1405.4858","created_at":"2026-05-18T02:38:59.379697+00:00"},{"alias_kind":"pith_short_12","alias_value":"L3UDQBELE7AA","created_at":"2026-05-18T12:28:35.611951+00:00"},{"alias_kind":"pith_short_16","alias_value":"L3UDQBELE7AAWECN","created_at":"2026-05-18T12:28:35.611951+00:00"},{"alias_kind":"pith_short_8","alias_value":"L3UDQBEL","created_at":"2026-05-18T12:28:35.611951+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2503.16355","citing_title":"DEMNUni: the Sunyaev-Zel'dovich effect in the presence of massive neutrinos and dynamical dark energy","ref_index":62,"is_internal_anchor":true},{"citing_arxiv_id":"2604.14504","citing_title":"Forecasting neutrino mass constraints from the Nancy Grace Roman Space Telescope","ref_index":34,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/L3UDQBELE7AAWECN6D5YAMP7RT","json":"https://pith.science/pith/L3UDQBELE7AAWECN6D5YAMP7RT.json","graph_json":"https://pith.science/api/pith-number/L3UDQBELE7AAWECN6D5YAMP7RT/graph.json","events_json":"https://pith.science/api/pith-number/L3UDQBELE7AAWECN6D5YAMP7RT/events.json","paper":"https://pith.science/paper/L3UDQBEL"},"agent_actions":{"view_html":"https://pith.science/pith/L3UDQBELE7AAWECN6D5YAMP7RT","download_json":"https://pith.science/pith/L3UDQBELE7AAWECN6D5YAMP7RT.json","view_paper":"https://pith.science/paper/L3UDQBEL","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1405.4858&json=true","fetch_graph":"https://pith.science/api/pith-number/L3UDQBELE7AAWECN6D5YAMP7RT/graph.json","fetch_events":"https://pith.science/api/pith-number/L3UDQBELE7AAWECN6D5YAMP7RT/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/L3UDQBELE7AAWECN6D5YAMP7RT/action/timestamp_anchor","attest_storage":"https://pith.science/pith/L3UDQBELE7AAWECN6D5YAMP7RT/action/storage_attestation","attest_author":"https://pith.science/pith/L3UDQBELE7AAWECN6D5YAMP7RT/action/author_attestation","sign_citation":"https://pith.science/pith/L3UDQBELE7AAWECN6D5YAMP7RT/action/citation_signature","submit_replication":"https://pith.science/pith/L3UDQBELE7AAWECN6D5YAMP7RT/action/replication_record"}},"created_at":"2026-05-18T02:38:59.379697+00:00","updated_at":"2026-05-18T02:38:59.379697+00:00"}