{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2003:EEIRCUX664G5D6AZWC3LLMH7WY","short_pith_number":"pith:EEIRCUX6","schema_version":"1.0","canonical_sha256":"21111152fef70dd1f819b0b6b5b0ffb603317a9c54734a60f83bfdc60e5826f4","source":{"kind":"arxiv","id":"astro-ph/0310473","version":4},"attestation_state":"computed","paper":{"title":"Particle decays during the cosmic dark ages","license":"","headline":"","cross_cats":["hep-ex","hep-ph"],"primary_cat":"astro-ph","authors_text":"Marc Kamionkowski, Xuelei Chen","submitted_at":"2003-10-16T20:18:51Z","abstract_excerpt":"We consider particle decays during the cosmic dark ages with two aims: (1) to explain the high optical depth reported by WMAP, and (2) to provide new constraints to the parameter space for decaying particles. We delineate the decay channels in which most of the decay energy ionizes and heats the IGM gas (and thus affects the CMB), and those in which most of the energy is carried away -- e.g. photons with energies 100 keV < E < 1 TeV -- and thus appears as a contribution to diffuse x-ray and gamma-ray backgrounds. The new constraints to the decay-particle parameters from the CMB power spectrum "},"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":"astro-ph/0310473","kind":"arxiv","version":4},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2003-10-16T20:18:51Z","cross_cats_sorted":["hep-ex","hep-ph"],"title_canon_sha256":"a5ea6c8c5574048ead2a9c603bd23239b05ff68e2de09d3f078468e989245704","abstract_canon_sha256":"94fcab7f470d2bb8b7e89fef0eaa073d1e0aa91b8902c27394ef57f78e80f7ad"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:19:41.617214Z","signature_b64":"2ui2+vZ17jWLBuIhZg0vPCvVwX6VZEn8RZg/zS90KQ5eUjlz4w0u/p+oOYCKx4jTdwTw2j8LghbTja3CYXmFAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"21111152fef70dd1f819b0b6b5b0ffb603317a9c54734a60f83bfdc60e5826f4","last_reissued_at":"2026-05-18T04:19:41.616426Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:19:41.616426Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Particle decays during the cosmic dark ages","license":"","headline":"","cross_cats":["hep-ex","hep-ph"],"primary_cat":"astro-ph","authors_text":"Marc Kamionkowski, Xuelei Chen","submitted_at":"2003-10-16T20:18:51Z","abstract_excerpt":"We consider particle decays during the cosmic dark ages with two aims: (1) to explain the high optical depth reported by WMAP, and (2) to provide new constraints to the parameter space for decaying particles. We delineate the decay channels in which most of the decay energy ionizes and heats the IGM gas (and thus affects the CMB), and those in which most of the energy is carried away -- e.g. photons with energies 100 keV < E < 1 TeV -- and thus appears as a contribution to diffuse x-ray and gamma-ray backgrounds. The new constraints to the decay-particle parameters from the CMB power spectrum "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0310473","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":"astro-ph/0310473","created_at":"2026-05-18T04:19:41.616558+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0310473v4","created_at":"2026-05-18T04:19:41.616558+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0310473","created_at":"2026-05-18T04:19:41.616558+00:00"},{"alias_kind":"pith_short_12","alias_value":"EEIRCUX664G5","created_at":"2026-05-18T12:25:51.375804+00:00"},{"alias_kind":"pith_short_16","alias_value":"EEIRCUX664G5D6AZ","created_at":"2026-05-18T12:25:51.375804+00:00"},{"alias_kind":"pith_short_8","alias_value":"EEIRCUX6","created_at":"2026-05-18T12:25:51.375804+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":6,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"1907.06485","citing_title":"CMB constraints on ultra-light primordial black holes with extended mass distributions","ref_index":34,"is_internal_anchor":true},{"citing_arxiv_id":"2504.17064","citing_title":"Imprints of energy injection by compact dark stars in the 21-cm signal","ref_index":62,"is_internal_anchor":true},{"citing_arxiv_id":"2002.12778","citing_title":"Constraints on Primordial Black Holes","ref_index":185,"is_internal_anchor":true},{"citing_arxiv_id":"2605.00648","citing_title":"Anisotropy of Cosmic Background Photons from Annihilating/Decaying Dark Matter","ref_index":21,"is_internal_anchor":false},{"citing_arxiv_id":"2604.19198","citing_title":"Cosmological constraints on TeV-scale dark matter subcomponents decaying between recombination and reionisation","ref_index":13,"is_internal_anchor":false},{"citing_arxiv_id":"2605.08080","citing_title":"CMB Limits on the Absorption of Light Vector and Axial-Vector Dark Matter","ref_index":16,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/EEIRCUX664G5D6AZWC3LLMH7WY","json":"https://pith.science/pith/EEIRCUX664G5D6AZWC3LLMH7WY.json","graph_json":"https://pith.science/api/pith-number/EEIRCUX664G5D6AZWC3LLMH7WY/graph.json","events_json":"https://pith.science/api/pith-number/EEIRCUX664G5D6AZWC3LLMH7WY/events.json","paper":"https://pith.science/paper/EEIRCUX6"},"agent_actions":{"view_html":"https://pith.science/pith/EEIRCUX664G5D6AZWC3LLMH7WY","download_json":"https://pith.science/pith/EEIRCUX664G5D6AZWC3LLMH7WY.json","view_paper":"https://pith.science/paper/EEIRCUX6","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0310473&json=true","fetch_graph":"https://pith.science/api/pith-number/EEIRCUX664G5D6AZWC3LLMH7WY/graph.json","fetch_events":"https://pith.science/api/pith-number/EEIRCUX664G5D6AZWC3LLMH7WY/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/EEIRCUX664G5D6AZWC3LLMH7WY/action/timestamp_anchor","attest_storage":"https://pith.science/pith/EEIRCUX664G5D6AZWC3LLMH7WY/action/storage_attestation","attest_author":"https://pith.science/pith/EEIRCUX664G5D6AZWC3LLMH7WY/action/author_attestation","sign_citation":"https://pith.science/pith/EEIRCUX664G5D6AZWC3LLMH7WY/action/citation_signature","submit_replication":"https://pith.science/pith/EEIRCUX664G5D6AZWC3LLMH7WY/action/replication_record"}},"created_at":"2026-05-18T04:19:41.616558+00:00","updated_at":"2026-05-18T04:19:41.616558+00:00"}