{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2005:FTLPYGSJZ6AON2JJVZR6IYR4GL","short_pith_number":"pith:FTLPYGSJ","schema_version":"1.0","canonical_sha256":"2cd6fc1a49cf80e6e929ae63e4623c32e603f721c2ab68d4d855f50b18b457fe","source":{"kind":"arxiv","id":"astro-ph/0503486","version":1},"attestation_state":"computed","paper":{"title":"Detecting Dark Matter Annihilation with CMB Polarization : Signatures and Experimental Prospects","license":"","headline":"","cross_cats":["hep-th"],"primary_cat":"astro-ph","authors_text":"Douglas P. Finkbeiner (Princeton), Nikhil Padmanabhan","submitted_at":"2005-03-23T20:26:19Z","abstract_excerpt":"Dark matter (DM) annihilation during hydrogen recombination (z ~ 1000) will alter the recombination history of the Universe, and affect the observed CMB temperature and polarization fluctuations. Unlike other astrophysical probes of DM, this is free of the significant uncertainties in modelling galactic physics, and provides a method to detect and constrain the cosmological abundances of these particles. We parametrize the effect of DM annihilation as an injection of ionizing energy at a rate e_{dm}, and argue that this simple \"on the spot'' modification is a good approximation to the complica"},"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/0503486","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2005-03-23T20:26:19Z","cross_cats_sorted":["hep-th"],"title_canon_sha256":"5df46168bf325ad96d9dac81ca89b2330f2b4a05e7ddad132ea94509fd0fab13","abstract_canon_sha256":"1de5acbd85d15e4e4c23e56e73c6a372fac304d656d936b22db5cb64df855b0b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:31:18.376554Z","signature_b64":"bBoPrqLyYlAIyiWEp0v8Zwp15stTANtJCbcIQLrZEtYAbyZVZAgygqHlNb1KGTlGizkD0++ItTxMPcIAiEfbBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2cd6fc1a49cf80e6e929ae63e4623c32e603f721c2ab68d4d855f50b18b457fe","last_reissued_at":"2026-07-04T15:31:18.376161Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:31:18.376161Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Detecting Dark Matter Annihilation with CMB Polarization : Signatures and Experimental Prospects","license":"","headline":"","cross_cats":["hep-th"],"primary_cat":"astro-ph","authors_text":"Douglas P. Finkbeiner (Princeton), Nikhil Padmanabhan","submitted_at":"2005-03-23T20:26:19Z","abstract_excerpt":"Dark matter (DM) annihilation during hydrogen recombination (z ~ 1000) will alter the recombination history of the Universe, and affect the observed CMB temperature and polarization fluctuations. Unlike other astrophysical probes of DM, this is free of the significant uncertainties in modelling galactic physics, and provides a method to detect and constrain the cosmological abundances of these particles. We parametrize the effect of DM annihilation as an injection of ionizing energy at a rate e_{dm}, and argue that this simple \"on the spot'' modification is a good approximation to the complica"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0503486","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/astro-ph/0503486/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":"astro-ph/0503486","created_at":"2026-07-04T15:31:18.376230+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0503486v1","created_at":"2026-07-04T15:31:18.376230+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0503486","created_at":"2026-07-04T15:31:18.376230+00:00"},{"alias_kind":"pith_short_12","alias_value":"FTLPYGSJZ6AO","created_at":"2026-07-04T15:31:18.376230+00:00"},{"alias_kind":"pith_short_16","alias_value":"FTLPYGSJZ6AON2JJ","created_at":"2026-07-04T15:31:18.376230+00:00"},{"alias_kind":"pith_short_8","alias_value":"FTLPYGSJ","created_at":"2026-07-04T15:31:18.376230+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":5,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2606.07106","citing_title":"Joint probes of dark matter annihilation from neutrino detectors and CMB targets","ref_index":69,"is_internal_anchor":true},{"citing_arxiv_id":"2605.18944","citing_title":"The Majoron Cosmological Window: Dark Matter and Thermal Leptogenesis","ref_index":105,"is_internal_anchor":true},{"citing_arxiv_id":"2605.00648","citing_title":"Anisotropy of Cosmic Background Photons from Annihilating/Decaying Dark Matter","ref_index":41,"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":19,"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":17,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/FTLPYGSJZ6AON2JJVZR6IYR4GL","json":"https://pith.science/pith/FTLPYGSJZ6AON2JJVZR6IYR4GL.json","graph_json":"https://pith.science/api/pith-number/FTLPYGSJZ6AON2JJVZR6IYR4GL/graph.json","events_json":"https://pith.science/api/pith-number/FTLPYGSJZ6AON2JJVZR6IYR4GL/events.json","paper":"https://pith.science/paper/FTLPYGSJ"},"agent_actions":{"view_html":"https://pith.science/pith/FTLPYGSJZ6AON2JJVZR6IYR4GL","download_json":"https://pith.science/pith/FTLPYGSJZ6AON2JJVZR6IYR4GL.json","view_paper":"https://pith.science/paper/FTLPYGSJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0503486&json=true","fetch_graph":"https://pith.science/api/pith-number/FTLPYGSJZ6AON2JJVZR6IYR4GL/graph.json","fetch_events":"https://pith.science/api/pith-number/FTLPYGSJZ6AON2JJVZR6IYR4GL/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/FTLPYGSJZ6AON2JJVZR6IYR4GL/action/timestamp_anchor","attest_storage":"https://pith.science/pith/FTLPYGSJZ6AON2JJVZR6IYR4GL/action/storage_attestation","attest_author":"https://pith.science/pith/FTLPYGSJZ6AON2JJVZR6IYR4GL/action/author_attestation","sign_citation":"https://pith.science/pith/FTLPYGSJZ6AON2JJVZR6IYR4GL/action/citation_signature","submit_replication":"https://pith.science/pith/FTLPYGSJZ6AON2JJVZR6IYR4GL/action/replication_record"}},"created_at":"2026-07-04T15:31:18.376230+00:00","updated_at":"2026-07-04T15:31:18.376230+00:00"}