{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:5E2E4DTVNSWLLS5CH6TNULWPZ3","short_pith_number":"pith:5E2E4DTV","schema_version":"1.0","canonical_sha256":"e9344e0e756cacb5cba23fa6da2ecfcec9805e9d06da0c7d13722e84f4f76edc","source":{"kind":"arxiv","id":"1612.05638","version":3},"attestation_state":"computed","paper":{"title":"Gamma-ray Constraints on Decaying Dark Matter and Implications for IceCube","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.HE"],"primary_cat":"hep-ph","authors_text":"Benjamin R. Safdi, Kohta Murase, Nicholas L. Rodd, Timothy Cohen, Yotam Soreq","submitted_at":"2016-12-16T21:00:00Z","abstract_excerpt":"Utilizing the Fermi measurement of the gamma-ray spectrum toward the Galactic Center, we derive some of the strongest constraints to date on the dark matter (DM) lifetime in the mass range from hundreds of MeV to above an EeV. Our profile-likelihood based analysis relies on 413 weeks of Fermi Pass 8 data from 200 MeV to 2 TeV, along with up-to-date models for diffuse gamma-ray emission within the Milky Way. We model Galactic and extragalactic DM decay and include contributions to the DM-induced gamma-ray flux resulting from both primary emission and inverse-Compton scattering of primary electr"},"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":"1612.05638","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"hep-ph","submitted_at":"2016-12-16T21:00:00Z","cross_cats_sorted":["astro-ph.CO","astro-ph.HE"],"title_canon_sha256":"c5639be126fd767f6900757bae9d964a43ca763d3c5a0957a254c71b28bf9f68","abstract_canon_sha256":"aa28f806ce3ddf76c31f82b64854374af2d26238bfc510e4bef0bb93ddab7cea"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-17T23:42:49.247699Z","signature_b64":"uXrwOuTSvDbvhYLlMeiQOO6Tpl0qPEQLFKGjGgPdKPMs/+gKttOGSUekRJoA529hNm2O7JRszkRsLZrfZ7jxBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e9344e0e756cacb5cba23fa6da2ecfcec9805e9d06da0c7d13722e84f4f76edc","last_reissued_at":"2026-05-17T23:42:49.247214Z","signature_status":"signed_v1","first_computed_at":"2026-05-17T23:42:49.247214Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Gamma-ray Constraints on Decaying Dark Matter and Implications for IceCube","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.HE"],"primary_cat":"hep-ph","authors_text":"Benjamin R. Safdi, Kohta Murase, Nicholas L. Rodd, Timothy Cohen, Yotam Soreq","submitted_at":"2016-12-16T21:00:00Z","abstract_excerpt":"Utilizing the Fermi measurement of the gamma-ray spectrum toward the Galactic Center, we derive some of the strongest constraints to date on the dark matter (DM) lifetime in the mass range from hundreds of MeV to above an EeV. Our profile-likelihood based analysis relies on 413 weeks of Fermi Pass 8 data from 200 MeV to 2 TeV, along with up-to-date models for diffuse gamma-ray emission within the Milky Way. We model Galactic and extragalactic DM decay and include contributions to the DM-induced gamma-ray flux resulting from both primary emission and inverse-Compton scattering of primary electr"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1612.05638","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":"1612.05638","created_at":"2026-05-17T23:42:49.247280+00:00"},{"alias_kind":"arxiv_version","alias_value":"1612.05638v3","created_at":"2026-05-17T23:42:49.247280+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1612.05638","created_at":"2026-05-17T23:42:49.247280+00:00"},{"alias_kind":"pith_short_12","alias_value":"5E2E4DTVNSWL","created_at":"2026-05-18T12:30:01.593930+00:00"},{"alias_kind":"pith_short_16","alias_value":"5E2E4DTVNSWLLS5C","created_at":"2026-05-18T12:30:01.593930+00:00"},{"alias_kind":"pith_short_8","alias_value":"5E2E4DTV","created_at":"2026-05-18T12:30:01.593930+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"1907.11926","citing_title":"Potential Dark Matter Signals at Neutrino Telescopes","ref_index":38,"is_internal_anchor":true},{"citing_arxiv_id":"2507.13432","citing_title":"INTEGRAL, eROSITA and Voyager Constraints on Light Bosonic Dark Matter: ALPs, Dark Photons, Scalars, $B-L$ and $L_{i}-L_{j}$ Vectors","ref_index":18,"is_internal_anchor":true},{"citing_arxiv_id":"2406.01705","citing_title":"Dark Matter","ref_index":142,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/5E2E4DTVNSWLLS5CH6TNULWPZ3","json":"https://pith.science/pith/5E2E4DTVNSWLLS5CH6TNULWPZ3.json","graph_json":"https://pith.science/api/pith-number/5E2E4DTVNSWLLS5CH6TNULWPZ3/graph.json","events_json":"https://pith.science/api/pith-number/5E2E4DTVNSWLLS5CH6TNULWPZ3/events.json","paper":"https://pith.science/paper/5E2E4DTV"},"agent_actions":{"view_html":"https://pith.science/pith/5E2E4DTVNSWLLS5CH6TNULWPZ3","download_json":"https://pith.science/pith/5E2E4DTVNSWLLS5CH6TNULWPZ3.json","view_paper":"https://pith.science/paper/5E2E4DTV","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1612.05638&json=true","fetch_graph":"https://pith.science/api/pith-number/5E2E4DTVNSWLLS5CH6TNULWPZ3/graph.json","fetch_events":"https://pith.science/api/pith-number/5E2E4DTVNSWLLS5CH6TNULWPZ3/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/5E2E4DTVNSWLLS5CH6TNULWPZ3/action/timestamp_anchor","attest_storage":"https://pith.science/pith/5E2E4DTVNSWLLS5CH6TNULWPZ3/action/storage_attestation","attest_author":"https://pith.science/pith/5E2E4DTVNSWLLS5CH6TNULWPZ3/action/author_attestation","sign_citation":"https://pith.science/pith/5E2E4DTVNSWLLS5CH6TNULWPZ3/action/citation_signature","submit_replication":"https://pith.science/pith/5E2E4DTVNSWLLS5CH6TNULWPZ3/action/replication_record"}},"created_at":"2026-05-17T23:42:49.247280+00:00","updated_at":"2026-05-17T23:42:49.247280+00:00"}