{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:YYXGHXXQT6NNPLM5U7CEFOXFOA","short_pith_number":"pith:YYXGHXXQ","schema_version":"1.0","canonical_sha256":"c62e63def09f9ad7ad9da7c442bae570203eae29053afa57b3c217aa9e722fed","source":{"kind":"arxiv","id":"1905.09284","version":2},"attestation_state":"computed","paper":{"title":"Supernova signals of light dark matter","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"hep-ph","authors_text":"Daniel Kasen, Gustavo Marques-Tavares, Peter W. Graham, Surjeet Rajendran, William DeRocco","submitted_at":"2019-05-22T18:00:00Z","abstract_excerpt":"Dark matter direct detection experiments have poor sensitivity to a galactic population of dark matter with mass below the GeV scale. However, such dark matter can be produced copiously in supernovae. Since this thermally-produced population is much hotter than the galactic dark matter, it can be observed with direct detection experiments. In this paper, we focus on a dark sector with fermion dark matter and a heavy dark photon as a specific example. We first extend existing supernova cooling constraints on this model to the regime of strong coupling where the dark matter becomes diffusively t"},"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":"1905.09284","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"hep-ph","submitted_at":"2019-05-22T18:00:00Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"47740b5da3b528b6f47d5465ecee5ce59b53bbfcc7ececf6b7083b1b484d0ca5","abstract_canon_sha256":"acf706f9d68846c296aa5317469fda3154b9af27a14b1667de2b6d11a71c54f8"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:12:26.414129Z","signature_b64":"LEWivokyqBCGYKW5bocwu2EbiIFsIoScRDwfmr9BhyljO8lDzavQfWxDcqoDEhDiUegA91/nxYd4nx3RyDoKDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"c62e63def09f9ad7ad9da7c442bae570203eae29053afa57b3c217aa9e722fed","last_reissued_at":"2026-07-05T00:12:26.413710Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:12:26.413710Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Supernova signals of light dark matter","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"hep-ph","authors_text":"Daniel Kasen, Gustavo Marques-Tavares, Peter W. Graham, Surjeet Rajendran, William DeRocco","submitted_at":"2019-05-22T18:00:00Z","abstract_excerpt":"Dark matter direct detection experiments have poor sensitivity to a galactic population of dark matter with mass below the GeV scale. However, such dark matter can be produced copiously in supernovae. Since this thermally-produced population is much hotter than the galactic dark matter, it can be observed with direct detection experiments. In this paper, we focus on a dark sector with fermion dark matter and a heavy dark photon as a specific example. We first extend existing supernova cooling constraints on this model to the regime of strong coupling where the dark matter becomes diffusively t"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1905.09284","kind":"arxiv","version":2},"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/1905.09284/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":"1905.09284","created_at":"2026-07-05T00:12:26.413764+00:00"},{"alias_kind":"arxiv_version","alias_value":"1905.09284v2","created_at":"2026-07-05T00:12:26.413764+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1905.09284","created_at":"2026-07-05T00:12:26.413764+00:00"},{"alias_kind":"pith_short_12","alias_value":"YYXGHXXQT6NN","created_at":"2026-07-05T00:12:26.413764+00:00"},{"alias_kind":"pith_short_16","alias_value":"YYXGHXXQT6NNPLM5","created_at":"2026-07-05T00:12:26.413764+00:00"},{"alias_kind":"pith_short_8","alias_value":"YYXGHXXQ","created_at":"2026-07-05T00:12:26.413764+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.27521","citing_title":"From WIMP to FIMP during reheating: collider vs non-collider probes for p-wave annihilation","ref_index":114,"is_internal_anchor":false},{"citing_arxiv_id":"2604.17869","citing_title":"Probing Cosmic-Ray-Boosted and Supernova-Sourced Sub-GeV Dark Matter with Paleo-Detectors","ref_index":44,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/YYXGHXXQT6NNPLM5U7CEFOXFOA","json":"https://pith.science/pith/YYXGHXXQT6NNPLM5U7CEFOXFOA.json","graph_json":"https://pith.science/api/pith-number/YYXGHXXQT6NNPLM5U7CEFOXFOA/graph.json","events_json":"https://pith.science/api/pith-number/YYXGHXXQT6NNPLM5U7CEFOXFOA/events.json","paper":"https://pith.science/paper/YYXGHXXQ"},"agent_actions":{"view_html":"https://pith.science/pith/YYXGHXXQT6NNPLM5U7CEFOXFOA","download_json":"https://pith.science/pith/YYXGHXXQT6NNPLM5U7CEFOXFOA.json","view_paper":"https://pith.science/paper/YYXGHXXQ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1905.09284&json=true","fetch_graph":"https://pith.science/api/pith-number/YYXGHXXQT6NNPLM5U7CEFOXFOA/graph.json","fetch_events":"https://pith.science/api/pith-number/YYXGHXXQT6NNPLM5U7CEFOXFOA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/YYXGHXXQT6NNPLM5U7CEFOXFOA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/YYXGHXXQT6NNPLM5U7CEFOXFOA/action/storage_attestation","attest_author":"https://pith.science/pith/YYXGHXXQT6NNPLM5U7CEFOXFOA/action/author_attestation","sign_citation":"https://pith.science/pith/YYXGHXXQT6NNPLM5U7CEFOXFOA/action/citation_signature","submit_replication":"https://pith.science/pith/YYXGHXXQT6NNPLM5U7CEFOXFOA/action/replication_record"}},"created_at":"2026-07-05T00:12:26.413764+00:00","updated_at":"2026-07-05T00:12:26.413764+00:00"}