{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:WZKC7SFLLMAOCGYWXCS4NH2HVH","short_pith_number":"pith:WZKC7SFL","schema_version":"1.0","canonical_sha256":"b6542fc8ab5b00e11b16b8a5c69f47a9c7c5fc2f98b0f8fb2d1dbdc22d196f9f","source":{"kind":"arxiv","id":"1206.2644","version":1},"attestation_state":"computed","paper":{"title":"First Direct Detection Limits on sub-GeV Dark Matter from XENON10","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ex","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Aaron Manalaysay, Jeremy Mardon, Peter Sorensen, Rouven Essig, Tomer Volansky","submitted_at":"2012-06-12T20:00:02Z","abstract_excerpt":"The first direct detection limits on dark matter in the MeV to GeV mass range are presented, using XENON10 data. Such light dark matter can scatter with electrons, causing ionization of atoms in a detector target material and leading to single- or few-electron events. We use 15 kg-days of data acquired in 2006 to set limits on the dark-matter-electron scattering cross section. The strongest bound is obtained at 100 MeV where sigma_e < 3 x 10^{-38} cm^2 at 90% CL, while dark matter masses between 20 MeV and 1 GeV are bounded by sigma_e < 10^{-37} cm^2 at 90% CL. This analysis provides a first p"},"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":"1206.2644","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2012-06-12T20:00:02Z","cross_cats_sorted":["hep-ex","hep-ph"],"title_canon_sha256":"63fa5010eebb209ba09b871564945f1f1ec7693524e3a39242d4534d9832215f","abstract_canon_sha256":"36d9e6f082ca820956ddd7d7bcb06ed97e8c0c05347c551364f9a49297f32fdb"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:56:59.283698Z","signature_b64":"v6n7XmfHIxXhd9bYSaa/kCP3Ei7ExvSqEz+ZqP3wlbj3UTDu7/0guE+2hGhjhjE3A/uO/xYpt8lr/uFh8vmtCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b6542fc8ab5b00e11b16b8a5c69f47a9c7c5fc2f98b0f8fb2d1dbdc22d196f9f","last_reissued_at":"2026-05-18T01:56:59.283220Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:56:59.283220Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"First Direct Detection Limits on sub-GeV Dark Matter from XENON10","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ex","hep-ph"],"primary_cat":"astro-ph.CO","authors_text":"Aaron Manalaysay, Jeremy Mardon, Peter Sorensen, Rouven Essig, Tomer Volansky","submitted_at":"2012-06-12T20:00:02Z","abstract_excerpt":"The first direct detection limits on dark matter in the MeV to GeV mass range are presented, using XENON10 data. Such light dark matter can scatter with electrons, causing ionization of atoms in a detector target material and leading to single- or few-electron events. We use 15 kg-days of data acquired in 2006 to set limits on the dark-matter-electron scattering cross section. The strongest bound is obtained at 100 MeV where sigma_e < 3 x 10^{-38} cm^2 at 90% CL, while dark matter masses between 20 MeV and 1 GeV are bounded by sigma_e < 10^{-37} cm^2 at 90% CL. This analysis provides a first p"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1206.2644","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":""},"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":"1206.2644","created_at":"2026-05-18T01:56:59.283290+00:00"},{"alias_kind":"arxiv_version","alias_value":"1206.2644v1","created_at":"2026-05-18T01:56:59.283290+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1206.2644","created_at":"2026-05-18T01:56:59.283290+00:00"},{"alias_kind":"pith_short_12","alias_value":"WZKC7SFLLMAO","created_at":"2026-05-18T12:27:27.928770+00:00"},{"alias_kind":"pith_short_16","alias_value":"WZKC7SFLLMAOCGYW","created_at":"2026-05-18T12:27:27.928770+00:00"},{"alias_kind":"pith_short_8","alias_value":"WZKC7SFL","created_at":"2026-05-18T12:27:27.928770+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2602.04858","citing_title":"Primordial black holes as cosmic accelerators of light dark matter: Novel direct detection constraints","ref_index":106,"is_internal_anchor":true},{"citing_arxiv_id":"2603.16863","citing_title":"New benchmarks for direct detection of freeze-in dark matter in vector portal models","ref_index":3,"is_internal_anchor":true},{"citing_arxiv_id":"2604.21969","citing_title":"Dive deeper with SUBMARINE: SUB-Mev dArk matter diRect detectIon using bilayer grapheNE","ref_index":69,"is_internal_anchor":false},{"citing_arxiv_id":"2604.06929","citing_title":"Direct-detection constraints on inelastic dark matter with a scalar mediator","ref_index":53,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/WZKC7SFLLMAOCGYWXCS4NH2HVH","json":"https://pith.science/pith/WZKC7SFLLMAOCGYWXCS4NH2HVH.json","graph_json":"https://pith.science/api/pith-number/WZKC7SFLLMAOCGYWXCS4NH2HVH/graph.json","events_json":"https://pith.science/api/pith-number/WZKC7SFLLMAOCGYWXCS4NH2HVH/events.json","paper":"https://pith.science/paper/WZKC7SFL"},"agent_actions":{"view_html":"https://pith.science/pith/WZKC7SFLLMAOCGYWXCS4NH2HVH","download_json":"https://pith.science/pith/WZKC7SFLLMAOCGYWXCS4NH2HVH.json","view_paper":"https://pith.science/paper/WZKC7SFL","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1206.2644&json=true","fetch_graph":"https://pith.science/api/pith-number/WZKC7SFLLMAOCGYWXCS4NH2HVH/graph.json","fetch_events":"https://pith.science/api/pith-number/WZKC7SFLLMAOCGYWXCS4NH2HVH/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/WZKC7SFLLMAOCGYWXCS4NH2HVH/action/timestamp_anchor","attest_storage":"https://pith.science/pith/WZKC7SFLLMAOCGYWXCS4NH2HVH/action/storage_attestation","attest_author":"https://pith.science/pith/WZKC7SFLLMAOCGYWXCS4NH2HVH/action/author_attestation","sign_citation":"https://pith.science/pith/WZKC7SFLLMAOCGYWXCS4NH2HVH/action/citation_signature","submit_replication":"https://pith.science/pith/WZKC7SFLLMAOCGYWXCS4NH2HVH/action/replication_record"}},"created_at":"2026-05-18T01:56:59.283290+00:00","updated_at":"2026-05-18T01:56:59.283290+00:00"}