{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:MUK5QHSMFTI3ORVU7G5VTG767K","short_pith_number":"pith:MUK5QHSM","schema_version":"1.0","canonical_sha256":"6515d81e4c2cd1b746b4f9bb599bfefab067bf09b19ef5e8f6ec9129bc459d4f","source":{"kind":"arxiv","id":"2110.00025","version":3},"attestation_state":"computed","paper":{"title":"Exclusion limits on Dark Matter-Neutrino Scattering Cross-section","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"hep-ph","authors_text":"Atanu Guha, Diptimoy Ghosh, Divya Sachdeva","submitted_at":"2021-09-30T18:00:03Z","abstract_excerpt":"We derive new constraints on combination of dark matter - electron cross-section ($\\sigma_{\\chi e}$) and dark matter - neutrino cross-section ($\\sigma_{\\chi \\nu}$) utilising the gain in kinetic energy of the dark matter (DM) particles due to scattering with the cosmic ray electrons and the diffuse supernova neutrino background (DSNB). Since the flux of the DSNB neutrinos is comparable to the CR electron flux in the energy range $\\sim 1\\,{\\rm MeV} - 50 \\,{\\rm MeV}$, scattering with the DSNB neutrinos can also boost low-mass DM significantly in addition to the boost due to interaction with the c"},"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":"2110.00025","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"hep-ph","submitted_at":"2021-09-30T18:00:03Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"433115d247e3bb63af791e844242e27a9158944a5cb4b9faae41e4061fca7d8c","abstract_canon_sha256":"dcbbe54143fc0da3721aa00c22ec2fdbacce133c4014fc121ee8872bcb9e1545"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:26:45.886450Z","signature_b64":"abJLLrsFR62mTeaC004YLtmZdjnoEpXtKa0iasT/3FobmDW49F+G1/iHpKvgGAUba6apmdAtYeWgG2rCYkkrDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6515d81e4c2cd1b746b4f9bb599bfefab067bf09b19ef5e8f6ec9129bc459d4f","last_reissued_at":"2026-07-05T04:26:45.885986Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:26:45.885986Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Exclusion limits on Dark Matter-Neutrino Scattering Cross-section","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"hep-ph","authors_text":"Atanu Guha, Diptimoy Ghosh, Divya Sachdeva","submitted_at":"2021-09-30T18:00:03Z","abstract_excerpt":"We derive new constraints on combination of dark matter - electron cross-section ($\\sigma_{\\chi e}$) and dark matter - neutrino cross-section ($\\sigma_{\\chi \\nu}$) utilising the gain in kinetic energy of the dark matter (DM) particles due to scattering with the cosmic ray electrons and the diffuse supernova neutrino background (DSNB). Since the flux of the DSNB neutrinos is comparable to the CR electron flux in the energy range $\\sim 1\\,{\\rm MeV} - 50 \\,{\\rm MeV}$, scattering with the DSNB neutrinos can also boost low-mass DM significantly in addition to the boost due to interaction with the c"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2110.00025","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2110.00025/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":"2110.00025","created_at":"2026-07-05T04:26:45.886044+00:00"},{"alias_kind":"arxiv_version","alias_value":"2110.00025v3","created_at":"2026-07-05T04:26:45.886044+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2110.00025","created_at":"2026-07-05T04:26:45.886044+00:00"},{"alias_kind":"pith_short_12","alias_value":"MUK5QHSMFTI3","created_at":"2026-07-05T04:26:45.886044+00:00"},{"alias_kind":"pith_short_16","alias_value":"MUK5QHSMFTI3ORVU","created_at":"2026-07-05T04:26:45.886044+00:00"},{"alias_kind":"pith_short_8","alias_value":"MUK5QHSM","created_at":"2026-07-05T04:26:45.886044+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2602.04858","citing_title":"Primordial black holes as cosmic accelerators of light dark matter: Novel direct detection constraints","ref_index":81,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/MUK5QHSMFTI3ORVU7G5VTG767K","json":"https://pith.science/pith/MUK5QHSMFTI3ORVU7G5VTG767K.json","graph_json":"https://pith.science/api/pith-number/MUK5QHSMFTI3ORVU7G5VTG767K/graph.json","events_json":"https://pith.science/api/pith-number/MUK5QHSMFTI3ORVU7G5VTG767K/events.json","paper":"https://pith.science/paper/MUK5QHSM"},"agent_actions":{"view_html":"https://pith.science/pith/MUK5QHSMFTI3ORVU7G5VTG767K","download_json":"https://pith.science/pith/MUK5QHSMFTI3ORVU7G5VTG767K.json","view_paper":"https://pith.science/paper/MUK5QHSM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2110.00025&json=true","fetch_graph":"https://pith.science/api/pith-number/MUK5QHSMFTI3ORVU7G5VTG767K/graph.json","fetch_events":"https://pith.science/api/pith-number/MUK5QHSMFTI3ORVU7G5VTG767K/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/MUK5QHSMFTI3ORVU7G5VTG767K/action/timestamp_anchor","attest_storage":"https://pith.science/pith/MUK5QHSMFTI3ORVU7G5VTG767K/action/storage_attestation","attest_author":"https://pith.science/pith/MUK5QHSMFTI3ORVU7G5VTG767K/action/author_attestation","sign_citation":"https://pith.science/pith/MUK5QHSMFTI3ORVU7G5VTG767K/action/citation_signature","submit_replication":"https://pith.science/pith/MUK5QHSMFTI3ORVU7G5VTG767K/action/replication_record"}},"created_at":"2026-07-05T04:26:45.886044+00:00","updated_at":"2026-07-05T04:26:45.886044+00:00"}