{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:OMPR4GPLESM72ONHUDO7725DUE","short_pith_number":"pith:OMPR4GPL","schema_version":"1.0","canonical_sha256":"731f1e19eb2499fd39a7a0ddffeba3a1318d747ecf954fe02e61298e8690cd7d","source":{"kind":"arxiv","id":"1709.02384","version":2},"attestation_state":"computed","paper":{"title":"Observational constraints on dark matter-dark energy scattering cross section","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.CO","authors_text":"Rafael C. Nunes, Suresh Kumar","submitted_at":"2017-09-07T13:47:10Z","abstract_excerpt":"In this letter, we report precise and robust observational constraints on dark matter-dark energy scattering cross section, using the latest data from cosmic microwave background (CMB) Planck temperature and polarization, baryon acoustic oscillations (BAO) measurements and weak gravitational lensing data from Canada-France-Hawaii Telescope Lensing Survey (CFHTLenS). The scattering scenario consists of a pure momentum exchange between the dark components, and we find $\\sigma_d < 10^{-29} \\, {\\rm cm^2}$ at 95\\% CL from the joint analysis (CMB + BAO + CFHTLenS), for typical dark matter particle m"},"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":"1709.02384","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2017-09-07T13:47:10Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"ed89075258e12e8f4ed4a3312c92a64f090606aa8df41947907dfb798f482328","abstract_canon_sha256":"5dbc5f411f1e869ee816cc13068dbedc3dda9fde43c085920fc03de19d6da50b"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:31:23.547810Z","signature_b64":"o60izcI0/PydXXPIF1ph0KG0aCoGrkzWqmAahihbD/rqxVZcnZ6cS7pQm3HF3IES4hAuNVX1sqYTBdXY15FXAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"731f1e19eb2499fd39a7a0ddffeba3a1318d747ecf954fe02e61298e8690cd7d","last_reissued_at":"2026-05-18T00:31:23.547171Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:31:23.547171Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Observational constraints on dark matter-dark energy scattering cross section","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.CO","authors_text":"Rafael C. Nunes, Suresh Kumar","submitted_at":"2017-09-07T13:47:10Z","abstract_excerpt":"In this letter, we report precise and robust observational constraints on dark matter-dark energy scattering cross section, using the latest data from cosmic microwave background (CMB) Planck temperature and polarization, baryon acoustic oscillations (BAO) measurements and weak gravitational lensing data from Canada-France-Hawaii Telescope Lensing Survey (CFHTLenS). The scattering scenario consists of a pure momentum exchange between the dark components, and we find $\\sigma_d < 10^{-29} \\, {\\rm cm^2}$ at 95\\% CL from the joint analysis (CMB + BAO + CFHTLenS), for typical dark matter particle m"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1709.02384","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":""},"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":"1709.02384","created_at":"2026-05-18T00:31:23.547260+00:00"},{"alias_kind":"arxiv_version","alias_value":"1709.02384v2","created_at":"2026-05-18T00:31:23.547260+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1709.02384","created_at":"2026-05-18T00:31:23.547260+00:00"},{"alias_kind":"pith_short_12","alias_value":"OMPR4GPLESM7","created_at":"2026-05-18T12:31:34.259226+00:00"},{"alias_kind":"pith_short_16","alias_value":"OMPR4GPLESM72ONH","created_at":"2026-05-18T12:31:34.259226+00:00"},{"alias_kind":"pith_short_8","alias_value":"OMPR4GPL","created_at":"2026-05-18T12:31:34.259226+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"1907.08010","citing_title":"Cosmological searches for the neutrino mass scale and mass ordering","ref_index":277,"is_internal_anchor":true},{"citing_arxiv_id":"2604.25813","citing_title":"Geometric Constraints on the Pre-Recombination Expansion History from the Hubble Tension","ref_index":17,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OMPR4GPLESM72ONHUDO7725DUE","json":"https://pith.science/pith/OMPR4GPLESM72ONHUDO7725DUE.json","graph_json":"https://pith.science/api/pith-number/OMPR4GPLESM72ONHUDO7725DUE/graph.json","events_json":"https://pith.science/api/pith-number/OMPR4GPLESM72ONHUDO7725DUE/events.json","paper":"https://pith.science/paper/OMPR4GPL"},"agent_actions":{"view_html":"https://pith.science/pith/OMPR4GPLESM72ONHUDO7725DUE","download_json":"https://pith.science/pith/OMPR4GPLESM72ONHUDO7725DUE.json","view_paper":"https://pith.science/paper/OMPR4GPL","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1709.02384&json=true","fetch_graph":"https://pith.science/api/pith-number/OMPR4GPLESM72ONHUDO7725DUE/graph.json","fetch_events":"https://pith.science/api/pith-number/OMPR4GPLESM72ONHUDO7725DUE/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OMPR4GPLESM72ONHUDO7725DUE/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OMPR4GPLESM72ONHUDO7725DUE/action/storage_attestation","attest_author":"https://pith.science/pith/OMPR4GPLESM72ONHUDO7725DUE/action/author_attestation","sign_citation":"https://pith.science/pith/OMPR4GPLESM72ONHUDO7725DUE/action/citation_signature","submit_replication":"https://pith.science/pith/OMPR4GPLESM72ONHUDO7725DUE/action/replication_record"}},"created_at":"2026-05-18T00:31:23.547260+00:00","updated_at":"2026-05-18T00:31:23.547260+00:00"}