{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:OD6TLINZTAJYCDJ237KDJ6BH3Y","short_pith_number":"pith:OD6TLINZ","schema_version":"1.0","canonical_sha256":"70fd35a1b99813810d3adfd434f827de32f75af0755c65efb2e2d9cb6c4c9ef4","source":{"kind":"arxiv","id":"1601.03947","version":2},"attestation_state":"computed","paper":{"title":"SKA Weak Lensing I: Cosmological Forecasts and the Power of Radio-Optical Cross-Correlations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Ian Harrison, Joe Zuntz, Michael L. Brown, Stefano Camera","submitted_at":"2016-01-15T15:05:27Z","abstract_excerpt":"We construct forecasts for cosmological parameter constraints from weak gravitational lensing surveys involving the Square Kilometre Array (SKA). Considering matter content, dark energy and modified gravity parameters, we show that the first phase of the SKA (SKA1) can be competitive with other Stage III experiments such as the Dark Energy Survey (DES) and that the full SKA (SKA2) can potentially form tighter constraints than Stage IV optical weak lensing experiments, such as those that will be conducted with LSST, WFIRST-AFTA or Euclid-like facilities. Using weak lensing alone, going from SKA"},"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":"1601.03947","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2016-01-15T15:05:27Z","cross_cats_sorted":[],"title_canon_sha256":"bc28a769e0f84a3e7fa87c87ceaee6a1db8823108f0fa1ee3af18cba6626488f","abstract_canon_sha256":"37484402d74d93ee9a2a407ee836b364e5f028a7db30702facbe201bed83d908"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:01:28.814388Z","signature_b64":"rFIBYz9Ale5eveWmTHhKAQTJ2MukKS3iCW1VfNAgbpt620EUYAJJklaOznmCJ9y0R37EttDYEy7NgiPB+ZRVCA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"70fd35a1b99813810d3adfd434f827de32f75af0755c65efb2e2d9cb6c4c9ef4","last_reissued_at":"2026-05-18T01:01:28.813938Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:01:28.813938Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"SKA Weak Lensing I: Cosmological Forecasts and the Power of Radio-Optical Cross-Correlations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"Ian Harrison, Joe Zuntz, Michael L. Brown, Stefano Camera","submitted_at":"2016-01-15T15:05:27Z","abstract_excerpt":"We construct forecasts for cosmological parameter constraints from weak gravitational lensing surveys involving the Square Kilometre Array (SKA). Considering matter content, dark energy and modified gravity parameters, we show that the first phase of the SKA (SKA1) can be competitive with other Stage III experiments such as the Dark Energy Survey (DES) and that the full SKA (SKA2) can potentially form tighter constraints than Stage IV optical weak lensing experiments, such as those that will be conducted with LSST, WFIRST-AFTA or Euclid-like facilities. Using weak lensing alone, going from SKA"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1601.03947","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":"1601.03947","created_at":"2026-05-18T01:01:28.814006+00:00"},{"alias_kind":"arxiv_version","alias_value":"1601.03947v2","created_at":"2026-05-18T01:01:28.814006+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1601.03947","created_at":"2026-05-18T01:01:28.814006+00:00"},{"alias_kind":"pith_short_12","alias_value":"OD6TLINZTAJY","created_at":"2026-05-18T12:30:36.002864+00:00"},{"alias_kind":"pith_short_16","alias_value":"OD6TLINZTAJYCDJ2","created_at":"2026-05-18T12:30:36.002864+00:00"},{"alias_kind":"pith_short_8","alias_value":"OD6TLINZ","created_at":"2026-05-18T12:30:36.002864+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.08465","citing_title":"How to augment cosmic shear measurements with radio polarimetry of galaxies?","ref_index":20,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OD6TLINZTAJYCDJ237KDJ6BH3Y","json":"https://pith.science/pith/OD6TLINZTAJYCDJ237KDJ6BH3Y.json","graph_json":"https://pith.science/api/pith-number/OD6TLINZTAJYCDJ237KDJ6BH3Y/graph.json","events_json":"https://pith.science/api/pith-number/OD6TLINZTAJYCDJ237KDJ6BH3Y/events.json","paper":"https://pith.science/paper/OD6TLINZ"},"agent_actions":{"view_html":"https://pith.science/pith/OD6TLINZTAJYCDJ237KDJ6BH3Y","download_json":"https://pith.science/pith/OD6TLINZTAJYCDJ237KDJ6BH3Y.json","view_paper":"https://pith.science/paper/OD6TLINZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1601.03947&json=true","fetch_graph":"https://pith.science/api/pith-number/OD6TLINZTAJYCDJ237KDJ6BH3Y/graph.json","fetch_events":"https://pith.science/api/pith-number/OD6TLINZTAJYCDJ237KDJ6BH3Y/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OD6TLINZTAJYCDJ237KDJ6BH3Y/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OD6TLINZTAJYCDJ237KDJ6BH3Y/action/storage_attestation","attest_author":"https://pith.science/pith/OD6TLINZTAJYCDJ237KDJ6BH3Y/action/author_attestation","sign_citation":"https://pith.science/pith/OD6TLINZTAJYCDJ237KDJ6BH3Y/action/citation_signature","submit_replication":"https://pith.science/pith/OD6TLINZTAJYCDJ237KDJ6BH3Y/action/replication_record"}},"created_at":"2026-05-18T01:01:28.814006+00:00","updated_at":"2026-05-18T01:01:28.814006+00:00"}