{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:O4L2M2B6A5O4LHTYEEUMEIYAA6","short_pith_number":"pith:O4L2M2B6","schema_version":"1.0","canonical_sha256":"7717a6683e075dc59e782128c2230007b004f6abef3e2be8f3f66b2f938f6a20","source":{"kind":"arxiv","id":"1706.02892","version":2},"attestation_state":"computed","paper":{"title":"KiDS-450: The tomographic weak lensing power spectrum and constraints on cosmological parameters","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Choi, B. Joachimi, C. Heymans, D. Klaes, E.A. Valentijn, E. van Uitert, F. K\\\"ohlinger, H. Hildebrandt, H. Hoekstra, J. Merten, K. Kuijken, L. Miller, M. Viola, P. Schneider, S. Joudaki, T. Erben","submitted_at":"2017-06-09T11:07:44Z","abstract_excerpt":"We present measurements of the weak gravitational lensing shear power spectrum based on $450$ sq. deg. of imaging data from the Kilo Degree Survey. We employ a quadratic estimator in two and three redshift bins and extract band powers of redshift auto-correlation and cross-correlation spectra in the multipole range $76 \\leq \\ell \\leq 1310$. The cosmological interpretation of the measured shear power spectra is performed in a Bayesian framework assuming a $\\Lambda$CDM model with spatially flat geometry, while accounting for small residual uncertainties in the shear calibration and redshift dist"},"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":"1706.02892","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2017-06-09T11:07:44Z","cross_cats_sorted":[],"title_canon_sha256":"b61e7e11cdda7d7d660211e4cc959081711e09ea3340f4cbd1a1939ddc6ec369","abstract_canon_sha256":"7616483a2dea5880a68449609f84d312e2e25b63dc7072306d93897fb2d97b45"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:38:35.563236Z","signature_b64":"1L/b/VJDBndtBmJa8GhIZ00yMlL3GGDkj6ffgLvkv+xJR/gTic20vrQqBrqDuSoiPAZtFe6g2U7llCn9eu35Bw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7717a6683e075dc59e782128c2230007b004f6abef3e2be8f3f66b2f938f6a20","last_reissued_at":"2026-05-18T00:38:35.562767Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:38:35.562767Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"KiDS-450: The tomographic weak lensing power spectrum and constraints on cosmological parameters","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Choi, B. Joachimi, C. Heymans, D. Klaes, E.A. Valentijn, E. van Uitert, F. K\\\"ohlinger, H. Hildebrandt, H. Hoekstra, J. Merten, K. Kuijken, L. Miller, M. Viola, P. Schneider, S. Joudaki, T. Erben","submitted_at":"2017-06-09T11:07:44Z","abstract_excerpt":"We present measurements of the weak gravitational lensing shear power spectrum based on $450$ sq. deg. of imaging data from the Kilo Degree Survey. We employ a quadratic estimator in two and three redshift bins and extract band powers of redshift auto-correlation and cross-correlation spectra in the multipole range $76 \\leq \\ell \\leq 1310$. The cosmological interpretation of the measured shear power spectra is performed in a Bayesian framework assuming a $\\Lambda$CDM model with spatially flat geometry, while accounting for small residual uncertainties in the shear calibration and redshift dist"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1706.02892","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":"1706.02892","created_at":"2026-05-18T00:38:35.562830+00:00"},{"alias_kind":"arxiv_version","alias_value":"1706.02892v2","created_at":"2026-05-18T00:38:35.562830+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1706.02892","created_at":"2026-05-18T00:38:35.562830+00:00"},{"alias_kind":"pith_short_12","alias_value":"O4L2M2B6A5O4","created_at":"2026-05-18T12:31:34.259226+00:00"},{"alias_kind":"pith_short_16","alias_value":"O4L2M2B6A5O4LHTY","created_at":"2026-05-18T12:31:34.259226+00:00"},{"alias_kind":"pith_short_8","alias_value":"O4L2M2B6","created_at":"2026-05-18T12:31:34.259226+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"1907.04473","citing_title":"CMB-S4 Science Case, Reference Design, and Project Plan","ref_index":169,"is_internal_anchor":true},{"citing_arxiv_id":"2105.13549","citing_title":"Dark Energy Survey Year 3 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing","ref_index":61,"is_internal_anchor":true},{"citing_arxiv_id":"2605.15078","citing_title":"KiDS+VIKING-450 cosmology with Bayesian hierarchical model redshift distributions","ref_index":67,"is_internal_anchor":true},{"citing_arxiv_id":"1807.06209","citing_title":"Planck 2018 results. VI. Cosmological parameters","ref_index":200,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/O4L2M2B6A5O4LHTYEEUMEIYAA6","json":"https://pith.science/pith/O4L2M2B6A5O4LHTYEEUMEIYAA6.json","graph_json":"https://pith.science/api/pith-number/O4L2M2B6A5O4LHTYEEUMEIYAA6/graph.json","events_json":"https://pith.science/api/pith-number/O4L2M2B6A5O4LHTYEEUMEIYAA6/events.json","paper":"https://pith.science/paper/O4L2M2B6"},"agent_actions":{"view_html":"https://pith.science/pith/O4L2M2B6A5O4LHTYEEUMEIYAA6","download_json":"https://pith.science/pith/O4L2M2B6A5O4LHTYEEUMEIYAA6.json","view_paper":"https://pith.science/paper/O4L2M2B6","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1706.02892&json=true","fetch_graph":"https://pith.science/api/pith-number/O4L2M2B6A5O4LHTYEEUMEIYAA6/graph.json","fetch_events":"https://pith.science/api/pith-number/O4L2M2B6A5O4LHTYEEUMEIYAA6/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/O4L2M2B6A5O4LHTYEEUMEIYAA6/action/timestamp_anchor","attest_storage":"https://pith.science/pith/O4L2M2B6A5O4LHTYEEUMEIYAA6/action/storage_attestation","attest_author":"https://pith.science/pith/O4L2M2B6A5O4LHTYEEUMEIYAA6/action/author_attestation","sign_citation":"https://pith.science/pith/O4L2M2B6A5O4LHTYEEUMEIYAA6/action/citation_signature","submit_replication":"https://pith.science/pith/O4L2M2B6A5O4LHTYEEUMEIYAA6/action/replication_record"}},"created_at":"2026-05-18T00:38:35.562830+00:00","updated_at":"2026-05-18T00:38:35.562830+00:00"}