{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:SZ7OOKYWOQG22FXTL6JDV2KKV5","short_pith_number":"pith:SZ7OOKYW","schema_version":"1.0","canonical_sha256":"967ee72b16740dad16f35f923ae94aaf7fe7f61bc37e9a337e51aa7015b95197","source":{"kind":"arxiv","id":"1603.05040","version":1},"attestation_state":"computed","paper":{"title":"Cosmology constraints from shear peak statistics in Dark Energy Survey Science Verification data","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Amara, A. A. Plazas, A. Benoit-L\\'evy, A. Carnero Rosell, A. E. Evrard, A. Fausti Neto, A. K. Romer, A. Nicola, A. Refregier, A. Roodman, A. R. Walker, B. Flaugher, B. Nord, C. B. D'Andrea, C. Bonnett, C. Chang, C. J. Miller, D. A. Goldstein, D. Bacon, D. Brooks, D. Gruen, D. J. James, D. Kirk, D. L. Burke, D. Thomas, D. W. Gerdes, E. Bertin, E. Krause, E.M. Huff, E. Sanchez, E. Sheldon, E. S. Rykoff, E. Suchyta, F. B. Abdalla, F. J. Castander, F. Sobreira, G. Gutierrez, G. Tarle, H. T. Diehl, I. Sevilla-Noarbe, J. Aleksi\\'c, J. Carretero, J. Frieman, J. J. Mohr, J. L. Marshall, J. P. Dietrich, J. Weller, J. Zuntz, K. Honscheid, K. Kuehn, L. Marian, L. N. da Costa, M. A. Troxel, M. Carrasco Kind, M. Crocce, M. E. C. Swanson, M. Lima, M. March, M. R. Becker, M. Schubnell, M. Soares-Santos, N. Kuropatkin, N. MacCrann, O. Friedrich, O. Lahav, P. Fosalba, P. Martini, P. Melchior, R. A. Bernstein, R. A. Gruendl, R. Armstrong, R. C. Nichol, R. C. Smith, R. Miquel, S. Desai, S. L. Bridle, S. Samuroff, T. F. Eifler, T. Kacprzak, T. M. C. Abbott, V. Scarpine, V. Vikram, W. Hartley, Y. Zhang (The Dark Energy Survey Collaboration)","submitted_at":"2016-03-16T11:26:53Z","abstract_excerpt":"Shear peak statistics has gained a lot of attention recently as a practical alternative to the two point statistics for constraining cosmological parameters. We perform a shear peak statistics analysis of the Dark Energy Survey (DES) Science Verification (SV) data, using weak gravitational lensing measurements from a 139 deg$^2$ field. We measure the abundance of peaks identified in aperture mass maps, as a function of their signal-to-noise ratio, in the signal-to-noise range $0<\\mathcal S / \\mathcal N<4$. To predict the peak counts as a function of cosmological parameters we use a suite of $N"},"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":"1603.05040","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2016-03-16T11:26:53Z","cross_cats_sorted":[],"title_canon_sha256":"1d9d868d66bae57169381180db8fa250bf31cc349068c39e45a6354dc03390aa","abstract_canon_sha256":"056c0e73ac0a8fd0ab14d9ae9cdb24aa4f9888f5db79b02108c309563509938f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:07:16.980792Z","signature_b64":"KHFL5AiwgDzFmWz7RFvSqNgm3SYtLn8bQSKzLgJSvilU1gNierUZruk9sJfFl5JfxvJ/DfQPnvaDnLyH4weMDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"967ee72b16740dad16f35f923ae94aaf7fe7f61bc37e9a337e51aa7015b95197","last_reissued_at":"2026-05-18T01:07:16.980231Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:07:16.980231Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Cosmology constraints from shear peak statistics in Dark Energy Survey Science Verification data","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Amara, A. A. Plazas, A. Benoit-L\\'evy, A. Carnero Rosell, A. E. Evrard, A. Fausti Neto, A. K. Romer, A. Nicola, A. Refregier, A. Roodman, A. R. Walker, B. Flaugher, B. Nord, C. B. D'Andrea, C. Bonnett, C. Chang, C. J. Miller, D. A. Goldstein, D. Bacon, D. Brooks, D. Gruen, D. J. James, D. Kirk, D. L. Burke, D. Thomas, D. W. Gerdes, E. Bertin, E. Krause, E.M. Huff, E. Sanchez, E. Sheldon, E. S. Rykoff, E. Suchyta, F. B. Abdalla, F. J. Castander, F. Sobreira, G. Gutierrez, G. Tarle, H. T. Diehl, I. Sevilla-Noarbe, J. Aleksi\\'c, J. Carretero, J. Frieman, J. J. Mohr, J. L. Marshall, J. P. Dietrich, J. Weller, J. Zuntz, K. Honscheid, K. Kuehn, L. Marian, L. N. da Costa, M. A. Troxel, M. Carrasco Kind, M. Crocce, M. E. C. Swanson, M. Lima, M. March, M. R. Becker, M. Schubnell, M. Soares-Santos, N. Kuropatkin, N. MacCrann, O. Friedrich, O. Lahav, P. Fosalba, P. Martini, P. Melchior, R. A. Bernstein, R. A. Gruendl, R. Armstrong, R. C. Nichol, R. C. Smith, R. Miquel, S. Desai, S. L. Bridle, S. Samuroff, T. F. Eifler, T. Kacprzak, T. M. C. Abbott, V. Scarpine, V. Vikram, W. Hartley, Y. Zhang (The Dark Energy Survey Collaboration)","submitted_at":"2016-03-16T11:26:53Z","abstract_excerpt":"Shear peak statistics has gained a lot of attention recently as a practical alternative to the two point statistics for constraining cosmological parameters. We perform a shear peak statistics analysis of the Dark Energy Survey (DES) Science Verification (SV) data, using weak gravitational lensing measurements from a 139 deg$^2$ field. We measure the abundance of peaks identified in aperture mass maps, as a function of their signal-to-noise ratio, in the signal-to-noise range $0<\\mathcal S / \\mathcal N<4$. To predict the peak counts as a function of cosmological parameters we use a suite of $N"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1603.05040","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":"1603.05040","created_at":"2026-05-18T01:07:16.980332+00:00"},{"alias_kind":"arxiv_version","alias_value":"1603.05040v1","created_at":"2026-05-18T01:07:16.980332+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1603.05040","created_at":"2026-05-18T01:07:16.980332+00:00"},{"alias_kind":"pith_short_12","alias_value":"SZ7OOKYWOQG2","created_at":"2026-05-18T12:30:44.179134+00:00"},{"alias_kind":"pith_short_16","alias_value":"SZ7OOKYWOQG22FXT","created_at":"2026-05-18T12:30:44.179134+00:00"},{"alias_kind":"pith_short_8","alias_value":"SZ7OOKYW","created_at":"2026-05-18T12:30:44.179134+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.12877","citing_title":"Machine-learning applications for weak-lensing cosmology","ref_index":25,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/SZ7OOKYWOQG22FXTL6JDV2KKV5","json":"https://pith.science/pith/SZ7OOKYWOQG22FXTL6JDV2KKV5.json","graph_json":"https://pith.science/api/pith-number/SZ7OOKYWOQG22FXTL6JDV2KKV5/graph.json","events_json":"https://pith.science/api/pith-number/SZ7OOKYWOQG22FXTL6JDV2KKV5/events.json","paper":"https://pith.science/paper/SZ7OOKYW"},"agent_actions":{"view_html":"https://pith.science/pith/SZ7OOKYWOQG22FXTL6JDV2KKV5","download_json":"https://pith.science/pith/SZ7OOKYWOQG22FXTL6JDV2KKV5.json","view_paper":"https://pith.science/paper/SZ7OOKYW","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1603.05040&json=true","fetch_graph":"https://pith.science/api/pith-number/SZ7OOKYWOQG22FXTL6JDV2KKV5/graph.json","fetch_events":"https://pith.science/api/pith-number/SZ7OOKYWOQG22FXTL6JDV2KKV5/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/SZ7OOKYWOQG22FXTL6JDV2KKV5/action/timestamp_anchor","attest_storage":"https://pith.science/pith/SZ7OOKYWOQG22FXTL6JDV2KKV5/action/storage_attestation","attest_author":"https://pith.science/pith/SZ7OOKYWOQG22FXTL6JDV2KKV5/action/author_attestation","sign_citation":"https://pith.science/pith/SZ7OOKYWOQG22FXTL6JDV2KKV5/action/citation_signature","submit_replication":"https://pith.science/pith/SZ7OOKYWOQG22FXTL6JDV2KKV5/action/replication_record"}},"created_at":"2026-05-18T01:07:16.980332+00:00","updated_at":"2026-05-18T01:07:16.980332+00:00"}