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Rykoff, E. Suchyta, F. B. Abdalla, F. Menanteau, F. Sobreira, G. Gutierrez, G. Tarle, H. Lin, H. T. Diehl, I. Sevilla-Noarbe, J. Carretero, J. DeRose, J. De Vicente, J. Estrada, J. Frieman, J. Garc\\'ia-Bellido, J. Gschwend, J. J. Mohr, J. L. Marshall, J. P. Dietrich, J. Weller, K. Bechtol, K. Honscheid, K. Kuehn, L. N. da Costa, M. A. G. Maia, M. Carrasco Kind, M. Costanzi, M. Crocce, M. E. C. Swanson, M. Lima, M. March, M. Schubnell, M. Simet, M. Smith, M. Soares-Santos, N. Kuropatkin, P. Doel, P. Fosalba, P. Giles, P. Martini, R. A. Gruendl, R. H. Wechsler, R. L. C. Ogando, R. Miquel, R. Schindler, S. Allen T. McClintock, S. Avila, S. Bhargava, S. Serrano, T. F. Eifler, T. Giannantonio, T. Jeltema, T. M. C. Abbott, T. N. Varga, V. Scarpine, W. G. Hartley, X. Chen, Y. Zhang","submitted_at":"2018-10-22T18:00:01Z","abstract_excerpt":"We perform the first blind analysis of cluster abundance data. 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This value is both consistent and competitive with that derive"},"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":"1810.09456","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.CO","submitted_at":"2018-10-22T18:00:01Z","cross_cats_sorted":[],"title_canon_sha256":"d3fb037f9a6291c0ab7147af20e7c45ba19d1a7263ac17cd2fb0ec3e0bca2a3b","abstract_canon_sha256":"cebee0707dba938683dc9321f3e6a8ed76d16010e86da1dd832184a68d93f045"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:18:31.800233Z","signature_b64":"VS4v2FYZKFPr5unZJKT6VqTXNx2NrVQdS2k4X4xrgitXWzo/yvKFn6TuNawUqpxUsmiWtakXn5WQiiT8olCqAg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2519f9d256b394465449553a2b4021788a56464fead0a85e5243dfe7753bbb5b","last_reissued_at":"2026-07-05T00:18:31.799660Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:18:31.799660Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Dark Energy Survey Year 1 Results: Methods for Cluster Cosmology and Application to the SDSS","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. 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Avila, S. Bhargava, S. Serrano, T. F. Eifler, T. Giannantonio, T. Jeltema, T. M. C. Abbott, T. N. Varga, V. Scarpine, W. G. Hartley, X. Chen, Y. Zhang","submitted_at":"2018-10-22T18:00:01Z","abstract_excerpt":"We perform the first blind analysis of cluster abundance data. Specifically, we derive cosmological constraints from the abundance and weak-lensing signal of \\redmapper\\ clusters of richness $\\lambda\\geq 20$ in the redshift range $z\\in[0.1,0.3]$ as measured in the Sloan Digital Sky Survey (SDSS). We simultaneously fit for cosmological parameters and the richness--mass relation of the clusters. For a flat $\\Lambda$CDM cosmological model with massive neutrinos, we find $S_8 \\equiv \\sigma_{8}(\\Omega_m/0.3)^{0.5}=0.79^{+0.05}_{-0.04}$. 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