{"paper":{"title":"Dark Energy Survey Year 1 Results: Weak Lensing Mass Calibration of redMaPPer Galaxy Clusters","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. A. Plazas, A. Bermeo, A. Carnero Rosell, A. Drlica-Wagner, A. E. Evrard, A. Farahi, A. K. Romer, A. Mantz, A. Palmese, A. Roodman, A. R. Walker, A. von der Linden, B. Flaugher, B. Hoyle, B. Nord, C. B. D'Andrea, C. Davis, C. E. Cunha, C. Vergara Cervantes, D. Brooks, D. Gruen, D. J. James, D. Kirk, D. L. Burke, D. L. Hollowood, D. L. Tucker, D. W. Gerdes, E. Gaztanaga, E. Krause, E. Rozo, E. Sanchez, E. Sheldon, E. S. Rykoff, E. Suchyta, F. B. Abdalla, F. J. Castander, F. Menanteau, F. Sobreira, G. Gutierrez, G. Morris, G. Pollina, G. Tarle, H. Israel, H. T. Diehl, I. Sevilla-Noarbe, J. Annis, J. Carretero, J. DeRose, J. De Vicente, J. Frieman, J. Garc\\'ia-Bellido, J. J. Mohr, J. L. Marshall, J. P. Dietrich, J. Weller, J. Zuntz, K. Honscheid, K. Kuehn, L. N. da Costa, M. A. Troxel, M. Carrasco Kind, M. Costanzi, M. Crocce, M. E. C. Swanson, M. Lima, M. March, M. M. Rau, M. R. Becker, M. Simet, M. Smith, M. Soares-Santos, N. Hamaus, N. MacCrann, O. Lahav, P. Doel, P. Fosalba, P. Li, P. Melchior, R. A. Gruendl, R. C. Smith, R. H. Wechsler, R. L. C. Ogando, R. Miquel, R. Schindler, S. Allam, S. Allen, S. Avila, S. Bhargava, S. Everett, S. L. Bridle, S. Seitz, T. Giannantonio, T. Jeltema, T. M. C. Abbott, T. McClintock, T. N. Varga, T. Shin, T. S. Li, V. Scarpine, V. Vikram, W. G. Hartley, Y. Zhang","submitted_at":"2018-04-30T18:01:07Z","abstract_excerpt":"We constrain the mass--richness scaling relation of redMaPPer galaxy clusters identified in the Dark Energy Survey Year 1 data using weak gravitational lensing. We split clusters into $4\\times3$ bins of richness $\\lambda$ and redshift $z$ for $\\lambda\\geq20$ and $0.2 \\leq z \\leq 0.65$ and measure the mean masses of these bins using their stacked weak lensing signal. By modeling the scaling relation as $\\langle M_{\\rm 200m}|\\lambda,z\\rangle = M_0 (\\lambda/40)^F ((1+z)/1.35)^G$, we constrain the normalization of the scaling relation at the 5.0 per cent level as $M_0 = [3.081 \\pm 0.075 ({\\rm stat"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1805.00039","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"}