{"paper":{"title":"Constraints on the Richness-Mass Relation and the Optical-SZE Positional Offset Distribution for SZE-Selected Clusters","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. A. Plazas, A. A. Stark, A. Benoit-Levy, A. Carnero Rosell, A. E. Evrard, A. Fausti Neto, A.H. Bauer, A. K. Romer, A. Roodman, A. R. Walker, A. Saro, A. von der Linden, A. Zenteno, B. A. Benson, B. Flaugher, B. Jain, B. Nord, B. Stalder, C. B. D'Andrea, C. E Cunha, C. Gangkofner, C. Hennig, C. J. Miller, C. L. Reichardt, D. Brooks, D. Capozzi, D. Gerdes, D. Gruen, D. James, D. L. Burke, D. L. DePoy, D. Thomas, D. Tucker, E. Bertin, E. Buckley-Geer, E. Fernandez, E. Gaztanaga, E. Rozo, E. Sanchez, E. S. Rykoff, E. Suchyta, F. B. Abdalla, F. Sobreira, G. M. Bernstein, G. Tarle, H. Lin, H. T. Diehl, I. Chiu, I. Sevilla, J. E. Carlstrom, J. Frieman, J. L. Marshall, J. Mohr, J. P. Dietrich, J. Thaler, J. Weller, K. E. Ziegler, K. Honscheid, K. Kuehn, L. Bleem, L. N. da Costa, M. A. G. Maia, M. Banerji, M. Bayliss, M. Brodwin, M. Carrasco Kind, M. Crocce, M. E. C. Swanson, M. March, M. McDonald, M. Sako, M. Schubnell, M. Soares-Santos, N. Gupta, N. Kuropatkin, O. Lahav, Paul Martini, P. Doel, P. Fosalba, P. Melchior, R. A. Gruendl, R. Armstrong, R. Capasso, R. Covarrubias, R. C. Smith, R. H. Wechsler, R. Miquel, R. Ogando, S. Allam, S. Bocquet, S. Desai, S. Dodelson, T. Abbott, T. de Haan, T. F. Eifler, T. M. Crawford, T. S. Li, V. Strazzullo, V. Upadhyay, V. Vikram, W. L. Holzapfel, W. Wester","submitted_at":"2015-06-25T17:00:43Z","abstract_excerpt":"We cross-match galaxy cluster candidates selected via their Sunyaev-Zel'dovich effect (SZE) signatures in 129.1 deg$^2$ of the South Pole Telescope 2500d SPT-SZ survey with optically identified clusters selected from the Dark Energy Survey (DES) science verification data. We identify 25 clusters between $0.1\\lesssim z\\lesssim 0.8$ in the union of the SPT-SZ and redMaPPer (RM) samples. RM is an optical cluster finding algorithm that also returns a richness estimate for each cluster. We model the richness $\\lambda$-mass relation with the following function $\\langle\\ln\\lambda|M_{500}\\rangle\\propt"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1506.07814","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"}