{"paper":{"title":"Baryon Content in a Sample of 91 Galaxy Clusters Selected by the South Pole Telescope at 0.2 < z < 1.25","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. A. Plazas, A. Benoit-L\\'evy, A. Carnero Rosell, A. Drlica-Wagner, A. E. Evrard, A. Gonzalez, A. K. Romer, A. Roodman, A. R. Walker, A. Saro, A. Stanford, B. A. Benson, B. Flaugher, B. Nord, B. Stalder, C. B. D'Andrea, C. Davis, C. E. Cunha, C. L. Reichardt, C. Stern, D. Brooks, D. Gruen, D. J. James, D. Rapetti, D. W. Gerdes, E. Bertin, E. Buckley-Geer, E. Bulbul, E. Gaztanaga, E. Krause, E. Sanchez, E. Suchyta, F. B. Abdalla, F. J. Castander, F. Menanteau, F. Sobreira, G. Garmire, G. Gutierrez, G. Tarle, H. Israel, H. T. Diehl, I. Chiu, J. Annis, J. Carretero, J. E. Carlstrom, J. Garc\\'ia-Bellido, J. Gschwend, J. Hlavacek-L., J. J. Mohr, J. L. Marshall, J. P. Dietrich, J. Weller, K. Honscheid, K. Kuehn, K. Sharon, L. Bleem, L. N. da Costa, M. A. G. Maia, M. Bayliss, M. Brodwin, M. E. C. Swanson, M. Klein, M. Lima, M. L. N. Ashby, M. McDonald, M. Schubnell, M. Smith, M. Soares-Santos, N. Gupta, N. Kuropatkin, O. Lahav, P. Doel, P. Melchior, R. A. Gruendl, R. Capasso, R. C. Smith, R. Kraft, R. L. C. Ogando, R. Miquel, R. Schindler, S. Allam, S. Bocquet, S. Desai, S. Kuhlmann, S. Murray, T. F. Eifler, T. Jeltema, T. M. C. Abbott, V. Scarpine, V. Strazzullo, V. Vikram, Y. Zhang","submitted_at":"2017-11-02T20:25:27Z","abstract_excerpt":"We estimate total mass ($M_{500}$), intracluster medium (ICM) mass ($M_{\\mathrm{ICM}}$) and stellar mass ($M_{\\star}$) in a Sunyaev-Zel'dovich effect (SZE) selected sample of 91 galaxy clusters with masses $M_{500}\\gtrsim2.5\\times10^{14}M_{\\odot}$ and redshift $0.2 < z < 1.25$ from the 2500 deg$^2$ South Pole Telescope SPT-SZ survey. The total masses $M_{500}$ are estimated from the SZE observable, the ICM masses $M_{\\mathrm{ICM}}$ are obtained from the analysis of $Chandra$ X-ray observations, and the stellar masses $M_{\\star}$ are derived by fitting spectral energy distribution templates to "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1711.00917","kind":"arxiv","version":3},"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"}