{"paper":{"title":"Testing the $\\mathbf{\\Lambda}$CDM Cosmological Model with Forthcoming Measurements of the Cosmic Microwave Background with SPT-3G","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. A. Stark, A. Coerver, A. Cukierman, A. Doussot, A. E. Gambrel, A. E. Lowitz, A. Foster, A. Hryciuk, A. J. Anderson, A. Maniyar, A. N. Bender, A. Rahlin, A. Suzuki, A. T. Lee, A. Vitrier, B. A. Benson, B. Ansarinejad, B. Thorne, C. Daley, C. Feng, C. L. Chang, C.-L. Kuo, C. L. Reichardt, C. Lu, C. Tandoi, C. Trendafilova, C. Tucker, C. Umilta, D. Dutcher, E. Anderes, E. Camphuis, E. Hivon, E. Schiappucci, F. Bianchini, F. Ge, F. Guidi, F. K\\'eruzor\\'e, F. Menanteau, F. R. Bouchet, G. I. Noble, G. Lynch, G. P. Holder, G. Smecher, G. Wang, J. A. Sobrin, J. A. Zebrowski, J. C. Hood, J. D. Vieira, J. E. Carlstrom, J. E. Ruhl, J. Montgomery, J. Stephen, K. A. Phadke, K. Benabed, K. Fichman, K. Kornoelje, K. Levy, K. L. Thompson, K. Prabhu, K. R. Dibert, K. R. Ferguson, L. Balkenhol, L. Bryant, L. E. Bleem, L. Knox, M. A. Dobbs, M. Archipley, M. Korman, M. Millea, M. Rahimi, M. Rouble, M. R. Young, N. Goeckner-Wald, N. Huang, N. W. Halverson, N. Whitehorn, P. A. R. Ade, P. Chaubal, P. M. Chichura, P. Paschos, R. Gualtieri, R. W. Gardner, S. Galli, S. Guns, S. Padin, S. Raghunathan, T. de Haan, T.-L. Chou, T. M. Crawford, T. Natoli, T. W. Cecil, V. Novosad, V. Yefremenko, W. Everett, W. L. Holzapfel, W. L. K. Wu, W. Quan, Y. Nakato, Y. Omori, Y. Wan, Z. Pan","submitted_at":"2024-03-26T17:57:20Z","abstract_excerpt":"We forecast constraints on cosmological parameters enabled by three surveys conducted with SPT-3G, the third-generation camera on the South Pole Telescope. The surveys cover separate regions of 1500, 2650, and 6000 ${\\rm deg}^{2}$ to different depths, in total observing 25% of the sky. These regions will be measured to white noise levels of roughly 2.5, 9, and 12 $\\mu{\\rm K-arcmin}$, respectively, in CMB temperature units at 150 GHz by the end of 2024. The survey also includes measurements at 95 and 220 GHz, which have noise levels a factor of ~1.2 and 3.5 times higher than 150 GHz, respective"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2403.17925","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2403.17925/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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"}