{"paper":{"title":"The Dark Energy Survey Year 3 high redshift sample: Selection, characterization and analysis of galaxy clustering","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.IM"],"primary_cat":"astro-ph.CO","authors_text":"A. Alarcon, A. Amon, A. A. Plazas Malag\\'on, A. Campos, A. Carnero Rosell, A. Choi, A. Drlica-Wagner, A. Palmese, A. Pieres, A. Porredon, B. Flaugher, B. Jain, B. Yanny, B. Yin, C. Chang, C. Conselice, C. Doux, C. S\\'anchez, C. To, D. Brooks, D. Cross, D. Gruen, D. J. James, D. L. Burke, D. L. Hollowood, D. Thomas, E. Baxter, E. Bertin, E. Krause, E. M. Huff, E. Sanchez, E. Sheldon, E. S. Rykoff, E. Suchyta, F. Andrade-Oliveira, F. J. Castander, F. Menanteau, F. Paz-Chinch\\'on, G. Gutierrez, G. M. Bernstein, G. Tarle, H. Huang, H. T. Diehl, I. Ferrero, I. Harrison, I. Sevilla-Noarbe, J. Blazek, J. Carretero, J. DeRose, J. Elvin-Poole, J. Frieman, J. Garc\\'ia-Bellido, J. L. Marshall, J. McCullough, J. Mena-Fern\\'andez, J. Myles, J. Prat, J. Sanchez, J. Zuntz, K. Bechtol, K. Eckert, K. Herner, K. Honscheid, K. Kuehn, L. F. Secco, M. Aguena, M. A. Troxel, M. Carrasco Kind, M. Costanzi, M. Crocce, M. E. S. Pereira, M. Raveri, M. R. Becker, M. Rodriguez-Monroy, M. Schubnell, M. Smith, N. Kuropatkin, N. MacCrann, N. Weaverdyck, O. Alves, P. Doel, P. Fosalba, R. A. Gruendl, R. Cawthon, R. L. C. Ogando, R. Miquel, S. Allam, S. Bocquet, S. Desai, S. Dodelson, S. Everett, S. Pandey, S. R. Hinton, T. F. Eifler, T. M. C. Abbott, V. Scarpine, W. G. Hartley, X. Fang, Y. Omori, Y. Zhang","submitted_at":"2022-11-29T21:07:25Z","abstract_excerpt":"The fiducial cosmological analyses of imaging galaxy surveys like the Dark Energy Survey (DES) typically probe the Universe at redshifts $z < 1$. This is mainly because of the limited depth of these surveys, and also because such analyses rely heavily on galaxy lensing, which is more efficient at low redshifts. In this work we present the selection and characterization of high-redshift galaxy samples using DES Year 3 data, and the analysis of their galaxy clustering measurements. In particular, we use galaxies that are fainter than those used in the previous DES Year 3 analyses and a Bayesian "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2211.16593","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2211.16593/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"}