{"paper":{"title":"Dark Energy Survey Year 1 Results: Measurement of the Baryon Acoustic Oscillation scale in the distribution of galaxies to redshift 1","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Alarcon, A. A. Plazas, A. Carnero Rosell, A. Drlica-Wagner, A. E. Evrard, A. J. Ross, A. K. Romer, A. Porredon, A. Roodman, A. R. Walker, B. Flaugher, B. Hoyle, B. Jain, B. Santiago, B. Yanny, C. B. D'Andrea, C. Davis, C. E. Cunha, C. J. Miller, D. Brooks, D. Gruen, D. Hollowood, D. J. James, D. L. Burke, D. L. DePoy, D. L. Tucker, D. Thomas, D. W. Gerdes, E. Bertin, E. Buckley-Geer, E. Gaztanaga, E. Krause, E. Neilsen, E. Rozo, E. Sanchez, E. Sheldon, E. S. Rykoff, E. Suchyta, F. Andrade-Oliveira, F. B. Abdalla, F. J. Castander, F. Lacasa, F. Menanteau, F. Sobreira, G. Gutierrez, G. M. Bernstein, G. Tarle, H. Camacho, H. Lin, H. T. Diehl, I. Sevilla-Noarbe, J. Annis, J. Carretero, J. De Vicente, J. Elvin-Poole, J. Estrada, J. Frieman, J. Garcia-Bellido, J. Gschwend, J. J. Mohr, J. L. Marshall, J. Marriner, J. Weller, K. Bechtol, K. C. Chan, K. Honscheid, K. Kuehn, L. N. da Costa, M. A. G. Maia, M. A. Troxel, M. Banerji, M. Carrasco Kind, M. Crocce, M. D. Johnson, M. E. C. Swanson, M. Lima, M. Manera, M. Sako, M. Schubnell, M. Smith, N. Banik, N. Kokron, N. Kuropatkin, O. Lahav, P. Doel, P. Fosalba, P. Martini, P. Melchior, R. A. Bernstein, R. A. Gruendl, R. Cawthon, R. C. Smith, R. H. Wechsler, R. Miquel, R. Rosenfeld, R. Schindler, S. Allam, S. Avila, S. Desai, S. Kent, S. Kuhlmann, S. Serrano, T. F. Eifler, T. Giannantonio, The Dark Energy Survey Collaboration: T. M. C. Abbott, T. Jeltema, V. Scarpine, V. Vikram, W. G. Hartley, W. J. Percival, Y. Zhang","submitted_at":"2017-12-17T23:48:05Z","abstract_excerpt":"We present angular diameter distance measurements obtained by locating the BAO scale in the distribution of galaxies selected from the first year of Dark Energy Survey data. We consider a sample of over 1.3 million galaxies distributed over a footprint of 1318 deg$^2$ with $0.6 < z_{\\rm photo} < 1$ and a typical redshift uncertainty of $0.03(1+z)$. This sample was selected, as fully described in a companion paper, using a color/magnitude selection that optimizes trade-offs between number density and redshift uncertainty. We investigate the BAO signal in the projected clustering using three con"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1712.06209","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"}