{"paper":{"title":"Wide-Field Lensing Mass Maps from DES Science Verification Data: Methodology and Detailed Analysis","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Amara, A. A. Plazas, A. Benoit-Levy, A. Carnero Rosell, A. E. Evrard, A. Fausti Neto, A. H. Bauer, A. Kovacs, A. K. Romer, A. Roodman, A. R. Walker, B. Flaugher, B. Jain, B. Leistedt, B. Nord, C. B. D'Andrea, C. Bonnett, C. Chang, C. E. Cunha, C. J. Miller, C. Sanchez, D. Bacon, D. Brooks, D. Brout, D. Capozzi, D. Gerdes, D. Gruen, D. James, D. L. Burke, D. L. DePoy, D. Thomas, E. Bertin, E. Buckley-Geer, E. Fernandez, E. Gaztanaga, E. Neilsen, E. Rozo, E. Rykoff, E. Sanchez, E. Sheldon, E. Suchyta, F. B. Abdalla, F. J. Castander, F. Sobreira, G. Bernstein, G. Tarle, H. Lin, H. Peiris, H. T. Diehl, I. Sevilla, J. Estrada, J. Frieman, J. Marshall, J. P. Dietrich, J. Thaler, J. Weller, J. Zuntz, K. Honscheid, K. Kuehn, K. W. Merritt, L. N. da Costa, M. A. G. Maia, M. A. Troxel, M. Banerji, M. Busha, M. Carrasco Kind, M. Crocce, M. E. C. Swanson, M. Jarvis, M. Makler, M. March, M. R. Becker, M. Soares-Santos, N. Kuropatkin, O. Lahav, P. Fosalba, P. Martini, P. Melchior, R. A. Gruendl, R. Armstrong, R. C. Nichol, R. C. Smith, R. Miquel, R. Ogando, R. Wechsler, S. Bridle, S. Desai, S. Kent, T. Abbott, T. Kacprzak, T. S. Li, V. Scarpine, V. Vikram, W. Hartley","submitted_at":"2015-04-12T18:45:38Z","abstract_excerpt":"Weak gravitational lensing allows one to reconstruct the spatial distribution of the projected mass density across the sky. These \"mass maps\" provide a powerful tool for studying cosmology as they probe both luminous and dark matter. In this paper, we present a weak lensing mass map reconstructed from shear measurements in a 139 sq. deg area from the Dark Energy Survey (DES) Science Verification (SV) data. We compare the distribution of mass with that of the foreground distribution of galaxies and clusters. The overdensities in the reconstructed map correlate well with the distribution of opti"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1504.03002","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"}