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Dark Energy Survey year 1 results: Cosmological constraints from galaxy clustering and weak lensing

Physical review. D/Physical review. D.2018Vol. 98(4)

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T. M. C. Abbott, F. B. Abdalla, A. Alarcon, J. Aleksić, S. Allam, S. W. Allen, A. Amara, J. Annis, J. Asorey, S. Àvila, David Bacon, E. Balbinot, M. Banerji, Nilanjan Banik, Wayne Barkhouse, Michael Baumer, Eric J. Baxter, K. Bechtol, M. R. Becker, A. Benoit-Lévy, B. A. Benson, G. M. Bernstein, E. Bertin, J. Blazek, Sarah Bridle, D. Brooks, Dillon Brout, E. Buckley‐Geer, D. L. Burke, Michael T. Busha, A. Campos, D. Capozzi, A. Carnero Rosell, M. Carrasco Kind, J. Carretero, F. J. Castander, R. Cawthon, C. Chang, Nianyi Chen, M. Childress, A. Choi, Christopher J. Conselice, Robert Crittenden, M. Crocce, C. E. Cunha, C. B. D’Andrea, L. da Costa, Ritanjan Das, T. M. Davis, C. Davis, J. De Vicente, D. L. DePoy, Joseph DeRose, S. Desai, H. T. Diehl, J. P. Dietrich, Scott Dodelson, P. Doel, A. Drlica-Wagner, T. F. Eifler, A. Elliott, F. Elsner, J. Elvin-Poole, J. Estrada, A. E. Evrard, Y Fang, E. Fernández, A. Ferté, D. A. Finley, B. Flaugher, P. Fosalba, O. Friedrich, J. Frieman, J. García-Bellido, M. Garcia-Fernandez, M. Gatti, E. Gaztañaga, D. W. Gerdes, T. Giannantonio, M. S. S. Gill, Karl Glazebrook, D. A. Goldstein, D. Gruen, R. A. Gruendl, J. Gschwend, G. Gutiérrez, S. Hamilton, W. G. Hartley, S. R. Hinton, K. Honscheid, B. Hoyle, Dragan Huterer, Bhuvnesh Jain, D. J. James, Mike Jarvis, T. Jeltema, M. D. Johnson, Michele Johnson, Tomasz Kacprzak, S. Kent, A. G. Kim, A. L. King, D. Kirk, Nickolas Kokron, András Kovács, E. Krause, C. Krawiec, S. W. Allen, K. Kuehn, S. E. Kuhlmann, N. Kuropatkin, F. Lacasa, O. Lahav, T. S. Li, Andrew R. Liddle, C. Lidman, M. Lima, H. Lin, N. MacCrann, M. A. G. Maia, M. Makler, Marc Manera, M. March, J. L. Marshall, Paul Martini, R. G. McMahon, P. Melchior, F. Menanteau, R. Miquel, Vivian Miranda, D. Mudd, J. Muir, A. Möller, Eric H. Neilsen, R. C. Nichol, B. Nord, P. Nugent, R. L. C. Ogando, A. Palmese, J. A. Peacock, Hiranya V. Peiris, J. Peoples, Will J. Percival, D. Petravick, A. A. Plazas, A. Porredon, J. Prat, Arnau Pujol, Markus Michael Rau, Alexandre Réfrégier, P. M. Ricker, N. Roe, R. P. Rollins, A. K. Romer, A. Roodman, R. Rosenfeld, Ashley J. Ross, Eduardo Rozo, E. S. Rykoff, M. Šako, A. I. Salvador, S. Samuroff, C. Sánchez, E. Sánchez, B. X. Santiago, V. Scarpine, R. Schindler, D. Scolnic, L. F. Secco, S. Serrano, I. Sevilla-Noarbe, E. Sheldon, R. C. Smith, M. Smith, J. A. Smith, M. Soares-Santos, F. Sobreira, E. Suchyta, G. Tarlé, D. Thomas, M. A. Troxel, D. L. Tucker, B. Tucker, S. A. Uddin, T N Varga, P Vielzeuf, V. Vikram, A. K. Vivas, A. R. Walker, M. Wang, Risa H. Wechsler, J. Weller, W. C. Wester, R. C. Wolf, B. Yanny, F. Yuan, A. Zenteno, B. Zhang, Y. Zhang, J. Zuntz

Abstract

We present cosmological results from a combined analysis of galaxy clustering and weak gravitational lensing, using 1321 deg 2 of griz imaging data from the first year of the Dark Energy Survey (DES Y1). We combine three two-point functions: (i) the cosmic shear correlation function of 26 million source galaxies in four redshift bins, (ii) the galaxy angular autocorrelation function of 650,000 luminous red galaxies in five redshift bins, and (iii) the galaxy-shear cross-correlation of luminous red galaxy positions and source galaxy shears. To demonstrate the robustness of these results, we use independent pairs of galaxy shape, photometric-redshift estimation and validation, and likelihood analysis pipelines. To prevent confirmation bias, the bulk of the analysis was carried out while "blind" to the true results; we describe an extensive suite of systematics checks performed and passed during this blinded phase. The data are modeled in flat CDM and wCDM cosmologies, marginalizing over 20 nuisance parameters, varying 6 (for CDM) or 7 (for wCDM) cosmological parameters including the neutrino mass density and including the 457 457 element analytic covariance matrix. We find consistent cosmological results from these three two-point functions and from their combination obtain S 8 8 m =0.3 0.5 0.773 0.026 -0.020 and m 0.267 0.030 -0.017 for CDM; for wCDM, we find S 8 0.782 0.036 -0.024 , m 0.284 0.033 -0.030 , and w -0.82 0.21 -0.20 at 68% C.L. The precision of these DES Y1 constraints rivals that from the Planck cosmic microwave background measurements, allowing a comparison of structure in the very

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Abstract

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