Dark Energy Survey Year 1 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing. (arXiv:1708.01530v3 [astro-ph.CO] UPDATED)

Dark Energy Survey Year 1 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing. (arXiv:1708.01530v3 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_DES/0/1/0/all/0/1">DES Collaboration</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Abbott_T/0/1/0/all/0/1">T. M. C. Abbott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abdalla_F/0/1/0/all/0/1">F. B. Abdalla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alarcon_A/0/1/0/all/0/1">A. Alarcon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aleksic_J/0/1/0/all/0/1">J. Aleksić</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allam_S/0/1/0/all/0/1">S. Allam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allen_S/0/1/0/all/0/1">S. Allen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amara_A/0/1/0/all/0/1">A. Amara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Annis_J/0/1/0/all/0/1">J. Annis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Asorey_J/0/1/0/all/0/1">J. Asorey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avila_S/0/1/0/all/0/1">S. Avila</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bacon_D/0/1/0/all/0/1">D. Bacon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Balbinot_E/0/1/0/all/0/1">E. Balbinot</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Banerji_M/0/1/0/all/0/1">M. Banerji</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Banik_N/0/1/0/all/0/1">N. Banik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barkhouse_W/0/1/0/all/0/1">W. Barkhouse</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baumer_M/0/1/0/all/0/1">M. Baumer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baxter_E/0/1/0/all/0/1">E. Baxter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bechtol_K/0/1/0/all/0/1">K. Bechtol</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Becker_M/0/1/0/all/0/1">M. R. Becker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benoit_Levy_A/0/1/0/all/0/1">A. Benoit-Lévy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benson_B/0/1/0/all/0/1">B. A. Benson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernstein_G/0/1/0/all/0/1">G. M. Bernstein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertin_E/0/1/0/all/0/1">E. Bertin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blazek_J/0/1/0/all/0/1">J. Blazek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bridle_S/0/1/0/all/0/1">S. L. Bridle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brooks_D/0/1/0/all/0/1">D. Brooks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brout_D/0/1/0/all/0/1">D. Brout</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Buckley_Geer_E/0/1/0/all/0/1">E. Buckley-Geer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burke_D/0/1/0/all/0/1">D. L. Burke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Busha_M/0/1/0/all/0/1">M. T. Busha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Capozzi_D/0/1/0/all/0/1">D. Capozzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosell_A/0/1/0/all/0/1">A. Carnero Rosell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kind_M/0/1/0/all/0/1">M. Carrasco Kind</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carretero_J/0/1/0/all/0/1">J. Carretero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castander_F/0/1/0/all/0/1">F. J. Castander</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cawthon_R/0/1/0/all/0/1">R. Cawthon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chang_C/0/1/0/all/0/1">C. Chang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_N/0/1/0/all/0/1">N. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Childress_M/0/1/0/all/0/1">M. Childress</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choi_A/0/1/0/all/0/1">A. Choi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Conselice_C/0/1/0/all/0/1">C. Conselice</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crittenden_R/0/1/0/all/0/1">R. Crittenden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crocce_M/0/1/0/all/0/1">M. Crocce</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cunha_C/0/1/0/all/0/1">C. E. Cunha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DAndrea_C/0/1/0/all/0/1">C. B. D'Andrea</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Costa_L/0/1/0/all/0/1">L. N. da Costa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Das_R/0/1/0/all/0/1">R. Das</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davis_T/0/1/0/all/0/1">T. M. Davis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davis_C/0/1/0/all/0/1">C. Davis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vicente_J/0/1/0/all/0/1">J. De Vicente</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DePoy_D/0/1/0/all/0/1">D. L. DePoy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DeRose_J/0/1/0/all/0/1">J. DeRose</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Desai_S/0/1/0/all/0/1">S. Desai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diehl_H/0/1/0/all/0/1">H. T. Diehl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dietrich_J/0/1/0/all/0/1">J. P. Dietrich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dodelson_S/0/1/0/all/0/1">S. Dodelson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doel_P/0/1/0/all/0/1">P. Doel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drlica_Wagner_A/0/1/0/all/0/1">A. Drlica-Wagner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eifler_T/0/1/0/all/0/1">T. F. Eifler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elliott_A/0/1/0/all/0/1">A. E. Elliott</a>, et al. (139 additional authors not shown)

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 $Lambda$CDM and $w$CDM
cosmologies, marginalizing over 20 nuisance parameters, varying 6 (for
$Lambda$CDM) or 7 (for $w$CDM) cosmological parameters including the neutrino
mass density and including the 457 $times$ 457 element analytic covariance
matrix. We find consistent cosmological results from these three two-point
functions, and from their combination obtain $S_8 equiv sigma_8
(Omega_m/0.3)^{0.5} = 0.783^{+0.021}_{-0.025}$ and $Omega_m =
0.264^{+0.032}_{-0.019}$ for $Lambda$CDM for $w$CDM, we find $S_8 =
0.794^{+0.029}_{-0.027}$, $Omega_m = 0.279^{+0.043}_{-0.022}$, and
$w=-0.80^{+0.20}_{-0.22}$ at 68% CL. The precision of these DES Y1 results
rivals that from the Planck cosmic microwave background measurements, allowing
a comparison of structure in the very early and late Universe on equal terms.
Although the DES Y1 best-fit values for $S_8$ and $Omega_m$ are lower than the
central values from Planck …

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