Dark Energy Survey Year 1 Results: Cross-correlation between DES Y1 galaxy weak lensing and SPT+Planck CMB weak lensing
Creators: name: Omori, Y.
name: Baxter, E.
name: Chang, C.
name: Kirk, D.
name: Alarcon, A.
name: Bernstein, G. M.
name: Bleem, L. E.
name: Cawthon, R.
name: Choi, A.
name: Chown, R.
name: Crawford, T. M.
name: Davis, C.
name: De Vicente, J.
name: DeRose, J.
name: Dodelson, S.
name: Eifler, T. F.
name: Fosalba, P.
name: Friedrich, O.
name: Gatti, M.
name: Gaztanaga, E.
name: Giannantonio, T.
name: Gruen, D.
name: Hartley, W. G.
name: Holder, G. P.
name: Hoyle, B.
name: Huterer, D.
name: Jain, B.
name: Jarvis, M.
name: Krause, E.
name: MacCrann, N.
name: Miquel, R.
name: Prat, J.
name: Rau, M. M.
name: Reichardt, C. L.
name: Rozo, E.
name: Samuroff, S.
name: Sánchez, C.
name: Secco, L. F.
name: Sheldon, E.
name: Simard, G.
name: Troxel, M. A.
name: Vielzeuf, P.
name: Wechsler, R. H.
name: Zuntz, J.
name: Abbott, T. M. C.
name: Abdalla, F. B.
name: Allam, S.
name: Annis, J.
name: Avila, S.
name: Aylor, K.
name: Benson, B. A.
name: Bertin, E.
name: Bridle, S. L.
name: Brooks, D.
name: Burke, D. L.
name: Carlstrom, J. E.
name: Rosell, A. Carnero
name: Kind, M. Carrasco
name: Carretero, J.
name: Castander, F. J.
name: Chang, C. L.
name: Cho, H-M.
name: Crites, A. T.
name: Crocce, M.
name: Cunha, C. E.
name: da Costa, L. N.
name: de Haan, T.
name: Desai, S.
name: Diehl, H. T.
name: Dietrich, J. P.
name: Dobbs, M. A.
name: Everett, W. B.
name: Fernandez, E.
name: Flaugher, B.
name: Frieman, J.
name: García-Bellido, J.
name: George, E. M.
name: Gruendl, R. A.
name: Gutierrez, G.
name: Halverson, N. W.
name: Harrington, N. L.
name: Hollowood, D. L.
name: Honscheid, K.
name: Holzapfel, W. L.
name: Hou, Z.
name: Hrubes, J. D.
name: James, D. J.
name: Jeltema, T.
name: Kuehn, K.
name: Kuropatkin, N.
name: Lima, M.
name: Lin, H.
name: Lee, A. T.
name: Leitch, E. M.
name: Luong-Van, D.
name: Maia, M. A. G.
name: Manzotti, A.
name: Marrone, D. P.
name: Marshall, J. L.
name: Martini, P.
name: McMahon, J. J.
name: Melchior, P.
name: Menanteau, F.
name: Meyer, S. S.
name: Mocanu, L. M.
name: Mohr, J. J.
name: Natoli, T.
name: Ogando, R. L. C.
name: Padin, S.
name: Plazas, A. A.
name: Pryke, C.
name: Romer, A. K.
name: Roodman, A.
name: Ruhl, J. E.
name: Rykoff, E. S.
name: Sanchez, E.
name: Scarpine, V.
name: Schaffer, K. K.
name: Schindler, R.
name: Sevilla-Noarbe, I.
name: Shirokoff, E.
name: Smith, M.
name: Smith, R. C.
name: Soares-Santos, M.
name: Sobreira, F.
name: Staniszewski, Z.
name: Stark, A. A.
name: Story, K. T.
name: Suchyta, E.
name: Swanson, M. E. C.
name: Tarle, G.
name: Thomas, D.
name: Vanderlinde, K.
name: Vieira, J. D.
name: Vikram, V.
name: Walker, A. R.
name: Weller, J.
name: Williamson, R.
name: Wu, W. L. K.
name: Zahn, O.
Publisher: name: arXiv
Year: 2018
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We cross-correlate galaxy weak lensing measurements from the Dark Energy Survey (DES) year-one (Y1) data with a cosmic microwave background (CMB) weak lensing map derived from South Pole Telescope (SPT) and Planck data, with an effective overlapping area of 1289 deg$^{2}$. With the combined measurements from four source galaxy redshift bins, we reject the hypothesis of no lensing with a significance of $10.8σ$. When employing angular scale cuts, this significance is reduced to $6.8σ$, which remains the highest signal-to-noise measurement of its kind to date. We fit the amplitude of the correlation functions while fixing the cosmological parameters to a fiducial $Λ$CDM model, finding $A = 0.99 \pm 0.17$. We additionally use the correlation function measurements to constrain shear calibration bias, obtaining constraints that are consistent with previous DES analyses. Finally, when performing a cosmological analysis under the $Λ$CDM model, we obtain the marginalized constraints of $Ω_{\rm m}=0.261^{+0.070}_{-0.051}$ and $S_{8}\equiv σ_{8}\sqrt{Ω_{\rm m}/0.3} = 0.660^{+0.085}_{-0.100}$. These measurements are used in a companion work that presents cosmological constraints from the joint analysis of two-point functions among galaxies, galaxy shears, and CMB lensing using DES, SPT and Planck data.
description: 15 pages, 6 figures