Dark Energy Survey Year 3 Results: High-precision measurement and modeling of galaxy-galaxy lensing
Creators: name: Prat, J.
name: Blazek, J.
name: Sánchez, C.
name: Tutusaus, I.
name: Pandey, S.
name: Elvin-Poole, J.
name: Krause, E.
name: Troxel, M. A.
name: Secco, L. F.
name: Amon, A.
name: DeRose, J.
name: Zacharegkas, G.
name: Chang, C.
name: Jain, B.
name: MacCrann, N.
name: Park, Y.
name: Sheldon, E.
name: Giannini, G.
name: Bocquet, S.
name: To, C.
name: Alarcon, A.
name: Alves, O.
name: Andrade-Oliveira, F.
name: Baxter, E.
name: Bechtol, K.
name: Becker, M. R.
name: Bernstein, G. M.
name: Camacho, H.
name: Campos, A.
name: Rosell, A. Carnero
name: Kind, M. Carrasco
name: Cawthon, R.
name: Chen, R.
name: Choi, A.
name: Cordero, J.
name: Crocce, M.
name: Davis, C.
name: De Vicente, J.
name: Diehl, H. T.
name: Dodelson, S.
name: Doux, C.
name: Drlica-Wagner, A.
name: Eckert, K.
name: Eifler, T. F.
name: Elsner, F.
name: Everett, S.
name: Fang, X.
name: Farahi, A.
name: Ferté, A.
name: Fosalba, P.
name: Friedrich, O.
name: Gatti, M.
name: Gruen, D.
name: Gruendl, R. A.
name: Harrison, I.
name: Hartley, W. G.
name: Herner, K.
name: Huang, H.
name: Huff, E. M.
name: Huterer, D.
name: Jarvis, M.
name: Kuropatkin, N.
name: Leget, P. -F.
name: Lemos, P.
name: Liddle, A. R.
name: McCullough, J.
name: Muir, J.
name: Myles, J.
name: Navarro-Alsina, A.
name: Porredon, A.
name: Raveri, M.
name: Rodriguez-Monroy, M.
name: Rollins, R. P.
name: Roodman, A.
name: Rosenfeld, R.
name: Ross, A. J.
name: Rykoff, E. S.
name: Sanchez, J.
name: Sevilla-Noarbe, I.
name: Shin, T.
name: Troja, A.
name: Varga, T. N.
name: Weaverdyck, N.
name: Wechsler, R. H.
name: Yanny, B.
name: Yin, B.
name: Zuntz, J.
name: Abbott, T. M. C.
name: Aguena, M.
name: Allam, S.
name: Annis, J.
name: Bacon, D.
name: Brooks, D.
name: Burke, D. L.
name: Carretero, J.
name: Conselice, C.
name: Costanzi, M.
name: da Costa, L. N.
name: Pereira, M. E. S.
name: Desai, S.
name: Dietrich, J. P.
name: Doel, P.
name: Evrard, A. E.
name: Ferrero, I.
name: Flaugher, B.
name: Frieman, J.
name: García-Bellido, J.
name: Gaztanaga, E.
name: Gerdes, D. W.
name: Giannantonio, T.
name: Gschwend, J.
name: Gutierrez, G.
name: Hinton, S. R.
name: Hollowood, D. L.
name: Honscheid, K.
name: James, D. J.
name: Kuehn, K.
name: Lahav, O.
name: Lin, H.
name: Maia, M. A. G.
name: Marshall, J. L.
name: Martini, P.
name: Melchior, P.
name: Menanteau, F.
name: Miller, C. J.
name: Miquel, R.
name: Mohr, J. J.
name: Morgan, R.
name: Ogando, R. L. C.
name: Palmese, A.
name: Paz-Chinchón, F.
name: Petravick, D.
name: Malagón, A. A. Plazas
name: Sanchez, E.
name: Serrano, S.
name: Smith, M.
name: Soares-Santos, M.
name: Suchyta, E.
name: Tarle, G.
name: Thomas, D.
name: Weller, J.
Publisher: name: arXiv
Year: 2021
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We present and characterize the galaxy-galaxy lensing signal measured using the first three years of data from the Dark Energy Survey (DES Y3) covering 4132 deg$^2$. These galaxy-galaxy measurements are used in the DES Y3 3$\times$2pt cosmological analysis, which combines weak lensing and galaxy clustering information. We use two lens samples: a magnitude-limited sample and the redMaGic sample, which span the redshift range $\sim 0.2-1$ with 10.7 M and 2.6 M galaxies respectively. For the source catalog, we use the Metacalibration shape sample, consisting of $\simeq$100 M galaxies separated into 4 tomographic bins. Our galaxy-galaxy lensing estimator is the mean tangential shear, for which we obtain a total S/N of $\sim$148 for MagLim ($\sim$120 for redMaGic), and $\sim$67 ($\sim$55) after applying the scale cuts of 6 Mpc/$h$. Thus we reach percent-level statistical precision, which requires that our modeling and systematic-error control be of comparable accuracy. The tangential shear model used in the 3$\times$2pt cosmological analysis includes lens magnification, a five-parameter intrinsic alignment model (TATT), marginalization over a point-mass to remove information from small scales and a linear galaxy bias model validated with higher-order terms. We explore the impact of these choices on the tangential shear observable and study the significance of effects not included in our model, such as reduced shear, source magnification and source clustering. We also test the robustness of our measurements to various observational and systematics effects, such as the impact of observing conditions, lens-source clustering, random-point subtraction, scale-dependent Metacalibration responses, PSF residuals, and B-modes.
description: 33 pages, 18 figures, accepted by PRD