Dark Energy Survey year 1 results: curved-sky weak lensing mass map

C. Chang, A. Pujol, B. Mawdsley, D. Bacon, J. Elvin-Poole, P. Melchior, A. Kovács, B. Jain, B. Leistedt, T. Giannantonio, A. Alarcon, E. Baxter, K. Bechtol, M. R. Becker, A. Benoit-Lévy, G. M. Bernstein, C. Bonnett, M. T. Busha, A. Carnero Rosell, F. J. CastanderR. Cawthon, L. N. da Costa, C. Davis, J. De Vicente, J. DeRose, A. Drlica-Wagner, P. Fosalba, M. Gatti, E. Gaztanaga, D. Gruen, J. Gschwend, W. G. Hartley, B. Hoyle, E. M. Huff, M. Jarvis, N. Jeffrey, T. Kacprzak, H. Lin, N. MacCrann, M. A. G. Maia, R. L. C. Ogando, J. Prat, M. M. Rau, R. P. Rollins, A. Roodman, E. Rozo, E. S. Rykoff, S. Samuroff, C. Sánchez, I. Sevilla-Noarbe, E. Sheldon, M. A. Troxel, T. N. Varga, P. Vielzeuf, V. Vikram, R. H. Wechsler, J. Zuntz, T. M. C. Abbott, F. B. Abdalla, S. Allam, J. Annis, E. Bertin, D. Brooks, E. Buckley-Geer, D. L. Burke, M. Carrasco Kind, J. Carretero, M. Crocce, C. E. Cunha, C. B. D'Andrea, S. Desai, H. T. Diehl, J. P. Dietrich, P. Doel, J. Estrada, A. Fausti Neto, E. Fernandez, B. Flaugher, J. Frieman, J. García-Bellido, R. A. Gruendl, G. Gutierrez, K. Honscheid, D. J. James, T. Jeltema, M. W. G. Johnson, M. D. Johnson, S. Kent, D. Kirk, E. Krause, K. Kuehn, S. Kuhlmann, O. Lahav, T. S. Li, M. Lima, M. March, P. Martini, F. Menanteau, R. Miquel, J. J. Mohr, E. Neilsen, R. C. Nichol, D. Petravick, A. A. Plazas, A. K. Romer, M. Sako, E. Sanchez, V. Scarpine, M. Schubnell, Matthew Smith, R. C. Smith, M. Soares-Santos, F. Sobreira, E. Suchyta, G. Tarle, D. Thomas, D. L. Tucker, A. R. Walker, W. Wester, Y. Zhang

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We construct the largest curved-sky galaxy weak lensing mass map to date from the DES first-year (DES Y1) data. The map, about 10 times larger than previous work, is constructed over a contiguous ≈1,500deg2, covering a comoving volume of ≈10Gpc3. The effects of masking, sampling, and noise are tested using simulations. We generate weak lensing maps from two DES Y1 shear catalogs, Metacalibration and Im3shape, with sources at redshift 0.2<z<1.3, and in each of four bins in this range. In the highest signal-to-noise map, the ratio between the mean signal-to-noise in the E-mode and the B-mode map is ∼1.5 (∼2) when smoothed with a Gaussian filter of σG=30 (80) arcminutes. The second and third moments of the convergence κ in the maps are in agreement with simulations. We also find no significant correlation of κ with maps of potential systematic contaminants. Finally, we demonstrate two applications of the mass maps: (1) cross-correlation with different foreground tracers of mass and (2) exploration of the largest peaks and voids in the maps.
Original languageEnglish
JournalMonthly Notices of the Royal Astronomical Society
Early online date4 Jan 2018
Publication statusEarly online - 4 Jan 2018


  • astro-ph.CO
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  • STFC


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