Dark Energy Survey Year 1 results: curved-sky weak lensing mass map
Author
Chang, CPujol, A
Mawdsley, B
Bacon, D
Elvin-Poole, J
Melchior, P
Kovács, A
Jain, B
Leistedt, B
Giannantonio, T
Alarcon, A
Baxter, E
Bechtol, K
Becker, M R
Benoit-Lévy, A
Bernstein, G M
Bonnett, C
Busha, M T
Rosell, A Carnero
Castander, F J
Cawthon, R
da Costa, L N
Davis, C
De Vicente, J
DeRose, J
Drlica-Wagner, A
Fosalba, P
Gatti, M
Gaztanaga, E
Gruen, D
Gschwend, J
Hartley, W G
Hoyle, B
Huff, E M
Jarvis, M
Jeffrey, N
Kacprzak, T
Lin, H
MacCrann, N
Maia, M A G
Ogando, R L C
Prat, J
Rau, M M
Rollins, R P
Roodman, A
Rozo, E
Rykoff, E S
Samuroff, S
Sánchez, C
Sevilla-Noarbe, I
Sheldon, E
Troxel, M A
Varga, T N
Vielzeuf, P
Vikram, V
Wechsler, R H
Zuntz, J
Abbott, T M C
Abdalla, F B
Allam, S
Annis, J
Bertin, E
Brooks, D
Buckley-Geer, E
Burke, D L
Kind, M Carrasco
Carretero, J
Crocce, M
Cunha, C E
D'Andrea, C B
Desai, S
Diehl, H T
Dietrich, J P
Doel, P
Estrada, J
Neto, A Fausti
Fernandez, E
Flaugher, B
Frieman, J
García-Bellido, J
Gruendl, R A
Gutierrez, G
Honscheid, K
James, D J
Jeltema, T
Johnson, M W G
Johnson, M D
Kent, S
Kirk, D
Krause, E
Kuehn, K
Kuhlmann, S
Lahav, O
Li, T S
Lima, M
March, M
Martini, P
Menanteau, F
Miquel, R
Mohr, J J
Neilsen, E
Nichol, R C
Petravick, D
Plazas, A A
Romer, A K
Sako, M
Sanchez, E
Scarpine, V
Schubnell, M
Smith, M
Smith, R C
Soares-Santos, M
Sobreira, F
Suchyta, E
Tarle, G
Thomas, D
Tucker, D L
Walker, A R
Wester, W
Zhang, Y
Affiliation
Univ Arizona, Dept PhysIssue Date
2018-04
Metadata
Show full item recordPublisher
OXFORD UNIV PRESSCitation
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 Castander, R 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, M 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, (DES Collaboration); Dark Energy Survey Year 1 results: curved-sky weak lensing mass map, Monthly Notices of the Royal Astronomical Society, Volume 475, Issue 3, 11 April 2018, Pages 3165–3190, https://doi.org/10.1093/mnras/stx3363Rights
© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
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 the previous work, is constructed over a contiguous approximate to 1500 deg(2), covering a comoving volume of approximate to 10 Gpc(3). The effects of masking, sampling, and noise are tested using simulations. We generate weak lensing maps from two DES Y1 shear catalogues, METACALIBRATION and IM3SHAPE, with sources at red-shift 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 map and the B-mode map is similar to 1.5 (similar to 2) when smoothed with a Gaussian filter of sigma(G) = 30 (80) arcmin. The second and third moments of the convergence kappa in the maps are in agreement with simulations. We also find no significant correlation of kappa 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.ISSN
0035-87111365-2966
Version
Final published versionSponsors
Kavli Institute for Cosmological Physics at the University of Chicago [NSF PHY-1125897]; Generalitat de Catalunya [2009-SGR-1398]; MICINN [AYA2012-39620, AYA2015-71825]; European Research Council [LENA-678282]; NASA through Einstein Postdoctoral Fellowship - Chandra X-ray Center [PF5-160138]; NASA [NAS8-03060]; NASA through Einstein Postdoctoral Fellowship Award [PF6-170154]; US Department of Energy grant [DE-SC0007901]; University of Pennsylvania; DOE grant [DE-AC02-98CH10886]; U.S. Department of Energy; U.S. National Science Foundation; Ministry of Science and Education of Spain; Science and Technology Facilities Council of the United Kingdom; Higher Education Funding Council for England; National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign; Kavli Institute of Cosmological Physics at the University of Chicago; Center for Cosmology and Astro-Particle Physics at the Ohio State University; Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University; Financiadora de Estudos e Projetos; Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico; Ministrio da Ciencia, Tecnologia e Inovacao; Deutsche Forschungsgemeinschaft; Argonne National Laboratory; University of California at Santa Cruz; University of Cambridge; Centro de Investigaciones Energrticas, Medioambientales y Tecnologicas-Madrid; University of Chicago; University College London; DES-Brazil Consortium; University of Edinburgh; Eidgenossische Technische Hochschule (ETH) Zubrich; Fermi National Accelerator Laboratory; University of Illinois at Urbana-Champaign; Institut de Ciencies de l'Espai (IEEC/CSIC); Institut de Fisica d'Altes Energies; Lawrence Berkeley National Laboratory; Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster Universe; University of Michigan; National Optical Astronomy Observatory; University of Nottingham; Ohio State University; University of Portsmouth; SLAC National Accelerator Laboratory; Stanford University; University of Sussex; Texas AM University; OzDES Membership Consortium; National Science Foundation [AST-1138766, AST-1536171]; MINECO [AYA2015-71825, ESP2015-88861, FPA2015-68048, SEV-2012-0234, SEV-2016-0597, MDM-2015-0509]; European Union; CERCA program of the Generalitat de Catalunya; ERC grant [240672, 291329, 306478]; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; U.S. Department of Energy, Office of Science, Office of High Energy Physics [DE-AC02-07CH11359]; European Research Council under the European Union's Seventh Framework Program (FP7)Additional Links
https://academic.oup.com/mnras/article/475/3/3165/4788801ae974a485f413a2113503eed53cd6c53
10.1093/mnras/stx3363