Abstract
Optical imaging surveys measure both the galaxy density and the gravitational lensing-induced shear fields across the sky. Recently, the Dark Energy Survey (DES) Collaboration used a joint fit to two-point correlations between these observables to place tight constraints on cosmology (T. M. C. Abbott (Dark Energy Survey Collaboration), Phys. Rev. D 98, 043526 (2018)PRVDAQ2470-001010.1103/PhysRevD.98.043526). In this work, we develop the methodology to extend the DES Year 1 joint probes analysis to include cross-correlations of the optical survey observables with gravitational lensing of the cosmic microwave background as measured by the South Pole Telescope (SPT) and Planck. Using simulated analyses, we show how the resulting set of five two-point functions increases the robustness of the cosmological constraints to systematic errors in galaxy lensing shear calibration. Additionally, we show that contamination of the SPT+Planck cosmic microwave background lensing map by the thermal Sunyaev-Zel'dovich effect is a potentially large source of systematic error for two-point function analyses but show that it can be reduced to acceptable levels in our analysis by masking clusters of galaxies and imposing angular scale cuts on the two-point functions. The methodology developed here will be applied to the analysis of data from the DES, the SPT, and Planck in a companion work.
| Original language | English (US) |
|---|---|
| Article number | 023508 |
| Journal | Physical Review D |
| Volume | 99 |
| Issue number | 2 |
| DOIs | |
| State | Published - Jan 15 2019 |
All Science Journal Classification (ASJC) codes
- Nuclear and High Energy Physics
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In: Physical Review D, Vol. 99, No. 2, 023508, 15.01.2019.
Research output: Contribution to journal › Article › peer-review
TY - JOUR
T1 - Dark Energy Survey Year 1 results
T2 - Methodology and projections for joint analysis of galaxy clustering, galaxy lensing, and CMB lensing two-point functions
AU - Baxter, E. J.
AU - Omori, Y.
AU - Chang, C.
AU - Giannantonio, T.
AU - Kirk, D.
AU - Krause, E.
AU - Blazek, J.
AU - Bleem, L.
AU - Choi, A.
AU - Crawford, T. M.
AU - Dodelson, S.
AU - Eifler, T. F.
AU - Friedrich, O.
AU - Gruen, D.
AU - Holder, G. P.
AU - Jain, B.
AU - Jarvis, M.
AU - Maccrann, N.
AU - Nicola, A.
AU - Pandey, S.
AU - Prat, J.
AU - Reichardt, C. L.
AU - Samuroff, S.
AU - Sánchez, C.
AU - Secco, L. F.
AU - Sheldon, E.
AU - Troxel, M. A.
AU - Zuntz, J.
AU - Abbott, T. M.C.
AU - Abdalla, F. B.
AU - Annis, J.
AU - Avila, S.
AU - Bechtol, K.
AU - Benson, B. A.
AU - Bertin, E.
AU - Brooks, D.
AU - Buckley-Geer, E.
AU - Burke, D. L.
AU - Carnero Rosell, A.
AU - Carrasco Kind, M.
AU - Carretero, J.
AU - Castander, F. J.
AU - Cawthon, R.
AU - Cunha, C. E.
AU - D'Andrea, C. B.
AU - Da Costa, L. N.
AU - Davis, C.
AU - De Vicente, J.
AU - Depoy, D. L.
AU - Diehl, H. T.
AU - Doel, P.
AU - Estrada, J.
AU - Evrard, A. E.
AU - Flaugher, B.
AU - Fosalba, P.
AU - Frieman, J.
AU - García-Bellido, J.
AU - Gaztanaga, E.
AU - Gerdes, D. W.
AU - Gruendl, R. A.
AU - Gschwend, J.
AU - Gutierrez, G.
AU - Hartley, W. G.
AU - Hollowood, D.
AU - Hoyle, B.
AU - James, D. J.
AU - Kent, S.
AU - Kuehn, K.
AU - Kuropatkin, N.
AU - Lahav, O.
AU - Lima, M.
AU - Maia, M. A.G.
AU - March, M.
AU - Marshall, J. L.
AU - Melchior, P.
AU - Menanteau, F.
AU - Miquel, R.
AU - Plazas, A. A.
AU - Roodman, A.
AU - Rykoff, E. S.
AU - Sanchez, E.
AU - Schindler, R.
AU - Schubnell, M.
AU - Sevilla-Noarbe, I.
AU - Smith, M.
AU - Smith, R. C.
AU - Soares-Santos, M.
AU - Sobreira, F.
AU - Suchyta, E.
AU - Swanson, M. E.C.
AU - Tarle, G.
AU - Walker, A. R.
AU - Wu, W. L.K.
AU - Weller, J.
N1 - Funding Information: Given the large degradation in the signal-to-noise ratio that results from cutting scales affected by tSZ contamination, future work to model or remove such contamination is strongly motivated. More accurate estimates of the contamination could be achieved with a high signal-to-noise ratio and high resolution Compton- maps. Alternatively, such contamination could be removed from the maps either using multifrequency component separation methods to remove tSZ from the CMB temperature maps or by constructing the maps instead from maps of the CMB polarization, since the tSZ signal is nearly unpolarized. ACKNOWLEDGMENTS . E. B. is partially supported by the U.S. Department of Energy Grant No. DE-SC0007901. The Reichardt and Bianchini acknowledge support from the Australian Research Council’s Future Fellowships scheme (Grant No. FT150100074). P. F. is funded by MINECO, Projects No. ESP2013-48274-C3-1-P, No. ESP2014-58384-C3-1-P, and No. ESP2015-66861-C3-1-R. E. R. is supported by DOE Grant No. DE-SC0015975 and by the Sloan Foundation, Grant No. FG- 2016-6443. Support for D. G. was provided by NASA through Einstein Postdoctoral Fellowship Grant No. PF5-160138 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under Contract No. NAS8-03060. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the collaborating institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai, the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. This work is based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under Grants No. AYA2015-71825, No. ESP2015-88861, No. FPA2015-68048, No. SEV-2012-0234, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. Institut de Física d’Altes Energies is partially funded by the Centres de Recerca de Catalunya program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (Grant No. FP7/2007-2013) including ERC Grants No. 240672, No. 291329, and No. 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics, through Project No. CE110001020. The South Pole Telescope program is supported by the National Science Foundation through Grant No. PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center Grant No. PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation through Grant No. 947 to the University of Chicago. Argonne National Laboratory’s work was supported under the U.S. Department of Energy Contract No. DE-AC02- 06CH11357. This manuscript has been authored by Fermi Research Alliance, LLC, under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a nonexclusive, paid-up, irrevocable, worldwide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. Publisher Copyright: © 2019 American Physical Society.
PY - 2019/1/15
Y1 - 2019/1/15
N2 - Optical imaging surveys measure both the galaxy density and the gravitational lensing-induced shear fields across the sky. Recently, the Dark Energy Survey (DES) Collaboration used a joint fit to two-point correlations between these observables to place tight constraints on cosmology (T. M. C. Abbott (Dark Energy Survey Collaboration), Phys. Rev. D 98, 043526 (2018)PRVDAQ2470-001010.1103/PhysRevD.98.043526). In this work, we develop the methodology to extend the DES Year 1 joint probes analysis to include cross-correlations of the optical survey observables with gravitational lensing of the cosmic microwave background as measured by the South Pole Telescope (SPT) and Planck. Using simulated analyses, we show how the resulting set of five two-point functions increases the robustness of the cosmological constraints to systematic errors in galaxy lensing shear calibration. Additionally, we show that contamination of the SPT+Planck cosmic microwave background lensing map by the thermal Sunyaev-Zel'dovich effect is a potentially large source of systematic error for two-point function analyses but show that it can be reduced to acceptable levels in our analysis by masking clusters of galaxies and imposing angular scale cuts on the two-point functions. The methodology developed here will be applied to the analysis of data from the DES, the SPT, and Planck in a companion work.
AB - Optical imaging surveys measure both the galaxy density and the gravitational lensing-induced shear fields across the sky. Recently, the Dark Energy Survey (DES) Collaboration used a joint fit to two-point correlations between these observables to place tight constraints on cosmology (T. M. C. Abbott (Dark Energy Survey Collaboration), Phys. Rev. D 98, 043526 (2018)PRVDAQ2470-001010.1103/PhysRevD.98.043526). In this work, we develop the methodology to extend the DES Year 1 joint probes analysis to include cross-correlations of the optical survey observables with gravitational lensing of the cosmic microwave background as measured by the South Pole Telescope (SPT) and Planck. Using simulated analyses, we show how the resulting set of five two-point functions increases the robustness of the cosmological constraints to systematic errors in galaxy lensing shear calibration. Additionally, we show that contamination of the SPT+Planck cosmic microwave background lensing map by the thermal Sunyaev-Zel'dovich effect is a potentially large source of systematic error for two-point function analyses but show that it can be reduced to acceptable levels in our analysis by masking clusters of galaxies and imposing angular scale cuts on the two-point functions. The methodology developed here will be applied to the analysis of data from the DES, the SPT, and Planck in a companion work.
UR - http://www.scopus.com/inward/record.url?scp=85060853236&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85060853236&partnerID=8YFLogxK
U2 - 10.1103/PhysRevD.99.023508
DO - 10.1103/PhysRevD.99.023508
M3 - Article
AN - SCOPUS:85060853236
SN - 2470-0010
VL - 99
JO - Physical Review D
JF - Physical Review D
IS - 2
M1 - 023508
ER -