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Title: Monte Carlo control loops for cosmic shear cosmology with DES Year 1 data

Abstract

Weak lensing by large-scale structure is a powerful probe of cosmology and of the dark universe. This cosmic shear technique relies on the accurate measurement of the shapes and redshifts of background galaxies and requires precise control of systematic errors. Monte Carlo control loops (MCCL) is a forward modeling method designed to tackle this problem. It relies on the ultra fast image generator (UFig) to produce simulated images tuned to match the target data statistically, followed by calibrations and tolerance loops. Here, we present the first end-to-end application of this method, on the Dark Energy Survey (DES) Year 1 wide field imaging data. We simultaneously measure the shear power spectrum $$C_ℓ$$ and the redshift distribution $n(z)$ of the background galaxy sample. The method includes maps of the systematic sources, point spread function (PSF), an approximate Bayesian computation (ABC) inference of the simulation model parameters, a shear calibration scheme, and a fast method to estimate the covariance matrix. We find a close statistical agreement between the simulations and the DES Y1 data using an array of diagnostics. In a nontomographic setting, we derive a set of $$C_ℓ$$ and $n(z)$ curves that encode the cosmic shear measurement, as well as the systematic uncertainty. Following a blinding scheme, we measure the combination of $$Ω_m$$, $$σ_8$$, and intrinsic alignment amplitude $$A_{IA}$$, defined as $$S_8D_{IA}=σ_8(Ω_m/0.3)^{0.5}D_{IA}$$, where $$D_{IA}=1-0.11(A_{IA}-1)$$. We find $$S_8D_{IA}=0.8954_{-0.039}^{+0.054}$$, where systematics are at the level of roughly 60% of the statistical errors. We discuss these results in the context of earlier cosmic shear analyses of the DES Y1 data. Our findings indicate that this method and its fast runtime offer good prospects for cosmic shear measurements with future wide-field surveys.

Authors:
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Publication Date:
Research Org.:
SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States); Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States)
Sponsoring Org.:
USDOE Office of Science (SC), High Energy Physics (HEP); Swiss National Science Foundation (SNSF), National Science Foundation (NSF); Ministry of Science and Education of Spain; Science and Technology Facilities Council (STFC) (United Kingdom); European Union (EU)
Contributing Org.:
The DES Collaboration; DES Collaboration
OSTI Identifier:
1633431
Alternate Identifier(s):
OSTI ID: 1661217
Grant/Contract Number:  
AC02-76SF00515; 200021_169130; AST-1138766; AST-1536171; 465376/2014-2; AYA2015-71825; ESP2015-66861; FPA2015-68048; SEV-2016-0588; SEV-2016-0597; MDM-2015-0509; FP7/2007-2013; 240672; 291329; 306478; AC02-07CH11359; AC05-00OR22725
Resource Type:
Accepted Manuscript
Journal Name:
Physical Review. D.
Additional Journal Information:
Journal Volume: 101; Journal Issue: 8; Journal ID: ISSN 2470-0010
Publisher:
American Physical Society (APS)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; Cosmological parameters; Large scale structure of the Universe; Astrophysical & cosmological simulations

Citation Formats

Kacprzak, T., Herbel, J., Nicola, A., Sgier, R., Tarsitano, F., Bruderer, C., Amara, A., Refregier, A., Bridle, S. L., Drlica-Wagner, A., Gruen, D., Hartley, W. G., Hoyle, B., Secco, L. F., Zuntz, J., Annis, J., Avila, S., Bertin, E., Brooks, D., Buckley-Geer, E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., García-Bellido, J., Gaztanaga, E., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Jarvis, M., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Vikram, V., and Weller, J. Monte Carlo control loops for cosmic shear cosmology with DES Year 1 data. United States: N. p., 2020. Web. doi:10.1103/physrevd.101.082003.
Kacprzak, T., Herbel, J., Nicola, A., Sgier, R., Tarsitano, F., Bruderer, C., Amara, A., Refregier, A., Bridle, S. L., Drlica-Wagner, A., Gruen, D., Hartley, W. G., Hoyle, B., Secco, L. F., Zuntz, J., Annis, J., Avila, S., Bertin, E., Brooks, D., Buckley-Geer, E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., García-Bellido, J., Gaztanaga, E., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Jarvis, M., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Vikram, V., & Weller, J. Monte Carlo control loops for cosmic shear cosmology with DES Year 1 data. United States. https://doi.org/10.1103/physrevd.101.082003
Kacprzak, T., Herbel, J., Nicola, A., Sgier, R., Tarsitano, F., Bruderer, C., Amara, A., Refregier, A., Bridle, S. L., Drlica-Wagner, A., Gruen, D., Hartley, W. G., Hoyle, B., Secco, L. F., Zuntz, J., Annis, J., Avila, S., Bertin, E., Brooks, D., Buckley-Geer, E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., da Costa, L. N., De Vicente, J., Desai, S., Diehl, H. T., Doel, P., García-Bellido, J., Gaztanaga, E., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Jarvis, M., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Vikram, V., and Weller, J. Mon . "Monte Carlo control loops for cosmic shear cosmology with DES Year 1 data". United States. https://doi.org/10.1103/physrevd.101.082003. https://www.osti.gov/servlets/purl/1633431.
@article{osti_1633431,
title = {Monte Carlo control loops for cosmic shear cosmology with DES Year 1 data},
author = {Kacprzak, T. and Herbel, J. and Nicola, A. and Sgier, R. and Tarsitano, F. and Bruderer, C. and Amara, A. and Refregier, A. and Bridle, S. L. and Drlica-Wagner, A. and Gruen, D. and Hartley, W. G. and Hoyle, B. and Secco, L. F. and Zuntz, J. and Annis, J. and Avila, S. and Bertin, E. and Brooks, D. and Buckley-Geer, E. and Carnero Rosell, A. and Carrasco Kind, M. and Carretero, J. and da Costa, L. N. and De Vicente, J. and Desai, S. and Diehl, H. T. and Doel, P. and García-Bellido, J. and Gaztanaga, E. and Gruendl, R. A. and Gschwend, J. and Gutierrez, G. and Hollowood, D. L. and Honscheid, K. and James, D. J. and Jarvis, M. and Lima, M. and Maia, M. A. G. and Marshall, J. L. and Melchior, P. and Menanteau, F. and Miquel, R. and Paz-Chinchón, F. and Plazas, A. A. and Sanchez, E. and Scarpine, V. and Serrano, S. and Sevilla-Noarbe, I. and Smith, M. and Suchyta, E. and Swanson, M. E. C. and Tarle, G. and Vikram, V. and Weller, J.},
abstractNote = {Weak lensing by large-scale structure is a powerful probe of cosmology and of the dark universe. This cosmic shear technique relies on the accurate measurement of the shapes and redshifts of background galaxies and requires precise control of systematic errors. Monte Carlo control loops (MCCL) is a forward modeling method designed to tackle this problem. It relies on the ultra fast image generator (UFig) to produce simulated images tuned to match the target data statistically, followed by calibrations and tolerance loops. Here, we present the first end-to-end application of this method, on the Dark Energy Survey (DES) Year 1 wide field imaging data. We simultaneously measure the shear power spectrum $C_ℓ$ and the redshift distribution $n(z)$ of the background galaxy sample. The method includes maps of the systematic sources, point spread function (PSF), an approximate Bayesian computation (ABC) inference of the simulation model parameters, a shear calibration scheme, and a fast method to estimate the covariance matrix. We find a close statistical agreement between the simulations and the DES Y1 data using an array of diagnostics. In a nontomographic setting, we derive a set of $C_ℓ$ and $n(z)$ curves that encode the cosmic shear measurement, as well as the systematic uncertainty. Following a blinding scheme, we measure the combination of $Ω_m$, $σ_8$, and intrinsic alignment amplitude $A_{IA}$, defined as $S_8D_{IA}=σ_8(Ω_m/0.3)^{0.5}D_{IA}$, where $D_{IA}=1-0.11(A_{IA}-1)$. We find $S_8D_{IA}=0.8954_{-0.039}^{+0.054}$, where systematics are at the level of roughly 60% of the statistical errors. We discuss these results in the context of earlier cosmic shear analyses of the DES Y1 data. Our findings indicate that this method and its fast runtime offer good prospects for cosmic shear measurements with future wide-field surveys.},
doi = {10.1103/physrevd.101.082003},
journal = {Physical Review. D.},
number = 8,
volume = 101,
place = {United States},
year = {Mon Apr 27 00:00:00 EDT 2020},
month = {Mon Apr 27 00:00:00 EDT 2020}
}

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