CaltechAUTHORS
Published July 15, 2020 | Version Published + Submitted
Journal Article Open

Atacama Cosmology Telescope: Component-separated maps of CMB temperature and the thermal Sunyaev-Zel'dovich effect

Creators

  • 1. ROR icon Perimeter Institute
  • 2. ROR icon Princeton University
  • 3. ROR icon Columbia University
  • 4. ROR icon Institute for Advanced Study
  • 5. ROR icon Johns Hopkins University
  • 6. ROR icon University of Michigan–Ann Arbor
  • 7. ROR icon Cornell University
  • 8. ROR icon Canadian Institute for Theoretical Astrophysics
  • 9. ROR icon Cardiff University
  • 10. ROR icon University of Cambridge
  • 11. ROR icon University of Pennsylvania
  • 12. ROR icon Pontificia Universidad Católica de Chile
  • 13. ROR icon Lawrence Berkeley National Laboratory
  • 14. ROR icon University of Southern California
  • 15. ROR icon University of British Columbia
  • 16. ROR icon Stony Brook University
  • 17. ROR icon University of KwaZulu-Natal
  • 18. ROR icon University of Toronto
  • 19. ROR icon Florida State University
  • 20. ROR icon Rutgers, The State University of New Jersey
  • 21. ROR icon Yale University
  • 22. ROR icon University of Pittsburgh
  • 23. ROR icon University of Paris-Saclay
  • 24. ROR icon Institut d'Astrophysique Spatiale
  • 25. ROR icon University of Milano-Bicocca
  • 26. ROR icon Haverford College
  • 27. ROR icon California Institute of Technology
  • 28. ROR icon Pontificial Catholic University of Valparaiso
  • 29. ROR icon Arizona State University
  • 30. ROR icon Goddard Space Flight Center

Abstract

Optimal analyses of many signals in the cosmic microwave background (CMB) require map-level extraction of individual components in the microwave sky, rather than measurements at the power spectrum level alone. To date, nearly all map-level component separation in CMB analyses has been performed exclusively using satellite data. In this paper, we implement a component separation method based on the internal linear combination (ILC) approach which we have designed to optimally account for the anisotropic noise (in the 2D Fourier domain) often found in ground-based CMB experiments. Using this method, we combine multifrequency data from the Planck satellite and the Atacama Cosmology Telescope Polarimeter (ACTPol) to construct the first wide-area (≈2100 sq. deg.), arcminute-resolution component-separated maps of the CMB temperature anisotropy and the thermal Sunyaev-Zel'dovich (tSZ) effect sourced by the inverse-Compton scattering of CMB photons off hot, ionized gas. Our ILC pipeline allows for explicit deprojection of various contaminating signals, including a modified blackbody approximation of the cosmic infrared background (CIB) spectral energy distribution. The cleaned CMB maps will be a useful resource for CMB lensing reconstruction, kinematic SZ cross-correlations, and primordial non-Gaussianity studies. The tSZ maps will be used to study the pressure profiles of galaxies, groups, and clusters through cross-correlations with halo catalogs, with dust contamination controlled via CIB deprojection. The data products described in this paper are available on LAMBDA.

Additional Information

© 2020 American Physical Society. Received 5 December 2019; accepted 17 June 2020; published 22 July 2020. We are grateful to Hans Kristian Eriksen, Reijo Keskitalo, and Mathieu Remazeilles for informative discussions related to Planck products and analysis. Some of the results in this paper have been derived using the healpy [126] and healpix [127] packages. This research made use of Astropy,8 a community-developed core python package for Astronomy [128,129]. We also acknowledge use of the matplotlib [130] package and the Python Image Library for producing plots in this paper, and use of the Boltzmann code camb [97] for calculating theory spectra. This work was supported by the U.S. National Science Foundation through Grants No. AST-1440226, No. AST0965625 and No. AST-0408698 for the ACT project, as well as Grants No. PHY-1214379 and No. PHY-0855887. Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque Astronómico Atacama in northern Chile under the auspices of the Comisión Nacional de Investigación Científica y Tecnológica de Chile (CONICYT). Computations were performed on the GPC and Niagara supercomputers at the SciNet HPC Consortium. SciNet is funded by the CFI under the auspices of Compute Canada, the Government of Ontario, the Ontario Research Fund—Research Excellence; and the University of Toronto. The development of multichroic detectors and lenses was supported by NASA Grants No. NNX13AE56G and No. NNX14AB58G. Colleagues at AstroNorte and RadioSky provide logistical support and keep operations in Chile running smoothly. We also thank the Mishrahi Fund and the Wilkinson Fund for their generous support of the project. M. S. M. acknowledges support from NSF Grant No. AST-1814971. J. C. H. acknowledges support from the Simons Foundation and the W. M. Keck Foundation Fund at the Institute for Advanced Study. Flatiron Institute is supported by the Simons Foundation. R. B. and V. C. acknowledge DoE Grant No. DE-SC0011838, NASA ATP grants No. NNX14AH53G and No. 80NSSC18K0695, NASA ROSES grant No. 12-EUCLID12-0004 and funding related to the WFIRST Science Investigation Team. E. C. is supported by a STFC Ernest Rutherford Fellowship ST/M004856/2. S. K. C. acknowledges support from the Cornell Presidential Postdoctoral Fellowship. R. D. thanks CONICYT for Grant No. BASAL CATA AFB-170002. M. H. acknowledges funding support from the National Research Foundation, the South African Radio Astronomy Observatory, and the University of KwaZulu-Natal. L. M. received funding from CONICYT FONDECYT Grant No. 3170846. K. M. acknowledges support from the National Research Foundation of South Africa. N. S. acknowledges support from NSF Grant No. 1513618.

Attached Files

Published - PhysRevD.102.023534.pdf

Submitted - 1911.05717.pdf

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1911.05717.pdf

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Additional details

Identifiers

Eprint ID
104512
Resolver ID
CaltechAUTHORS:20200722-123057402

Related works

Describes
https://arxiv.org/abs/1911.05717 (URL)

Funding

NSF
AST-1440226
NSF
AST-0965625
NSF
AST-0408698
NSF
PHY-1214379
NSF
PHY-0855887
Princeton University
University of Pennsylvania
Canada Foundation for Innovation
Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)
Compute Canada
Government of Ontario
Ontario Research Fund-Research Excellence
University of Toronto
NASA
NNX13AE56G
NASA
NNX14AB58G
Mishrahi Fund
Wilkinson Fund
NSF
AST-1814971
Simons Foundation
W. M. Keck Foundation
Flatiron Institute
Simons Foundation
Department of Energy (DOE)
DE-SC0011838
NASA
NNX14AH53G
NASA
80NSSC18K0695
NASA
12-EUCLID12-0004
Science and Technology Facilities Council (STFC)
ST/M004856/2
Cornell University
BASAL-CATA
AFB-170002
National Research Foundation (South Africa)
South African Radio Astronomy Observatory (SARAO)
University of KwaZulu-Natal
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)
3170846
NSF
AST-1513618

Dates

Created
2020-07-22
Created from EPrint's datestamp field
Updated
2021-11-16
Created from EPrint's last_modified field