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

Madhavacheril, Mathew S. and Hill, J. Colin and Næss, Sigurd and Addison, Graeme E. and Aiola, Simone and Baildon, Taylor and Battaglia, Nicholas and Bean, Rachel and Bond, J. Richard and Calabrese, Erminia and Calafut, Victoria and Choi, Steve K. and Darwish, Omar and Datta, Rahul and Devlin, Mark J. and Dunkley, Joanna and Dünner, Rolando and Ferraro, Simone and Gallardo, Patricio A. and Gluscevic, Vera and Halpern, Mark and Han, Dongwon and Hasselfield, Matthew and Hilton, Matt and Hincks, Adam D. and Hložek, Renée and Ho, Shuay-Pwu Patty and Huffenberger, Kevin M. and Hughes, John P. and Koopman, Brian J. and Kosowsky, Arthur and Lokken, Martine and Louis, Thibaut and Lungu, Marius and MacInnis, Amanda and Maurin, Loïc and McMahon, Jeffrey J. and Moodley, Kavilan and Nati, Federico and Niemack, Michael D. and Page, Lyman A. and Partridge, Bruce and Robertson, Naomi and Sehgal, Neelima and Schaan, Emmanuel and Schillaci, Alessandro and Sherwin, Blake D. and Sifón, Cristóbal and Simon, Sara M. and Spergel, David N. and Staggs, Suzanne T. and Storer, Emilie R. and van Engelen, Alexander and Vavagiakis, Eve M. and Wollack, Edward J. and Xu, Zhilei (2020) Atacama Cosmology Telescope: Component-separated maps of CMB temperature and the thermal Sunyaev-Zel’dovich effect. Physical Review D, 102 (2). Art. No. 023534. ISSN 2470-0010. https://resolver.caltech.edu/CaltechAUTHORS:20200722-123057402

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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.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1103/physrevd.102.023534DOIArticle
https://arxiv.org/abs/1911.05717arXivDiscussion Paper
ORCID:
AuthorORCID
Madhavacheril, Mathew S.0000-0001-6740-5350
Bond, J. Richard0000-0003-2358-9949
Halpern, Mark0000-0002-1760-0868
Huffenberger, Kevin M.0000-0001-7109-0099
Page, Lyman A.0000-0002-9828-3525
Sifón, Cristóbal0000-0002-8149-1352
Spergel, David N.0000-0002-5151-0006
Wollack, Edward J.0000-0002-7567-4451
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.
Funders:
Funding AgencyGrant Number
NSFAST-1440226
NSFAST-0965625
NSFAST-0408698
NSFPHY-1214379
NSFPHY-0855887
Princeton UniversityUNSPECIFIED
University of PennsylvaniaUNSPECIFIED
Canada Foundation for InnovationUNSPECIFIED
Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)UNSPECIFIED
Compute CanadaUNSPECIFIED
Government of OntarioUNSPECIFIED
Ontario Research Fund-Research ExcellenceUNSPECIFIED
University of TorontoUNSPECIFIED
NASANNX13AE56G
NASANNX14AB58G
Mishrahi FundUNSPECIFIED
Wilkinson FundUNSPECIFIED
NSFAST-1814971
Simons FoundationUNSPECIFIED
W. M. Keck FoundationUNSPECIFIED
Flatiron InstituteUNSPECIFIED
Simons FoundationUNSPECIFIED
Department of Energy (DOE)DE-SC0011838
NASANNX14AH53G
NASA80NSSC18K0695
NASA12-EUCLID12-0004
Science and Technology Facilities Council (STFC)ST/M004856/2
Cornell UniversityUNSPECIFIED
BASAL-CATAAFB-170002
National Research Foundation (South Africa)UNSPECIFIED
South African Radio Astronomy Observatory (SARAO)UNSPECIFIED
University of KwaZulu-NatalUNSPECIFIED
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)3170846
NSFAST-1513618
Issue or Number:2
Record Number:CaltechAUTHORS:20200722-123057402
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20200722-123057402
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:104512
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:22 Jul 2020 21:05
Last Modified:22 Jul 2020 21:05

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