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The Atacama Cosmology Telescope: measurement and analysis of 1D beams for DR4

Lungu, Marius and Storer, Emilie R. and Hasselfield, Matthew and Duivenvoorden, Adriaan J. and Calabrese, Erminia and Chesmore, Grace E. and Choi, Steve K. and Dunkley, Jo and Dünner, Rolando and Gallardo, Patricio A. and Golec, Joseph E. and Guan, Yilun and Hill, J. Colin and Hincks, Adam D. and Hubmayr, Johannes and Madhavacheril, Mathew S. and Mallaby-Kay, Maya and McMahon, Jeff and Moodley, Kavilan and Naess, Sigurd and Nati, Federico and Niemack, Michael D. and Page, Lyman A. and Partridge, Bruce and Puddu, Roberto and Schillaci, Alessandro and Sifón, Cristóbal and Staggs, Suzanne and Sunder, Dhaneshwar D. and Wollack, Edward J. and Xu, Zhilei (2022) The Atacama Cosmology Telescope: measurement and analysis of 1D beams for DR4. Journal of Cosmology and Astroparticle Physics, 2022 (5). Art. No. 044. ISSN 1475-7516. doi:10.1088/1475-7516/2022/05/044. https://resolver.caltech.edu/CaltechAUTHORS:20220708-681479700

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Abstract

We describe the measurement and treatment of the telescope beams for the Atacama Cosmology Telescope's fourth data release, DR4. Observations of Uranus are used to measure the central portion (<12') of the beams to roughly -40 dB of the peak. Such planet maps in intensity are used to construct azimuthally averaged beam profiles, which are fit with a physically motivated model before being transformed into Fourier space. We investigate and quantify a number of percent-level corrections to the beams, all of which are important for precision cosmology. Uranus maps in polarization are used to measure the temperature-to-polarization leakage in the main part of the beams, which is ≲ 1% (2.5%) at 150 GHz (98 GHz). The beams also have polarized sidelobes, which are measured with observations of Saturn and deprojected from the ACT time-ordered data. Notable changes relative to past ACT beam analyses include an improved subtraction of the atmospheric effects from Uranus calibration maps, incorporation of a scattering term in the beam profile model, and refinements to the beam model uncertainties and the main temperature-to-polarization leakage terms in the ACT power spectrum analysis.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1088/1475-7516/2022/05/044DOIArticle
https://arxiv.org/abs/2112.12226arXivDiscussion Paper
ORCID:
AuthorORCID
Storer, Emilie R.0000-0003-1592-9659
Hasselfield, Matthew0000-0002-2408-9201
Duivenvoorden, Adriaan J.0000-0003-2856-2382
Calabrese, Erminia0000-0003-0837-0068
Chesmore, Grace E.0000-0001-6702-0450
Choi, Steve K.0000-0002-9113-7058
Dunkley, Jo0000-0002-7450-2586
Dünner, Rolando0000-0003-3892-1860
Gallardo, Patricio A.0000-0001-9731-3617
Golec, Joseph E.0000-0002-4421-0267
Guan, Yilun0000-0002-1697-3080
Hill, J. Colin0000-0002-9539-0835
Hincks, Adam D.0000-0003-1690-6678
Hubmayr, Johannes0000-0002-2781-9302
Madhavacheril, Mathew S.0000-0001-6740-5350
Mallaby-Kay, Maya0000-0002-2018-3807
McMahon, Jeff0000-0002-7245-4541
Moodley, Kavilan0000-0001-6606-7142
Naess, Sigurd0000-0002-4478-7111
Nati, Federico0000-0002-8307-5088
Niemack, Michael D.0000-0001-7125-3580
Page, Lyman A.0000-0002-9828-3525
Partridge, Bruce0000-0001-6541-9265
Schillaci, Alessandro0000-0002-0512-1042
Sifón, Cristóbal0000-0002-8149-1352
Staggs, Suzanne0000-0002-7020-7301
Sunder, Dhaneshwar D.0000-0001-9949-1361
Wollack, Edward J.0000-0002-7567-4451
Xu, Zhilei0000-0001-5112-2567
Additional Information:© 2022 IOP Publishing Ltd and Sissa Medialab. Received 26 December 2021; Accepted 17 March 2022; Published 26 May 2022. Support for ACT was through the U.S. National Science Foundation through awards AST-0408698, AST-0965625, and AST-1440226 for the ACT project, as well as awards PHY-0355328, PHY-0855887 and PHY-1214379. 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 Astronomico Atacama in northern Chile under the auspices of the Agencia Nacional de Investigacion y Desarrollo (ANID). The development of multichroic detectors and lenses was supported by NASA grants NNX13AE56G and NNX14AB58G. Detector research at NIST was supported by the NIST Innovations in Measurement Science program. Computations were performed on Tiger and Della as part of Princeton Research Computing resources at Princeton University, on Feynman at Princeton University, and on the Niagara supercomputer 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. Research at Perimeter Institute is supported in part by the Government of Canada through the Department of Innovation, Science and Industry Canada and by the Province of Ontario through the Ministry of Colleges and Universities. ML was supported by a Dicke Fellowship. ES and JD are supported through NSF grant AST-1814971 and AST-2108126. EC acknowledges support from the STFC Ernest Rutherford Fellowship ST/M004856/2, STFC Consolidated Grant ST/S00033X/ and from the Horizon 2020 ERC Starting Grant (Grant agreement No 849169). SKC acknowledges support from NSF award AST-2001866. JCH acknowledges support from NSF grant AST-2108536. ADH acknowledges support from the Sutton Family Chair in Science, Christianity and Cultures and from the Faculty of Arts and Science, University of Toronto. KM acknowledges support from the National Research Foundation of South Africa. LP gratefully acknowledges support from the Mishrahi and Wilkinson funds. ZX is supported by the Gordon and Betty Moore Foundation through grant GBMF5215 to the Massachusetts Institute of Technology. We gratefully acknowledge the publicly available software packages that were used for parts of this analysis. They include healpy (Zonca et al. 2019), HEALPix (Goorski et al. 2005b), libsharp (Reinecke & Seljebotn 2013), and pixell34. This research made use of Astropy35, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013; Price-Whelan et al. 2018). We also acknowledge use of the matplotlib (Hunter 2007) package and the Python Image Library for producing plots in this paper.
Funders:
Funding AgencyGrant Number
NSFAST-0408698
NSFAST-0965625
NSFAST-1440226
NSFPHY-0355328
NSFPHY-0855887
NSFPHY-1214379
Princeton UniversityUNSPECIFIED
University of PennsylvaniaUNSPECIFIED
Canada Foundation for InnovationUNSPECIFIED
Agencia Nacional de Investigación y Desarrollo (ANID)UNSPECIFIED
NASANNX13AE56G
NASANNX14AB58G
National Institute of Standards and Technology (NIST)UNSPECIFIED
Compute CanadaUNSPECIFIED
Ontario Research Fund-Research ExcellenceUNSPECIFIED
University of TorontoUNSPECIFIED
Department of Innovation, Science and Industry (Canada)UNSPECIFIED
Ontario Ministry of Colleges and UniversitiesUNSPECIFIED
NSFAST-1814971
NSFAST-2108126
Science and Technology Facilities Council (STFC)ST/M004856/2
Science and Technology Facilities Council (STFC)ST/S00033X/1
European Research Council (ERC)849169
NSFAST-2001866
NSFAST-2108536
National Research Foundation (South Africa)UNSPECIFIED
Mishrahi FundUNSPECIFIED
Wilkinson FundUNSPECIFIED
Gordon and Betty Moore FoundationGBMF5215
Issue or Number:5
DOI:10.1088/1475-7516/2022/05/044
Record Number:CaltechAUTHORS:20220708-681479700
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20220708-681479700
Official Citation:Marius Lungu et al JCAP05(2022)044
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:115445
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:11 Jul 2022 17:35
Last Modified:11 Jul 2022 17:35

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