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Atacama Cosmology Telescope: a measurement of the Cosmic Microwave Background power spectra at 98 and 150 GHz

Choi, Steve K. and Hasselfield, Matthew and Ho, Shuay-Pwu Patty and Koopman, Brian and Lungu, Marius and Abitbol, Maximilian H. and Addison, Graeme E. and Ade, Peter A. R. and Aiola, Simone and Alonso, David and Amiri, Mandana and Amodeo, Stefania and Angile, Elio and Austermann, Jason E. and Baildon, Taylor and Battaglia, Nick and Beall, James A. and Bean, Rachel and Becker, Daniel T. and Bond, J. Richard and Bruno, Sarah Marie and Calabrese, Erminia and Calafut, Victoria and Campusano, Luis E. and Carrero, Felipe and Chesmore, Grace E. and Cho, Hsiao-mei and Clark, Susan E. and Cothard, Nicholas F. and Crichton, Devin and Crowley, Kevin T. and Darwish, Omar and Datta, Rahul and Denison, Edward V. and Devlin, Mark J. and Duell, Cody J. and Duff, Shannon M. and Duivenvoorden, Adriaan J. and Dunkley, Jo and Dünner, Rolando and Essinger-Hileman, Thomas and Fankhanel, Max and Ferraro, Simone and Fox, Anna E. and Fuzia, Brittany and Gallardo, Patricio A. and Gluscevic, Vera and Golec, Joseph E. and Grace, Emily and Gralla, Megan and Guan, Yilun and Hall, Kirsten and Halpern, Mark and Han, Dongwon and Hargrave, Peter and Henderson, Shawn and Hensley, Brandon and Hill, J. Colin and Hilton, Gene C. and Hilton, Matt and Hincks, Adam D. and Hložek, Renée and Hubmayr, Johannes and Huffenberger, Kevin M. and Hughes, John P. and Infante, Leopoldo and Irwin, Kent and Jackson, Rebecca and Klein, Jeff and Knowles, Kenda and Kosowsky, Arthur and Lakey, Vincent and Li, Dale and Li, Yaqiong and Li, Zack and Lokken, Martine and Louis, Thibaut and MacInnis, Amanda and Madhavacheril, Mathew and Maldonado, Felipe and Mallaby-Kay, Maya and Marsden, Danica and Maurin, Loïc and McMahon, Jeff and Menanteau, Felipe and Moodley, Kavilan and Morton, Tim and Naess, Sigurd and Namikawa, Toshiya and Nati, Federico and Newburgh, Laura and Nibarger, John P. and Nicola, Andrina and Niemack, Michael D. and Nolta, Michael R. and Orlowski-Sherer, John and Page, Lyman A. and Pappas, Christine G. and Partridge, Bruce and Phakathi, Phumlani and Prince, Heather and Puddu, Roberto and Qu, Frank J. and Rivera, Jesus and Robertson, Naomi and Rojas, Felipe and Salatino, Maria and Schaan, Emmanuel and Schillaci, Alessandro and Schmitt, Benjamin L. and Sehgal, Neelima and Sherwin, Blake D. and Sierra, Carlos and Sievers, Jon and Sifón, Cristóbal and Sikhosana, Precious and Simon, Sara and Spergel, David N. and Staggs, Suzanne T. and Stevens, Jason and Storer, Emilie and Sunder, Dhaneshwar D. and Switzer, Eric R. and Thorne, Ben and Thornton, Robert and Trac, Hy and Treu, Jesse and Tucker, Carole and Vale, Leila R. and Van Engelen, Alexander and Van Lanen, Jeff and Vavagiakis, Eve M. and Wagoner, Kasey and Wang, Yuhang and Ward, Jonathan T. and Wollack, Edward J. and Xu, Zhilei and Zago, Fernando and Zhu, Ningfeng (2020) Atacama Cosmology Telescope: a measurement of the Cosmic Microwave Background power spectra at 98 and 150 GHz. Journal of Cosmology and Astroparticle Physics, 2020 (12). Art. No 45. ISSN 1475-7516.

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We present the temperature and polarization angular power spectra of the CMB measured by the Atacama Cosmology Telescope (ACT) from 5400 deg² of the 2013–2016 survey, which covers >15000 deg² at 98 and 150 GHz. For this analysis we adopt a blinding strategy to help avoid confirmation bias and, related to this, show numerous checks for systematic error done before unblinding. Using the likelihood for the cosmological analysis we constrain secondary sources of anisotropy and foreground emission, and derive a "CMB-only" spectrum that extends to ℓ=4000. At large angular scales, foreground emission at 150 GHz is ~1% of TT and EE within our selected regions and consistent with that found by Planck. Using the same likelihood, we obtain the cosmological parameters for ΛCDM for the ACT data alone with a prior on the optical depth of τ=0.065±0.015. ΛCDM is a good fit. The best-fit model has a reduced χ² of 1.07 (PTE=0.07) with H₀=67.9±1.5 km/s/Mpc. We show that the lensing BB signal is consistent with ΛCDM and limit the celestial EB polarization angle to ψP =−0.07o±0.09o. We directly cross correlate ACT with Planck and observe generally good agreement but with some discrepancies in TE. All data on which this analysis is based will be publicly released.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Choi, Steve K.0000-0002-9113-7058
Ade, Peter A. R.0000-0002-5127-0401
Aiola, Simone0000-0002-1035-1854
Amodeo, Stefania0000-0002-4200-9965
Austermann, Jason E.0000-0002-6338-0069
Bond, J. Richard0000-0003-2358-9949
Darwish, Omar0000-0003-2946-1866
Devlin, Mark J.0000-0002-3169-9761
Duff, Shannon M.0000-0002-9693-4478
Ferraro, Simone0000-0003-4992-7854
Gallardo, Patricio A.0000-0001-9731-3617
Hall, Kirsten0000-0002-4176-845X
Halpern, Mark0000-0002-1760-0868
Hargrave, Peter0000-0002-3109-6629
Hensley, Brandon0000-0001-7449-4638
Hill, J. Colin0000-0002-9539-0835
Hilton, Gene C.0000-0003-4247-467X
Hilton, Matt0000-0002-8490-8117
Hubmayr, Johannes0000-0002-2781-9302
Huffenberger, Kevin M.0000-0001-7109-0099
Hughes, John P.0000-0002-8816-6800
Kosowsky, Arthur0000-0002-3734-331X
Madhavacheril, Mathew0000-0001-6740-5350
Moodley, Kavilan0000-0001-6606-7142
Morton, Tim0000-0002-8537-5711
Naess, Sigurd0000-0002-4478-7111
Namikawa, Toshiya0000-0003-3070-9240
Nati, Federico0000-0002-8307-5088
Niemack, Michael D.0000-0001-7125-3580
Page, Lyman A.0000-0002-9828-3525
Partridge, Bruce0000-0001-6541-9265
Salatino, Maria0000-0003-4006-1134
Schaan, Emmanuel0000-0002-4619-8927
Schillaci, Alessandro0000-0002-0512-1042
Sehgal, Neelima0000-0002-9674-4527
Sievers, Jon0000-0001-6903-5074
Sifón, Cristóbal0000-0002-8149-1352
Sikhosana, Precious0000-0003-3199-1161
Spergel, David N.0000-0002-5151-0006
Staggs, Suzanne T.0000-0002-7020-7301
Stevens, Jason0000-0002-7762-9662
Sunder, Dhaneshwar D.0000-0001-9949-1361
Switzer, Eric R.0000-0002-0457-0153
Thorne, Ben0000-0002-0457-0153
Thornton, Robert0000-0002-3180-674X
Trac, Hy0000-0001-6778-3861
Treu, Jesse0000-0001-5733-2717
Tucker, Carole0000-0002-1851-3918
Vale, Leila R.0000-0001-8561-2580
Vavagiakis, Eve M.0000-0002-2105-7589
Wang, Yuhang0000-0001-5336-5183
Wollack, Edward J.0000-0002-7567-4451
Xu, Zhilei0000-0001-5112-2567
Additional Information:© 2020 IOP Publishing Ltd and Sissa Medialab. Received 16 July 2020; Accepted 19 November 2020; Published 30 December 2020. This work was supported by 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 Astronómico Atacama in northern Chile under the auspices of the Comisión Nacional de Investigación (CONICYT). Computations were performed on the Niagara supercomputer at the SciNet HPC Consortium and on the Simons-Popeye cluster of the Flatiron Institute. 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. Cosmological analyses were performed on the Hawk high-performance computing cluster at the Advanced Research Computing at Cardiff (ARCCA). We would like to thank the Scientific Computing Core (SCC) team at the Flatiron Institute, especially Nick Carriero, for their support. Flatiron Institute is supported by the Simons Foundation. Additional computations were performed on Hippo at the University of KwaZulu-Natal, on Tiger as part of Princeton Research Computing resources at Princeton University, on Feynman at Princeton University, and on Cori at NERSC. 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. We thank Bert Harrop for his extensive efforts on the assembly of the detector arrays. The shops at Penn and Princeton have time and again built beautiful instrumentation on which ACT depends. We also thank Toby Marriage for numerous contributions. SKC acknowledges support from the Cornell Presidential Postdoctoral Fellowship. RD thanks CONICYT for grant BASAL CATA AFB-170002. ZL, ES and JD are supported through NSF grant AST-1814971. KM and MHi acknowledge support from the National Research Foundation of South Africa. MDN acknowledges support from NSF award AST-1454881. DH, AM, and NS acknowledge support from NSF grant numbers AST-1513618 and AST-1907657. EC acknowledges support from the STFC Ernest Rutherford Fellowship ST/M004856/2 and STFC Consolidated Grant ST/S00033X/1, and from the Horizon 2020 ERC Starting Grant (Grant agreement No 849169). NB acknowledges support from NSF grant AST-1910021. ML was supported by a Dicke Fellowship. LP gratefully acknowledges support from the Mishrahi and Wilkinson funds. RH acknowledges support as an Azrieli Global Scholar in CIfAR's Gravity & the Extreme Universe Program and as an Alfred. P. Sloan Research Fellow. RH is also supported by Canada's NSERC Discovery Grants program and the Dunlap Institute, which was established with an endowment by the David Dunlap family and the University of Toronto. We thank our many colleagues from ALMA, APEX, CLASS, and Polarbear/Simons Array who have helped us at critical junctures. Colleagues at AstroNorte and RadioSky provide logistical support and keep operations in Chile running smoothly. Lastly, we gratefully acknowledge the many publicly available software packages that were essential for parts of this analysis. They include CosmoMC (Lewis 2013; Lewis & Bridle 2002), CAMB (Lewis et al. 2000), healpy (Zonca et al. 2019), HEALPix (Górski et al. 2005), the SLATEC29 Fortran subroutine DRC3JJ.F9, the SOFA library (IAU SOFA Board 2019), libsharp (Reinecke & Seljebotn 2013), and pixell30. This research made use of Astropy31, 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.
Funding AgencyGrant Number
Princeton UniversityUNSPECIFIED
University of PennsylvaniaUNSPECIFIED
Canada Foundation for Innovation (CFI)UNSPECIFIED
Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)UNSPECIFIED
Flatiron InstituteUNSPECIFIED
Government of OntarioUNSPECIFIED
Ontario Research Fund-Research ExcellenceUNSPECIFIED
University of TorontoUNSPECIFIED
Simons FoundationUNSPECIFIED
National Institute of Standards and Technology (NIST)UNSPECIFIED
Cornell UniversityUNSPECIFIED
National Research Foundation (South Africa)UNSPECIFIED
Science and Technology Facilities Council (STFC)ST/M004856/2
Science and Technology Facilities Council (STFC)ST/S00033X/1
European Research Council (ERC)849169
Canadian Institute for Advanced Research (CIFAR)UNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Dunlap InstituteUNSPECIFIED
David Dunlap FamilyUNSPECIFIED
Issue or Number:12
Record Number:CaltechAUTHORS:20210212-080400390
Persistent URL:
Official Citation:Steve K. Choi et al JCAP12(2020)045
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:108029
Deposited By: Tony Diaz
Deposited On:12 Feb 2021 17:51
Last Modified:12 Feb 2021 17:51

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