Aiola, Simone and Calabrese, Erminia and Maurin, Loïc and Naess, Sigurd and Schmitt, Benjamin L. and Abitbol, Maximilian H. and Addison, Graeme E. and Ade, Peter A. R. 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 Calafut, Victoria and Campusano, Luis E. and Carrero, Felipe and Chesmore, Grace E. and Cho, Hsiao-mei and Choi, Steve K. 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 Hasselfield, Matthew and Helton, Jakob M. 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 Ho, Shuay-Pwu Patty 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 Koopman, Brian J. and Kosowsky, Arthur and Lakey, Vincent and Li, Dale and Li, Yaqiong and Li, Zack and Lokken, Martine and Louis, Thibaut and Lungu, Marius and MacInnis, Amanda and Madhavacheril, Mathew and Maldonado, Felipe and Mallaby-Kay, Maya and Marsden, Danica and McMahon, Jeff and Menanteau, Felipe and Moodley, Kavilan and Morton, Tim 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 Pisano, Giampaolo 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 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) The Atacama Cosmology Telescope: DR4 maps and cosmological parameters. Journal of Cosmology and Astroparticle Physics, 2020 (12). Art. No. 47. ISSN 1475-7516. doi:10.1088/1475-7516/2020/12/047. https://resolver.caltech.edu/CaltechAUTHORS:20210212-133817397
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Abstract
We present new arcminute-resolution maps of the Cosmic Microwave Background temperature and polarization anisotropy from the Atacama Cosmology Telescope, using data taken from 2013–2016 at 98 and 150 GHz. The maps cover more than 17,000 deg², the deepest 600 deg² with noise levels below 10μK-arcmin. We use the power spectrum derived from almost 6,000 deg² of these maps to constrain cosmology. The ACT data enable a measurement of the angular scale of features in both the divergence-like polarization and the temperature anisotropy, tracing both the velocity and density at last-scattering. From these one can derive the distance to the last-scattering surface and thus infer the local expansion rate, H₀. By combining ACT data with large-scale information from WMAP we measure H₀ = 67.6 ± 1.1 km/s/Mpc, at 68% confidence, in excellent agreement with the independently-measured Planck satellite estimate (from ACT alone we find H₀ = 67.9 ± 1.5 km/s/Mpc). The ΛCDM model provides a good fit to the ACT data, and we find no evidence for deviations: both the spatial curvature, and the departure from the standard lensing signal in the spectrum, are zero to within 1σ; the number of relativistic species, the primordial Helium fraction, and the running of the spectral index are consistent with ΛCDM predictions to within 1.5–2.2σ. We compare ACT, WMAP, and Planck at the parameter level and find good consistency; we investigate how the constraints on the correlated spectral index and baryon density parameters readjust when adding CMB large-scale information that ACT does not measure. The DR4 products presented here will be publicly released on the NASA Legacy Archive for Microwave Background Data Analysis.
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| Additional Information: | © 2020 IOP Publishing Ltd and Sissa Medialab. Received 16 July 2020. Accepted 13 November 2020. Published 30 December 2020. This work was supported by the U.S. National Science Foundation through awards AST-0408698, AST0965625, and AST-1440226 for the ACT project, as well as awards PHY-0355328, PHY-0855887 and PHY1214379. 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. 2005b), the SLATEC Fortran subroutine DRC3JJ.F9, the SOFA library (IAU SOFA Board 2019), libsharp (Reinecke & Seljebotn 2013), and pixell. This research made use of Astropy, 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. | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
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| Issue or Number: | 12 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| DOI: | 10.1088/1475-7516/2020/12/047 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Record Number: | CaltechAUTHORS:20210212-133817397 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20210212-133817397 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Official Citation: | Simone Aiola et al JCAP12(2020)047 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| ID Code: | 108047 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Collection: | CaltechAUTHORS | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited By: | George Porter | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited On: | 16 Feb 2021 15:14 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Last Modified: | 12 Jul 2022 19:48 |
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