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.
Original language | English (US) |
---|---|
Article number | 047 |
Journal | Journal of Cosmology and Astroparticle Physics |
Volume | 2020 |
Issue number | 12 |
DOIs | |
State | Published - Dec 2020 |
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
Keywords
- CMBR experiments
- CMBR polarisation
- Cosmological parameters from CMBR
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In: Journal of Cosmology and Astroparticle Physics, Vol. 2020, No. 12, 047, 12.2020.
Research output: Contribution to journal › Article › peer-review
TY - JOUR
T1 - The Atacama Cosmology Telescope
T2 - DR4 maps and cosmological parameters
AU - Aiola, Simone
AU - Calabrese, Erminia
AU - Maurin, Loïc
AU - Naess, Sigurd
AU - Schmitt, Benjamin L.
AU - Abitbol, Maximilian H.
AU - Addison, Graeme E.
AU - Ade, Peter A.R.
AU - Alonso, David
AU - Amiri, Mandana
AU - Amodeo, Stefania
AU - Angile, Elio
AU - Austermann, Jason E.
AU - Baildon, Taylor
AU - Battaglia, Nick
AU - Beall, James A.
AU - Bean, Rachel
AU - Becker, Daniel T.
AU - Richard Bond, J.
AU - Bruno, Sarah Marie
AU - Calafut, Victoria
AU - Campusano, Luis E.
AU - Carrero, Felipe
AU - Chesmore, Grace E.
AU - Cho, Hsiao Mei
AU - Choi, Steve K.
AU - Clark, Susan E.
AU - Cothard, Nicholas F.
AU - Crichton, Devin
AU - Crowley, Kevin T.
AU - Darwish, Omar
AU - Datta, Rahul
AU - Denison, Edward V.
AU - Devlin, Mark J.
AU - Duell, Cody J.
AU - Duff, Shannon M.
AU - Duivenvoorden, Adriaan J.
AU - Dunkley, Jo
AU - Dünner, Rolando
AU - Essinger-Hileman, Thomas
AU - Fankhanel, Max
AU - Ferraro, Simone
AU - Fox, Anna E.
AU - Fuzia, Brittany
AU - Gallardo, Patricio A.
AU - Gluscevic, Vera
AU - Golec, Joseph E.
AU - Grace, Emily
AU - Gralla, Megan
AU - Guan, Yilun
AU - Hall, Kirsten
AU - Halpern, Mark
AU - Han, Dongwon
AU - Hargrave, Peter
AU - Hasselfield, Matthew
AU - Helton, Jakob M.
AU - Henderson, Shawn
AU - Hensley, Brandon
AU - Colin Hill, J.
AU - Hilton, Gene C.
AU - Hilton, Matt
AU - Hincks, Adam D.
AU - Hložek, Renée
AU - Ho, Shuay Pwu Patty
AU - Hubmayr, Johannes
AU - Huffenberger, Kevin M.
AU - Hughes, John P.
AU - Infante, Leopoldo
AU - Irwin, Kent
AU - Jackson, Rebecca
AU - Klein, Jeff
AU - Knowles, Kenda
AU - Koopman, Brian
AU - Kosowsky, Arthur
AU - Lakey, Vincent
AU - Li, Dale
AU - Li, Yaqiong
AU - Li, Zack
AU - Lokken, Martine
AU - Louis, Thibaut
AU - Lungu, Marius
AU - MacInnis, Amanda
AU - Madhavacheril, Mathew
AU - Maldonado, Felipe
AU - Mallaby-Kay, Maya
AU - Marsden, Danica
AU - McMahon, Jeff
AU - Menanteau, Felipe
AU - Moodley, Kavilan
AU - Morton, Tim
AU - Namikawa, Toshiya
AU - Nati, Federico
AU - Newburgh, Laura
AU - Nibarger, John P.
AU - Nicola, Andrina
AU - Niemack, Michael D.
AU - Nolta, Michael R.
AU - Orlowski-Sherer, John
AU - Page, Lyman A.
AU - Pappas, Christine G.
AU - Partridge, Bruce
AU - Phakathi, Phumlani
AU - Pisano, Giampaolo
AU - Prince, Heather
AU - Puddu, Roberto
AU - Qu, Frank J.
AU - Rivera, Jesus
AU - Robertson, Naomi
AU - Rojas, Felipe
AU - Salatino, Maria
AU - Schaan, Emmanuel
AU - Schillaci, Alessandro
AU - Sehgal, Neelima
AU - Sherwin, Blake D.
AU - Sierra, Carlos
AU - Sievers, Jon
AU - Sifon, Cristobal
AU - Sikhosana, Precious
AU - Simon, Sara
AU - Spergel, David N.
AU - Staggs, Suzanne T.
AU - Stevens, Jason
AU - Storer, Emilie
AU - Sunder, Dhaneshwar D.
AU - Switzer, Eric R.
AU - Thorne, Ben
AU - Thornton, Robert
AU - Trac, Hy
AU - Treu, Jesse
AU - Tucker, Carole
AU - Vale, Leila R.
AU - van Engelen, Alexander
AU - van Lanen, Jeff
AU - Vavagiakis, Eve M.
AU - Wagoner, Kasey
AU - Wang, Yuhan
AU - Ward, Jonathan T.
AU - Wollack, Edward J.
AU - Xu, Zhilei
AU - Zago, Fernando
AU - Zhu, Ningfeng
N1 - Funding Information: 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. Funding Information: 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 Flat-iron 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. Funding Information: 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. Publisher Copyright: © 2020 IOP Publishing Ltd and Sissa Medialab.
PY - 2020/12
Y1 - 2020/12
N2 - 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.
AB - 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.
KW - CMBR experiments
KW - CMBR polarisation
KW - Cosmological parameters from CMBR
UR - http://www.scopus.com/inward/record.url?scp=85099392804&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85099392804&partnerID=8YFLogxK
U2 - 10.1088/1475-7516/2020/12/047
DO - 10.1088/1475-7516/2020/12/047
M3 - Article
AN - SCOPUS:85099392804
SN - 1475-7516
VL - 2020
JO - Journal of Cosmology and Astroparticle Physics
JF - Journal of Cosmology and Astroparticle Physics
IS - 12
M1 - 047
ER -