The Atacama Cosmology Telescope: DR4 maps and cosmological parameters

Simone Aiola; Erminia Calabrese; Loïc Maurin; Sigurd Naess; Benjamin L. Schmitt; Maximilian H. Abitbol; Graeme E. Addison; Peter A.R. Ade; David Alonso; Mandana Amiri; Stefania Amodeo; Elio Angile; Jason E. Austermann; Taylor Baildon; Nick Battaglia; James A. Beall; Rachel Bean; Daniel T. Becker; J. Richard Bond; Sarah Marie Bruno; Victoria Calafut; Luis E. Campusano; Felipe Carrero; Grace E. Chesmore; Hsiao Mei Cho; Steve K. Choi; Susan E. Clark; Nicholas F. Cothard; Devin Crichton; Kevin T. Crowley; Omar Darwish; Rahul Datta; Edward V. Denison; Mark J. Devlin; Cody J. Duell; Shannon M. Duff; Adriaan J. Duivenvoorden; Jo Dunkley; Rolando Dünner; Thomas Essinger-Hileman; Max Fankhanel; Simone Ferraro; Anna E. Fox; Brittany Fuzia; Patricio A. Gallardo; Vera Gluscevic; Joseph E. Golec; Emily Grace; Megan Gralla; Yilun Guan; Kirsten Hall; Mark Halpern; Dongwon Han; Peter Hargrave; Matthew Hasselfield; Jakob M. Helton; Shawn Henderson; Brandon Hensley; J. Colin Hill; Gene C. Hilton; Matt Hilton; Adam D. Hincks; Renée Hložek; Shuay Pwu Patty Ho; Johannes Hubmayr; Kevin M. Huffenberger; John P. Hughes; Leopoldo Infante; Kent Irwin; Rebecca Jackson; Jeff Klein; Kenda Knowles; Brian Koopman; Arthur Kosowsky; Vincent Lakey; Dale Li; Yaqiong Li; Zack Li; Martine Lokken; Thibaut Louis; Marius Lungu; Amanda MacInnis; Mathew Madhavacheril; Felipe Maldonado; Maya Mallaby-Kay; Danica Marsden; Jeff McMahon; Felipe Menanteau; Kavilan Moodley; Tim Morton; Toshiya Namikawa; Federico Nati; Laura Newburgh; John P. Nibarger; Andrina Nicola; Michael D. Niemack; Michael R. Nolta; John Orlowski-Sherer; Lyman A. Page; Christine G. Pappas; Bruce Partridge; Phumlani Phakathi; Giampaolo Pisano; Heather Prince; Roberto Puddu; Frank J. Qu; Jesus Rivera; Naomi Robertson; Felipe Rojas; Maria Salatino; Emmanuel Schaan; Alessandro Schillaci; Neelima Sehgal; Blake D. Sherwin; Carlos Sierra; Jon Sievers; Cristobal Sifon; Precious Sikhosana; Sara Simon; David N. Spergel; Suzanne T. Staggs; Jason Stevens; Emilie Storer; Dhaneshwar D. Sunder; Eric R. Switzer; Ben Thorne; Robert Thornton; Hy Trac; Jesse Treu; Carole Tucker; Leila R. Vale; Alexander van Engelen; Jeff van Lanen; Eve M. Vavagiakis; Kasey Wagoner; Yuhan Wang; Jonathan T. Ward; Edward J. Wollack; Zhilei Xu; Fernando Zago; Ningfeng Zhu

doi:10.1088/1475-7516/2020/12/047

The Atacama Cosmology Telescope: DR4 maps and cosmological parameters

Simone Aiola, Erminia Calabrese, Loïc Maurin, Sigurd Naess, Benjamin L. Schmitt, Maximilian H. Abitbol, Graeme E. Addison, Peter A.R. Ade, David Alonso, Mandana Amiri, Stefania Amodeo, Elio Angile, Jason E. Austermann, Taylor Baildon, Nick Battaglia, James A. Beall, Rachel Bean, Daniel T. Becker, J. Richard Bond, Sarah Marie BrunoVictoria Calafut, Luis E. Campusano, Felipe Carrero, Grace E. Chesmore, Hsiao Mei Cho, Steve K. Choi, Susan E. Clark, Nicholas F. Cothard, Devin Crichton, Kevin T. Crowley, Omar Darwish, Rahul Datta, Edward V. Denison, Mark J. Devlin, Cody J. Duell, Shannon M. Duff, Adriaan J. Duivenvoorden, Jo Dunkley, Rolando Dünner, Thomas Essinger-Hileman, Max Fankhanel, Simone Ferraro, Anna E. Fox, Brittany Fuzia, Patricio A. Gallardo, Vera Gluscevic, Joseph E. Golec, Emily Grace, Megan Gralla, Yilun Guan, Kirsten Hall, Mark Halpern, Dongwon Han, Peter Hargrave, Matthew Hasselfield, Jakob M. Helton, Shawn Henderson, Brandon Hensley, J. Colin Hill, Gene C. Hilton, Matt Hilton, Adam D. Hincks, Renée Hložek, Shuay Pwu Patty Ho, Johannes Hubmayr, Kevin M. Huffenberger, John P. Hughes, Leopoldo Infante, Kent Irwin, Rebecca Jackson, Jeff Klein, Kenda Knowles, Brian Koopman, Arthur Kosowsky, Vincent Lakey, Dale Li, Yaqiong Li, Zack Li, Martine Lokken, Thibaut Louis, Marius Lungu, Amanda MacInnis, Mathew Madhavacheril, Felipe Maldonado, Maya Mallaby-Kay, Danica Marsden, Jeff McMahon, Felipe Menanteau, Kavilan Moodley, Tim Morton, Toshiya Namikawa, Federico Nati, Laura Newburgh, John P. Nibarger, Andrina Nicola, Michael D. Niemack, Michael R. Nolta, John Orlowski-Sherer, Lyman A. Page, Christine G. Pappas, Bruce Partridge, Phumlani Phakathi, Giampaolo Pisano, Heather Prince, Roberto Puddu, Frank J. Qu, Jesus Rivera, Naomi Robertson, Felipe Rojas, Maria Salatino, Emmanuel Schaan, Alessandro Schillaci, Neelima Sehgal, Blake D. Sherwin, Carlos Sierra, Jon Sievers, Cristobal Sifon, Precious Sikhosana, Sara Simon, David N. Spergel, Suzanne T. Staggs, Jason Stevens, Emilie Storer, Dhaneshwar D. Sunder, Eric R. Switzer, Ben Thorne, Robert Thornton, Hy Trac, Jesse Treu, Carole Tucker, Leila R. Vale, Alexander van Engelen, Jeff van Lanen, Eve M. Vavagiakis, Kasey Wagoner, Yuhan Wang, Jonathan T. Ward, Edward J. Wollack, Zhilei Xu, Fernando Zago, Ningfeng Zhu

Research output: Contribution to journal › Article › peer-review

188 Scopus citations

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	https://doi.org/10.1088/1475-7516/2020/12/047
State	Published - Dec 2020

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics

Keywords

CMBR experiments
CMBR polarisation
Cosmological parameters from CMBR

Access to Document

10.1088/1475-7516/2020/12/047

Cite this

Aiola, S., Calabrese, E., Maurin, L., Naess, S., Schmitt, B. L., Abitbol, M. H., Addison, G. E., Ade, P. A. R., Alonso, D., Amiri, M., Amodeo, S., Angile, E., Austermann, J. E., Baildon, T., Battaglia, N., Beall, J. A., Bean, R., Becker, D. T., Richard Bond, J., ... Zhu, N. (2020). The Atacama Cosmology Telescope: DR4 maps and cosmological parameters. Journal of Cosmology and Astroparticle Physics, 2020(12), [047]. https://doi.org/10.1088/1475-7516/2020/12/047

@article{1868c450b8904efe8756ab6b56123276,

title = "The Atacama Cosmology Telescope: DR4 maps and cosmological parameters",

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.",

keywords = "CMBR experiments, CMBR polarisation, Cosmological parameters from CMBR",

author = "Simone Aiola and Erminia Calabrese and Lo{\"i}c Maurin and Sigurd Naess and Schmitt, {Benjamin L.} and Abitbol, {Maximilian H.} and Addison, {Graeme E.} and Ade, {Peter A.R.} and David Alonso and Mandana Amiri and Stefania Amodeo and Elio Angile and Austermann, {Jason E.} and Taylor Baildon and Nick Battaglia and Beall, {James A.} and Rachel Bean and Becker, {Daniel T.} and {Richard Bond}, J. and Bruno, {Sarah Marie} and Victoria Calafut and Campusano, {Luis E.} and Felipe Carrero and Chesmore, {Grace E.} and Cho, {Hsiao Mei} and Choi, {Steve K.} and Clark, {Susan E.} and Cothard, {Nicholas F.} and Devin Crichton and Crowley, {Kevin T.} and Omar Darwish and Rahul Datta and Denison, {Edward V.} and Devlin, {Mark J.} and Duell, {Cody J.} and Duff, {Shannon M.} and Duivenvoorden, {Adriaan J.} and Jo Dunkley and Rolando D{\"u}nner and Thomas Essinger-Hileman and Max Fankhanel and Simone Ferraro and Fox, {Anna E.} and Brittany Fuzia and Gallardo, {Patricio A.} and Vera Gluscevic and Golec, {Joseph E.} and Emily Grace and Megan Gralla and Yilun Guan and Kirsten Hall and Mark Halpern and Dongwon Han and Peter Hargrave and Matthew Hasselfield and Helton, {Jakob M.} and Shawn Henderson and Brandon Hensley and {Colin Hill}, J. and Hilton, {Gene C.} and Matt Hilton and Hincks, {Adam D.} and Ren{\'e}e Hlo{\v z}ek and Ho, {Shuay Pwu Patty} and Johannes Hubmayr and Huffenberger, {Kevin M.} and Hughes, {John P.} and Leopoldo Infante and Kent Irwin and Rebecca Jackson and Jeff Klein and Kenda Knowles and Brian Koopman and Arthur Kosowsky and Vincent Lakey and Dale Li and Yaqiong Li and Zack Li and Martine Lokken and Thibaut Louis and Marius Lungu and Amanda MacInnis and Mathew Madhavacheril and Felipe Maldonado and Maya Mallaby-Kay and Danica Marsden and Jeff McMahon and Felipe Menanteau and Kavilan Moodley and Tim Morton and Toshiya Namikawa and Federico Nati and Laura Newburgh and Nibarger, {John P.} and Andrina Nicola and Niemack, {Michael D.} and Nolta, {Michael R.} and John Orlowski-Sherer and Page, {Lyman A.} and Pappas, {Christine G.} and Bruce Partridge and Phumlani Phakathi and Giampaolo Pisano and Heather Prince and Roberto Puddu and Qu, {Frank J.} and Jesus Rivera and Naomi Robertson and Felipe Rojas and Maria Salatino and Emmanuel Schaan and Alessandro Schillaci and Neelima Sehgal and Sherwin, {Blake D.} and Carlos Sierra and Jon Sievers and Cristobal Sifon and Precious Sikhosana and Sara Simon and Spergel, {David N.} and Staggs, {Suzanne T.} and Jason Stevens and Emilie Storer and Sunder, {Dhaneshwar D.} and Switzer, {Eric R.} and Ben Thorne and Robert Thornton and Hy Trac and Jesse Treu and Carole Tucker and Vale, {Leila R.} and {van Engelen}, Alexander and {van Lanen}, Jeff and Vavagiakis, {Eve M.} and Kasey Wagoner and Yuhan Wang and Ward, {Jonathan T.} and Wollack, {Edward J.} and Zhilei Xu and Fernando Zago and Ningfeng Zhu",

note = "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 Astron{\'o}mico Atacama in northern Chile under the auspices of the Comisi{\'o}n Nacional de Investigaci{\'o}n (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{\textquoteright}s Gravity & the Extreme Universe Program and as an Alfred. P. Sloan Research Fellow. RH is also supported by Canada{\textquoteright}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 Astron{\'o}mico Atacama in northern Chile under the auspices of the Comisi{\'o}n Nacional de Investigaci{\'o}n (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{\textquoteright}s Gravity & the Extreme Universe Program and as an Alfred. P. Sloan Research Fellow. RH is also supported by Canada{\textquoteright}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: {\textcopyright} 2020 IOP Publishing Ltd and Sissa Medialab.",

year = "2020",

month = dec,

doi = "10.1088/1475-7516/2020/12/047",

language = "English (US)",

volume = "2020",

journal = "Journal of Cosmology and Astroparticle Physics",

issn = "1475-7516",

publisher = "IOP Publishing Ltd.",

number = "12",

}

Aiola, S, Calabrese, E, Maurin, L, Naess, S, Schmitt, BL, Abitbol, MH, Addison, GE, Ade, PAR, Alonso, D, Amiri, M, Amodeo, S, Angile, E, Austermann, JE, Baildon, T, Battaglia, N, Beall, JA, Bean, R, Becker, DT, Richard Bond, J, Bruno, SM, Calafut, V, Campusano, LE, Carrero, F, Chesmore, GE, Cho, HM, Choi, SK, Clark, SE, Cothard, NF, Crichton, D, Crowley, KT, Darwish, O, Datta, R, Denison, EV, Devlin, MJ, Duell, CJ, Duff, SM, Duivenvoorden, AJ, Dunkley, J, Dünner, R, Essinger-Hileman, T, Fankhanel, M, Ferraro, S, Fox, AE, Fuzia, B, Gallardo, PA, Gluscevic, V, Golec, JE, Grace, E, Gralla, M, Guan, Y, Hall, K, Halpern, M, Han, D, Hargrave, P, Hasselfield, M, Helton, JM, Henderson, S, Hensley, B, Colin Hill, J, Hilton, GC, Hilton, M, Hincks, AD, Hložek, R, Ho, SPP, Hubmayr, J, Huffenberger, KM, Hughes, JP, Infante, L, Irwin, K, Jackson, R, Klein, J, Knowles, K, Koopman, B, Kosowsky, A, Lakey, V, Li, D, Li, Y, Li, Z, Lokken, M, Louis, T, Lungu, M, MacInnis, A, Madhavacheril, M, Maldonado, F, Mallaby-Kay, M, Marsden, D, McMahon, J, Menanteau, F, Moodley, K, Morton, T, Namikawa, T, Nati, F, Newburgh, L, Nibarger, JP, Nicola, A, Niemack, MD, Nolta, MR, Orlowski-Sherer, J, Page, LA, Pappas, CG, Partridge, B, Phakathi, P, Pisano, G, Prince, H, Puddu, R, Qu, FJ, Rivera, J, Robertson, N, Rojas, F, Salatino, M, Schaan, E, Schillaci, A, Sehgal, N, Sherwin, BD, Sierra, C, Sievers, J, Sifon, C, Sikhosana, P, Simon, S, Spergel, DN, Staggs, ST, Stevens, J, Storer, E, Sunder, DD, Switzer, ER, Thorne, B, Thornton, R, Trac, H, Treu, J, Tucker, C, Vale, LR, van Engelen, A, van Lanen, J, Vavagiakis, EM, Wagoner, K, Wang, Y, Ward, JT, Wollack, EJ, Xu, Z, Zago, F & Zhu, N 2020, 'The Atacama Cosmology Telescope: DR4 maps and cosmological parameters', Journal of Cosmology and Astroparticle Physics, vol. 2020, no. 12, 047. https://doi.org/10.1088/1475-7516/2020/12/047

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 -

The Atacama Cosmology Telescope: DR4 maps and cosmological parameters

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