Abstract
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 ` = 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 = −0.07◦ ±0.09◦. 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.
Original language | English (US) |
---|---|
Article number | 045 |
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
Access to Document
Other files and links
Fingerprint
Dive into the research topics of 'The atacama cosmology telescope: A measurement of the cosmic microwave background power spectra at 98 and 150 GHz'. Together they form a unique fingerprint.Cite this
- APA
- Author
- BIBTEX
- Harvard
- Standard
- RIS
- Vancouver
}
In: Journal of Cosmology and Astroparticle Physics, Vol. 2020, No. 12, 045, 12.2020.
Research output: Contribution to journal › Article › peer-review
TY - JOUR
T1 - The atacama cosmology telescope
T2 - A measurement of the cosmic microwave background power spectra at 98 and 150 GHz
AU - Choi, Steve K.
AU - Hasselfield, Matthew
AU - Ho, Shuay Pwu Patty
AU - Koopman, Brian
AU - Lungu, Marius
AU - Abitbol, Maximilian H.
AU - Addison, Graeme E.
AU - Ade, Peter A.R.
AU - Aiola, Simone
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 - Calabrese, Erminia
AU - Calafut, Victoria
AU - Campusano, Luis E.
AU - Carrero, Felipe
AU - Chesmore, Grace E.
AU - Cho, Hsiao Mei
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 - Henderson, Shawn
AU - Hensley, Brandon
AU - Colin Hill, J.
AU - Hilton, Gene C.
AU - Hilton, Matt
AU - Hincks, Adam D.
AU - Hložek, Renée
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 - Kosowsky, Arthur
AU - Lakey, Vincent
AU - Li, Dale
AU - Li, Yaqiong
AU - Li, Zack
AU - Lokken, Martine
AU - Louis, Thibaut
AU - MacInnis, Amanda
AU - Madhavacheril, Mathew
AU - Maldonado, Felipe
AU - Mallaby-Kay, Maya
AU - Marsden, Danica
AU - Maurin, Loïc
AU - McMahon, Jeff
AU - Menanteau, Felipe
AU - Moodley, Kavilan
AU - Morton, Tim
AU - Naess, Sigurd
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 - 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 - Schmitt, Benjamin L.
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 per- Funding Information: formed 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 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 ` = 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 = −0.07◦ ±0.09◦. 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.
AB - 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 ` = 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 = −0.07◦ ±0.09◦. 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.
KW - CMBR experiments
KW - CMBR polarisation
KW - Cosmological parameters from CMBR
UR - http://www.scopus.com/inward/record.url?scp=85099357810&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85099357810&partnerID=8YFLogxK
U2 - 10.1088/1475-7516/2020/12/045
DO - 10.1088/1475-7516/2020/12/045
M3 - Article
AN - SCOPUS:85099357810
SN - 1475-7516
VL - 2020
JO - Journal of Cosmology and Astroparticle Physics
JF - Journal of Cosmology and Astroparticle Physics
IS - 12
M1 - 045
ER -