TY - JOUR
T1 - Atacama Cosmology Telescope
T2 - Constraints on prerecombination early dark energy
AU - Hill, J. Colin
AU - Calabrese, Erminia
AU - Aiola, Simone
AU - Battaglia, Nicholas
AU - Bolliet, Boris
AU - Choi, Steve K.
AU - Devlin, Mark J.
AU - Duivenvoorden, Adriaan J.
AU - Dunkley, Jo
AU - Ferraro, Simone
AU - Gallardo, Patricio A.
AU - Gluscevic, Vera
AU - Hasselfield, Matthew
AU - Hilton, Matt
AU - Hincks, Adam D.
AU - HloŽek, Renée
AU - Koopman, Brian J.
AU - Kosowsky, Arthur
AU - La Posta, Adrien
AU - Louis, Thibaut
AU - Madhavacheril, Mathew S.
AU - McMahon, Jeff
AU - Moodley, Kavilan
AU - Naess, Sigurd
AU - Natale, Umberto
AU - Nati, Federico
AU - Newburgh, Laura
AU - Niemack, Michael D.
AU - Page, Lyman A.
AU - Partridge, Bruce
AU - Qu, Frank J.
AU - Salatino, Maria
AU - Schillaci, Alessandro
AU - Sehgal, Neelima
AU - Sherwin, Blake D.
AU - Sifón, Cristóbal
AU - Spergel, David N.
AU - Staggs, Suzanne T.
AU - Storer, Emilie R.
AU - Van Engelen, Alexander
AU - Vavagiakis, Eve M.
AU - Wollack, Edward J.
AU - Xu, Zhilei
N1 - Funding Information:
Support for ACT was through the U.S. National Science Foundation through Grants No. AST-0408698, No. AST-0965625, and No. AST-1440226 for the Atacama Cosmology Telescope (ACT) project, as well as Grants No. PHY-0355328, No. PHY-0855887, and No. 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 Agencia Nacional de Investigación y Desarrollo (ANID). The development of multichroic detectors and lenses was supported by NASA Grants No. NNX13AE56G and No. NNX14AB58G. Detector research at NIST was supported by the NIST Innovations in Measurement Science program.
Funding Information:
We are grateful to Evan McDonough and Michael Toomey for their contributions to the development of class _ ede and for useful conversations, and we thank the Scientific Computing Core staff at the Flatiron Institute for computational support. The Flatiron Institute is supported by the Simons Foundation. E. C. acknowledges support from the STFC Ernest Rutherford Fellowship No. ST/M004856/2 and STFC Consolidated Grant No. ST/S00033X/1. EC and U. N. acknowledge support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant Agreement No. 849169). J. D. and E. S. acknowledge support from NSF Grant No. AST-1814971. N. S. acknowledges support from NSF Grant No. AST-1907657. M. Hi. and K. M. acknowledge support from the National Research Foundation of South Africa. V. G. is supported by the National Science Foundation under Grant No. PHY-2013951. Z. X. is supported by the Gordon and Betty Moore Foundation. Research at Perimeter Institute is supported in part by the Government of Canada through the Department of Innovation, Science, and Industry Canada and by the Province of Ontario through the Ministry of Colleges and Universities. A. D. H. acknowledges support from the Sutton Family Chair in Science, Christianity, and Cultures and from the Faculty of Arts and Science, University of Toronto. S. K. C. acknowledges support from NSF Grant No. AST-2001866. E. V. acknowledges support from the NSF GRFP via Grant No. DGE-1650441. C. S. acknowledges support from the Agencia Nacional de Investigación y Desarrollo (ANID) under FONDECYT Grant No. 11191125. This work was completed at the Aspen Center for Physics, which is supported by National Science Foundation Grant No. PHY-1607611.
Publisher Copyright:
© 2022 us.
PY - 2022/6/15
Y1 - 2022/6/15
N2 - The early dark energy (EDE) scenario aims to increase the value of the Hubble constant (H0) inferred from cosmic microwave background (CMB) data over that found in the standard cosmological model (ΛCDM), via the introduction of a new form of energy density in the early Universe. The EDE component briefly accelerates cosmic expansion just prior to recombination, which reduces the physical size of the sound horizon imprinted in the CMB. Previous work has found that nonzero EDE is not preferred by Planck CMB power spectrum data alone, which yield a 95% confidence level (C.L.) upper limit fEDE<0.087 on the maximal fractional contribution of the EDE field to the cosmic energy budget. In this paper, we fit the EDE model to CMB data from the Atacama Cosmology Telescope (ACT) data release 4. We find that a combination of ACT, large-scale Planck TT (similar to WMAP), Planck CMB lensing, and BAO data prefers the existence of EDE at >99.7% C.L.: fEDE=0.091-0.036+0.020, with H0=70.9-2.0+1.0 km/s/Mpc (both 68% C.L.). From a model-selection standpoint, we find that EDE is favored over ΛCDM by these data at roughly 3σ significance. In contrast, a joint analysis of the full Planck and ACT data yields no evidence for EDE, as previously found for Planck alone. We show that the preference for EDE in ACT alone is driven by its TE and EE power spectrum data. The tight constraint on EDE from Planck alone is driven by its high-ℓ TT power spectrum data. Understanding whether these differing constraints are physical in nature, due to systematics, or simply a rare statistical fluctuation is of high priority. The best-fit EDE models to ACT and Planck exhibit coherent differences across a wide range of multipoles in TE and EE, indicating that a powerful test of this scenario is anticipated with near-future data from ACT and other ground-based experiments.
AB - The early dark energy (EDE) scenario aims to increase the value of the Hubble constant (H0) inferred from cosmic microwave background (CMB) data over that found in the standard cosmological model (ΛCDM), via the introduction of a new form of energy density in the early Universe. The EDE component briefly accelerates cosmic expansion just prior to recombination, which reduces the physical size of the sound horizon imprinted in the CMB. Previous work has found that nonzero EDE is not preferred by Planck CMB power spectrum data alone, which yield a 95% confidence level (C.L.) upper limit fEDE<0.087 on the maximal fractional contribution of the EDE field to the cosmic energy budget. In this paper, we fit the EDE model to CMB data from the Atacama Cosmology Telescope (ACT) data release 4. We find that a combination of ACT, large-scale Planck TT (similar to WMAP), Planck CMB lensing, and BAO data prefers the existence of EDE at >99.7% C.L.: fEDE=0.091-0.036+0.020, with H0=70.9-2.0+1.0 km/s/Mpc (both 68% C.L.). From a model-selection standpoint, we find that EDE is favored over ΛCDM by these data at roughly 3σ significance. In contrast, a joint analysis of the full Planck and ACT data yields no evidence for EDE, as previously found for Planck alone. We show that the preference for EDE in ACT alone is driven by its TE and EE power spectrum data. The tight constraint on EDE from Planck alone is driven by its high-ℓ TT power spectrum data. Understanding whether these differing constraints are physical in nature, due to systematics, or simply a rare statistical fluctuation is of high priority. The best-fit EDE models to ACT and Planck exhibit coherent differences across a wide range of multipoles in TE and EE, indicating that a powerful test of this scenario is anticipated with near-future data from ACT and other ground-based experiments.
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U2 - 10.1103/PhysRevD.105.123536
DO - 10.1103/PhysRevD.105.123536
M3 - Article
AN - SCOPUS:85134244067
SN - 2470-0010
VL - 105
JO - Physical Review D
JF - Physical Review D
IS - 12
M1 - e123536
ER -