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University of Chicago Press:PO Box 37005, Journals Division:Chicago, IL 60637:(877)705-1878, (877)705-1878, (773)753-2247, EMAIL: [email protected], INTERNET: http://www.press.uchicago.edu, Fax: (877)705-1879, (773)753-0811
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Abstract
We present a measurement of the angular power spectrum of the cosmic microwave background (CMB) radiation
observed at 148 GHz. The measurement uses maps with 1. 4 angular resolution made with data from the Atacama
Cosmology Telescope (ACT). The observations cover 228 deg2 of the southern sky, in a 4. ◦ 2 wide strip centered on
declination 53◦ south. The CMB at arcminute angular scales is particularly sensitive to the Silk damping scale, to
the Sunyaev–Zel’dovich (SZ) effect from galaxy clusters, and to emission by radio sources and dusty galaxies. After
masking the 108 brightest point sources in our maps, we estimate the power spectrum between 600 < < 8000
using the adaptive multi-taper method to minimize spectral leakage and maximize use of the full data set. Our
absolute calibration is based on observations of Uranus. To verify the calibration and test the fidelity of our map at
large angular scales, we cross-correlate the ACT map to the WMAP map and recover the WMAP power spectrum
from 250 < l < 1150. The power beyond the Silk damping tail of the CMB (l ∼ 5000) is consistent with models
of the emission from point sources. We quantify the contribution of SZ clusters to the power spectrum by fitting
to a model normalized to σ8 = 0.8. We constrain the model’s amplitude ASZ < 1.63 (95% CL). If interpreted as
a measurement of σ8, this implies σSZ
8 < 0.86 (95% CL) given our SZ model. A fit of ACT and WMAP five-year
data jointly to a six-parameter ΛCDM model plus point sources and the SZ effect is consistent with these results
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