Journal
ASTROPHYSICAL JOURNAL
Volume 722, Issue 2, Pages 1148-1161Publisher
IOP Publishing Ltd
DOI: 10.1088/0004-637X/722/2/1148
Keywords
cosmic background radiation; cosmology: observations
Categories
Funding
- ACT
- NASA [NNX08AH30G]
- Natural Science and Engineering Research Council of Canada (NSERC)
- NSF [AST-0546035, AST-0606975]
- FONDAP Centro de Astrofisica
- CONICYT
- MECESUP
- Fundacion Andes
- NSF Physics Frontier Center [PHY-0114422]
- South African National Research Foundation (NRF)
- Meraka Institute via funding for the South African Centre for High Performance Computing (CHPC)
- South African Square Kilometer Array (SKA) Project
- RCUK
- Rhodes Trust
- Berkeley Center for Cosmological Physics
- World Premier International Research Center Initiative, MEXT, Japan
- STFC [ST/G002711/1] Funding Source: UKRI
- ICREA Funding Source: Custom
- NASA [101243, NNX08AH30G] Funding Source: Federal RePORTER
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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 deg(2) of the southern sky, in a 4 degrees.2 wide strip centered on declination 53 degrees 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 < l < 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 similar to 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 sigma(8) = 0.8. We constrain the model's amplitude A(SZ) < 1.63 (95% CL). If interpreted as a measurement of sigma(8), this implies sigma(SZ)(8) < 0.86 (95% CL) given our SZ model. A fit of ACT and WMAP five-year data jointly to a six-parameter Lambda CDM model plus point sources and the SZ effect is consistent with these results.
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