期刊
ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
卷 209, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0067-0049/209/1/17
关键词
cosmology: observations; planets and satellites: individual (Saturn, Uranus)
资金
- U.S. National Science Foundation [AST-0408698, AST-0965625]
- Princeton University
- University of Pennsylvania
- Canada Foundation for Innovation (CFI) award
- Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT)
- CFI under Compute Canada
- Government of Ontario
- Ontario Research Fund-Research Excellence
- University of Toronto
- [PHY-0855887]
- [PHY-1214379]
- STFC [ST/K00106X/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/K00106X/1] Funding Source: researchfish
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [0965625] Funding Source: National Science Foundation
We describe the measurement of the beam profiles and window functions for the Atacama Cosmology Telescope (ACT), which operated from 2007 to 2010 with kilopixel bolometer arrays centered at 148, 218, and 277 GHz. Maps of Saturn are used to measure the beam shape in each array and for each season of observations. Radial profiles are transformed to Fourier space in a way that preserves the spatial correlations in the beam uncertainty to derive window functions relevant for angular power spectrum analysis. Several corrections are applied to the resulting beam transforms, including an empirical correction measured from the final cosmic microwave background (CMB) survey maps to account for the effects of mild pointing variation and alignment errors. Observations of Uranus made regularly throughout each observing season are used to measure the effects of atmospheric opacity and to monitor deviations in telescope focus over the season. Using the WMAP-based calibration of the ACT maps to the CMB blackbody, we obtain precise measurements of the brightness temperatures of the Uranus and Saturn disks at effective frequencies of 149 and 219 GHz. For Uranus we obtain thermodynamic brightness temperatures T-U(149) = 106.7 +/- 2.2 K and T-U(219) = 100.1 +/- 3.1 K. For Saturn, we model the effects of the ring opacity and emission using a simple model and obtain resulting (unobscured) disk temperatures of T-S(149) = 137.3 +/- 3.2 K and T-S(219) = 137.3 +/- 4.7 K.
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