TY - JOUR
T1 - Anisotropy in the microwave sky at 90 ghz
T2 - Results from python ii
AU - Ruhl, J. E.
AU - Dragovan, M.
AU - Platt, S. R.
AU - Kovac, J.
AU - Novak, G.
N1 - Funding Information:
We thank the Antarctic Support Associates staff at the South Pole for making a successful season possible, and Ted Griffith, Bob Pernic, and Bill Vinje for valuable assistance there. This research was supported by the James S. McDonnell Foundation, PYI grant NSF AST 90-57089, and the National Science Foundation under a cooperative agreement with the Center for Astrophysical Research in Antarctica (CARA), grant NSF OPP 89-20223. CARA is an NSF Science and Technology Center. J. R. was supported by the McCormick Fellowship at the University of Chicago.
PY - 1995/11/1
Y1 - 1995/11/1
N2 - We report on additional observations of degree-scale anisotropy at 90 GHz from the Amundsen-Scott South Pole Station in Antarctica. Observations during the first season with the Python instrument yielded a statistically significant sky signal with an amplitude of ΔT/T ~ 3.5 X 10-5 for a Gaussian autocorrelation function model with a coherence angle 6c = 1°. In this Letter we report the confirmation of that signal with data taken in the second year, and on results from an interleaving set of fields. Using the entire data set, we find ΔT/T = C1/20 = 2.8+1.1-0.7X 10-5for the Gaussian autocorrelation model mentioned above, and ΔT/T = [∫e(∫e +1) C1/(2ᴨ)]1/2 = 2.I+0.7-0.5 X 10-5 for a band power estimate, where le = 93 is the effective center of our window function. The stated errors represent a 68% confidence interval in the likelihood added in quadrature with a 20% calibration uncertainty.
AB - We report on additional observations of degree-scale anisotropy at 90 GHz from the Amundsen-Scott South Pole Station in Antarctica. Observations during the first season with the Python instrument yielded a statistically significant sky signal with an amplitude of ΔT/T ~ 3.5 X 10-5 for a Gaussian autocorrelation function model with a coherence angle 6c = 1°. In this Letter we report the confirmation of that signal with data taken in the second year, and on results from an interleaving set of fields. Using the entire data set, we find ΔT/T = C1/20 = 2.8+1.1-0.7X 10-5for the Gaussian autocorrelation model mentioned above, and ΔT/T = [∫e(∫e +1) C1/(2ᴨ)]1/2 = 2.I+0.7-0.5 X 10-5 for a band power estimate, where le = 93 is the effective center of our window function. The stated errors represent a 68% confidence interval in the likelihood added in quadrature with a 20% calibration uncertainty.
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U2 - 10.1086/309739
DO - 10.1086/309739
M3 - Article
AN - SCOPUS:11944275750
SN - 0004-637X
VL - 453
SP - L1-L4
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
ER -