The Anisotropy in the Cosmic Microwave Background At Degree Angular Scales

Details The Anisotropy in the Cosmic Microwave Background At Degree Angular Scales The Anisotropy in the Cosmic Microwave Background At Degree Angular Scales

1994-11-08

arxiv.org/abs/astro-ph/9411035v1

Astrophys.J.445:L69-L72,1995

Astronomy and Astrophysics

Astrophysics

16 pages, 2 figures. Saskatoon 1993/1994 combined analysis

Scientific paper

10.1086/187892

We detect anisotropy in the cosmic microwave background (CMB) at degree angular scales and confirm a previous detection reported by Wollack et al. (1993). The root-mean-squared amplitude of the fluctuations is $44^{+13}_{-7} \mu$K. This may be expressed as the square root of the angular power spectrum in a band of multipoles between $l_{eff}=69^{+29}_{-22}$. We find $\delta T_l = \sqrt{l(2l+1)<|a_l^m|^2>/4\pi} = 42^{+12}_{-7} \mu$K. The measured spectral index of the fluctuations is consistent with zero, the value expected for the CMB. The spectral index corresponding to Galactic free-free emission, the most likely foreground contaminant, is rejected at approximately $3\sigma$. The analysis is based on three independent data sets. The first, taken in 1993, spans the 26 - 36 GHz frequency range with three frequency bands; the second was taken with the same radiometer as the first but during an independent observing campaign in 1994; and the third, also take in 1994, spans the 36-46 GHz range in three bands. For each telescope position and radiometer channel, the drifts in the instrument offset are $\le 4~\mu$K/day over a period of one month. The dependence of the inferred anisotropy on the calibration and data editing is addressed.

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