The Anisotropy in the Cosmic Microwave Background At Degree Angular Scales

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dc.creatorNetterfield, C. B.
dc.creatorJarosik, N.
dc.creatorPage, L.
dc.creatorWilkinson, D.
dc.creatorWollack, E.
dc.date1994-11-08
dc.date.accessioned2026-07-07T11:29:46Z
dc.date.available2026-07-07T11:29:46Z
dc.descriptionWe 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 $44^{+13}_{-7} μ$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 $δT_l = \sqrt{l(2l+1)<|a_l^m|^2>/4π} = 42^{+12}_{-7} μ$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 $3σ$. 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 $\le 4~μ$K/day over a period of one month. The dependence of the inferred anisotropy on the calibration and data editing is addressed.
dc.description16 pages, 2 figures. Saskatoon 1993/1994 combined analysis
dc.identifierhttps://arxiv.org/abs/astro-ph/9411035
dc.identifierhttp://arxiv.org/abs/astro-ph/9411035
dc.identifierAstrophys.J.445:L69-L72,1995
dc.identifierdoi:10.1086/187892
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/196818
dc.subjectAstrophysics
dc.titleThe Anisotropy in the Cosmic Microwave Background At Degree Angular Scales
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