1994/12/07 by J. Gundersen, J. O. Gundersen, M. Lim +26
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics (astro-ph) #FOS: Physical sciences #Geophysics and Gravity Measurements #Radio Astronomy Observations and Technology #Scientific Research and Discoveries #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9412020
14 pgs., LaTeX, 2 figs., submitted to APJL
arxiv created 1994/12/07 · openalex publication_date 1994/12/07 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We present results from 2 observations of the CMB performed from the South Pole during the 93-94 austral summer. Each observation employed a 3∘ peak to peak sinusoidal, single difference chop and consisted of a 20∘× 1∘ strip on the sky near our SP91 observations. The first observation used a Q-band receiver which operates in 3 bands between 38 and 45 GHz with a 1∘ to 1⋅∘ 15 FWHM beam. The second observation overlapped the first observation and used a Ka-band receiver which operates in 4 bands between 26 and 36 GHz with a 1⋅∘25 to 1⋅∘7 FWHM beam. Significant correlated structure is observed in all bands for each observation. The spectrum of the structure is consistent with a CMB spectrum; however, the data do not discriminate against flat or inverted spectrum point sources. The root mean square amplitude (± 1σ) of the combined (Ka+Q) data is ΔTrms=42.0-6.8+15.8 μK in a band of multipoles between ℓ=68+38-32. A band power estimate of the CMB power spectrum, C_ℓ, gives ⟨ (C_ℓ ℓ (ℓ+1))/(2π)⟩B= 1.77-0.54+1.58× 10-10. The band power estimates for the seperate Ka and Q-band results are larger than but consistent with the band power estimate of the combined Ka-band SP91 results.