We present results from the two observations of the cosmic background (CMB) performed from the South Pole during the 1993-1994 austral summer. Each observation employed a 3 degree peak-to-peak sinusoidal, single difference chop and consisted of a 20 degree x 1 degree strip on the sky. The first observation used a receiver which operates in three channels between 38 and 45 GHz (Q-band) with a FWHM beam which varies from 1 degree to 1.15 degrees. The second observation overlapped the first observation and used a reciever which operates in four channels between 26 and 36 GHz (Ka-band) with a FWHM beam which varies from 1.5 degrees to 1.7 degrees. Significant correlated structure is observed in all channels for each observation. The spectrum of the structure is consistant with a CMB spectrum and is formally inconsistant with a diffuse synchrotron and free-free emission at the 5 level. The amplitude of the structure is inconsistant with 20 K interstellar dust; however, the data do not discriminate against flat or inverted spectrum point sources. The root mean square amplitude of the combined (Ka + Q) data is for an average window function which has a peak value of 0.97 at and drops to of the peak value at A band power estimate of the CMB power spectrum,
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