MEASUREMENTS OF ANISOTROPY IN THE COSMIC MICROWAVE BACKGROUND-RADIATION AT DEGREE ANGULAR SCALES NEAR THE STARS SIGMA HERCULIS AND IOTA DRACONIS

We present results from two four-frequency observations centered near the stars Sigma Herculis and Iota Draconis during the fourth flight of the Millimeter-wave Anisotropy eXperiment (MAX). The observations were made of 6-degrees x 0.6-degrees strips of the sky with a 1.4-degrees peak to peak sinusoidal chop in all bands. The FWHM beam sizes were calculated 0.55-degrees + 0.05-degrees at 3.5 cm-1 and a 0.75-degrees + 0.05-degrees, at 6, 9, and 14 cm-1. Significant correlated structures were observed at 3.5, 6, and 9 cm-1. The spectra of these signals are inconsistent with thermal emission from known interstellar dust populations. The extrapolated amplitudes of synchrotron and free-free emission are too small to account for the amplitude of the observed structures. If the observed structures are attributed to CMB anisotropy with a Gaussian autocorrelation function and a coherence angle of 25', then the most probable values at DELTAT/T(CMB) = 3.1(+1.7/-1.3) x 10(-5) for the Sigma Herculis scan, and DELTAT/T(CMB) = 3.3(-1.1/+1.1) x 10(-5) for the Iota Draconis scan (95% confidence upper, lower limits).