  We present measurements of cosmic microwave background (CMB) anisotropy near
the stars HR5127 and Phi Herculis from the fifth flight of the Millimeter-wave
Anisotropy eXperiment (MAX). We scanned 8\arcdeg\ strips of the sky with an
approximately Gaussian 0\fdg5 FWHM beam and a 1\fdg4 peak to peak sinusoidal
chop. The instrument has four frequency bands centered at 3.5, 6, 9, and
14~cm$^{-1}$. The IRAS 100~\micron\ map predicts that these two region have low
interstellar dust contrast. The HR5127 data are consistent with CMB anisotropy.
The Phi Herculis data, which were measured at lower flight altitudes, show time
variability at 9 and 14~cm$^{-1}$ which we believe to be due to atmospheric
emission. However, the Phi Herculis data at 3.5 and 6~cm$^{-1}$ are essentially
independent of this atmospheric contribution and are consistent with CMB
anisotropy. Confusion from galactic foregrounds is unlikely based on the
spectrum and amplitude of the structure at these frequencies. If the observed
HR5127 structure and the atmosphere independent Phi Herculis structure are
attributed to CMB anisotropy, then we find $\Delta T/T =
\langle\frac{l(l+1)C_l}{2\pi}\rangle^{1/2} = 1.2^{+0.4}_{-0.3}\times 10^{-5}$
for HR5127 and $1.9^{+0.7}_{-0.4}\times 10^{-5}$ for Phi Herculis in the flat
band approximation. The upper and lower limits represent a 68\% confidence
interval added in quadrature with a 10\% calibration uncertainty.
