  During the fifth flight of the Microwave Anisotropy Experiment (MAX5), we
revisited a region with significant dust emission near the star Mu Pegasi. A
3.5 cm$^{-1}$ low frequency channel has been added since the previous
measurement (\cite{mei93a}). The data in each channel clearly show structure
correlated with IRAS 100 \micron\ dust emission. The spectrum of the structure
in the 6, 9 and 14 cm$^{-1}$ channels is described by
$I_{\nu}\propto\nu^{\beta}B_{\nu}(T_{dust})$, where $\beta$ = 1.3 and
$T_{dust}$ = 19~K and $B_{\nu}$ is the Planck function. However, this model
predicts a smaller amplitude in the 3.5 cm$^{-1}$ band than is observed.
Considering only linear combinations of the data independent of the best fit
foreground spectrum for the three lower channels, we find an upper limit to
CMBR fluctuations of $\Delta T/T = \langle
\frac{C_l~l(l+1)}{2\pi}\rangle^{\frac{1}{2}} \leq 1.3\times 10^{-5}$ at the
95\% confidence level. The result is for a flat band power spectrum and does
not include a 10\% uncertainty in calibration. It is consistent with our
previous observation in the region.
