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We have conducted B, g, V, and R-band imaging in a 45x40 arcmin^2 fieldcontaining part of the high Galactic latitude translucent cloud MBM32, andcorrelated the intensity of diffuse optical light S_\nu(\lambda) with that of100 micron emission S_\nu(100um). A chi^2 minimum analysis is applied to fit alinear function to the measured correlation and derive the slope parameterb(\lambda)= \Delta S_\nu(\lambda) / \Delta S_\nu(100um) of the best-fit linearfunction. Compiling a sample by combining our b(\lambda) and published ones, weshow that the b(\lambda) strength varies from cloud to cloud by a factor of 4.Finding that b(\lambda) decreases as S_\nu(100um) increases in the sample, wesuggest that a non-linear correlation including a quadratic term ofS_\nu(100um)^2 should be fitted to the measured correlation. The variation ofoptical depth, which is A_V = 0.16 - 2.0 in the sample, can change b(\lambda)by a factor of 2 - 3. There would be some contribution to the large b(\lambda)variation from the forward-scattering characteristic of dust grains which iscoupled to the non-isotropic interstellar radiation field (ISRF). Models of thescattering of diffuse Galactic light (DGL) underestimate the b(\lambda) valuesby a factor of 2. This could be reconciled by deficiency in UV photons in theISRF or by a moderate increase in dust albedo. Our b(\lambda) spectrum favors acontribution from extended red emission (ERE) to the diffuse optical light;b(\lambda) rises from B to V faster than the models, seems to peak around 6000\AA, and decreases towards long wavelengths. Such a characteristic is expectedfrom the models in which the DGL is combined with ERE.

Diffuse Galactic Light in the Field of the Translucent High Galactic Latitude Cloud MBM32