Interstellar Polarization in M31
  The wavelength dependence of interstellar polarization due to dust in M31 has been observed along four sightlines. Only one sightline had been measured previously.The globular clusters, S78, S150, S233 and Baade 327 were used as point sources to probe the interstellar dust in M31. The Serkowski law produces good fits for all the sightlines although the relationship between K and lambda(max) may be different from that found in the Galaxy. The results of this study imply that the slope K/lambda(max) may be significantly larger in M31. The Serkowski curves are significantly narrower than those of the same lambda(max) in the Galaxy and may require extreme modifications to the size distributions of silicate particles. The fits for the four sightlines reveal values of lambda(max) ranging from 4800 to 5500 A. These are consistent with average values of lambda(max) measured in the Galaxy and the Magellanic Clouds. The range measured for M31 corresponds to R(V) values of 2.7 to 3.1. The range in R(V) seen in the Galaxy is 2.5 to 5.5 implying, for this small sample, that the average size ofinterstellar grains in M31 is typically smaller than that seen for Galactic grains if the nature of the grains is the same. Also, the polarization efficiency for these sightlines is large although some bias is expected since sightlines known to have significant interstellar polarization were selected for the sample. 
Geoffrey C. Clayton, Michael J. Wolff, Karl D. Gordon, Paul S. Smith,   Kenneth H. Nordsieck, and Brian L. Babler