Grain Growth in the Dark Cloud L1251

Abstract

We have performed optical imaging observations of the dark cloud L1251 at multiple wavelengths, B, V, R, and I, using the 105 cm Schmidt telescope at the Kiso Observatory, Japan. The cloud has a cometary shape with a dense "head" showing star formation activity and a relatively diffuse "tail" without any signs of star formation. We derived extinction maps of A_B and A_V with a star count method, and also revealed the color excess (E_{B-V}, E_{V-R}, and E_{V-I}) distributions. On the basis of the color excess measurements we derived the distribution of the ratio of total to selective extinction R_V over the cloud using an empirical relation between R_V and A_lambda/A_V reported by Cardelli et al. In the tail of the cloud, R_V has a uniform value of ~3.2, close to that often found in the diffuse interstellar medium (~3.1), while higher values of R_V=4-6 are found in the dense head. Since R_V is closely related to the size of dust grains, the high R_V-values are most likely to represent the growth of dust grains in the dense star-forming head of the cloud.