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We studied the ISM distribution in and around the star forming cloud L1251with optical star counts. A careful calculation with a maximum likelihood basedstatistical approach resulted in B,V,R,I extinction distributions from the starcount maps. A distance of 330+/-30 pc was derived. The extinction maps revealedan elongated dense cloud with a bow shock at its eastern side. We estimated aMach number of M~2 for the bow shock. A variation of the apparent dustproperties is detected, i.e. the Rv=Av/E{B-V} total to selective extinctionratio varies from 3 to 5.5, peaking at the densest part of L1251. The spatialstructure of the head of L1251 is well modelled with a Schuster-sphere (i.e.n=5 polytropic sphere). The observed radial distribution of mass fits the modelwith high accuracy out to 2.5pc distance from the assumed center. Unexpectedly,the distribution of NH3 1.3 cm line widths is also well matched by the Schustersolution even in the tail of the cloud. Since the elongated head-tail structureof L1251 is far from the spherical symmetry the good fit of the linewidths inthe tail makes it reasonable to assume that the present cloud structure hasbeen formed by isothermal contraction.Comment: 9 pages, 9 figures, accepted in Astronomy & Astrophysic

Star count analysis of the interstellar matter in the region of L1251