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LDN 1157, is one of the several clouds situated in the cloud complex, LDN1147/1158, represents a coma-shaped morphology with a well-collimated bipolaroutflow emanating from a Class 0 protostar, LDN 1157-mm. The main goals of thiswork are (a) to map the inter-cloud magnetic field (ICMF) geometry of theregion surrounding LDN 1157 to investigate its relationship with the cloudmorphology, with the outflow direction and with the core magnetic field (CMF)geometry inferred from the mm- and sub-mm polarization results from theliterature, and (b) to investigate the kinematic structure of the cloud. Wecarried out R-band polarization observations of the stars projected on thecloud to map the pc-scale magnetic field geometry and made spectroscopicobservations of the entire cloud in 12CO, C18O and N2H+ (J=1-0) lines toinvestigate its kinematic structure. We obtained a distance of 340$\pm$3 pc tothe LDN 1147/1158, complex based on the Gaia DR2 parallaxes and proper motionvalues of the three YSOs associated with the complex. A single filament of$\sim1.2$ pc in length and $\sim0.09$ pc in width is found to run all along thecoma-shaped cloud. Based on the relationships between the ICMF, CMF, filamentorientations, outflow direction, and the presence of an hour-glass morphologyof the magnetic field, it is likely that the magnetic field had played animportant role in the star formation process in LDN 1157. Combining the propermotions of the YSOs and the radial velocity of LDN 1147/1158 and anothercomplex LDN 1172/1174 which is situated $\sim2$\dgr~east of it, we found thatboth the complexes are moving collectively toward the Galactic plane. Thefilamentary morphology of the east-west segment of LDN 1157 may have formed asa result of mass lost by ablation due to the interaction of the moving cloudwith the ambient interstellar medium.

Distance, magnetic field and kinematics of a filamentary cloud LDN 1157