Observational 2D model of H-2 emission from bow shock in the Orion Molecular Cloud

Aims. We present a new method for reproducing high spatial resolution observations of bow shocks by using 1D plane parallel shock models. As an example we analyse one bow shock located in the Orion Molecular Cloud (OMC1). Methods. We use high spatial resolution near-infrared observations of H-2 rovibrational emission to constrain shock models. These observations have been made at the ESO-VLT using a combination of the NACO adaptive optics system and infrared camera array and the Fabry-Perot interferometer. Three rovibrational H-2 lines have been observed: v = 1-0 S(1) Lit 2.12 mu m, v = 1-0 S(0) at 2.23 mu m and v = 2-1 S(1) at 2.25 mu m. The spatial resolution is 0.'' 15 similar to 70 AU. We analyse a single bow shock located in our field, featuring a very well defined morphology and high brightness. Results. One dimensional shock models are combined to estimate the physical properties of pre-shock density, shock velocity and transverse magnetic field strength along the bow shock. We find that the pre-shock density is constant at similar to 5 x 10(5) cm(-3) and shock velocities lie between similar to 35 km s(-1) in the wings of the shock and similar to 50 km s(-1) at the apex. We also find that the transverse magnetic field is stronger at the apex and weaker further down the wings varying between similar to 2 and 4 mGauss. Predictions of shock velocity and magnetic field strength agree with previous independent observations.