We present high spatial resolution spectroscopic observations of the proplyd 167-317 ( LV2 ) near the Trapezium cluster in the Orion nebula , obtained during the System Verification run of the Gemini Multi Object Spectrograph ( GMOS ) Integral Field Unit ( IFU ) at the Gemini South Observatory .
We have detected 38 forbidden and permitted emission lines associated with the proplyd and its redshifted jet .
We have been able to detect three velocity components in the profiles of some of these lines : a peak with a 28-33 km s ^ { -1 } systemic velocity that is associated with the photoevaporated proplyd flow , a highly redshifted component associated with a previously reported jet ( which has receding velocities of about 80-120 km s ^ { -1 } with respect to the systemic velocity and is spatially distributed to the southeast of the proplyd ) and a less obvious , approaching structure , which may possibly be associated with a faint counter-jet with systemic velocity of ( -75 \pm 15 ) km s ^ { -1 } .
We find evidences that the redshifted jet has a variable velocity , with slow fluctuations as a function of the distance from the proplyd .
We present several background subtracted , spatially distributed emission line maps and we use this information to obtain the dynamical characteristics over the observed field .
Using a simple model and with the extinction corrected H \alpha fluxes , we estimate the mass loss rate for both the proplyd photoevaporated flow and the redshifted microjet , obtaining \dot { M } _ { proplyd } = ( 6.2 \pm 0.6 ) \times 10 ^ { -7 } M _ { \sun } year ^ { -1 } and \dot { M } _ { jet } = ( 2.0 \pm 0.7 ) \times 10 ^ { -8 } M _ { \sun } year ^ { -1 } , respectively .