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A. Noriega-Crespo (SIRTF Science Center, California Institute of Technology), P. M. Garnavich (University of Notre Dame)
A key ingredient to understand the dynamics of stellar outflows is their proper motion. We have used optical images in the [SII] emission at 6717/31 A and the red Digitized Palomar Sky Survey plates to determine the proper motion of HH 7-11 system and the optical knot of Cep E (HH 377). Our measurements span nearly 50 years, although their main limitation is the relatively low angular resolution of the early images and the evolving morphology of the objects themselves. HH 377 has a proper motion of 0.031±0.003 arcsec/yr with a PA = 206 arcdeg, i.e. moving away from IRAS 230111+63, that at a distance of 730 pc, corresponds to a tangential velocity of 107±14 km/s. The proper motions of HH 7, 8, 9, 10 and 11 range from 0.038±0.006 (HH 11) to 0.015±0.009 (HH 9) arcsec/yr, and the flow is moving away from SVS 13 with a mean PA~ 136 arcdeg. At a distance of 330 pc these motions correspond to tangential velocities of ~60 - 20 km/s, i.e. comparable to the original values obtained by Herbig & Jones (1983).