Spatial Structure of the High Excitation Herbig-Haro Objects HH 80/81

Details Spatial Structure of the High Excitation Herbig-Haro Objects HH 80/81 Spatial Structure of the High Excitation Herbig-Haro Objects HH 80/81

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995hst..prop.6128h&link_type=abstract

HST Proposal ID #6128

Physics

Hst Proposal Id #6128 Interstellar Medium

Scientific paper

Herbig-Haro outflows have in recent years been the subject of intense study, and it is now clear that they are an integral part of the star formation process and can provide insight into the very earliest stages of stellar evolution. They are also an excellent laboratory for the investigation of the physics of interstellar shock waves. We propose to use HST with the PC CCD of WFPC2 to study HH 80 and HH 81, the twin working surfaces at the terminus of a powerful jet driven by a luminous young star. As well as being the brightest known HH objects, HH 80 and HH 81 are unique in having a high excitation emission zone of considerable spatial extent. Because of their large, ~300km/s shock velocity and only modest, ~50 cm^-3 preshock density, the postshock cooling zone in these objects should be easily resolvable with HST. Narrow band filters will be used to obtain images in H Alpha, a high excitation line ([O III] 5007), and a low excitation line ([S II] 6717/31). We expect the emission regions for these species to be displaced by up to 0.2" in HH 80/81 offering the first opportunity to directly observe the stratification of high and low excitation/ionization lines in HH objects. The HH 80/81 system is the best known laboratory for performing this experiment. The high spatial resolution of HST is mandatory for its success.

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