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Session 105 - Molecular Cores and Protostars.
Display session, Thursday, January 16
Metropolitan Ballroom,
We have observed the molecular cloud NGC 7129 in several emission lines of CO in order to assess the effects of recent and ongoing star formation on the cloud core. The cloud contains a very young star cluster surrounded by a sharply-bounded molecular cavity, as well as an energetic molecular outflow centered on or near the Be star LkH\alpha234 (Edwards amp; Snell, 1983, ApJ, 270, 605; Mitchell amp; Matthews, 1994, ApJ, 423, L55). With new, high resolution data in CO J=3-2, \rm^13CO J=3-2, CO J=2-1, and C\rm^18O J=3-2, we have re-assessed the energetics and structure of the molecular flow. We find that the blueshifted lobe of the flow consists of an extended molecular fragment which has been sculpted into a bow shock-like, swept back, shape. This molecular fragment contains two high velocity HH objects, GGD 32 and HH 103, apparently embedded within it. We have found a curious molecular outflow centred on an embedded submillimetre source. The blueshifted and redshifted molecular lobes of this second flow are almost identical in shape, yet are orthogonal rather than aligned. In the ridge between the molecular cavity and the molecular cloud, the \rm^13CO map shows several molecular clumps, including one associated with LkH\alpha234. We suggest LkH\alpha234 was recently (0.5 million years ago) formed in swept-up gas, thus providing an example of triggered star formation. The remaining clumps may collapse to form stars in the near future.
