Star formation in NGC 6334 I and I(N)

The northern section of the molecular cloud complex NGC 6334 has been mappe d in the CO and CS spectral line emission and in continuum emission at a wa velength of 1300 mu m. Our observations highlight the two dominant sources, I and I(N), and a host of weaker sources. NGC 6334 I is associated with a cometary ultracompact H II region and a hot, compact core less than or equa l to 10 arcsec in size, Mid-infrared and CH3OH observations indicate that i t is also associated with at least two protostellar sources, each of which may drive a molecular outflow. For region I we confirm the extreme high-vel ocity outflow first discovered by Bachiller & Cernicharo and find that it i s very energetic with a mechanical luminosity of 390 L.. A dynamical age fo r the outflow is similar to 3000 yr, We also find a weaker outflow originat ing from the vicinity of NGC 6334 I, In CO and CS this outflow is quite pro minent to the north-west, but much less so on the eastern side of I, where there is very little molecular gas, Spectral survey data show a molecular e nvironment at position I which is rich in methanol, methyl formate and dime thyl ether, with lines ranging in energy up to 900 K above the ground state , NGC 6334 I(N) is more dense than I, but cooler, and has none of the high- excitation lines observed toward I. I(N) also has an associated outflow but it is less energetic than the outflow from I. The fully sampled continuum map shows a network of filaments, voids and cores, many of which are likely to be sites of star formation. A striking feature is a narrow, linear ridg e which defines the western boundary. It is unclear if there is a connectio n between this filament and the many potential sites of star formation, or if the filament existed prior to the star formation activity.