Mon. Not. R. Astron. Soc., 316, 152-164 (2000/July-3)
Star formation in NGC 6334 I and I(N).
McCUTCHEON W.H., SANDELL G., MATTHEWS H.E., KUIPER T.B.H., SUTTON E.C., DANCHI W.C. and SATO T.
Abstract (from CDS):
The northern section of the molecular cloud complex NGC 6334 has been mapped in the CO and CS spectral line emission and in continuum emission at a wavelength of 1300µm. Our observations highlight the two dominant sources, I and I(N), and a host of weaker sources. NGC6334 I is associated with a cometary ultracompact Hii region and a hot, compact core ≤10arcsec in size. Mid-infrared and CH3OH observations indicate that it 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-velocity outflow first discovered by Bachiller & Cernicharo and find that it is very energetic with a mechanical luminosity of 390L☉. A dynamical age for the outflow is ∼3000yr. We also find a weaker outflow originating from the vicinity of NGC6334 I. In CO and CS this outflow is quite prominent 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 environment at position I which is rich in methanol, methyl formate and dimethyl ether, with lines ranging in energy up to 900K 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 ridge which defines the western boundary. It is unclear if there is a connection between this filament and the many potential sites of star formation, or if the filament existed prior to the star formation activity.
The Royal Astronomical Society
stars: formation - ISM: individual: NGC 6334 - ISM: jets and outflows - ISM: molecules - radio continuum: ISM - radio lines: ISM
Fig.8: SM1 to 8 = [S2000e] SM1 to 8.
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