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Astron. Astrophys. 358, 242-256 (2000)

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(Sub)mm continuum mapping of NGC 6334 I & I(N)

A cobweb of filaments and protostars

G. Sandell

National Radio Astronomy Observatory *, P.O. Box 2, Green Bank, WV 24944, USA (gsandell@nrao.edu)

Received 7 June 1999 / Accepted 16 March 2000


We present high resolution (sub)mm continuum maps obtained with the bolometer UKT14 on the JCMT of the high mass star formation complex NGC 6334 I and I(N), the latter also known as Gezari's cold source (Gezari 1982). The maps at 1.1 mm and 800 µm cover the whole northern part of the NGC 6334 complex ([FORMULA][FORMULA] 8´), while the coverage is more limited at 450 µm and 350 µm and centered on NGC 6334 I(N).

The strongest dust emission at all wavelengths originates from a compact source near or coincident with the Ultracompact HII - region NGC 6334 F and the FIR-source and hot core region NGC 6334 I. The dust in NGC 6334 I is hot, Td [FORMULA] 100 K, and we derive a total mass (gas + dust) of [FORMULA] 200 [FORMULA]. We resolve Gezari's cold source into a compact (deconvolved FWHM [FORMULA] 10 ") dust source, which appears optically thick even at 1.1 mm. I(N) is embedded in a dense cloud core, [FORMULA] 2.5´ [FORMULA] 1.5 ´, with a mass of [FORMULA] 2200 [FORMULA]. I(N) is clearly a high-mass Class 0 object . It emits a large fraction of its luminosity in the sub-mm (Lbol [FORMULA] 1.7 104 [FORMULA]), it drives a molecular outflow and coincides with a CH3OH maser, suggesting that I(N) has already formed a hot accretion disk. We derive a total mass of 250-400 [FORMULA], corresponding to an average gas density 1.6-2.6 107 cm-3 and a line of sight visual extinction of [FORMULA] 2000m, rendering it impossible to detect I(N) even in the thermal or mid-IR.

We also find eight additional compact sub-mm sources. Some of these are probable high-to-intermediate mass protostars, some may be massive cold starless cloud cores that eventually will collapse to form stars. Our sub-mm maps also show a remarkable narrow, lumpy, linear filament, which has no optical or near-IR counterpart. This filament bounds the dust emission to the west and is at least 7´ (3.5 pc) in length with a width of [FORMULA] 15 "-20 ". It breaks up into dense condensations with a separation of 3-4 times the width of the filament.

Key words: ISM: dust, extinction – ISM: H ii regions – ISM: jets and outflows – ISM: individual objects: NGC 6334 I

* The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.

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© European Southern Observatory (ESO) 2000

Online publication: June 26, 2000