(Sub)mm continuum mapping of NGC 6334 I & I(N). A cobweb of filaments and protostars

Details (Sub)mm continuum mapping of NGC 6334 I & I(N). A cobweb of filaments and protostars (Sub)mm continuum mapping of NGC 6334 I & I(N). A cobweb of filaments and protostars

Jun 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26a...358..242s&link_type=abstract

Astronomy and Astrophysics, v.358, p.242-256 (2000)

Astronomy and Astrophysics

Astrophysics

57

Ism: Dust, Extinction, Ism: H Ii Regions, Ism: Jets And Outflows, Ism: Individual Objects: Ngc 6334 I

Scientific paper

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 \cite{Gezari82}). The maps at 1.1 mm and 800 {mu m} cover the whole northern part of the NGC 6334 complex ({ ~ } 5{'} x 8{'}), while the coverage is more limited at 450 {mu m} and 350 {mu m} 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, T_d >= 100 K, and we derive a total mass (gas + dust) of ~ 200 Msun. We resolve Gezari's cold source into a compact (deconvolved FWHM ~ 10 {''}) dust source, which appears optically thick even at 1.1 mm. I(N) is embedded in a dense cloud core, ~ 2.5{'} x 1.5 {'}, with a mass of ~ 2200 Msun. I(N) is clearly a high-mass Class 0 object. It emits a large fraction of its luminosity in the sub-mm (Lbol ~ 1.7 104 Lsun), it drives a molecular outflow and coincides with a CH_3OH maser, suggesting that I(N) has already formed a hot accretion disk. We derive a total mass of 250-400 Msun, corresponding to an average gas density 1.6-2.6 107 cm-3 and a line of sight visual extinction of >= 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 ~ 15 {''}-20 {''}. It breaks up into dense condensations with a separation of 3-4 times the width of the filament.

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