Open AccessStar formation in massive protoclusters in the Monoceros OB1 dark cloud
Author(s) -
WolfChase G.,
MoriartySchieven G.,
Fich M.,
Barsony M.
Publication year - 2003
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2003.06863.x
Subject(s) - physics , astrophysics , protostar , outflow , flux (metallurgy) , astronomy , star formation , james clerk maxwell telescope , point source , luminosity , infrared , galaxy , materials science , meteorology , optics , metallurgy
We present far‐infrared, submillimetre and millimetre observations of bright IRAS sources and outflows that are associated with massive CS clumps in the Monoceros OB1 dark cloud. Individual star‐forming cores are identified within each clump. We show that combining submillimetre maps, obtained with SCUBA on the James Clerk Maxwell Telescope, with HIRES‐processed and modelled IRAS data is a powerful technique that can be used to place better limits on individual source contributions to the far‐infrared flux in clustered regions. Three previously categorized ‘Class I objects’ are shown to consist of multiple sources in different evolutionary stages. In each case, the IRAS point source dominates the flux at 12 and 25 μm. In two cases, the IRAS point source is not evident at submillimetre wavelengths. The submillimetre sources contribute significantly to the 60‐ and 100‐μm fluxes, dominating the flux in the 100‐μm waveband. Using fluxes derived from our technique, we present the spectral energy distribution and physical parameters for an intermediate‐mass Class 0 object in one of the regions. Our new CO J = 2 → 1 outflow maps of the three regions studied indicate complex morphology suggestive of multiple driving sources. We discuss the possible implications of our results for published correlations between outflow momentum deposition rates and ‘source’ luminosities, and for using these derived properties to estimate the ratio of mass ejection rates to mass accretion rates on to protostars.