Astrophys. J., 509, 299-308 (1998/December-2)
350 micron continuum imaging of the Orion A molecular cloud with the submillimeter high angular resolution camera.
LIS D.C., SERABYN E., KEENE J., DOWELL C.D., BENFORD D.J., PHILLIPS T.G., HUNTER T.R. and WANG N.
Abstract (from CDS):
We have used the Submillimeter High Angular Resolution Camera (SHARC) bolometer camera at the Caltech Submillimeter Observatory to map the distribution of the broadband 350 µm continuum emission toward the Orion A molecular cloud. A comparison of the 350 µm flux densities in OMC-1 with previous 1100 µm measurements indicates a strong spatial variation of the grain emissivity exponent, β. The lowest value of the exponent (β ≃ 1.75) is found toward the Orion Bar photon-dominated region (PDR), while the highest value (β ≃ 2.5) is found toward the Orion Ridge north of IRc2. This variation is consistent with the destruction of grain mantles by the UV photons from the Trapezium cluster. The observed spatial variation of β in OMC-1 suggests that the long-wavelength grain emissivity may also vary significantly in GMC cores on small linear scales (≲0.5 pc), affecting H2 column density and mass estimates. The 350 µm continuum emission in the Orion Bar region correlates well with the CO (6-5) peak brightness temperature and is shifted by ∼10" from the molecular component traced by the 13CO (6-5) emission. This indicates that the 350 µm dust emission in this region originates predominantly in the outer high-temperature PDR layers. Several filamentary structures previously detected in molecular tracers are also seen in our map at flux levels comparable to those seen in the Bar. Over 30 compact dust sources are detected in the OMC-2 and OMC-3 clouds, including a dozen sources not previously known. The average 350/1300 µm flux ratio based on our data and previous observations of this region (63 ±19) indicates low dust temperatures (17±4 K, assuming β = 2) for most of the sources. The brightest 350 µm source in OMC-3 has a low 350/1300 µm ratio (∼23), indicating a very low dust temperature (∼10 K), or a significant opacity at 350 µm (∼2.5). This source appears to be a deeply embedded and cold young protostar. A comparison of the mass estimate for the OMC-2/3 filament based on the 350 µm continuum emission with previous C18O mass estimates indicates a relatively high grain emissivity, Q(350) = 4x10–4, in this region.
ISM: Dust, Extinction - Infrared: ISM: Continuum - ISM: Clouds - ISM: individual (OMC-1, OMC-2) - ISM: Individual: Alphanumeric: OMC-3 - Stars: Formation
Table 1: [LSK98] NN (Nos 1-33).
T.1: MMS = [CRW97] OMC-3 MMS, FIR = [MWZ90] OMC-2 FIR
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