HIGH-RESOLUTION, FAR-INFRARED OBSERVATIONS OF NGC-2071

High-resolution scans of infrared sources in the NGC 2071 region show that the source is resolved at both 50 μm (size∼12″) and 100 μm (size ∼16″). There is no evidence that the far-infrared emission is elongated, either parallel or perpendicular to the outflow. Models of the source with a spherical radiative transport code indicate a total source luminosity of 520 L⊙, an optical depth at 100 μm of 0.2, and a mass of 1.2-10 M⊙ inside a region of diameter 5900 AU. The scans are best fitted with a density distribution of the form n(r) = ni(r/ri)-α, with an inner radius, ri = 5″ (2000 AU). The other parameters depend somewhat on the choice of dust grain opacities: for the dust opacities of Mathis, Mezger, and Panagia, the best fit is obtained for α = 1.5 and ni = 7 × 105 cm-3; for the dust opacities of Draine and Lee, the best fit is given for α = 2.0 and ni = 8 × 106 cm-3. These values for α are in reasonable agreement with theoretical predictions of infalling envelopes around protostars. The values for n, are somewhat higher than would be predicted by a simple application of theory, but somewhat lower than implied by analysis of molecular line data.