THE S140 CORE - APERTURE SYNTHESIS HCO+ AND SO OBSERVATIONS

We present 5''-8'' resolution images of the S140 region in the HCO+ J = 1-0 and SO J(K) = 2(2)-1(1) lines. The maps encompass the well-known S140 dense core, bipolar outflow, and photodissociation region. Unlik e previous aperture synthesis maps of molecular tracers in this source , the HCO+ images, constructed from a combination of Hat Creek millime ter-array data and NRAO 12 m telescope data, show significant structur e in the dense gas associated with the embedded cluster. The brightest emission in the HCO+ maps arises from the periphery of the bipolar fl ow, suggesting the limb-brightened edges of a cavity with an apex at I RS 1. Although HCO+ abundance variations might be expected as a result of shock processing, comparisons with CO isotope data indicate no sig nificant differences between the ambient material and the low-velocity outflow (< 10 km s-1). The SO maps provide evidence for variations of at least an order of magnitude in SO column density in the quiescent gas on 10'' scales, with localized enhancements to the north and west of the embedded cluster. SO emission was not detected at velocities ch aracteristic of the outflow. No compact 89 GHz continuum emission was detected from the IRS sources to a 3 sigma limit of 60 mJy, consistent with previous measurements. In an appendix we discuss the effect of ' 'holes'' in the (u, v) sampling on synthesis imaging extended molecula r emission. We derive expressions to quantify the effects of holes for Gaussian and uniform disk source distributions. We note that while sy nthesis observations are often said to be ''sensitive'' to structures on scales lambda/S(min), where S(min) is the length of the shortest ba seline, the central brightness recovered from a Gaussian distribution characterized by FWHM = lambda/S(min) is only about 3%. If the S140 HC O+ data are typical of molecular cloud sources, then the central hole gives rise to more significant image distortions than many scattered o uter holes.