Submillimeter Array Observations of NGC 2264-C: Molecular Outflows and
  Driving Sources
  We present 1.3mm Submillimeter Array (SMA) observations at
$\sim$3$^{\prime\prime}$ resolution towards the brightest section of the
intermediate/massive star forming cluster NGC 2264-C. The millimetre continuum
emission reveals ten 1.3mm continuum peaks, of which four are new detections.
The observed frequency range includes the known molecular jet/outflow tracer
SiO (5-4), thus providing the first high resolution observations of SiO towards
NGC 2264-C. We also detect molecular lines of twelve additional species towards
this region, including CH$_3$CN, CH$_3$OH, SO, H$_2$CO, DCN, HC$_3$N, and
$^{12}$CO. The SiO (5-4) emission reveals the presence of two collimated, high
velocity (up to 30kms$^{-1}$ with respect to the systemic velocity) bi-polar
outflows in NGC 2264-C. In addition, the outflows are traced by emission from
$^{12}$CO, SO, H$_2$CO, and CH$_3$OH. We find an evolutionary spread between
cores residing in the same parent cloud. The two unambiguous outflows are
driven by the brightest mm continuum cores, which are IR-dark, molecular line
weak, and likely the youngest cores in the region. Furthermore, towards the RMS
source AFGL 989-IRS1, the IR-bright and most evolved source in NGC 2264-C, we
observe no molecular outflow emission. A molecular line rich ridge feature,
with no obvious directly associated continuum source, lies on the edge of a low
density cavity and may be formed from a wind driven by AFGL 989-IRS1. In
addition, 229GHz class I maser emission is detected towards this feature.
