Submillimeter Array Observations of NGC 2264-C: Molecular Outflows and Driving Sources

TL;DR

This study uses high-resolution submillimeter observations to identify and analyze molecular outflows and their driving sources in the star-forming region NGC 2264-C, revealing new cores and outflow characteristics.

Contribution

First high-resolution SiO observations of NGC 2264-C, identifying two collimated outflows driven by the youngest cores, and revealing an evolutionary spread among cores in the region.

Findings

Detected two high-velocity bipolar outflows driven by the youngest cores.

Identified ten 1.3mm continuum peaks, including four new detections.

Observed no outflow emission from the most evolved IR-bright source.

Abstract

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.