Outflow activities in the young high-mass stellar object G23.44-0.18

• Published in: arXiv.org 2011-07
• Main Authors: Jeremy Zhiyuan Ren, Liu, Tie, Wu, Yuefang, Li, Lixin
• Format: Article
• Language: English
• Subjects: Abundance; Astrochemistry; Collimation; Continuum radiation; Ejection; Emission; Inspection; Massive stars; Molecular gases; Organic chemistry; Outflow; Star formation; Stellar evolution; Tracers
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.1107.1542

We present an observational study towards the young high-mass star forming region G23.44-0.18 using the Submillimeter Array. Two massive, radio-quiet dusty cores MM1 and MM2 are observed in 1.3 mm continuum emission and dense molecular gas tracers including thermal CH\(_3\)OH, CH\(_3\)CN, HNCO, SO, and OCS lines. The \(^{12}\)CO (2--1) line reveals a strong bipolar outflow originated from MM2. The outflow consists of a low-velocity component with wide-angle quasi-parabolic shape and a more compact and collimated high-velocity component. The overall geometry resembles the outflow system observed in the low-mass protostar which has a jet-driven fast flow and entrained gas shell. The outflow has a dynamical age of \(6\times10^3\) years and a mass ejection rate \(\sim10^{-3} M_{\odot}\) year\(^{-1}\). A prominent shock emission in the outflow is observed in SO and OCS, and also detected in CH\(_3\)OH and HNCO. We investigated the chemistry of MM1, MM2 and the shocked region. The dense core MM2 have molecular abundances of 3 to 4 times higher than those in MM1. The abundance excess, we suggest, can be a net effect of the stellar evolution and embedded shocks in MM2 that calls for further inspection.