Spectroscopically resolved far-IR observations of the massive star-forming region G5.89--0.39
Spectroscopically resolved far-IR observations of the massive star-forming region G5.89--0.39
复制标题
大质量恒星形成区域 G5.89--0.39 的光谱分辨远红外观测
DOI：
--
复制
发表时间：
2015
期刊：
影响因子：
--
通讯作者：
H. Richter
中科院分区：
文献类型：
--
作者：
S. Leurini;F. Wyrowski;H. Wiesemeyer;A. Gusdorf;R. Güsten;K. Menten;M. Gerin;F. Levrier;H. Hübers;K. Jacobs;O. Ricken;H. Richter
63微米的[OI]精细结构线是天体物理各个领域的重要诊断工具。然而，我们对这条谱线的了解依赖于低光谱分辨率的观测，并且对恒星形成区(SFR)复杂环境中每个分量(PDR、JET)的真实贡献知之甚少。我们研究了喷流和PDR发射以及对[OI]63微米谱线的吸收对超致密H{sc II}区G5.89-0.39的贡献，并通过[OI]、[CII]、CO、OH和H2O研究了它在不同速度区的远红外谱线光度。我们将[OI]中的G5.89-0.39和CO(16-15)中的G5.89-0.39与Sofia上的伟大接收器进行了映射。我们在OH^2pi{3/2}，J=5/2OJ=3/2和^2pi{1/2}，J=3/2OJ=1/2谱线中观察到了源的中心位置。这些数据与APEX CO(6-5)和CO(7-6)和高保真地图以及在[CII]、H2O和HF中的单点观测相补充。G5.89-0.39中的[OI]光谱受到来自包层和视线沿线不同云团的吸收的严重污染。仅在HV处检测到排放，这显然与极HV低J CO追踪到的南北向紧凑外流有关。从[OI]得到的质量损失率和能量学与来自CO的估计很好地一致，这表明G5.89-0.39中的分子外流是由[OI]中看到的喷流系统驱动的。在HV下，G5.89-0.39的远红外谱线光度主要由[OI]主导；在此速度区，第二冷却剂是CO，而[CII]、OH和H2O对流出冷却的贡献较小。我们的研究表明，[OI]63微米的光谱分辨数据对于将这条谱线用作SFRS诊断的重要性。尽管到目前为止这是不可能的，但索非亚号上的伟大接收器最近已经开启了对这条线路进行详细研究的可能性，以调查其探测不同环境的潜力。
The fine-structure line of [OI] at 63micron is an important diagnostic tool in different fields of astrophysics. However, our knowledge of this line relies on observations with low spectral resolution, and the real contribution of each component (PDR, jet) in complex environment of star-forming regions (SFRs) is poorly understood. We investigate the contribution of jet and PDR emission, and of absorption to the [OI]63micron line towards the ultra-compact H{sc ii} region G5.89--0.39 and study its far-IR line luminosity in different velocity regimes through [OI], [CII], CO, OH, and H2O. We mapped G5.89--0.39 in [OI] and in CO(16--15) with the GREAT receiver onboard SOFIA. We observed the central position of the source in the OH^2Pi_{3/2}, J=5/2 oJ=3/2 and ^2Pi_{1/2}, J=3/2 oJ=1/2 lines. These data were complemented with APEX CO(6-5) and CO(7-6) and HIFI maps and single-pointing observations in [CII], H2O, and HF. The [OI] spectra in G5.89--0.39 are severely contaminated by absorptions from the envelope and from different clouds along the line of sight. Emission is detected only at HV, clearly associated with the compact north-south outflows traced by extremely HV low-J CO. The mass-loss rate and energetics of derived from [OI] agree well with estimates from CO, suggesting that the molecular outflows in G5.89--0.39 are driven by the jet system seen in [OI]. The far-IR line luminosity of G5.89--0.39 is dominated by [OI] at HV; the second coolant in this velocity regime is CO, while [CII], OH and H2O are minor contributors to the cooling in the outflow. Our study shows the importance of spectroscopically resolved data of [OI]63micron for using this line as diagnostic of SFRs. While this was not possible until now, the GREAT receiver onboard SOFIA has recently opened the possibility of detailed studies of this line to investigate its potential for probing different environments.
GREAT/SOFIA 大气校准
影响因子：
6.5
作者：
Stutzki;Güsten;Requena- Torres;Wiesemeyer
通讯作者：
Wiesemeyer