HH 80 N前恒星形成核中含氮分子种类的干涉测量观测
Interferometric observations of nitrogen-bearing molecular species in the star-forming core ahead of HH 80N
摘要：
我们目前的VLA NH 3和PdBI NH 2D和H13 NC的恒星形成的核心提前HH 80 N，光学模糊的赫比格-哈罗对象HH 80/81的北部对应的观测。主要目标是确定高密度区域的核心（$n\lesssim 10^5$ cm $^{-3}$）的运动学信息，错过了在以前的工作，由于所观察到的物种（如CS）的耗尽。得到的地图显示不同的运动学签名之间的东部和西部的核心部分，这表明可能的动力学相互作用的核心HH 80/81/80 N流出。这些物种的位置-速度（PV）图的分析排除了先前的解释，即具有$6\times 10^4$ AU半径的分子环状结构，由CS落在核心（IRS 1）中发现的中央原恒星上追踪。相对于IRS 1核心的中心部分，氘代度高，在东部，尘埃凝结（SE）的位置。NH3的氘代趋势表明SE处于星前演化阶段，比IRS 1更早。由于SE是最接近HH 80 N/81/80 N外流的凝结，在外流-核动力学相互作用的情况下，它应该首先受到扰动，并且是核中最演化的凝结。因此，SE和IRS 1的演化序列使得IRS 1上的外流触发恒星形成不太可能。
英文摘要：
We present VLA NH3 and PdBI NH2D and H13NC observations of the star forming core ahead of HH 80N, the optically obscured northern counterpart of the Herbig-Haro objects HH 80/81. The main goal is to determine the kinematical information of the high density regions of the core ($n\lesssim 10^5$ cm$^{-3}$), missed in previous works due to the depletion of the species observed (e.g. CS). The obtained maps show different kinematical signatures between the eastern and western parts of the core, suggesting a possible dynamical interaction of the core with the HH 80/81/80N outflow. The analysis of the Position-Velocity (PV) plots of these species rules out a previous interpretation of having a molecular ring-like structure of $6\times 10^4$ AU of radius traced by CS infalling onto a central protostar found in the core (IRS1). High degree of deuteration, with respect to the central part of the core harboring IRS1, is derived in the eastern part, where a dust condensation (SE) is located. This deuteration trend of NH3 suggests that SE is in a prestellar evolutionary stage, earlier than that of the IRS1. Since SE is the closest condensation to the HH 80N/81/80N outflow, in case of having outflow-core dynamical interaction, it should be perturbed first and be the most evolved condensation in the core. Therefore, the derived evolutionary sequence for SE and IRS1 makes the outflow triggered star formation on IRS1 unlikely.
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