标题： 猎户座分子云中空间和速度结构的观测 显示英文标题

标题： Observations of spatial and velocity structure in the Orion Molecular Cloud

摘要： 报告了在猎户分子云OMC1中使用加拿大-法国-夏威夷望远镜上的GriF仪器观测到的H2红外发射在2.121微米处S(1)v=1-0线的情况。GriF结合了自适应光学和法布里-珀罗干涉仪，提供了0.15"至0.18"的空间分辨率以及高达1 km/s的速度分辨能力。 由于GriF数据具有高空间和速度分辨率，可以在OMC1中识别出193个明亮的H2发射区域。这些特征的一般特性通过径向速度、亮度和最大速度与亮度的空间位移来描述，后者用于确定天空平面上流的方向。 发现速度和明亮H2发射之间存在强烈的空间相关性，并用以识别许多特征为冲击波。重要结果包括：(i) 兴奋气体的速度显示，在BN-IRc2和Peak 1南部以及Peak 2西部存在一个区域，其中有一个强大的蓝移喷流，平均速度为-18公里/秒。这被证明是源I（一颗非常年轻的O型星）在无线电波段中识别出的喷流的近红外对应物。(ii) 在Peak 1中有一条弱速度特征（<5公里/秒），可能通过爆炸事件与OMC1西北部的快速移动的手指（或子弹）共享共同起源，位于BN-IRc2区域。(iii) 部分流很可能代表低质量恒星形成的地点，几个区域显示出多个喷流，可能表明OMC1内有多颗恒星形成。GriF数据的高空间和速度分辨率比以往更详细地展示了这些和其他特征。 显示英文摘要

摘要： Observations are reported of H2 IR emission in the S(1) v=1-0 line at 2.121 microns in the Orion Molecular Cloud, OMC1, using the GriF instrument on the Canada-France-Hawaii Telescope. GriF is a combination of adaptive optics and Fabry-Perot interferometry, yielding a spatial resolution of 0.15" to 0.18" and a velocity discrimination as high as 1 km/s. Thanks to the high spatial and velocity resolution of the GriF data, 193 bright H2 emission regions can be identified in OMC1. The general characteristics of these features are described in terms of radial velocities, brightness and spatial displacement of maxima of velocity and brightness, the latter to yield the orientation of flows in the plane of the sky. Strong spatial correlation between velocity and bright H2 emission is found and serves to identify many features as shocks. Important results are: (i) velocities of the excited gas illustrate the presence of a zone to the south of BN-IRc2 and Peak 1, and the west of Peak 2, where there is a powerful blue-shifted outflow with an average velocity of -18 km/s. This is shown to be the NIR counterpart of an outflow identified in the radio from source I, a very young O-star. (ii) There is a band of weak velocity features (<5 km/s) in Peak 1 which may share a common origin through an explosive event, in the BN-IRc2 region, with the fast-moving fingers (or bullets) to the NW of OMC1. (iii) A proportion of the flows are likely to represent sites of low mass star formation and several regions show multiple outflows, probably indicative of multiple star formation within OMC1. The high spatial and velocity resolution of the GriF data show these and other features in more detail than has previously been possible.