Galatic Survey of Temperature of Molecular Clouds by using Mizusawa 10m Antenna

去年，使用Mizusawa 10米天线对氨气分子线进行了观测，从而检查了声光光谱仪的性能。这一年我们开发了数据简化软件。因此，有大量的数据可供分析。我们还开发了使用水泽10米天线进行观测的软件，以便更有效地进行分子云温度的星系调查。观测区域为金牛座分子云、英仙座分子云、猎户座A分子云、银河系中心、W30H和W49N。通过研究氨分子（1,1,1,1）和（2,2,2,2）跃迁的谱线强度分布，可以测量这些分子的气体动力学温度。结果表明，当气体动力学温度高于50K时，分子云的尺寸较小。我们还研究了分子云中致密气体体积比大于10000/cc的填充因子的分布。我们的结果与其他不同光束大小的氨数据的比较表明，银河系中心的填充因子与猎户座A分子冷的填充因子不同。为了研究填充因子的详细结构，我们计划对分子色块进行10000多个点的观测。我们还监测了著名的活跃恒星形成区W49N的水蒸气脉泽发射强度。

In the last year, performation of the Acousto-Optical-Spectrometer has checkedby observations of anmonia moelcuar lines using the Mizusawa 10m antenna.We developed software for data reduction in this year. Therefore, huge amount of data was availiable to be analyzed. We also developed software for observations of using the Mizusawa 10m antenna in order to perform the galatic survey of temperature of molecular coluds more efficiently.The observed regions are Taurus molecular cloud, Perseus molecular cloud, Orion A molecular coloud, Galactic center, W30H,and W49N.Gas kinetic temperature of these molecular coulds are measured by studying distribution of line intensities of (1,1-1,1) and (2,2-2,2) transitions of anmonia molecules. The result is that sizes of the molecular coluds, in which gas kinetic temperature is higher than 50K,are small.We also studied distribution of filling factor which is a volume ratio of dense gas higher than 10000/cc in molecular clouds. Conparison of our results with the other anmonia data in different beam size indicates that the filling factor of Galatic center is different from that of Orion A molecular colud.We have plan to observe more than 10,000 points for molecular coluds in order to study the detailed structure of the filling factor.We also monitored the strength of water vaper maser emission from a famous active star forming region, W49N.