MID-INFRARED SPECTROSCOPIC STUDY OF BRIGHT INFRARED GALAXIES

明亮红外星系的中红外光谱研究

基本信息

批准号：
06452019
负责人：
MATSUHARA Hideo
金额：
$ 4.29万
依托单位：
Nagoya University
依托单位国家：
日本
项目类别：
Grant-in-Aid for General Scientific Research (B)
财政年份：
1994
资助国家：
日本
起止时间：
1994 至 1995
项目状态：
已结题

项目摘要

A unique technical aspect of this research is to develop a Mid-Infrared Fabry-Perot Imager (MIRFI), which is designed for ground-based observations of mid-infrared spectral lines located in the 10mum atomospheric window. MIRFI is now tuned to observe [Ne II] 12.814mum line from neon ions, and consists of a scanning Fabry-Perot interferometer with a spectral resolving power of -2500 and a Si : P photoconductive detector array (5x5 format), both are cooled by liquid-He. Achieved sensitivity of 1.6*10^<-20> Wcm^<-2>pixel^<-1> (per spectral resolution, 17sec integration) is sufficient to observe the [Ne II] line from neaby bright infrared galaxies with burst of star formation (starburst galaxies).Major scientific goal of this research is to investigate the structure of central region of neaby starburst galaxies by the [Ne II] line. Infrared luminous starburst galaxies are heavily obscured by dust and hence are not visible at optical wavelenth, but at 12.8mum dust extinction is almost negligible. We have made the first observing run with NASA/IRTF (Mauna Kea, Hawaii, USA) in April 1995, but no scientific data due to bad weather. In March and October 1996, and March 1997, we have made observing runs with Wyoming Infrared Observatory (Wyoming, USA), and finally detected [Ne II] line from the starburst galaxy M82, as well as rich [Ne II] flux data for Galactic ultracompact H II regions (W51d, G29.96-0.02, etc.). We could not obtain much data for infrared galaxies : to do this we need very good weather condition. However, MIRFI is proved to work efficiently for observation of Galactic objects and will provide much scientific results in the near future.

这项研究的一个独特的技术方面是开发一个中红外的Fabry-Perot Imager（MirFI），该成像仪是针对地面观测的，该观察结果是对位于10mum atomlosper窗口中的中红外光谱线。现在，对Mirfi进行调整以观察[NE II] 12.814MUM来自霓虹灯离子，由扫描Fabry -Perot干涉仪组成，光谱解析功率为-2500和si：p光电传导探测器阵列（5x5格式），都冷却由Liquid-He。达到的灵敏度为1.6*10^<-20> WCM^<-2> Pixel^<-1>（通过光谱分辨率，17秒集成）足以观察来自NEABY明亮的红外星系的[NE II]线，并与星星爆发形成（Starburst星系）。这项研究的Major科学目标是研究[NE II]线的Neaby Starburst星系中央区域的结构。红外发光的恒星星系被尘埃遮盖，因此在光学上看不到，但在12.8mum的尘埃灭绝几乎可以忽略不计。我们于1995年4月与NASA/IRTF（美国夏威夷州Mauna Kea）进行了第一次观察，但由于天气恶劣，没有科学数据。在1996年3月和10月，以及1997年3月，我们与怀俄明州红外天文台（美国怀俄明州）进行了观察，并最终从Starburst Galaxy M82中检测到[NE II]线，以及丰富的[NE II]通量数据银河系超级反理H II区域（W51D，G29.96-0.02等）。我们无法获得太多的红外星系数据：为此，我们需要很好的天气状况。但是，事实证明，Mirfi在观察银河对象方面有效地工作，并将在不久的将来提供很多科学的结果。