Study of Star Forming Regions with An Infrared 2-Dimensional Array Photometer

该项目的目的是利用红外二维阵列光度计对银河系和外部星系中的漫射源进行光谱测量。该阵列光度计的元素数量很少（4 x 4 = 16），但是，它覆盖了大视场，并且在与宽视场光谱仪（例如Fabry-Perot光谱仪）一起使用的情况下，具有高灵敏度，可以检测来自扩展源的弱发射线。不幸的是，我们还没有用这台仪器获得科学数据，我们期望这台仪器在不久的将来会产生有意义的数据。线光谱观测的一个重要例子是在各种星系源中对分子氢发射的一系列观测。这使我们认识到不同来源的H_2荧光辐射的贡献是非常重要的。迄今为止，几乎所有可探测到的H_2辐射都被认为是由振动现象激发的，然而，我们证明了这是不正确的。我们发现，在星暴星系中，荧光激发占主导地位。我们的研究结果解决了假设为振荡激励时，观测到的H_2发射强度远大于期望值的难题。在解释外星系（塞弗特星系和星暴星系）的H_2辐射时，测量H_2辐射不仅可以揭示发射区域分子气体的物理条件，还可以揭示恒星形成的历史以及星际物质和物质的分布。本项目所推动的研究，即高灵敏度、宽视场的扩展源红外谱线的光谱观测，将在不久的将来对广泛的天体物理现象产生丰硕的科学成果。

The objective of this project is to make spectroscopic measurements of diffuse sources in our Galaxy and external galaxies by using an infrared 2-dimensional array, photometer. This array photometer has a small number, 4 x 4 = 16, of elements, however, it covers large field-of-view and has high sensitivity to detect weak emission lines from extended sources in case of using together with a wide-field spectrometer, for example, a Fabry-Perot spectrometer. Unfortunately, we have not yet obtained scientific data with this instrument, we expect that this instrument will produce meaningful data in the near future.An significant example of line spectroscopic observations is a series of observations of molecular hydrogen emission at 2 mum in various kinds of galactic sources. It made us understand that contributions of fluorescent H_2 emission in various sources are much important. So far almost all detectable H_2 emission was considered to be excited by shook phenomena, however, we showed it was not correct. We found fluorescent excitation is dominant in a starburst galaxy. Our results solve the puzzle that the observed intensity of H_2 emission is much stronger than the expected value if a shook excitation is assumed. In the interpretation of H_2 emission in external galaxies: Seyfert and starburst galaxies, the measurements of H_2 emission will reveal not only physical conditions of molecular gas at emission regions, but also histories of star formation and distribution of stats and interstellar matter.The study promoted by this project, that is, spectroscopic observations of infrared lines for extended sources with high sensitivity and wide field-of-view, will produce fruitful scientific results on a wide variety of astrophysioll phenomena in the near future.