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

这个项目的目标是使用红外二维阵列光度计对我们银河系和外部星系的漫射源进行光谱测量。这种阵列式光度计元素数量少，4×4=16，但它覆盖大视场，在与广场光谱仪(如法布里-珀罗光谱仪)一起使用时，对探测来自扩展源的微弱发射线具有很高的灵敏度。不幸的是，我们还没有用这台仪器获得科学数据，我们预计这台仪器将在不久的将来产生有意义的数据。线光谱观测的一个重要例子是在各种银河源中对分子氢发射的一系列2微米的观测。这使我们认识到荧光氢气在各种来源中的贡献是非常重要的。到目前为止，几乎所有可检测到的H_2发射都被认为是由抖动现象激发的，然而，我们证明了这是不正确的。我们发现，在恒星爆发星系中，荧光激发占主导地位。我们的结果解决了假设振动激发时，观测到的H_2发射强度比预期值强得多的问题。在解释外星系Seyfert星系和恒星暴增星系中的H_2发射时，对H_2发射的测量不仅将揭示发射区分子气体的物理条件，而且还将揭示恒星形成的历史和统计数据和星际物质的分布。这项计划推动的研究，即高灵敏度和大视场的延伸源红外光谱观测，将在不久的将来对各种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.