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

用红外二维阵列光度计研究恒星形成区域

基本信息

批准号：
62460009
负责人：
TANAKA Masuo
金额：
$ 4.61万
依托单位：
The University of Tokyo
依托单位国家：
日本
项目类别：
Grant-in-Aid for General Scientific Research (B)
财政年份：
1987
资助国家：
日本
起止时间：
1987 至 1989
项目状态：
已结题

来源：
https://kaken.nii.ac.jp/en/grant/KAKENHI-PROJECT-62460009/
关键词：
Infrared Astronomy Star Forming Regions Infrared Sources Wide-Field Photometer 2-Dim. Array Detector InSb Detector

项目摘要

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.

该项目的目标是利用红外二维阵列光度计对银河系和外星系中的漫射源进行光谱测量。该阵列光度计具有少量的元件，4 × 4 = 16，然而，它覆盖大的视场，并且在与宽视场光谱仪（例如，法布里-珀罗光谱仪）一起使用的情况下具有高灵敏度以检测来自扩展源的弱发射线。不幸的是，我们还没有得到科学数据与此仪器，我们希望，这台仪器将产生有意义的数据在不久的将来。线光谱观测的一个重要的例子是在2妈妈在各种星系源的分子氢发射的一系列观测。这使我们认识到各种光源中荧光H_2发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辐射都被认为是由震动现象激发的，然而，我们证明了这是不正确的。我们发现荧光激发在星暴星系中占主导地位。我们的结果解决了H_2发射强度观测值远大于假设振动激发时的期望值的难题。在解释星系外H_2辐射时：Seyfert星系和星暴星系的H_2辐射测量，不仅可以揭示辐射区分子气体的物理条件，而且可以揭示星星的形成历史以及恒星和星际物质的分布。将在不久的将来对各种各样的天体物理学现象产生丰硕的科学成果。