Observations with Infrared Space Observatory (ISO)

该项目旨在通过国际联合研究，利用红外空间天文台(ISO)上的液氦冷却空间望远镜，寻找正在形成的星系，并研究恒星最后演化阶段的物理学。我们的ISO观测包括：(1)在洛克曼洞进行ISO深红外探测，以寻找光学探测中可能遗漏的正在形成的星系；(2)对麦哲伦星云中星团的中心部分进行ISO多色成像，以研究极晚恒星的质量损失；(3)绘制发射线的光谱图，以探测年轻热星附近的光致电离结构。为了实现上述目标，我们必须通过检查用于校准的ISO数据来了解ISO仪器在太空中的特性，并从地面进行后续观测。我们被允许派遣6名科学家前往法国分析ISO仪器的特性。因此，我们现在比以前更好地了解了ISO仪器及其行为，为减少数据提供了坚实的基础。因此，我们已经基本完成了数据简化，特别是ISO深红外测量项目。后续观测最初计划进行KPNO和IRAM。后来，由于合作者为寻求更好的观测设施而做出的努力，使位于美国夏威夷莫纳克亚天文台的加州理工大学亚毫米天文台的10M亚毫米望远镜和夏威夷大学的2.2M光学望远镜成为可能。后续观测才刚刚开始，将在接下来的几个月里继续进行。在这个项目中，我们发现(1)ISO远红外源的表面密度比非演化模型的预期高出10倍；(2)非常晚的恒星富含分子和尘埃，这是现有的任何恒星大气模型都无法解释的。

This project intends to search for forming galaxies and investigate physics at the last evolutionary stage of stars by using the liquid-helium-cooled space telescope onboard the Infrared Space Observatory (ISO) via international joint research. Our ISO observations include (1) ISO deep infrared survey in the Lockman Hole to search for forming galaxies which might have been missed in the optical surveys, (2) ISO multicolor imaging of central parts of star clusters in the Magellanic Clouds to study mass-loss of very-late stars, and (3) spectroscopic mapping of emission lines to probe the photo-ionized structure near young hot stars.To achieve the above objectives, we had to understand the characteristics of the ISO instrument in space through examining ISO data taken for calibration, and carry out follow-up observations from the ground.We were allowed to send six scientists to France to analyze the characteristics of the ISO instrument. As a result, we now understand the ISO instrument and their behavior much better than before, providing the firm basis for reducing data. Accordingly, we have almost completed the data reduction, which is especially true to the ISO deep infrared survey project.Follow-up observations were initally planned to carry out KPNO and IRAM.Subsequent efforts made by collaborators for seeking better observing facilities made it possible to use the 10m sub-millimeter telescope in the Caltech Sub-millimeter Observatory and the 2.2m optical telescope of the University of Hawaii, both located in the Mauna Kea Observatory, Hawaii, USA.The follow-up observations have just started, which will be continued for the next several months.During this project, we found (1) the surface density of ISO far-infrared sources is 10 times higher than expected from the non-evolution model, and (2) very late stars are rich in molecules and dust which cannot be explained by any existing models of stellar atmosphere.