Evolution and formation of galaxies seen through an ISO Far-infrared survey

我们利用1995年投入运行的ISO（红外空间天文台）上的ISOPHOT进行了95 & 175 μm的深远红外巡天。通过地面跟踪观测，对这些天体进行光学识别和红移测量是非常重要的。该项目的目的是：1.对ISO远红外巡天进行精确分析，编制高度可靠的ISO远红外源目录，为后续观测奠定坚实的基础，并将这些源的数量密度与星系模型进行比较，以获得关于星系形成和演化的信息;2.进行从光学到无线电的后续观测，并测量红移等基本量; 3.建立了CCD成像系统，对欧洲大面积ISO调查的野外进行了CCD成像，取得了良好的效果。 ...更多信息 1.我们根据ISO数据的最新校准，对ISO远红外调查进行了足够准确的数据分析，并成功地生成了可靠的远红外源目录。通过与远红外源计数模型的比较，我们发现：（1）z = 0.4附近的星星形成率（SFR）比现在的SFR高100倍，（2）由于受到宇宙背景红外辐射的限制，高红移处的SFR应该低于z = 0.4处的SFR。2我们在冈山天文台的1.8米望远镜上进行了光谱学研究，使用VLA（美国甚长阵）的20厘米成像，以及使用野边山天文台的45米望远镜、西班牙的IRAM 30米望远镜和夏威夷的CSO 10米望远镜的毫米/亚毫米观测。VLA观测非常成功，首次提供了远红外源的精确坐标。这确实是后续观察的一个里程碑。3 CCD成像系统已基本完成，将安装在澳大利亚AAO的英国施密特望远镜上。该系统将于2000年4月投入使用。少

We have carried out a deep far-infrared survey at 95 & 175 μm using ISOPHOT onboard ISO (Infrared Space Observatory) that was put in operation in 1995 This ISO far-infrared survey has detected 100 time more sources than expected from the no-evolution model. It is very important to make optical identification and to measure the redshift of these object by performing follow-up observations from the ground. This project intended to do :1 performing the accurate analysis of the ISO far-infrared survey, generating a highly reliable catalog of ISO far-infrared sources to give a firm base for follow-up observations, and comparing the number density of these sources with the models of galaxies for obtaining information on formation and evolution of galaxies ;2 executing follow-up observations from the optical to radio and measuring basic quantities such as redshift ;3 building a CCD imaging system and carrying out CCD imaging over the fields of European Large Area ISO Survey.We have achieved t … More he following :1 We have performed data analysis with sufficient accuracy of the ISO far-infrared survey based on the most recent calibration for ISO data, and successfully generated a reliable catalog of far-infrared sources. We have obtained number-flux relations using this catalog, and examined the completeness of the survey through simulation Comparing the relations with the models of far-infrared source counts, we found that (1) the star formation rate (SFR) around z 〜0.4 was 100 times higher than the present day SFR, and (2) SFR at high redshift should have been lower than SFR at z 〜0.4 due to the constraint from the Infrared Cosmic Background Radiation.2 We have carried out spectroscopy on the 1.8m telescope at the Okayama Observatory, 20cm imaging using VLA (Very Long Array in USA), and millimeter/submillimeter observations using the 45m telescope at the Nobeyama Observatory, IRAM 30m telescope at Spain, and CSO 10m telescope at Hawaii. The VLA observations were executed very successfully, providing the accurate coordinates of far-infrared sources for the first time. This is indeed a milestone of follow-up observations. Spectroscopy with the KECK telescope is scheduled in March this year.3 The CCD imaging system has almost been completed, and this will be installed on the UK Schmidt telescope at AAO in Australia. This will be commissioned in April in 2000. Less