Millimeter and Optical-Infrared Astronomical Observations by Using High-level Overseas Telescopes

Yoshida博士和Aoki博士使用位于夏威夷莫纳克亚的夏威夷大学2.2米望远镜的KSPEC对一个中等红移的宽线射电星系样本进行了近红外光谱分析。他们检测了7个射电星系的Paalpha、Pabeta和Halpha谱线，并将谱线轮廓相互比较。然后，通过对发射线剖面的分析，求出了各星系宽线区的吸收量，从而获得了揭示射电星系宽线区内部结构的线索。小林博士使用国立天文台制作的红外照相机PICNIC进行了红外观测。该相机连接到澳大利亚国立大学赛丁泉天文台的2.3米望远镜。他对银河系中心区域进行了JHK波段的光偏振测量，以确定那里的磁场结构。他还对银河系南极区域的fain星系进行了深入的调查。 ...更多信息 n，以便获得宇宙学参数。观测非常成功，数据正在处理中。使用美国西弗吉尼亚州绿色班克国家射电天文台的43 m射电望远镜，佐藤博士绘制了蛇夫座和天蝎座在HI 21厘米线上包含分子云的区域（l=342*-20*，B=+2*-+30*）。获得了9500多条谱线，角分辨率为20'，速度分辨率为0.26km/s。初步分析清楚地揭示了负速度下HI通道图中的平行结构，表明HI气体和分子气体的分布之间存在相关性或平行关系。谷口博士本财政年度两次访问莫纳克亚天文台，一个是用夏威夷大学的2.2米望远镜搜寻原星系，另一个是用JCMT 15米望远镜观测星暴星系为了寻找原星系，他使用2.2米望远镜和NICMOS 3相机对洛克曼HI洞进行了K波段的深度测量。他在K= 23等的水平上获得了30小时的积分。红外空间天文台将在7微米处观测到相同的场。这两个数据都将用于研究高红移宇宙中的星系形成。对于JCMT观测，他使用莫纳克亚天文台的JCMT 15米亚毫米波望远镜对附近的星暴星系进行了CO（J=3-2）观测。他还使用野边山射电天文台的45米射电望远镜对同一星系进行了CO（J=1-0）观测。两个跃迁数据的比较清楚地表明，相对于正常星系核中的分子云，星暴和塞弗特星系中的分子气体往往具有更致密和更高温度的分子云。永田博士对几十颗恒星进行了光谱学和光谱偏振测量。他发现了在弥漫的星际介质中变红的恒星中由于碳-氢键而产生的吸收特征。在卡内基研究所的合作下，关口博士和柏川博士使用他们的镶嵌CCD相机（4000 x7000像素）和LasCampnas天文台的望远镜，在BVR三个彩色波段上观测了A2670、A194、A458和A496星系团。他们发现在这些星系团的暗淡区域，光度函数有着显著的差异。这种差异主要是由于矮星系。他们正在做进一步的数据分析和准备文章。少

Drs.Yoshida and Aoki made near-infrared spectroscopy of a sample of broad line radio galaxies with moderate redshifte using KSPEC attached to the University of Hawaii 2.2m telescope at Mauna Kea, Hawaii. They detected the lines of Paalpha, Pabeta, and Halpha for seven radio galaxies andcompared the line profiles with each other. They then derived the amount of absorption in the broad line region of each galaxy from the analysis of the emission-line profiles, obtaining a hint to reveal the internal structure of broad line regions of radio galaxies.Dr.Kobayashi made infrared observations using the infrard camera PICNIC fabricated by the national astronomical observatory. The camera was attached to the Australian national university 2.3m telescope at the Siding Spring Observatory. He carried out JHK-bands photo-polarimetry of the Galactic center region in order to determine the magnetic field structure there. He also dis a deep survey for fain galaxies toward the Galactic south pole regio … More n for the puropose of obtaining the cosmological parameters. The observations were carried out quite successfuly and the data is being processed now.Using the 43m radio telescope at the National Radio Astronomy Observatory at Green Bank, West Virginia, U.S.A., Dr.Sato mapped the region (l=342*-20*, b=+2*-+30*) containing the molecular clouds in the Ophiuchus and Scorpius in the HI 21cm line. About 9500 spectra were obtained with the angular resolution of 20' , and the velocity resolution was 0.26 km/s. Preliminary analyzes clearly revealed filamentary structures in the HI channel maps at negative velocities, suggesting the correlation or anticorrelation between the distributions of the HI gas and that of the molecular gas.Dr.Taniguchi visited Mauna Kea Observatories twice this fiscal year, one for the search for protogalaxies w the University of Hawaii 2.2m telescope and the other for the observations starburst galaxies with the JCMT 15m telescope.For the protogalaxy search, he made a K-band deep survey of the Lockman HI hole by using of the 2.2m telescope with NICMOS3 camera. He obtained 30 hours of integration for one field at a level of K=23mag. The same field will be observed with Infrared Space Observatory at 7micron. Both the data will be utilized to study forming galaxies in the high-redshift universe.For the JCMT observations, he made CO (J=3-2) observations of nearby starburst galaxies by using JCMT 15m submillimeter-wave telescope at Mauna Kea Observatories. He also made CO (J=1-0) observations of the same galaxies with use of the 45m radio telescope at the Nobeyama Radio Observatory. The comparison between the two transition data clearly showed that the molecular gas resided in the starburst and teh Seyfert galaxies tend to have denser and higher-temperature molecular clouds with respect to those in normal galaxy nuclei.With their prism spectro-polarimeter PASP2 attached to the Wyoming Infrared Observatory 2.3m telescope and the 1.5-m telescope at Mt.Lemmon Observing Facility of University of Minnesota, Dr.Nagata made spectroscopy and spectro-polarimetry for several dozens of stars. He found absorption features due to the carbon-hydrogen bond in stars reddened in the diffuse interstellar medium. The distribution of interstellar ice has also been determined from the observation of stars behind the Taurus Dark cloud.In collaboration with the Carnegie Institution, Drs.Sekiguchi and Kashikawa observed clusters of galaxies s as A2670, A194, A458, and A496 in BVR three color bands, using their mosaic CCD camera (4000x7000pixels) with a telescope at LasCampnas observatory. They found a significat difference in the luminosity function in the faint regions of these clusters. This difference is mostly due to dwarf galaxies. They are doing further data analysis and preparing articles. Less