Milli-meter and Optical-Infrared Astronomical Observations by Using High-Level Overseas Telescopes.

T.Nagata和N.Kobayashi利用智利的1.5米CTIO红外望远镜，对距离银河系中心0.5度范围内的5个红外源进行了1.4至4.2微米波长的偏振光谱观测。他们探测到了偏振；它很好地用幂定律p(Lambda)来表示，但在整个2.8-4.2微米范围内，所有五个物体的偏振都远远超过了这个幂定律。这种额外的偏振可能是由位于一般弥散星际介质中的颗粒或内星系特有的颗粒引起的。极化增加的形状似乎与分子云源的形状不同。S.Deguchi于7月6-8日在美国马萨诸塞州波士顿附近的干草堆天文台用37米射电望远镜测量了22 GHz的NGC4258中极高速水脉泽的线偏振。由于大气和INS…由于东海岸的热浪造成的更大的麻烦，我们可以对极化的I、Q和U分量进行大约2小时的H2O谱积分。我们发现蛇夫座的线偏振度小于30%，这将限制NGC4258星系中高速脉泽的可能模型。K.Wakamatsu用CTIO1.5m和3.0m的Lick望远镜对蛇夫座CD星系团进行了广泛的红移观测。这个星系团是由Wakamatsu和Malkan发现的，是天空中第三亮的X射线星团。发现该星团是由几个不规则星团组成的，因此形成了蛇夫座超星系团。这个超星系团可能与大力神超星系团通过一个突出的壁结构联系在一起。谷口Y.Taniguchi在JCMT15-m和Nobeama 45-m射电望远镜上分别在CO(J=3-2)和CO(J=1-0)中观测到了几个附近的星暴核。光束匹配观测给出了CO(J=3-2)/CO(J=1-0)=0.9+-0.2的平均强度比。这个数值明显大于我们银河系中的巨型分子云(0.4+-0.05)。因此，我们得出结论，恒星暴增核中的分子气体是非常热的(Tkin和GT；25K)。我们的观测首先在恒星爆发现象的研究领域给出了非常可靠的光束匹配测量。Y.Taniguchi和他的同事们利用UH88望远镜上的高灵敏度红外相机NICMOS3进行了K波段的深度探测。他们获得了一个场的20小时积分数据，这些数据将由ISO观测。他们将在1994年4月观测到这个磁场，并将探测到K=23MAG的非常微弱的天体。由于这次调查是这一研究领域中最深入的一次，他们将有助于理解星系的形成和观测宇宙学。来自怀俄明州大学。明尼苏达大学和新墨西哥州立大学)，讨论在一些长期运行中使用中型望远镜进行合作的未来可能性。预计它将使用WIRO2.3-m和Mt.Lemmon 1.5-m望远镜，从6月到10月分别进行三次为期一周的运行和两次为期十天的运行。尽管阿帕奇点3.5米和1.0米望远镜是为光学目的而设计的，但有可能通过微小的改变将它们改装成红外作品。九人(谷口Y.Taniguchi、H.Suto、T.Hasegawa、K.Wakamatsu、M.Tanaka、K.Iwaawa、F.Sato、Y.Sofue和K.Ogura)被委托在光学、红外和射电区域进行不同波长的天文观测。较少

T.Nagata and N.Kobayashi have carried out spectropolarimetric observations for five infrared sources within 0.5 degree of the Galactic center in the wavelength from 1.4 to 4.2 microns using the 1.5m CTIO infrared telescope, Chile. They detected the polarization ; it is represented very well by a power law p(lambda), but all the five objects have polarization well in excess of this power law in the whole 2.8 - 4.2micron. This excess polarization might be caused by grains located in the general diffuse interstellar medium or grains specific to the inner Galaxy. The shape of the polarization increase seems different from that of the molecular cloud sources. The carrier of the 3.0 micron features is not distributed ubiquitously in the line of sight.S.Deguchi measured the linear polarization of the extreme high-velocity water masers in NGC4258 at 22 GHz with the 37-m radio telescope at Haystack Observatory near Boston, Massachusetts, U.S.A., during July 6 - 8. Because of atmospheric and ins … More trumental troubles due to heat waves in the east coast, we could integrate the H2O spectra for about 2 hours each for the I, Q, and U components of the polarization. We found the degree of linear polarization less than 30 % and this will restrict the possible model of the high velocity masers in the NGC4258 galaxy.K.Wakamatsu carried out an extensive redshift survey of Ophiuchus cD cluster with CTIO 1.5-m and 3.0-m Lick telescopes. The cluster was discovered by Wakamatsu and Malkan as the 3rd brightest X-ray cluster in the sky. The cluster is found to be accomplished with several irregular clusters and so to from "Ophiuchus supercluster". This supercluster may be connected with Hercules supercluster by a prominent wall structure.Y.Taniguchi observed several nearby starburst nuclei both in CO(J=3-2) and CO(J=1-0) at JCMT15-m and Nobeyama 45-m radio telescopes, respectively. The beam-matched observations give a mean intensity ratio of CO(J=3-2)/CO(J=1-0) = 0.9+-0.2. This value is significantly larger than that of giant molecular clouds in our Galaxy (0.4+-0.05). Hence, we conclude that the molecular gas in the starburst nuclei is significantly warm (T kin>25K). Our observations first give the very reliable beam-matched measurements in the research field of starburst phenomena.Y.Taniguchi and his collaborators made the K-band deep survey with a high-sensitivity infrared camera NICMOS3 on the UH88 telescope. They obtained 20 hours integration data of one filed which will be observed by ISO. They will observe this filed in April, 1994, and will detect very faint objects with K= 23 mag. Since this survey is the deepest one in this research fields, they will contribute to the understanding the formation of galaxies and the observational cosmology.S.Sato visited three University facilities (Univ. of Wyoming, Univ. of Minnesota, and New Mexico State University) to discuss the future possibility of collaboration using medium-size telescopes in some long-term runs. It is expected to use the WIRO2.3-m and Mt.Lemmon 1.5-m telescopes in the intervals of three one-week runs and two ten-days runs from June through October, respectively. Although Apache Point 3.5-m and 1.0-m telescopes are designed for optical purposes, there might be a possibility to modify them into infrared works by minor changes. Nine persons ( Y.Taniguchi, H.Suto, T.Hasegawa, K.Wakamatsu, M.Tanaka, K.Iwasawa, F.Sato, Y.Sofue, and K.Ogura ) were delegated for astronomical observations with various wavelengths in the optical, infrared and radio regions. Less