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

nagata和N.Kobayashi利用智利的1.5m CTIO红外望远镜对银河系中心0.5度范围内的5个红外源进行了光谱偏振观测，波长从1.4到4.2微米不等。他们探测到了极化；幂律p（λ）很好地表示了它，但所有五个物体在整个2.8 - 4.2微米范围内的极化都远远超过了幂律。这种过度极化可能是由位于一般漫射星际介质中的颗粒或内部星系特有的颗粒引起的。偏振增加的形状似乎与分子云源不同。7月6日至8日，s.d oguchi在美国马萨诸塞州波士顿附近的Haystack天文台用37米射电望远镜测量了NGC4258中22 GHz的超高速水脉波的线偏振。由于东部沿海地区受到热浪的影响，我们可以对偏振的I、Q和U分量分别进行约2小时的H2O光谱积分。我们发现线偏振度小于30%，这将限制NGC4258星系高速微波激射的可能模型。k . wakamatsu使用CTIO 1.5 m和3.0 m Lick望远镜对蛇夫座cD星团进行了广泛的红移调查。该星团是Wakamatsu和Malkan发现的，是天空中第三亮的x射线星团。该星团由几个不规则星团组成，由“蛇夫座超星团”组成。y.t aniguchi在JCMT15-m和Nobeyama 45-m射电望远镜上分别在CO（J=3-2）和CO（J=1-0）中观测到几个附近的星暴核。光束匹配观测的平均强度比为CO(J=3-2)/CO(J=1-0) = 0.9+-0.2。这个值明显大于我们银河系中巨大分子云的值（0.4+-0.05）。因此，我们得出结论，星爆核中的分子气体是明显温暖的（T - 50 - 25K）。我们的观测首次在星暴现象的研究领域提供了非常可靠的光束匹配测量。谷口和他的合作者使用UH88望远镜上的高灵敏度红外相机NICMOS3进行了k波段深度调查。他们获得了一个油田20小时的积分数据，该数据将由ISO进行观测。他们将在1994年4月观测这个区域，并将探测到K= 23等的非常微弱的物体。由于这次调查是该研究领域中最深的一次，他们将有助于理解星系的形成和观测宇宙学。s.s ato访问了三所大学的设施（怀俄明大学，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合作的未来可能性。预计从6月到10月，将分别使用wiro2.3米和Mt.Lemmon 1.5米望远镜进行为期一周的三次和为期十天的两次观测。虽然阿帕奇点3.5米和1.0米望远镜是为光学目的而设计的，但通过微小的改变，它们有可能被改造成红外望远镜。九个人（谷口y ., suto h .，长谷川t .，若松k .，田中m .，岩川k .，佐藤f ., sofue y .和小仓k .）被委派在光学、红外和无线电区域进行不同波长的天文观测。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