We present a fast reduction method of survey data obtained using a single-dish radio telescope. Along with a brief review of classical method, a new method of identification and elimination of negative and positive bad channels are introduced using cloud identification code and several IRAF (Image Reduction and Analysis Facility) tasks relating statistics. Removing of several ripple patterns using Fourier Transform is also discussed. It is found that BACKGROUND task within IRAF is very efficient for fitting and subtraction of base-line with varying functions. Cloud identification method along with the possibility of its application for analysis of cloud structure is described, and future data reduction method is discussed.

The purposes of spectroscopy in astronomy are to measure the radiation flux of the spectroscopic emission or absorption line and to measure the dynamical parameters of the line profile. In order to use an appropriate instrument for the scientific purpose, we need to understand the characteristics of various spectrometers, e.g., a prism spectrometer, a grating spectrometer, and a Fabry-Perot spectrometer (FPS), which are being used in ultra-violet, optical, and infrared bands. The Fabry­Perot spectrometer is not very popular compared to the grating spectrometer, because of its complex and tricky operations. The Fabry-Perot spectrometer, however, can get a two-dimensional image at one exposure, so we can study radiation mechanisms and dynamical properties of extended sources, e.g., clusters, nebula, and galaxies.

Infrared spectroscopic observations and their analysis revealed many physical and chemical characteristics of the various stars with dust envelopes. Especially, AGB stars and young stellar objects are believed to be major contributors of infrared radiation from galaxies. The wavelength of the peak spectral energy for typical galaxies is about 100μm 100μm . Therefore, infrared spectral observations of galaxies provide important information for their overall properties. The qualitative analysis of the infrared spectra which are made of various stars and interstellar matter will be possible through a new population synthesis.

X-ray astronomy deals with measurements of the electromagnetic radiation in the energy range of E \~ 0.1 − 100 k e V ( λ \~ 0.12 − 120 \AA ) . The wavelength of X-ray is comparable to the size of atoms, so that the photons in the X-ray range are usually produced and absorbed by the atomic processes. Since the launch of the first X-ray astronomy satellite 'Uhuru' in 1970, technological advances in a launch capability and a detection capability make X-ray astronomy one of the most rapidly evolving fields of astronomical research. Particularly, a spectral resolving power E / Δ E has been increased by an order of 2 - 3 (in the energy range of 0.1 - 10 keV) during the past 30years. In this paper, I briefly review a developing process of the resolving power and spectroscopic techniques. Then I describe important emission/absorption lines in X-ray astronomy, as well as diagnostics of gas property with line parameters.

We determined the precise three dimensional WGS84 Coordinates and the sea level height of Seoul Radio Astronomy Observatory (SRAO). In this study, we performed the simultaneous GPS observations at SRAO and Seoul GPS Reference Station(SGRS) of Korea Astronomy Observatory(KAO) for 3.5 hours from 17KST on October 27, 1999. We employed two different antennas, i.e., chokering antenna at SGRS of KAO and L1/L2 compact with groundplane antenna at SRAO. But we employed same type of receivers, i.e., Trimble 4000SSI at both observing places. The observed data were processed by GPSURVEY 2.30 software of Trimble with L1/L2 ION Free technique and broadcasting ephemeris of GPS Satellites because of very short baseline between SGRS of KAO and SRAO. We determined WGS84 latitude, longitude, height and the sea level height of SRAO with 37∘27′15.′6846N±0.′0004,126∘57′19.′0727E±0.′0002,204.89m±0.02m,181.38m±0.17m 37∘27′15.′6846N±0.′0004,126∘57′19.′0727E±0.′0002,204.89m±0.02m,181.38m±0.17m , respectively.

Detailed low spectral resolution observations of the spectrum have been made for three early spectral type standard stars, HR718, HR1544, HR3454, respectively, for the wavelength region 4,300 A to 7,500 A, using the Bohyunsan Optical Astronomy Observatory (BOAO) Middle- Dispersion Spectrograph. These standard stars were chosen from well-known bright northern standard stars. All of the observed long slit spectral data has been reduced and analyzed using the IRAF reduction procedure. The derived extinction coefficients are compared with the other observatory result. The derived value can be used in the determination of flux calibration of BOAO spectroscopic observation. However, until the high quality data are secured from a new series of observation in the blue region and are re-analyzed together, the extinction coefficients below the 4,000 A wavelength remains unknown.

There is a question, 'Which is beautiful, a flower or a star?'. Its answer is different from one person .to another. It is only a matter of what one is interested in. It is very difficult for most school pupils, who will have non-scientific jobs, to understand science courses taught currently in school, because each science (physics, chemistry, biology, and earth science) is independently taught from the other sciences. Therefore, their knowledge of sciences obtained during their school period does not significantly help their understanding of global environmental problems. I am proposing that several scientific stories should be prepared to connect all the related scientific phenomena in order to give those pupils ideas in understanding global environmental problems. I believe that astronomy is able to play an important role in this context.

We introduce the National Science Curriculum issued by the Education Ministry in Korea. Astronomy should be given and taught as compulsory courses in Nature of elementary school, Science of middle school, General Science of high school, and as elective courses in Earth Science I, II. Astronomy concepts have been designed in sprial pattern. College levels of astronomy have been given as majoring in astronomy course, cultivating one for earth science pre-teacher students and cultural subjects for non-major students

An x-ray astronomy experiment consisting of three collimated proportional counters and an X-ray Sky Monitor (XSM) was flown aboard the Indian Satellite IRS-P3 launched on March 21, 1996 from SHAR range in India. The Satellite is in a circular orbit of 830 km altitude with an orbital inclination of 98° and has three axis stabilized pointing capability. Each pointed-mode Proportional Counter (PPC) is a multilayer, multianode unit filled with P-10 gas (90% Ar + 10% CH4) at 800 torr and having an aluminized mylar window of 25 micron thickness. The three PPCs are identical and have a field of view of 2°×2° defined by silver coated aluminium honeycomb collimators. The total effective area of the three PPCs is about 1200 cm2. The PPCs are sensitive in 2-20 keV band. The XSM consists of a pin-hole of 1 cm2 area placed 16 cm above the anode plane of a 32 cm×32 cm position sensitive proportional counter sensitive in 3-8 keV interval. The position of the x-ray events is determined by charge division technique using nichrome wires as anodes. The principal objective of this experiment is to carry out timing studies of x-ray pulsars, x-ray binaries and other rapidly varying x-ray sources. The XSM will be used to detect transient x-ray sources and monitor intensity of bright x-ray binaries. Observations of black-hole binary Cyg X-1 and few other binary sources were carried out in early May and July-August 1996 period. Details of the x-ray detector characteristics are presented and preliminary results from the observations are discussed.

We present the update information on the International Radio Astronomy Observatory Suffa project and describe the original design of new 70-m radiotelescope RT-70 for millimeter astronomy as well. Some oreographic, seeing and climatic features of Suffa are also given.

In Korea Astronomy Observatory, we developed a S/W package to compile the Korean Nautical Almanac. We describe the motivation to develop the S/W and explain the S/W package in general terms. In appendix, we describe the procedure to calculate the polaris table in more detail. When we developed the S/W, we paid much attention to produce accurate data. We also made great effort to automate the compilation of Nautical Almanac as far as possible, since the compilation is time consuming and labour extensive. As a result, the S/W we developed turns out to be very accurate and efficient to compile Nautical Almanac. In fact, we could compile a Korean Nautical Almanac in a few days.