We present the detailed description on the fiber techniques adopted in the BOES: the design concepts and manufacturing of the v grooves, the procedures of the fiber polishing, adhering of the fibers to the v grooves, and the axis alignment of the fiber input and exit. The high efficiency and throughput of the BOES imply that the adopted fiber arts and the other optical components were well designed and properly treated. We learned that the relatively low efficiency of the 80 micron fiber comparing with the 200 and 300 micron fibers comes from the seeing and the guiding effects not from the poor fiber handling.

The characteristics of the BOES (Bohyunsan Observatory Echelle Spectrograph) CCD camera is presented. In order to get optimum gain and readout noise of the CCD, we examine the variation of the gain and readout noise by changing the value of output drain voltage of the CCD and measuring the gain using transfer curve, which is defined as the plot of variance versus mean exposure level of a homogeneous light onto the CCD surface. The gain and readout noises are optimised to be 0.5e −/ADU and 3e−, which is good for highest signal-to-noise ratio and contrast for the low light level characteristics of the BOES. We also measure the dark count of the CCD by getting five dark images with 3600 seconds exposure time. The mean dark count from median stacked dark images is essentially zero. A table of positions of defected pixels is also presented.

A CCD camera for the BOES (Bohyunsan Observatory Echelle Spectrograph) has been developed. The camera consists of a 2048 × 4096 format CCD, a SDSU Gen-I CCD controller, and a continuous flow cryostat (CFC) designed by the ESO. In order to control the CCD under SDSU Gen-I controller, the voltage level of all the biases and clocks were lowered by -6V. The CFC showed cooling time of about 10 hour, after which the chip temperature settled down with variation less than ±1°C. The final chip temperature is around -105 °C with the setting value for the CFC as -170 °C

In 2002, a new solar spectroscopic system with the Coelostat type has been installed at Korea Astronomical Observatory. It was designed to observe solar spectra in the range from 3000 to 8000 Å with the spectral resolution of 1 Å/mm. The system is composed of a 40cm diameter Coelostat with 9m focal length, spectroscopic system with 600groove/mm grating, and a IK × IK CCD detector. By developing observational softwares for this system, we have successfully observed solar Ha spectra. In this paper, we development of telescope control and observational softwares.

본 연구에서는 공주대학교 천문대 16인치 반사망원경의 원격 제어 시스템을 구축하였다. 이 시스템은 닫힌 루프 시스템이다. 전자제어부는 한국천문연구원에서 개발한 TCS-196를 활용했고, 기계부는 직접 개발하였다. 이 원격제어망원경의 마운트 모델링 후 얻은 지향정밀도는 시간각 방향에서는 ±50", 적위 방향에서 ±40"이며, 추적 정밀도도 약 1"/min정도였다. 이러한 예비관측 결과는 본 시스템이 천문학 연구 및 교육에 적당함을 의미한다.

We have analyzed 209 data of daily sunspot observations made during the period of January 3 to December 31 In 2001 and presented the daily relative sunspot numbers. During the year of 2001, our annual average of relative sunspot numbers is found to be 92.2. This number is obtained from the averaged daily number of 8.4 spot groups, in which there are about 57.5 distinct spots observed. According to the appearance of 370 spot groups, our analysis shows that the mean life time of spot groups is about 4 day and 20.4 hours.

We have analyzed 210 data of daily sunspot observations made during the period of January 3 to December 31 in 2000 and presented the daily relative sunspot numbers. For this work we estimated the conversion factors to derive the relative sunspot numbers: k=0.72 for the 20 cm refractor and k=0.56 for Solar Flare Telescope in KAO. During the year of 2000, our annual average of relative sunspot numbers is found to be 99.4. This number is obtained from the averaged daily number of 8.9 spot groups, in which there are about 62.5 distinct spots observed. According to the appearance of 423 spot groups, our analysis shows that the mean life time of the spot groups is about 4 day and 12.0 hours.

In this paper we present a newly improved telescope control software and a newly developed data analysis software package for effective use of the Solar Flare Telescope(SOFT) The telescope control software permits us to make not only auto tacking of the SOFT, but also quantitative measurement of the solar irradiation, allowing us to provide weather monitorings. In addition we introduce an IDL widget software package for both monochromatioc (MONO version) and polarimetric data (VMG version) analysis. The MONO version is capable of loading FITS files, changing colors and contrast, image processing, displaying plots, and saving displayed plots by selected formats The VMG version, on the other hand provides a calibration of polarimetric data and plots of reduced vector magnetic fields.

SOFT( So–––lar F––lare T––elescope So_larF_lareT_elescope ) installed at BOAO(Bohyunsan Optical Astronomy Observatory) is purposed for observing solar active regions using four refractors on single mount with a 400"×300" 400"×300" field of view: Two refractors with a diameter of 15cm(f15) are observe the white light and Hα Hα , and the other two refractors with a diameter of 20cm(f8) are observe the magnetic field distribution and Doppler shifts at the solar chromosphere. Three Lyot filters, one of the most important observational instruments, are installed on the optical rails for VMG, LMG, and Hα Hα that possible to very narrow pass band observation under high precision stability of temperature. From the combination of KD*P and quarter wave plate in the Lyot filter possible observe the magnetic fields strength and doppler shifts by using the characteristics of polarization components. In this paper, we introduce the basic characteristics, optical system, and monitor system of the SOFT.