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한국천문연구원 Hα 태양전면관측시스템의 바닥고르기 연구
박형민,김연한,봉수찬,박영득,조경석,장비호,최성환,나자경,이승민,채종철,Park, H.M.,Kim, Y.H.,Bong, S.C.,Park, Y.D.,Cho, K.S.,Jang, B.H.,Choi, S.,Nah, J.,Lee, S.M.,Chae, J. 한국천문학회 2008 天文學論叢 Vol.23 No.2
We have performed the flat-fielding correction for the $H{\alpha}$ full-disk monitoring system of KASI (Korea Astronomy and Space Science Institute), which is installed in the Solar Flare Telescope (SOFT) at the top of Bohyun Mountain. For this, we used a new method developed by Chae (2004), to determine the flat pattern from a set of relatively shifted images. Using this method, we successfully obtained the flat pattern for $H{\alpha}$ full-disk observations and compared our result with the image observed in Catania Astrophysical Observatory. The method that we used in this study seems to be quite powerful to obtain the flat image for solar observations. In near future, we will apply this method for the flat-fielding correction of all solar imaging instruments in KASI.
김연한,문용재,조경석,박영득,최성환,장비호,김수진,Kim, Y.H.,Moon, Y.J.,Cho, K.S.,Park, Y.D.,Choi, S.H.,Jang, B.H.,Kim, S. 한국천문학회 2006 天文學論叢 Vol.21 No.2
We have successfully developed the KASI (Korea Astronomy and Space Science Institute) Solar Imaging Spectrograph (KSIS), which has been originally upgraded from the KASI solar spectrograph that was able to record solar spectra for a given slit region and to inspect the response function of narrow band filters. A prototype KSIS was developed in 2004 by using a scanning mirror in front of the spectrograph slit and a SBIG ST-8XE CCD camera. Its main disadvantage is that it took a long time (about 13 minutes) to scan a whole active region. In this work, we have upgraded the KSIS by installing a much faster Dalsa 1M15 CCD camera, which gives a data acquisition time of about 2.5 minutes. The software for KSIS was also improved for the new CCD camera on the basis of component-based development method. We have successfully made a test observation for a simple and small active region (AR10910) using the improved KSIS system. Our observations show that H-alpha images for several wavelengths have typical features in a sunspot as well as a H-alpha centerline image is quite similar to a BBSO H-alpha image, demonstrating the capability of the KSIS system.
박병곤,성현철,장정균,장비호,이병철,박윤호,김강민,한인우,Park, B.G.,Seong, H.C.,Jang, J.G.,Jang, B.H.,Lee, B.C.,Park, Y.H.,Kim, K.M.,Han, I. 한국천문학회 2003 天文學論叢 Vol.18 No.1
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.
박은서,유성열,임형철,방승철,서윤경,박장현,조중현,박종욱,나자경,장정균,장비호,김광동,김병인,박철훈,이성휘,함상용,손영수,Park, Eun-Seo,Yu, S.Y.,Lim, H.C.,Bang, S.C.,Seo, Y.K.,Park, J.H.,Jo, J.H.,Park, J.U.,Nah, J.K.,Jang, J.G.,Jang, B.H.,Kim, K.D.,Kim, 한국천문학회 2012 天文學論叢 Vol.27 No.3
KASI (Korea Astronomy and Space Science Institute) has developed an SLR (Satellite Laser Ranging) system since 2008. The name of the development program is ARGO (Accurate Ranging system for Geodetic Observation). ARGO has a wide range of applications in the satellite precise orbit determination and space geodesy research using SLR with mm-level accuracy. ARGO-M (Mobile, bistatic 10 cm transmitting/40 cm receiving telescopes) and ARGO-F (Fixed stationary, about 1 m transmitting/receiving integrated telescope) SLR systems development will be completed by 2014. In 2011, ARGO-M system integration was completed. At present ARGO-M is in the course of system calibration, functionality, and performance tests. It consists of six subsystems, OPS (Optics System), TMS (Tracking Mount System), OES (Opto-Electronic System), CDS (Container-Dome System), LAS (Laser System) and AOS (ARGO Operation System). In this paper, ARGO-M system structure and integration status are introduced and described.
박병곤,장정균,성현철,장비호,김강민,한인우,Park, B.G.,Jang, J.G.,Seong, H.C.,Jang, B.H.,Kim, K.M.,Han, I. 한국천문학회 2003 天文學論叢 Vol.18 No.1
A CCD camera for the BOES (Bohyunsan Observatory Echelle Spectrograph) has been developed. The camera consists of a 2048 ${\times}$ 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 ${\pm}1^{\circ}C$. The final chip temperature is around -105$^{\circ}C$ with the setting value for the CFC as -170$^{\circ}C$.
조경석,조경석,문용재,장비호,김수진,김연한,Park, Y.D.,Cho, K.S.,Moon, Y.J.,Jang, B.H.,Kim, S.J.,Kim, Y.H. 한국천문학회 2003 天文學論叢 Vol.18 No.1
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${\AA}$ with the spectral resolution of 1${\AA}$/mm. The system is composed of a 40cm diameter Coelostat with 9m focal length, spectroscopic system with 600groove/mm grating, and a IK ${\times}$ 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.