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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$^{\circ}C$.
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.