• The Bulletin of The Korean Astronomical Society
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• v.24 no.2
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• pp.29-29
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• 1999

• The Bulletin of The Korean Astronomical Society
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• v.28 no.2
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• pp.38-38
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• 2003

• Bulletin of the Korean Space Science Society
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• 1998.10a
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• pp.22.1-22
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• 1998

No Abstract.See Full-text

• Bulletin of the Korean Space Science Society
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• 1999.09a
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• pp.21-21
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• 1999

No Abstract, See Full Text

• Journal of The Korean Astronomical Society
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• v.45 no.1
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• pp.7-17
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• 2012

Y-band is a broad passband that is centered at ~1 ${\mu}m$. It is becoming a new, popular window for extragalactic study especially for observations of red objects thanks to recent CCD technology developments. In order to better understand the general characteristics of objects in Y-band, and to investigate the promise of Y-band observations with small telescopes, we carried out imaging observations of several extragalactic fields, brown dwarfs, and high redshift quasars with Y-band filter at the Mt. Lemmon Optical Astronomy Observatory and the Maidanak observatory. From our observations, we constrain the bright end of the galaxy and the stellar number counts in Y-band. We also test the usefulness of high redshift quasar (z >6) selection via i - z - Y color-color diagram, to demonstrate that the i - z - Y color-color diagram is effective for the selection of high redshift quasars even with a conventional optical CCD camera installed at a 1-m class telescope.

• Journal of Astronomy and Space Sciences
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• v.11 no.2
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• pp.208-231
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• 1994

We have undertaken CCD observations of fie이 standard stars with H$\beta$ photometric system to investigate the reliability of H$\beta$ CCD photometry. Flat fielding with dome flat and sky flat for H$\beta$w and H$\beta$n filter was compared with that of B filter in UBV system and, from these, we have not found any difference. It was confirmed that there is a good linear relationship between our H$\beta$ values observed with 2.3m reflector and standard values. However, H$\beta$ values observed with 60cm reflector at Sobaeksan Astronomy Observatory showed very poor relationship. To investigate the accuracy of H$\beta$ CCD photometry for fainter objects, open cluster NGC2437 was observed and reduced with DoPHOT, and the results were compared with those for photoelectric photometry of Stetson(1981).

• Publications of The Korean Astronomical Society
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• v.16 no.1
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• pp.37-42
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• 2001

We developed an observation program for a 2K CCD camera, which was newly attached at the SOAO (Sobaeksan Optical Astronomy Observatory) 61cm telescope. The program was designed to control the telescope as well as the CCD camera and to monitor the CCD image quality, with very easy under the window-based graphical user interface (GUI). Furthermore, applying the automated differential photometric algorithm, we can obtain the instrumental magnitudes of several variable and comparison stars in real-time. Simultaneous photometry enables us to get precise differential magnitudes of variable stars even if the weather condition is not photometric. This new observation system has been using for many astronomical observations from September, 2001.

• Journal of Astronomy and Space Sciences
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• v.24 no.2
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• pp.99-110
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• 2007

A total of 824 observations (206 in ${\Delta}B$, 206 in ${\Delta}V$, 206 in ${\Delta}R$, 206 in ${\Delta}I$ for CC Com were made on 3 nights from March 3 to April 3 in 2002 using the 61cm telescope with 2K CCD camera of the Sobaeksan Optical Astronomy Observatory of KASI. From our observations 9 times of minimum light were newly determined. Combined analysis of our new BVRI light curves with the double-lined radial velocity curves of Pribulla et al. (2007) were made with the 2004 Wilson-Devinney(WD) binary model code to yield new physical parameters of the CC Com system. Small asymmetries in light curves were explained with the adoption of two hot spots on the cool secondary.

• Journal of Astronomy and Space Sciences
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• v.23 no.3
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• pp.177-188
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• 2006

A total of 920 observations (230 in ${\Delta}B$, 230 in ${\Delta}V$, 230 in ${\Delta}R$, 230 in ${\Delta}I$) for V523 Cas were made on 5 nights from January 6 to 24 in 2003 using the 61cm telescope with 2K CCD camera of the Sobaeksan Optical Astronomy Observatory of KASI. From our observations 9 times of minimum light were newly determined. Combined analysis of our new BVRI light curves with the double-lined radial velocity curves of the Rucinski et al.'s (2003) were made with the 2004 Wilson-Devinney (WD) binary model to yield new physical parameters of the V523 system. Small asymmetries in light curves were explained with the adoption of a cool spot on the hot primary and a hot spot on the cool secondary.

• Journal of the Korea Academia-Industrial cooperation Society
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• v.6 no.2
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• pp.129-133
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• 2005

It is very important to use the charge coupled devices (CCDs) in spectrometry because we can study the molecular energy level, molecular structure, absorption or emission, intermolecular reaction, weakly bound molecular energy, photochemistry, fluorescence and photodynamic therapy (PDT). CCD is very essential to study the molecular structure and medical engineering combining laser spectroscopy in the modem physicsal and chemistry. Therefore, this study has designed and manufactured the electromagnetic spectrometry with CCD and then analyzed the printed electronic circuit. In the yesterday, CCD was thought to be used in only broadcasting system. But nowadays, it is used by industrial demand in observations, instrumentations and robotics as the industry develop.