• 천문학회보
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• 제43권1호
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• pp.49.1-49.1
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• 2018

The MATS (Mesosphere Airglow/Aerosol Tomography Spectroscopy) satellite is the next Swedish science microsatellite. We report optical performance test results of the limb telescope, which is the major payload. This telescope is designed with "linear astigmatism-free" (LAF) off-axis optical system in order to have high optical performance across the wide field of view. We measured Modulation Transfer Function (MTF) and Encircled Energy Diameter (EED) of the limb telescope. Full field imaging tests show expected results without linear astigmatism across the full field of view ($5.67^{\circ}{\times}0.91^{\circ}$). Since the amount of stray light is from the earth and the sun, we also simulated and measured the stray light in the field image.

• 천문학회보
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• 제43권1호
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• pp.69.2-69.2
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• 2018

On 2018 March 27, a 1-m telescope was installed at the SNU Astronomical Observatory (SAO) which is a newly constructed building at the site where the previous Kwanak Observatory (Old observatory; 구천문대) stood. A series of test observations have been performed on this telescope, and we report the first results from the test observations in this poster. In particular, we present seeing values, limiting magnitudes and sample images taken with a $4k{\times}4k$ CCD camera ($21^{\prime}{\times}21^{\prime}$).

• 천문학회보
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• 제43권1호
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• pp.50.1-50.1
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• 2018

We present the development of tools for Echelle spectrograph of NYSC 1-m telescope. The eShel spectrograph(Shelyak) has operated at Deokheung Optical Astronomy Observatory since 2016. We carried out test observation in 2016 and completed the preprocessing and wavelength calibration of the spectroscopic data using IRAF. Based on the reduction process in IRAF, PySpecW, a set of tools for spectroscopic data was developed in 2017. PySpecW was optimized for NYSC 1m telescope, and written in Python for youth to use easily on any OS. PySpecW consists of preprocessing, aperture tracing, aperture extraction, wavelength calibration, and dispersion correction for extracted spectra.

• 항공우주기술
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• 제12권2호
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• pp.64-73
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• 2013

심우주을 더욱 효율적으로 관측하기 위해서는 지구 대기권에 천체 망원경을 탑재한 인공위성을 운용하는 것이다. 미국과 EU 등 우주 선진국에서는 허블우주망원경, 케플러 및 허셜 우주 관측 위성 등에 의해 우주 정보를 획득하여 분석하고 있다. 본 논문에서는 외국의 주요 우주 관측 위성에 대한 사양 및 현황을 고찰하고, 국내의 심우주 탐사를 위한 기술과 계획 등에 대해 기술하고자 한다.

• Journal of Astronomy and Space Sciences
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• 제19권3호
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• pp.173-180
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• 2002

Images taken with the Chandra X-ray telescope have for the the first time revealed the central, wind-driven, hot bubble (Chu et al. 2001), while Hubble Space Telescope (HST) WFPC2 images of the Cat's Eye nebula, NGC 6543, show that the temperature of the halo region of angular radius ~ 20", is much higher than that of the inner bright H II region. With the coupling of a photoionization calculation to a hydrodynamic simulation, we predict the observed 〔O III〕 line intensities of the halo region with the same O abundance as in the core H II region: oxygen abundance gradient does not appear to exist in the NGC 6543 inner halo. An interaction between a (leaky) fast stellar wind and halo gas may cause the higher excitation temperatures in the halo region and the inner hot bubble region observed with the Chandra X-ray telescope.

• 천문학회보
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• 제38권1호
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• pp.69.1-69.1
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• 2013

We are developing Adaptive Optics (AO) system for 1m telescope at Gwacheon National Science Museum Observatory. The beam spot of the Gwacheon 1m telescope. The tip-tilt correction system consists of a CMOS sensor, a tip-tilt mirror and a feed back loop. The beam spot location at the CMOS sensor indicates the tip-tilt components of the incoming light. The tip-tilt mirror is controlled by DAC output voltage calculated by proportional-integral-derivative (PID) controller. This system successfully corrects the tip-tilt motion of the spot.

• 천문학회보
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• 제41권1호
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• pp.63.3-63.3
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• 2016

NYSC 1m telescope is completely assembled now, and equipped with FLI PL-16803 4k CCD and Shelyak eShel spectrograph (R~10,000) on optical system of f/8. From 12th Jan 2016, optical system alignment and test observations have been performed. We present the result of M35 photometric observation for the performance test of the 1m telescope. The photometric observation was carried out for the central part of M35 with the field of view, ${\sim}15^{\prime}.8{\times}15^{\prime}.8$. Standard transformation to the UBVI system was done by the photometric data of M35 in Sung and Bessell(1999).

• 천문학논총
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• 제30권2호
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• pp.749-751
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• 2015

We here report on the outreach activity using the Keio University Internet telescope performed by Science agora 2012 and 2013 in Tokyo. Many visitors came to our booth and operated the Keio University Internet telescope, and our project was awarded the prize of the National Institute of Advanced Industrial Science and Technology. In addition, based on the questionnaire for that occasion, the usefulness of the Internet telescopes in outreach activities is considered.

• 천문학회보
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• 제37권2호
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• pp.219.2-219.2
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• 2012

We are developing Adaptive Optics (AO) system for 24 inch telescope at Seoul National University Observatory. It consists of the tip-tilt correction system and the residual wavefront error correction system with a deformable mirror and a wavefront sensor. We present the construction and performance measurements of the tip-tilt correction system. The tip-tilt component is the single largest contributor to wavefront error, especially for small telescope. The tip-tilt correction system consists of a quadrant photodiode, a tip-tilt mirror and a feed back loop. The collimated He-Ne laser beam is used for input light source and is artificially disturbed by air turbulence generated by a heat gun. Most of the turbulence is of low frequency less than 20 Hz, but extends to a few hundreds Hz. It is found that the closed loop system using proportional-integral-derivative (PID) control successfully corrects tip-tilt error at a rate as high as 300~400 Hz.

• 천문학회보
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• 제37권2호
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• pp.234.1-234.1
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• 2012

The largest array SKA (Square Kilometre Array) project was proposed by astronomers from 10 countries, and first coordinated by the LTWG (Large Telescope Working Group) formed at the General Assembly of URSI (International Union of Radio Science) in 1993. It enters the pre-construction phase (2012-2015), towards the 10% SKA construction (2016-2019) called SKA1 and the rest of SKA (2019-2023) called SKA 2, under the leadership of the SKA Organisation (SKAO) established on November 23, 2011. I will review the Chinese participation in the SKA project at national, regional and global levels in the past two decades. During such a Long March to the SKA, a number of national Megascience projects have taken root and have been (are being) successfully constructed, with costs at the 100 M US dollar level, including the largest dish FAST (Five-hundred meter Aperture Spherical Telescope), which can be seen as a forerunner of the KARST (Kilometre Area Radio Synthesis Telescope) project, being as one of the two LDSN (Large Diameter Small Number) concepts for realizing the SKA. A close look at the FAST project gives an impressive snapshot of the construction phase in China.