• 천문학회보
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• 제36권2호
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• pp.129.1-129.1
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• 2011

We have applied an advanced multi-aperture indexing photometry and sophisticated de-trending method to existing Taiwanese-American Occultation Survey (TAOS) data sets. TAOS, a wide-field ($3^{\circ}{\times}3^{\circ}$) and rapid photometry (5Hz) survey, is designed to detect small objects in the Kuiper Belt. Since TAOS has fast and multiple exposures per zipper mode image, point spread function (PSF) varies in a given image. Selecting appropriate aperture among various size apertures allows us to reflect these variations in each light curve. The survey data turned out to contain various trends such as telescope vibration, CCD noise, and unstable local weather. We select multiple sets of stars using a hierarchical clustering algorithm in such a way that the light curves in each cluster show strong correlations between them. We then determine a primary trend (PT) per cluster using a weighted sum of the normalized light curves, and we use the constructed PTs to remove trends in individual light curves. After removing the trend, we can get each synthetic light curve of star that has much higher signal-to-noise ratio. We compare the efficiency of the synthetic light curves with the efficiency of light curves made by previous existing photometry pipelines. Our photometric method is able to restore subtle brightness variation that tends to be missed in conventional aperture photometric methods, and can be applied to other wide-field surveys suffering from PSF variations and trends. We are developing an analysis package for the next generation TAOS survey (TAOS II) based on the current experiments.

• 천문학회지
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• 제49권6호
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• pp.289-293
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• 2016

We investigate the long-term spatial drift of the center and the temporal variation of the shutter delay time map of Y4KCam mounted on the CTIO 1.0 m telescope. We have collected shutter delay time maps over eight years as a part of our long-term survey program. We find that the center of the shutter delay time map can drift up to $450{\mu}m$, equivalent to ${\approx}30pixels$, on the CCD. This effect can result in a small amount of error in integration time without the proper shutter delay time correction, but it does not appear to cause any significant problems in photometric measurements. We obtain a mean shutter delay time of $69.1{\pm}0.8$ ms and find no temporal variation of the shutter delay time of Y4KCam over eight years, indicative of the mechanical stability of the shutter. We suggest that using a master shutter delay time correction frame would be sufficient to achieve high precision photometry, which does not exceed photometric errors ${\approx}1.7mmag$ across the CCD frame for exposure times longer than 1 s.

• 천문학회지
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• 제45권1호
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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.

• 한국지구과학회지
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• 제36권7호
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• pp.661-673
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• 2015

우즈베키스탄 Maidanak 천문대 AZT-22 1.5 m 망원경(f/7.74)과 SITe $2000{\times}800$CCD를 사용하여 3개의 ${\delta}$ Cep 변광성 CEa Cas, CEb Cas 및 CF Cas가 있는 중년 산개성단 NGC 7790의 UBVI 측광 관측을 수행하였다. 관측자료는 IRAF/DAOPHOT를 이용하여 PSF 측광을 수행하였으며, V와 I 필터에서 모두 측광된 별의 수는 총 1008개이며, 측광의 한계등급은 $V{\approx}22$등급이다. 대기소광계수 및 측광영점을 결정하기 위하여 천구적도에 있는 여러 표준별과 청색 및 적색 표준별을 다양한 대기투과량에서 관측하였다. 표준별 측광을 통해 대기소광계수 및 측광영점을 결정하고, 성단의 측광자료는 Johnson-Cousins UBVI 표준계로 변환하였다. NGC 7790의 UBVI 색-등급도와 색-색도에서 이 성단의 B와 V 필터에서의 색초과량 [$E(B-V)=0.58{\pm}0.02$], B와 V 필터에서의 선택적 소광량 [$R_V{{\equiv}}A_V/E(B-V)=3.02{\pm}0.09$] 및 거리지수($V_0-M_V=12.65{\pm}0.10$)를 얻었다. H-R도에서 세페이드 변광성의 위치를 고려하여 나이를 결정하였다. 이 과정에서 Padova 연구집단(Bressan et al., 2012)의 등연령곡선(Z=0.019)과 Geneva 연구집단($Ekstr{\ddot{o}}m$ et al., 2012)의 등연령곡선(Z=0.014)을 모두 사용하였고, 그중에서 자전을 고려한 Geneva 연구집단의 진화모형이 관측자료와 잘 일치하여 NGC 7790의 나이로 log $age=8.05{\pm}0.05$ [yr]를 얻었다. 또 NGC 7790내 세페이드 변광성의 절대등급은 세페이드 변광성의 평균 주기-광도 관계에 비해 분산 범위 내에 있기는 하지만 주어진 주기에서 평균적으로 약 0.5등급 정도 밝음을 확인하였다.

• Journal of Astronomy and Space Sciences
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• 제17권1호
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• pp.53-66
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• 2000

한국 천문연구원은 국내 관련 기업과 함께 열전냉각방식 (thermoelectric cooler, 이하 TEC)을 이용한 실용화 극미광 영상장비를 개발하였다. 개발한 모델을 구성하는 부품들은 Kodak사의 KAF-0401E($768{\times}512$ pixels, blue plus version) CCD 센서를 사용하였고, 국내 업체인 Thermotek의 TEC 모듈을 사용하여 $-25^{\circ}C$까지 냉각이 가능하다. 셔터는 Uniblitz사의 VS25S를 사용하여 최소 80ms의 노출을 할 수 있다. PC와의 인터페이스는 현재 한국 천문연구원에서 개발하여 사용중인 ISA 버스의 컨트롤러 보드를 사용하고 12bit 비디오 프로세서인 AD9816을 사용하여 영상을 얻는다. 암잡음은 $-10^{\circ}C$에서 $0.4e^-$/pixel/s이며 직선성은 $99.9{\pm}0.1%$, gain은 4.24e^-/ADU이고 전체 시스템 잡음은 $25.3e^-(rms)$이다. 실험한 모델은 측광이 가능할 정도 ($\pm$0.01등급)의 정밀도를 가지고 천문관측 뿐만 아니라 다른 분야의 영상획득에 유용하게 사용 할 수 있을 것이다.

• 천문학회보
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• 제40권1호
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• pp.89.1-89.1
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• 2015

Period changes found in the 10 years CCD BVR photometry data (2005 - 2014) of the Intermediate Polar MU Cam will be discussed. The timings of extrema of the data are determined and the new ephemeris for the spin period and orbital period have been calculated by using multi-periodic approximation as follows: BJD(orb)=2454085.46(19)+0.19664 $10(26){\cdot}E$ and BJD(spin)=2454085.50725(91)+0.013740942(13) ${\cdot}$ $E-1.51(10){\times}10^{-12}{\cdot}E^2$. The O-C diagram shows an increasing of the spin period as $P=-2.20(14){\cdot}10^{-12}s/s$. It is also found in MU Cam that the white dwarf's rotation seems to be switched from a state of spin-down to spin-up by the white dwarf's equilibrium spin period in 2005.

• 천문학논총
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• 제6권1호
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• pp.62-75
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• 1991

The small sized telescope can be best used if the control and observation can be made remotely and fully automatically by the aid of computers. We discuss the possible ways of automating the existing telescopes of various designs using personal computers. 'We have specifically designed the parts necessary to automate 16 inch Cassegrain Telescope at Pusan University Observatory. The degree of automation we have set for the present work is the interactive. remote observation including opening and shutting down of dome slit. The observational modes we have in mind are photoelectric photometry and CCD imaging. The basic components of the hardware are interface card for 16 or 32 bit IBM PC family of computers, relay switches for the control of telescope movements, stepping motor controller card for the control of observational equipments, and AID converter unit that accepts signal from sensors for the environment conditions such as temperature, wind speeds, precipitation, etc. We also have designed and built a photoelectric photometer that can be fully controlled by the command of a computer. Such observational equipment is also essential in order that the remote observation can be realized.

• 천문학회지
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• 제43권4호
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• pp.115-121
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• 2010

UBVI CCD photometry is obtained for the Ruprecht 93 (Ru 93)region. We are unable to confirm the existence of an intermediate-age open cluster in Ru 93 from the spatial distribution of blue stars. On the other hand, we find two young star groups in the observed field: the nearer one (Ru 93 group) comprises the field young stars in the Sgr-Car arm at $d{\approx}2.1$ kpc, while the farther one (WR 37 group) is the young stars around WR 37 at $d{\approx}4.8$ kpc. We derive an abnormal extinction law ($R_V$ = 3.5) in the Ruprecht 93 region.

• Journal of Astronomy and Space Sciences
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• 제23권2호
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• pp.97-104
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• 2006

From the BV images of the metal-poor globular cluster NGC 1904 obtained with the 2K CCD camera equipped on the BOAO 1.8m telescope, we construct (B - V, V) color-magnitude diagram of the cluster. The apparent V magnitudes of the RGB bump and tip have been measured from the luminosity function of the iteratively selected RGB stars in NGC 1904. Theoretical absolute $M_v$ magnitudes of the RGB bump and tip are estimated using the Yonsei-Yale isochrones. The distance modulus of NGC 1904 has been derived by comparing the observed apparent V magnitude with the estimated absolute $M_v$ magnitude of the RGB bump and tip.

• 천문학논총
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• 제26권4호
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• pp.141-146
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• 2011

In the region of the open cluster M48 (NGC 2548), time-series BV CCD images were taken for 22 nights from February 28 in 2008 to March 17 in 2011. From this observation, we found 10 new variable stars. They include five eclipsing binaries, an RR Lyrae, two ${\delta}$ Scuti, and two semi-periodic and/or slow irregular type variable stars. We fail to find the member stars of the open cluster among the 10 variable stars.