• 천문학회보
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• 제43권1호
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• pp.49.2-49.2
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• 2018

Flux calibration for narrow band photometric data gives us an opportunity to get a line flux of extended targets. We developed flux calibration processes for narrow band photometry using broad band filters as a continuum indicator. We derived parameters for color correction and zero point correction including color terms. Applying our method, we successfully subtracted continuum emissions and calibrated the emission lines from an FU Ori type object, V960 Mon.

• 천문학회보
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• 제36권1호
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• pp.59.2-59.2
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• 2011

Constraining physical (or stellar population) properties - such as stellar mass, star-formation rate, stellar population age, and dust-extinction - of galaxies from observation is crucial in the study of galaxy evolution. This is very challenging especially for high-redshift galaxies, and a widely-used method to estimate physical properties of high-redshift galaxies is to compare their photometric spectral energy distributions (SEDs) to spectral templates from stellar population synthesis models. I will show that the SED-fitting results of high-redshift galaxies are strongly dependent on the assumed forms of star-formation histories. I will also present the results of SED-fitting analysis of observed Lyman-break galaxies which show that parametric models with gradually increasing star-formation histories provide better estimates of physical parameters of high-redshift (z>3) star-forming galaxies than traditionally-used exponentially declining star-formation histories. This result is also consistent with the predictions from the modern galaxy formation models.

• 천문학회보
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• 제44권1호
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• pp.62.1-62.1
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• 2019

Current large observational projects perform both static and dynamic sky surveys. The Thirty-Minute Target of Opportunity (TMT) is the project focusing on the dynamic sky survey using Korea Microlensing Telescope Network (KMTNet) that is the best observing system to investigate the dynamic sky. TMT aims to perform and experiment on following components : 1) to select transient or variable sources having hour to day scale cadences for future science cases, 2) to optimize the observation strategy for these objects, 3) to provide automated photometric pipelines for the time series data, and 4) to test the data release environment for all astronomers. In the near future, it is expected that a huge number of events will be alerted through large area surveys such as LSST. Therefore, the TMT project will provide opportunities to prepare the future large survey era as well as to understand the nature of interesting astronomical events.

• 천문학회보
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• 제46권2호
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• pp.56.3-56.3
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• 2021

In a ΛCDM universe, most galaxies are believed to evolve by mergers and accretions. The debris resulting from such processes remains faint and/or diffuse structures, such as tidal streams and stellar halos. Although these structures are a good indicator of the recent mass assembly history of galaxies, they have the disadvantage of being difficult to observe due to their low surface brightness (LSB). To recover these LSB features by reducing the photometric uncertainties introduced by the optics system, we attempt to develop an optimized telescope, called a linear astigmatism free-three mirror system, that minimizes the loss and scattering of light within the telescope. With that prototype, we observe NGC 5907, known as a nearby galaxy with a fabulous loop structure(s), to inspect its performance. After a dedicated data reduction process, including flat-fielding with dark sky flat and sky subtraction, our observation reaches a 1σ surface brightness limit of μlim,r ≃ 28.3 mag arcsec-2 in 10×10 arcsec boxes. We finally identify a single tidal stream that is likely the remnant of a nearly disrupted galaxy. This finding emphasizes that the capability of LSB detection with our telescope is comparable to that of much larger telescopes.

• Journal of Astronomy and Space Sciences
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• 제23권4호
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• pp.435-444
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• 2006

인공우주물체는 출현 시간이 비교적 짧고 운동 특성이 고정적이지 않기 때문에 한 번의 관측으로 측광 및 분광 데이터를 획득하기 어렵다. 따라서 인공우주물체의 측광 및 분광 동시 관측을 위해서 경희대학교 인공위성 추적 및 관측시스템에 다중 광학계를 탑재할 수 있는 가대를 설계하였다. 이 연구에서는 구조해석을 통해 다중 광학계 탑재 시에 개조된 가대의 변형을 계산하고 인공 우주물체 추적 및 관측 시 발생할 수 있는 가대의 지향오차를 추론하여 관측시야에서 인공우주물체를 안정적으로 추적할 수 있음을 보였다. 또한 등가응력 해석을 수행하여 가대의 구조적 안전성을 확인하였다.

• 천문학회보
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• 제38권1호
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• pp.52.1-52.1
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• 2013

We present preliminary results of the photometric variability analysis in SDSS r, i and z bands for a newly confirmed FU Orionis-type object, HBC 722. We observed HBC 722 from 2011 April to 2012 November, with Camera for Quasars in Early uNiverse (CQUEAN) attached to the 2.1m Otto Struve telescope at McDonald Observatory, USA. The rapid cadence monitoring observations (minute timescale) were conducted in chosen photometric nights during observation campaigns to get adequate number of samples for short term period analysis. As this object is in active state, temperature at the inner disk/stellar surface can be characterized by the colors between r, i and z bands. Also, It is theorized that a sudden cataclysmic accretion associated with FU Orionis-type outburst can give rise to detectable "hot spots" on the central star and rotational asymmetries in the disk instability region. Thus the periodic variabilities of three bands would trace the stellar rotation or Keplerian rotation at the instability region of the inner accretion disk. Additionally, the range of instabilities could be estimated on the assumption of a temperature distribution for the HBC 722 disk. This analysis can provide a clue for understanding enhanced disk accretion of Class II young stellar object.

• 천문학회보
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• 제36권2호
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• pp.148.1-148.1
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• 2011

We report the result of post-outburst observation of HBC722, the new FU Orionis-like young stellar object (also known as LkHa 188-G4 and PTF 10qpf; A. Miller et al., 2011). We have been monitoring this object since Nov. 2010 with KASINICS (Korean Astronomy and Space Institute Near Infrared Camera System) at Bohyun Optical Astronomy Observatory (BOAO). The observations were performed two times; the first observation was conducted in Nov. 19, 24, and 25, 2010. And the second one was done in March 22 and 25, 2011. We used three filters: J, H, and Ks band. We did aperture photometry with IRAF packages and standardized the photometric result (instrumental magnitude) with 2MASS data that were used as standard stars. As a result, we have found that the brightness of the target decreased in all bands and its colors reddened: the magnitudes and colors of the target are J=10.37, H= 9.49, Ks=8.59, J-H=0.88, and J-Ks=1.36 on Nov. 19, 2010. And those are J=10.81, H=9.81, Ks=9.28, J-H=1.00, and J-Ks=1.53 on March 25, 2011. The previous study showed the similar decrease of brightness in J and H band except for Ks band., They were J= 10.03, H= 9.14, and Ks= 8.65 on Sept. 2010 and those were J= 10.02, H=9.24, and Ks= 8.59 on Nov. 2010. Consequently, we can conclude that HBC722 is fading out continuously from last November to this March.

• Journal of Astronomy and Space Sciences
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• 제23권4호
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• pp.319-326
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• 2006

한국천문연구원의 NEOPAT 팀과 연세대학교 천문대의 YSTAR 팀이 공동으로 호주 Siding Spring 천문대에 설치한 광시야 자동망원경 2호기를 이용하여 W UMa형 식쌍성 BL Eri의 측광관측을 수행하였다. 이 망원경을 이용하여, 호주와 한국에서 각각 자동관측 모드 및 원격관측 모드로 6일 밤을 관측하여, 새로운 VRI CCD광도곡선과, 5개의 새로운 극심시각을 얻었다. Wilson & Deviney(1971)의 쌍성모델 2005 버전을 이용하여 우리의 광도곡선을 분석하고, 새로운 광도곡선 해를 구하였다. 이 과정에서 우리가 구한 질량비 0.48은 이전의 연구자들이 구한 값과 차이를 보이고 있다. 한편 이 방성계의 접촉상태를 Wilson & Deviney모델을 적용하여 확인한 결과, 현재 BL Eri는 접촉상태에 있는 것으로 보인다.

• 한국지구과학회지
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• 제28권1호
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• pp.87-104
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• 2007

소형망원경을 이용하여 산개성단 내 단주기 미세 변광성을 체계적으로 탐사하기 위한 보현산 천문대 측광 모니터링 프로그램 Short Period Variability Survey(SPVS)의 일환으로, 젊은 산개성단 NGC 129의 $90'{\times}60'$ 영역에 대한 V필터 시계열 측광 관측을 수행하였다. 성단의 관측은 보현산 천문대 155mm 소형 굴절 망원경과 $3K{\times}2K$ CCD 카메라를 이용하여 2004년 10월 12일부터 2005년 11월 3일까지 총 11일간 수행되었으며, 그 결과 전체 2400장의 V 필터시계열 CCD 영상자료 및 성단의 색-등급도를 얻었다. 시계열 자료의 기기등급을 표준등급으로 변환하기 위하여 앙상블정규화 기법(ensemble normalization technique)을 사용하였다. 측광 후 총 9537개별의 시간에 따른 광도변화를 조사한결과 총 66개의 새로운 변광성을 발견 하였다. 새롭게 찾아낸 변광성들은 DFT(Discrete Fourier Transform) 분석과 위상 맞추기 방법(phase-matching technique)을 이용하여 변광 주기를 결정하였다. 결정된 변광성의 주기 및 진폭 변화, 색-등급도 상에서의 변광성의 위치 등을 고려하여 변광 유형을 조사한 결과 9개의 SPB형 변광성과 9개의 ${\delta}$ Scuti형 변광성, 29개의 식변광성, 17개의 장주기 변광성과 기타 2개의 변광성으로 분류할 수 있었다. 본 연구를 통해, 산개성단에서의 변광성 탐사 연구에 소형망원경이 유용하게 활용될 수 있음을 확인하였다.

• 천문학회보
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• 제41권2호
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• pp.44.1-44.1
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• 2016

The Sagittarius-Carina spiral arm in the Galaxy contains several massive young open clusters. We present a deep optical photometric study on the massive young open clusters in the Sagittarius-Carina arm, Westerlund 2 and the young open clusters in the ${\eta}$ Carina nebula. Westerlund 2 is a less studied starburst-type cluster in the Galaxy. An abnormal reddening law for the intracluster medium of the young starburst-type cluster Westerlund 2 is determined to be $R_{V,cl}=4.14{\pm}0.08$. The distance modulus is determined from zero-age main-sequence fitting to the reddening-corrected color-magnitude diagrams of the early-type members to be $V_0-M_V=13.9{\pm}0.14mag$. The pre-main sequence (PMS) members of Westerlund 2 are selected by identifying the optical counterparts of X-ray emission sources from the Chandra X-ray observation and mid-infrared emission sources from the Spitzer/IRAC (the Infrared Array Camera) observation. The initial mass function (IMF) shows a slightly flat slope of ${\Gamma}=-1.1{\pm}0.1$ down to $5M_{\odot}$. The age of Westerlund 2 is estimated to be. 1.5 Myr from the main-sequence turn-on luminosity and the age distribution of PMS stars. The ${\eta}$ Carina nebula is the best laboratory for the investigation of the Galactic massive stars and low-mass star formation under the influence of numerous massive stars. We have performed deep wide-field CCD photometry of stars in the ${\eta}$ Carina nebula to determine the reddening law, distance, and the IMF of the clusters in the nebula. We present VRI and $H{\alpha}$ photometry of 130,571 stars from the images obtained with the 4m telescope at Cerro Tololo Inter-American Observatory (CTIO). RV,cl in the η Carina nebula gradually decreases from the southern part (~4.5, around Trumpler 14 and Trumpler 16) to the northern part around Trumpler 15 (~3.5). Distance to the young open clusters in the ${\eta}$ Carina nebula is partly revised based on the zero-age main-sequence fitting to the reddening-corrected color-magnitude diagrams (CMDs) and the (semi-) reddening-independent CMDs. We select the PMS members and candidates by identifying the optical counterparts of X-ray sources from the Chandra Carina Complex Survey and mid-infrared excess emission stars from the Spitzer Vela-Carina survey. From the evolutionary stage of massive stars and PMS stars, we obtain that the northern young open cluster Trumpler 15 is distinctively older than the southern young open clusters, Trumpler 14 (${\leq}2.5 Myr$) and Trumpler 16 (2.5-3.5 Myr). The slopes of the IMF of Trumpler 14, Trumpler 15, and Trumpler 16 are determined to be $-1.2{\pm}0.1$, $-1.5{\pm}0.3$, and $-1.1{\pm}0.1$, respectively. Based on the RV,cl of several young open clusters determined in this work and the previous studies of our group, We suggest that higher RV,cl values are commonly found for very young open clusters with the age of < 4 Myr. We also confirm the correlation between the slope of the IMF and the surface mass density of massive stars.