http://chineseinput.net/에서 pinyin(병음)방식으로 중국어를 변환할 수 있습니다.
변환된 중국어를 복사하여 사용하시면 됩니다.
Calcium and CN bimodality of RGB stars in Globular clusters with Multiple Populations
임동욱,노동구,한상일,이영욱,Lim, Dongwook,Roh, Dong-Goo,Han, Sang-Il,Lee, Young-Wook 한국천문학회 2012 天文學會報 Vol.37 No.2
A number of recent observations have established that many globular clusters have double or multiple stellar populations. In particular, recent Calcium and Stromgren b & photometry shows a split in the RGB of some of these globular clusters, including M22, NGC 1851, and NGC 288. However, the origin of this split in the RGB is still controversial. In order to confirm the real difference in Calcium abundance between the two RGBs, we have performed low resolution spectroscopy for RGB stars in these globular clusters. The spectral data were obtained from WFCCD/duPont 2.5m telescope in Las Campanas Observatory. We found a significant bimodality of both Calcium and CN abundances in M22 and NGC 1851. NGC 288, however, shows a clear bimodality only in CN abundance.
박선엽,최진,노동구,박마루,조중현,임홍서,박영식,배영호,박장현,문홍규,최영준,조성기,최은정 한국우주과학회 2016 Journal of Astronomy and Space Sciences Vol.33 No.3
As described in the previous paper (Park et al. 2013), the detector subsystem of optical wide-field patrol (OWL) provides many observational data points of a single artificial satellite or space debris in the form of small streaks, using a chopper system and a time tagger. The position and the corresponding time data are matched assuming that the length of a streak on the CCD frame is proportional to the time duration of the exposure during which the chopper blades do not obscure the CCD window. In the previous study, however, the length was measured using the diagonal of the rectangle of the image area containing the streak; the results were quite ambiguous and inaccurate, allowing possible matching error of positions and time data. Furthermore, because only one (position, time) data point is created from one streak, the efficiency of the observation decreases. To define the length of a streak correctly, it is important to locate the endpoints of a streak. In this paper, a method using a differential convolution mask pattern is tested. This method can be used to obtain the positions where the pixel values are changed sharply. These endpoints can be regarded as directly detected positional data, and the number of data points is doubled by this result.
칼슘 및 협대역 측광 관측을 이용한 구상성단 NGC 6273의 항성종족 분석
서현주,한상일,노동구,임동욱,이영욱,Seo, Hyeon-Ju,Han, Sang-Il,No, Dong-Gu,Im, Dong-Uk,Lee, Yeong-Uk 한국천문학회 2012 天文學會報 Vol.37 No.2
NGC 6273은 우리은하 중앙팽대부 영역에 위치하고 수평계열이 확장되어 있는 구상성단으로 초신성에 의해 중원소 함량이 증가된 2세대 종족의 존재가 의심되는 성단 중 하나이다. 이를 보다 면밀히 조사하고자 2011년 6월, 칠레에 위치한 Las Campanas Observatory의 2.5m Du Pont 망원경과 2K CCD를 이용하여 Ca, b, 그리고 y 필터로 측광 관측을 수행하였다. 중원소 함량에 민감하게 반응하는 hk (hk=(Ca-b)-(b-y)) 색지수로 색등급도를 그려본 결과 적색거성계열이 관측오차의 8배 이상으로 매우 넓게 퍼져있는 것을 발견하였다. 이러한 현상이 중원소 함량 차이로 인한 것인지, 아니면 성간소광효과나 배경별에 의한 영향인지를 분석하였고, 그 결과 중원소 함량의 차이가 있는 다중종족의 존재 가능성을 배재할 수 없음을 확인하였다. 이를 확인하기 위한 저해상도 분광관측이 진행되고 있으며, 이의 예비분석 결과를 아울러 발표할 예정이다.
구상성단 M15에서 점근거성계열성에 의한 화학적 진화의 영향
장소희,주석주,노동구,한상일,김용철,김도균,이영욱 한국우주과학회 2011 한국우주과학회보 Vol.20 No.1
최근의 연구결과에 의하면 점근거성계열 단계에서 방출된 질소, 탄소, 산소 등 상대적으로 가벼운 원소들이 헬륨과 함께 구상성단의 화학적 진화에 영향을 미치는 것으로 밝혀졌다. 특히 Ventura & D'Anatona(2009)에 의하면 M15와 같이 중원소 함량이 낮은 구상성단일 경우 이 영향이 더욱 두드러진다. 우리는 이 효과가 구상성단 M15의 특이 수평계열 형태 및 Sandage 주기천이현상에 미치는 영향을 연구하기 위하여 질소 및 헬륨 함량이 대폭 증가된 항성진화트랙 및 종족합성모델을 구현하였다.
최진,조중현,김명진,노동구,박선엽,이희재,박마루,최영준,임홍서,배영호,박영식,조성기,문홍규,최은정,장현정,박장현 한국우주과학회 2016 Journal of Astronomy and Space Sciences Vol.33 No.2
Inactive space objects are usually rotating and tumbling as a result of internal or external forces. KOREASAT 1 has been inactive since 2005, and its drift trajectory has been monitored with the optical wide-field patrol network (OWL-Net). However, a quantitative analysis of KOREASAT 1 in regard to the attitude evolution has never been performed. Here, two optical tracking systems were used to acquire raw measurements to analyze the rotation period of two inactive satellites. During the optical campaign in 2013, KOREASAT 1 was observed by a 0.6 m class optical telescope operated by the Korea Astronomy and Space Science Institute (KASI). The rotation period of KOREASAT 1 was analyzed with the light curves from the photometry results. The rotation periods of the low Earth orbit (LEO) satellite ASTRO-H after break-up were detected by OWL-Net on April 7, 2016. We analyzed the magnitude variation of each satellite by differential photometry and made comparisons with the star catalog. The illumination effect caused by the phase angle between the Sun and the target satellite was corrected with the system tool kit (STK) and two line element (TLE) technique. Finally, we determined the rotation period of two inactive satellites on LEO and geostationary Earth orbit (GEO) with light curves from the photometry. The main rotation periods were determined to be 5.2 sec for ASTRO-H and 74 sec for KOREASAT 1.
최진,조중현,Yeuncheol Jeong,임홍서,최은정,노동구,김명진,박장현,조성기 한국우주과학회 2019 Journal of Astronomy and Space Sciences Vol.36 No.1
The Optical Wide-field patroL-Network (OWL-Net) is a global optical network for Space Situational Awareness in Korea. The primary operational goal of the OWL-Net is to track Low Earth Orbit (LEO) satellites operated by Korea and to monitor the Geostationary Earth Orbit (GEO) region near the Korean peninsula. To obtain dense measurements on LEO tracking, the chopper system was adopted in the OWL-Net’s back-end system. Dozens of angle-only measurements can be obtained for a single shot with the observation mode for LEO tracking. In previous work, the reduction process of the LEO tracking data was presented, along with the mechanical specification of the back-end system of the OWL-Net. In this research, we describe an integrity assessment method of time-position matching and verification of results from real observations of LEO satellites. The change rate of the angle of each streak in the shot was checked to assess the results of the matching process. The time error due to the chopper rotation motion was corrected after re-matching of time and position. The corrected measurements were compared with the simulated observation data, which were taken from the Consolidated Prediction File from the International Laser Ranging Service. The comparison results are presented in the In-track and Cross-track frame. The verification results show that the astrometric accuracy of the OWL-Net for LEO tracking was ±five arc seconds in the In-track direction.