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Near Infrared Wavelength Calibration without Telluric OH Lines
박수종,강원석,Nguyen, Ngan N.K.,Pak, Soojong,Kang, Wonseok 한국천문학회 2012 天文學會報 Vol.37 No.2
Grating spectrograph observation in near-infrared bands requires wavelength calibrations. We first need to extract order-strips from the echellogram data using flat images, and then to correct the spatial distortions and wavelength scales of the order strips using calibration arc lamps or the telluric OH emission lines. For very high resolution spectrograph using echelle, however, the arc lamps do not have enough emission lines in the order-strips, so we usually use the OH lines for accurate wavelength calibrations in wavelengths shorter than 2.3 microns. In this poster, we present wavelength calibration methods for longer wavelength bands using the telluric absorption lines in early-type stellar spectra and the telluric atmospheric transmission models. This technique will be applied to the data reduction pipeline for the IGRINS.
박수종,PAK SOOJONG 한국천문학회 2000 天文學論叢 Vol.15 No.suppl1
The purposes of spectroscopy in astronomy are to measure the radiation flux of the spectroscopic emission or absorption line and to measure the dynamical parameters of the line profile. In order to use an appropriate instrument for the scientific purpose, we need to understand the characteristics of various spectrometers, e.g., a prism spectrometer, a grating spectrometer, and a Fabry-Perot spectrometer (FPS), which are being used in ultra-violet, optical, and infrared bands. The FabryPerot spectrometer is not very popular compared to the grating spectrometer, because of its complex and tricky operations. The Fabry-Perot spectrometer, however, can get a two-dimensional image at one exposure, so we can study radiation mechanisms and dynamical properties of extended sources, e.g., clusters, nebula, and galaxies.
HIGH-RESOLUTION NEAR-INFRARED SPECTRA OF NEARBY QUASARS
박수종,임명신,Le, Huynh Anh Nguyen,Pak, Soojong,Im, Myungshin,Ho, LuisC. 한국천문학회 2012 天文學會報 Vol.37 No.2
We present high-resolution near-infrared host galaxy spectra of low-z quasars, PG0844+349 (z=0.064), PG1226+023 (z=0.158), and PG1426+015 (z=0.086). The observation was done by using the near-IR high resolution echelle spectrometer, IRCS, at the SUBARU 8.2 m telescope. The full width at half maximum of the point spread function was about 0.3 arcsec by using an Adaptive Optics system, which can effectively resolve the quasar spectra from the host galaxy spectra. The signal-to-noise ratios are increased by the total exposure time up to several hours per targets and the development of data reduction method. We compare our results to the stellar spectra library and sample spectra from Dasyra et al. (2007) and Watson et al. (2008). The identified spectral lines will be used to study the physical mechanism of quasars, and the velocity dispersions of the stars in the bulge of the host galaxy.
우주 기반 적외선 감시 정찰을 위한 초소형 위성용 비축 반사 광학계 연구
박수종(Soojong Pak),장승혁(Seunghyuk Chang),이대희(Daehee Lee) 한국국방우주학회 2023 한국국방우주학회지 Vol.1 No.1
최근 우주 기반 감시 정찰을 위한 다양한 방법이 시도되고 있다. 초소형 위성은 광학계 구경에 한계가 있어 중대형 위성에 비해 광학 해상도가 떨어지나 다수의 위성을 운용함으로써 광시야를 확보할 수 있고 재방문 주기를 단축할 수 있다. 본 연구에서는 f수 (초점거리/구경)가 작으면서 구경 대비 최적의 해상도를 갖는 초소형 위성 탑재용 적외선 망원경의 기술적 타당성을 검토했다. 일반적인 축대칭 반사 광학계는 부경에 의한 중앙 차폐 현상이 있어서 광학 해상도를 높이는 데 한계가 있다. 본 논문에서는 선형비점수차가 제거되는 혁신적인 동초점 비축 반사 이론을 적용하여 적외선 우주 관측에 최적화된 2-반사경 시스템과 3-반사경 시스템 망원경 시험 모델의 설계 및 성능 평가 결과를 보여준다. There are various methods for space-based surveillance and reconnaissance. While a small telescope onboard a CubeSat has limited optical resolution, satellite formation flying can maximize the surveillance area and the observation frequency. In this paper, we review the technical feasibility of the optics whose f-number (focal length to aperture size ratio) is small enough for a diffraction-limited infrared observation and whose size is compact enough for onboarding the CubeSat. A typical on-axis reflective optical system has limited optical resolution due to central obstruction caused by a secondary mirror. To overcome this problem, we apply an innovative confocal off-axis reflective theory that eliminates linear astigmatism aberration. We present the design and the test results of the prototype models for the 2-mirror and the 3-mirror confocal off-axis telescopes optimized for space-based infrared observations.
The Color Variability Monitoring of HBC722
백기선,박수종,강원석,전이슬,최창수,이정은,임명신,Baek, Giseon,Pak, Soojong,Green, Joel D.,Kang, Wonseok,Jeon, Yiseul,Choi, Changsu,Lee, Jeong-Eun,Im, Myungshin 한국천문학회 2012 天文學會報 Vol.37 No.2
We present the results of SDSS r, i and z band photometry for HBC722 (also known as $LkH{\alpha}$ 188 G4, PTF10qpf and V2493 Cyg), with Camera for Quasars in Early uNiverse (CQUEAN) attached to 2.1m Otto Struve telescope at McDonald Observatory, USA. HBC722 is a newly erupted FU Orionis type object, which produced optical outburst (${\Delta}V$=4.7 mag) over a year that peaked in 2010 September. We carried out the monitoring observations during 48 nights from 2011 April to 2012 June to check the short-term and the long-term variabilities for chasing the Keplerian rotation of the system. Comparing the photometric results of r, i and z band, we describe the color variability which is related to the physical properties of the system like circumstellar disk and accretion process.
김재영,박수종,강원석,최민호,Kim, Jaeyeong,Pak, Soojong,Kang, Wonseok,Choi, Minho 한국천문학회 2012 天文學會報 Vol.37 No.2
We performed near-IR imaging polarimetry of the $5{\times}9$ fields (${\sim}39^{\prime}{\times}69^{\prime}$) around 30 Doradus in the Large Magellanic Cloud (LMC), using the InfraRed Survey Facility (IRSF). We obtained polarimetry data in the J, H, and Ks bands using the JHKs-simultaneous imaging polarimeter SIRPOL in 2008 December and 2011 December. With the reliable LMC field data which were selected using a bad-data-rejection algorithm, we measured Stokes parameters of point-like sources to derive the degree of polarization and the polarization position angle. We present physical relationship between the three bands using the photometric and the polarimetric properties of the sources.
Environment Effects on the Stability of the CQUEAN CCD
최나현,박수종,최창수,박원기,임명신,전이슬,백기선,Choi, Nahyun,Pak, Soojong,Choi, Changsu,Park, Won-Kee,Im, Myungshin,Jeon, Yiseul,Baek, Giseon 한국천문학회 2012 天文學會報 Vol.37 No.2
Camera for QUasars in EArly uNiverse (CQUEAN) is an optical CCD camera attached to the 2.1m Otto Struve telescope at the McDonald Observatory, USA. CCD output signal contains the electrons generated by photoionization of incident light and thermal ionization. Therefore reliable photometric result can be obtained only under the stable condition of CCD thermal properties. We investigated the temperature dependency of the various characteristics of CQUEAN CCD chip, including bias level, dark level, gain, and quantum efficiency (QE), with the CQUEAN observation and calibration data obtained during 2012 May run. We discuss the environmental effects, i.e., ambient temperature, as well as CCD temperature on the stability of its characteristics.
유영삼,박수종,김민진,이성호,변용익,천무영,한원용,YU YOUNG SAM,PAK SOOJONG,KIM MINJIN,LEE SUNGHO,BYUN YONG-IK,CHUN MOO-YOUNG,HAN WONYONG 한국천문학회 2001 天文學論叢 Vol.16 No.1
We developed a CCD camera that can observe wide fields on the sky. We tested the field of views using various lenses. For cooling the CCD chip, we used a thermoelectric cooling device and tested the cooling efficiency. This camera will continuously observe a part of the sky. The data from the camera will be used to decide the current weather condition by the real-time star counting program (SCount) which will be developed later.
Type-Ia Supernova in M101: Latest Results
임명신,최창수,전이슬,전현성,박원기,김지훈,이지수,박수종,백기선,김상혁,오영석,전영범,성현일,윤태석,홍주은,김도형,김두호,장민성,현민희,박근홍,양희수,정일교,이방원,Im, Myungshin,Choi, Changsu,Jeon, Yiseul,Jun, Hyunsung,Park, Won-Kee,Kim, Ji Hoon,Lee, Jisoo,Pak, Soojong,Ba 한국천문학회 2012 天文學會報 Vol.37 No.2
SN 2011fe (also known as PTF 11kly) is a Type-1a supernova that appeared in M101, 2011 August. Being only 6.4 Mpc away, this supernova has been intensively observed by various facilities in the world. We monitored this supernova in UBVRI, grizY, and ZYJHK-bands using SNUO, LOAO, SOAO, CQUEAN/McDonald, UKIRT telescopes, and small telescopes in Korea and Mongolia. The monitoring observation is still ongoing, and the light curve has been accumulated over a year. We present the results of the long-term monitoring observation, together with a light-curve fitting result. We will also discuss our findings in terms of the usefulness of Type-Ia supernovae as a distance indicator.