• 천문학회보
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• 제39권1호
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• pp.52.2-52.2
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• 2014

The Immersion Grating Infrared Spectrometer (IGRINS) is an unprecedentedly minimized infrared cross-dispersed echelle spectrograph with a high-resolution and high-sensitivity optical performance. A silicon immersion grating features the instrument for the first time in this field. IGRINS will cover the entire portion of the wavelength range between 1.45 and $2.45{\mu}m$ accessible from the ground in a single exposure with spectral resolution of 40,000. Individual volume phase holographic (VPH) gratings serve as cross-dispersing elements for separate spectrograph arms covering the H and K bands. On the 2.7m Harlan J. Smith telescope at the McDonald Observatory, the slit size is $1^{\prime\prime}{\times}15^{\prime\prime}$. IGRINS has a $0.27^{\prime\prime}$ pixel-1 plate scale on a $2048{\times}2048$ pixel Teledyne Scientific & Imaging HAWAII-2RG detector with SIDECAR ASIC cryogenic controller. The instrument includes four subsystems; a calibration unit, an input relay optics module, a slit-viewing camera, and nearly identical H and K spectrograph modules. The use of a silicon immersion grating and a compact white pupil design allows the spectrograph collimated beam size to be 25mm, which permits the entire cryogenic system to be contained in a moderately sized rectangular vacuum chamber. The fabrication and assembly of the optical and mechanical hardware components were completed in 2013. In this presentation, we describe the major design characteristics of the instrument and the early performance estimated from the first light commissioning at the McDonald Observatory.

• Journal of Astronomy and Space Sciences
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• 제14권1호
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• pp.87-93
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• 1997

Radiometers in UV and visible wavelengths were onboard the Korean Sounding Rocket(KSR)-1 and 2 which were launched on June 4th and September 1st, 1993. These radiometers were designed to capture the solar radiation during the ascending period of the rocket flight. The purpose of the instrument was to measure the vertical profiles of stratospheric ozone densities. Since the instrument measured the solar radiation from the ground to its apogee, it is possible to investigate the altitude variation of the measured intensity and to estimate the effect of atmospheric scattering by comparing the UV and visible intensity. The visible channel was a reference because the 450-nm wavelength is in the atmospheric window region, where the solar radiation is transmitted through the atmosphere without being absorbed by other atmospheric gases. The use of 450-nm channel intensity as a reference should be limited to the altitude ranges above the certain altitudes, say 20 to 25km where the signals are not perturbed by atmospheric scattering effects.

• 천문학회보
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• 제35권2호
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• pp.25-25
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• 2010

With the aim of resolving important physical problems in the chromosphere of the Sun, we developed the Fast Imaging Solar Spectrograph for several years, and at last successfully installed it in the Coude room of the 1.6 meter New Solar Telescope at Big Bear in 2010 May. The instrument is an Echelle spectrograph with imaging capability based on slit scan, and can record two spectral bands (e.g., H alpha band and Ca II 8542 band) simultaneously. The early runs of the instrument produced data of high quality that are suited for the study of quiet Sun, filaments on the disk, prominences outside the limb, active regions and sunspots. We are ready to do good solar sciences using our own instrument, and will be able to do best sciences with the coming improvement of spatial resolution.

• 천문학회보
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• 제36권1호
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• pp.27.2-27.2
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• 2011

The Kepler(NASA) and CoRoT(ESA) space telescopes are surveying thousands of exoplanet for finding Earth-like exoplanets with similar environments of the Earth. Then the TPF(NASA), DARWIN(ESA) and many large-aperture ground telescopes have plan for spectroscopic observations of these earth-like exoplanets in next decades. Now, it has been started to simulate the disk averaged spectra of the earthlike exoplanets for comparing the observed spectra and suggesting solutions of environment of these planets. Previous research, the simulations are based on radiative transfer method, but these are limited by optical models of Earth system and instruments. We introduce a new simulation method, IRT(Integrated Ray Tracing) to overcome limitations of previous method. The 3 components are defined in IRT; 1)Sun model, 2)Earth system model (Atmosphere, Land and Ocean), 3)Instrument model. The ray tracing in IRT is simulated in composed 3D real scale space from inside the sun model to the detector of instrument. The Sun model has hemisphere structure with Lambertian scattering optical model. Atmosphere is composed of 16 distributed structures and each optical model includes BSDF with using 6SV radiative transfer code. Coastline and 5 kinds of vegetation distribution data are used to land model structure, and its non-Lambertian scattering optical model is defined with the semi-empirical "parametric kernel method" used for MODIS(NASA) and POLDER(CNES) missions. The ocean model includes sea ice cap structure with the monthly sea ice area variation, and sea water optical model which is considering non-lambertian sun-glint scattering. Computation of spectral imaging and radiative transfer performance of Earth system model is tested with hypothetical space instrument in IRT model. Then we calculated the disk averaged spectra of the Earth system model in IRT computation model for 8 cases; 4 viewing orientation cases with full illuminated phase, and 4 illuminated phase cases in a viewing orientation. Finally the DAS results are compared with previous researching results of radiative transfer method.

• 천문학회지
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• 제51권4호
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• pp.111-117
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• 2018

A numerical method is proposed to calculate the response of detectors measuring particle energies from incident isotropic fluxes of electrons and positive ions. The isotropic flux is generated by injecting particles moving radially inward on a hypothetical, spherical surface encompassing the detectors. A geometric projection of the field-of-view from the detectors onto the spherical surface allows for the identification of initial positions and momenta corresponding to the clear field-of-view of the detectors. The contamination of detector responses by particles penetrating through, or scattering off, the structure is also similarly identified by tracing the initial positions and momenta of the detected particles. The relative contribution from the contaminating particles is calculated using GEANT4 to obtain the geometric factor of the instrument as a function of the energy. This calculation clearly shows that the geometric factor is a strong function of incident particle energies. The current investigation provides a simple and decisive method to analyze the instrument geometric factor, which is a complicated function of contributions from the anticipated field-of-view particles, together with penetrating or scattered particles.

• 천문학논총
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• 제22권4호
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• pp.169-175
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• 2007

The international cooperation project CIBER (Cosmic Infrared Background ExpeRiment) is a rocket-borne instrument, of which the scientific goal is to measure the cosmic near-infrared extra-galactic background to search for signatures of primordial galaxy formation. CIBER consists of a wide-field two-color camera, a low-resolution absolute spectrometer, and a high-resolution narrow-band imaging spectrometer. Currently, all the subsystems have been built, and the integration, testing, and calibration of the CIBER system are on process for the scheduled launch in June 2008.

• 우주기술과 응용
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• 제2권1호
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• pp.41-51
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• 2022

큐브위성은 기존의 인공위성과 마찬가지로 지구 관측뿐만 아니라, 우주탐사 분야에도 폭넓게 활용되는 인공위성 플랫폼이다. 또한 우주 공간물리현상을 관측하기 위한 자기장관측 임무에서도 다양한 형태로 제작되어 활용되고 있다. 자기장 측정의 경우, 일반적으로 위성의 자기 교란을 최소화하기 위해 자기장측정기가 위성 몸체로부터 멀리 떨어져 있다. 그러나 큐브위성과 같은 작은 위성의 경우 공간적인 제약으로 인해 자기장 센서의 위치 설정이 제한적이다. 이에 이 논문에서는 큐브위성에서 생성된 자기장 간섭을 추정하여 자기장 측정의 신뢰성에 얼마나 영향을 줄 수 있는지 분석하였다. 주요 잡음원으로는 상대적으로 높은 소비전력을 가진 반작용 휠과 자기 토크로드를 대상으로 조사하였다. 이러한 부품의 자기 쌍극자 모멘트는 제조업체의 데이터 시트에 제공된 정보를 사용하였다. 외부 자기장이 없는 공간에서 3 U 큐브위성 중간에 위치한 자기 토크로드의 잔류 모멘트의 영향은 위성의 몸체 최 외곽 끝에서 약 36,000 nT까지 나타날 수 있음을 확인했다. 또한, 1 nT 미만의 정확한 자기장 측정의 임무라면, 자력계는 위성 본체에서 약 0.6 m 반경 거리 외곽에 있어야 함을 알 수 있었다. 이러한 분석 방법은 자기장 측정을 수행하기 위해 CubeSat을 설계할 때 자기 청결도 분석의 중요한 역할이 될 것으로 기대한다.

• Journal of Astronomy and Space Sciences
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• 제23권4호
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• pp.425-434
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• 2006

한국천문연구원에서 개발 중인 근적외선카메라 KASINICS(KASI Near Infrared Camera System)의 운용을 위한 온도 진공 모니터 시스템을 개발하였다. 이 시스템은 하드웨어 부분과 소프트웨어 부분으로 나누어지며, 온도와 진공도의 측정자료를 실시간으로 PC에서 출력하고 저장할 수 있도록 구성하였다. 이 시스템은 KASINICS와 같은 적외선카메라뿐만 아니라 극저온 냉각을 요하는 모든 장치에 적용할 수 있다. 우리는 KASINICS의 냉각 및 진공 시험을 수행하면서 우리가 개발한 모니터 시스템이 적외선카메라의 시험과 운용에 있어서 효율적이고 안정적이라는 것을 확인할 수 있었다.

• Journal of Astronomy and Space Sciences
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• 제22권1호
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• pp.59-68
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• 2005

현재 추진 중인 국제우주정거장 우주실험장비 개발에 대비하여 한국항공우주연구원에서는 우주 활용을 위한 데이터인터페이스를 조사/분석하였고, 이를 국제우주정거장 (ISS; International Space Station)의 데이터인터페이스 시뮬레이터에 적용하여 설계 및 제작을 완료하였다. 본 논문에서는 우주활용을 위한 국제우주정거장 데이터인터페이스 시뮬레이터 개발의 설계/구현에 관한 내용을 설명한다. 국제우주정 거장 데이터인터페이스 시뮬레이터는 실험장비, 탑재체, 주거 시설 등 국제우주정거장으로 데이터를 송수신하는 장치에 대한 모의 실험을 위한 장비로 범용적인 유인 우주 실험장비를 개발하는데 활용하기 장비이다. 또한 추후 탑재모듈 개발 시 GSE (Ground Station Equipment) 개발을 위한 초기연구로써의 의의도 있으며, 향후 개발될 우주실험 장비의 국제우주정거장과의 호환성 시험에도 활용 가능하다.

• Journal of Astronomy and Space Sciences
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• 제30권4호
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• pp.307-314
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• 2013

Infrared optical systems are operated at low temperature and vacuum (LT-V) condition, whereas the assembly and alignment are performed at room temperature and non-vacuum (RT-NV) condition. The differences in temperature and pressure between assembly/alignment environments and operation environment change the physical characteristics of optical and opto-mechanical parts (e.g., thickness, height, length, curvature, and refractive index), and the resultant optical performance changes accordingly. In this study, using input relay optics (IO), among the components of the Immersion GRating INfrared Spectrograph (IGRINS) which is an infrared spectrograph, a simulation based on the physical information of this optical system and an actual experiment were performed; and optical performances in the RT-NV, RT-V, and LT-V environments were predicted with an accuracy of $0.014{\pm}0.007{\lambda}$ rms WFE, by developing an adaptive fitting line. The developed adaptive fitting line can quantitatively control assembly and alignment processes below ${\lambda}/70$ rms WFE. Therefore, it is expected that the subsequent processes of assembly, alignment, and performance analysis could not be repeated.