• 천문학논총
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• 제29권3호
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• pp.35-44
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• 2014

In ground-based astronomical spectroscopic observations, there are many telluric absorption lines that are laid on the spectra of celestial objects. To study the physical properties of the celestial objects with these contaminated spectra, the telluric lines should be removed. A conventional method for removing the telluric lines is using the standard stellar spectrum as telluric line. In this paper, we introduce a technique to calculate synthetic telluric spectra and use them to remove telluric lines from a spectrum of a celestial object. We used Line-by-Line Radiative Transfer Model (LBLRTM) for calculating a synthetic spectrum and selected Michelson Interferometer for Passive Atmospheric Sounding (MIPAS) model as atmospheric model. We apply our method to some spectra obtained by Bohyunsan Observatory Echelle Spectrograph (BOES) to show that the telluric lines are well removed from the observed spectra by our model within an accuracy of 2% which is close to the 1-sigma rms of the original spectra.

• 천문학논총
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• 제24권1호
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• pp.35-41
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• 2009

We present a method to improve the RV (radial velocity) measurements accuracy by using telluric lines. Telluric lines are used to estimate the wavelength scale drift over the detector of the spectrograph. In the case of BOES, the Echelle spectrograph at BOAO (Bohyunsan Optical Astronomical Observatory), the wavelength scale drift can be several hundreds m/s over 24 hours. Due to the wavelength scale drift, the RV measurements accuracy of BOES is limited to several hundreds m/s. By estimating the wavelength scale drift by telluric lines, we can remove its effect to improve the RV measurements accuracy to about 40 m/s.

• 천문학회보
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• 제38권2호
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• pp.62.1-62.1
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• 2013

We present the Exposure Time Calculator of IGRINS (Immersion Grating Infrared Spectrograph). The noises of IGRINS and the simulated emission line can be calculated from the combination of Telluric background emission and absorptions, the emission and transmission of the telescope and instrument optics, and the dark noise and the read noise of the infrared arrays. For the atmospheric transmissions, we apply the simulated spectra depending on the Precipitable Water Vapor (PWV) values. In case of calculation of noises, the user needs to input the expected target magnitude, the weather conditions, and the desired exposure time. In addition to the simulated emission line, the parameters of rest wavelength, line-flux, Doppler shift and line-width are needed. The output would be the expected signal-to-noise for each spectral resolution element. The source-code of IGRINS-ETC v2.1.1 is available to be downloaded on the World Wide Web.

• 지구물리와물리탐사
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• 제6권2호
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• pp.64-70
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• 2003

본 연구에서는 토목현장에서 필요로하는 여러 파라미터들 중에서 물리탐사가 제공할 수 있는 영역을 한걸음 더 넓히고자 투수계수 산출을 위한 새로운 접근을 시도하였다. 전기비저항과 투수계수의 상관관계를 밝히기 위한 현장시험 결과 전기비저항검층과 수압시험(Lugeon test)에 의한 전기비저항-투수계수는 log-log 그래프상에서 반비례 관계를 만족하였다. 양산지역의 화강암과 안산암의 경우 $log(k){\approx}-0.85621\;log({\rho})+0.0031$ 의 관계를 보였으며 측선 상에서 수행된 AMT (Audio-frequency Magneto-Telluric) 탐사 결과와 이 식을 이용하여 전기비저항 단면을 2차원 투수계수 분포단면으로 변환하고 이를 지하수 유동모델링의 입력자료로 제공하였다.