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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.
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.
Fluorescent Ultraviolet Spectra of Molecular Hydrogen in Star Forming Clouds
박수종,Dae-Hee Lee,Ewine F. van Dishoeck,민경욱,Youngsam Yu 한국물리학회 2003 THE JOURNAL OF THE KOREAN PHYSICAL SOCIETY Vol.42 No.III
The far-UV photons from the newly born stars make Photo-dissociation Regions (PDRs) on the surfaces of the nearby molecular clouds. In the PDRs, molecular hydrogens which absorb the far- UV photons in the Lyman-Werner bands are electrically excited, and then de-excited to the ground electrical states, emitting far-UV lines. These observations are only possible from space telescopes and can be one of the scientic purposes of the rst Korean scientic satellite. In order to prove the feasibility of observations for various celestial sources, we run a radiative transfer code to simulate the H2 uorescent lines with various physical conditions, i.e., gas density, gas temperature, external far-UV eld strength, and spectral energy distribution of the external UV eld. The code considers bound-continuum transitions as well as bound-bound transitions. The total uorescent intensities and the spectral shapes depend on the physical conditions. By observing the far-UV spectra from the PDRs, we can study the interaction of the young stars with the ambient clouds and the evolution process of the star forming clouds.
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 한국천문학회 2000 天文學論叢 Vol.15 No.2
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.