• 천문학회보
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• 제35권2호
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• pp.36.1-36.1
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• 2010

The Redshift Search Receiver (RSR) is a sensitive, ultra-wideband spectrometer that is being built at the University of Massachusetts as one of the facility instruments for the 50-m Large Millimeter Telescope (LMT). It consists of four receivers each covering the entire 3 mm window from 74 to 111 GHz instantaneously. The primary goal of the receiver is to detect multiple molecular lines in galaxies at any distance and uniquely determine the redshift, in particular dust-obscured star forming systems at high-z which are not easily accessible. I will present some results from commissioning of the RSR on the Five College Radio Astronomy Observatory 14-m telescope, and discuss the future of the receiver.

• 천문학회보
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• 제35권1호
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• pp.28.1-28.1
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• 2010

Ground-based solar observations have several merits such as wider field of view and higher time cadence than those of satellite observations. The Domeless Solar Telescope of Hida Observatory is designed to acquire solar surface images at the highest possible spatial resolution using two types of spectrographs: a vertical spectrograph with the highest wavelength resolution in the world, and a horizontal spectrograph that can take images of the sun in multi-wavelength over the entire visible solar spectrum. The temporal variation of fine features such as chromospheric grains in the supergranulation cells and facular points in the network region has been obtained using DST Ca II K lines compared with Hinode Ca II H lines. This analysis is expected to provide a fundamental tool for research of diverse phenomena on the solar surface.

• 천문학회보
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• 제35권1호
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• pp.63.1-63.1
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• 2010

Over its 30-year lifetime, UKIRT has been the world's leading telescope devoted exclusively to observations in the infrared. Its outstanding success over this period is attributable to a number of factors, foremost among which are the size (3.6m) and high quality of the mirror, the excellent site at the summit of Mauna Kea, and the deployment of unique, world-beating instrumentation. In recent years, as the UK has re-directed its investment in astronomical facilities towards ESO, UKIRT has focussed on wide-field imaging in the near infrared, and we are currently conducting a definitive programme known as the UKIRT Infrared Deep Sky Survey (UKIDSS). In this presentation I will describe UKIRT's current capabilities, its evolving operation, opportunities for Korean participation, and possibilities for its future development.

• 천문학회보
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• 제35권2호
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• pp.31.1-31.1
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• 2010

We present a spectroscopic study of the globular clusters (GCs) in the giant elliptical galaxy (gE) NGC 4636 in the Virgo cluster. Line indices of GCs in NGC 4636 are measured from the integrated spectra obtained with Faint Object Camera and Spectrograph (FOCAS) on the Subaru Telescope. We derive the [Fe/H] of the GCs in NGC 4636 using Brodie & Huchra (1990) method. The [Z/H], age, and alpha-element of the GCs are obtained from the comparison of the Lick line indices with the SSP model grid. We investigate the distribution and radial variation of the metallicity, age, and alpha-element of NGC 4636 GCs. The metallicity distribution of NGC 4636 GCs shows a bimodality. The chemical properties of these GCs show little radial variation. These results will be discussed with regard to the formation and evolution of NGC 4636.

• 천문학회보
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• 제42권1호
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• pp.53.2-53.2
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• 2017

The origin of the well-known correlation between Hubble residual of Type Ia Supernova (SN Ia) and mass of their host galaxies is yet to be fully understood. In our first paper of our YOnsei Evolutionary Supernovae Evolutionary Investigation (YONSEI) project, we found a significant (${\sim}3.9{\sigma}$) correlation between host galaxy mass (velocity dispersion) and population age from high S/N host spectra observed using LCO 2.5 m telescope. Since there is no correlation with metallicity, our result suggests that stellar population age is mainly responsible for the relation between host mass and HR. In order to explore this more directly, we have subsequently observed more sample of nearby early-type host galaxies using MMT 6.5 m telescope. In this poster presentation, we will report our progress in this project and show the preliminary results from our MMT observations.

• 천문학회보
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• 제42권1호
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• pp.35.1-35.1
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• 2017

We present the characteristics and the performance of the new CCD camera system, SNUCAM-II (Seoul National University CAMera system II) that was installed on the Lee Sang Gak Telescope (LSGT) at the Siding Spring Observatory Australia in 2016. SNUCAM-II consists of a deep depletion chip covering a wide wavelength from $0.3{\mu}m$ to $1.1{\mu}m$ with high sensitivity (QE at 90%). It is equipped with SDSS ugriz filters and 13 medium band width (50nm) filters. On LSGT, SNUCAM-II covers $15.7{\times}15.7arcmin$ FOV at pixel scale of 0.92 arcsec and a limiting magnitude of g = 19.91 AB mag at $5{\sigma}$ with 180s exposure time. SNUCAM-II will enable us to study Spectral Energy Distributions (SEDs) of diverse objects from extragalactic sources to solar objects in the southern hemisphere for research and education activities.

• 천문학회보
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• 제42권1호
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• pp.36.2-36.2
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• 2017

Massive stars (${\geq}8M_{\odot}$) are believed to experience core-collapse and finish their lives as supernova (SN) explosions. Astronomers operating the current SN survey facilities try to catch the first moments of SN explosions. Since neutrinos are emitted first from the SNe before the electromagnetic lights, any neutrino detections from more than two sites within around 10 seconds could be useful alert for early follow-up observations, especially for optical SN follow-up telescopes. In this talk, I will brief the current SN follow-up observation projects, what they want to find out and contribute to SN sciences. Focus will be on the early detection and early sciences on SNe, which is what the Korean Neutrino Telescope can contribute most importantly.

• 천문학회보
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• 제43권1호
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• pp.67.1-67.1
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• 2018

We present high-resolution near infrared (IR) spectra of two candidate planetary nebulae (PNe) that were serendipitously found toward the Galactic center (GC). Our spectra obtained using GNIRS on Gemini North reveal strong Br ♑ and He I recombination lines. In one of the targets, we confidently detect Pa ♌ emission. Based on Br ♑ and Pa ♌ lines, we estimate a foreground reddening to be Av=27 mag, which confidently puts this object at the GC distance. Along with the presence of highly excited emission lines such as [S IV], [Ne III], [Ne V], and [O IV] detected in the mid-IR spectra from the Spitzer Space Telescope, and the extended emission in the Pa ♋ narrow-band image from the Hubble Space Telescope, this makes it the first spectroscopically confirmed PN in the GC.

• Journal of Astronomy and Space Sciences
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• 제17권2호
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• pp.221-232
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• 2000

밀리미터파 우주잔파 수신기의 국부 발진기로 사용될 수 있는 도파관형 건 발진기를 제작하였다. 제작한 건 발진기는 60 GHz에서 70 GHz까지 발진하는 광대역 특성을 보였다. 건 발진기는 공진 디스크와 포스트의 직경 변화와 다이오드 특성에 따라 발진 주파수의 특성이 달라진다. 본 논문에 우리는 광대역 발진 특성을 가지는 건 발진기의 설계 방법과 측정결과를 보였으며, 제작한 발진기는 대덕천파천문대의 100/150 GHz대 이중채널 수신기로 활용되고 있다.

• Journal of Astronomy and Space Sciences
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• 제32권3호
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• pp.269-279
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• 2015

Future space missions will have larger telescopes in order to look deeper into space while improvising on spatial resolution. The primary mirrors for these telescopes will be so large that using a monolithic mirror will be nearly impossible because of the difficulties associated with its fabrication, transportation, and installation on a launch vehicle. The feasibility of launching these huge mirrors is limited because of their small launch fairing diameter. The aerodynamic shape of the fairing requires a small diameter, but the height of the launch vehicle, which is available for designers to utilize, is larger than the fairing diameter. This paper presents the development of an axial deployment mechanism based on the screw jack principle. The mechanism was designed and developed, and a prototype was constructed in order to demonstrate a lab model.