• 한국통신학회논문지
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• 제34권1B호
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• pp.1-9
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• 2009

본 논문에서는 IETF NetLMM WG에서 표준화되고 있는 Proxy-MIPv6을 기반으로, 빠르고 효율적인 핸드오프를 지원하는 망 기반의 이동성 지원 방안을 제안하였다. 제안된 방식은 Mobile Access Gateway (MAG)간의 dynamic virtual hierarchy 망 구조를 활용함으로써 망의 확장성과 안정성을 제공하고, Policy Store(PS) 기반의 빠른 인증 및 프로파일 획득 기법을 활용함으로써 빠르고 효율적인 핸드오프를 제공할 수 있다. 또한, 제안된 방식과 기존의 PMIPv6의 성능 분석 및 토의를 통하여 제안된 방식의 우수성을 알 수 있다.

• 천문학회보
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• 제38권1호
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• pp.56.1-56.1
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• 2013

We have carried out follow-up observations of transiting extrasolar planets using small- to medium-sized reflectors located in Korea. Using the 0.60m telescope stationed at CbNUO (Chungbuk National University Observatory) we have achieved a photometric precision of 1.48 milli-magnitudes (root-mean-square scatter of data) of a HAT-P-09b (transit duration of 3.43 hrs) transit light curve (transit depth ~ 1.3%) with V=12.3 mag for the host star. We expect a photometric precision of 1.0 - 1.2 milli-magnitude for brighter targets (V ~ 10 - 11 mag). The transit technique and its application will be outlined. The results of test observations will be presented and the defocus technique will be discussed.

• 천문학회보
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• 제44권2호
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• pp.38.3-38.3
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• 2019

We present newly discovered dwarf galaxy candidates in deep wide-field images of NGC 1291 obtained with KMTNet. We identify 15 dwarf galaxy candidates by visual inspection within the virial radius of NGC 1291. Using imaging simulations, we demonstrate that our imaging data is complete up to 26 mag arcsec^-2 or -10 abs.mag with > 70% of the completeness rate. We also apply automated detection method to find the dwarfs. However, the completeness and the reliability are relatively low compared to the visual inspection. We find that structural and photometric properties of dwarf candidates such as effective radius, central surface brightness, Sérsic index, and absolute magnitude appear to be consistent with those of known dwarf galaxies in nearby groups and clusters, except for color. NGC 1291, residing in a relatively isolated environment, tends to accompany bluer dwarf galaxies (≃0.58) than those in denser environment. It shows that the quenching of dwarfs is susceptible to the environment.

• 한국항해학회지
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• 제23권3호
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• pp.29-34
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• 1999

In this paper, an X-band power amplifier using GaAs FET was designed and fabricated, which is to be used as SART transmitter sweeping at the frequency range of 9.2 GHz~9.5 GHz. The amplifier is consist of two stages using ATF-46101 FET of Hewllett-Packard. Finally, the amplifier using microstrip line matching solution shows that MAG is 23 dB at the center frequency of 9.35 GHz.

• 천문학회지
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• 제29권spc1호
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• pp.145-146
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• 1996

We have estimated a metal abundance of [Fe/H]= -0.04 $\pm$ 0.05 dex, a reddening of E(B- V)= 0.28 mag, an age of 1.1 $\pm$ 0.1 Gyr, and a distance of 2.5 $\pm$ 0.2 kpc for NGC 1245 using the Washington filter system.

• 천문학회지
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• 제29권spc1호
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• pp.147-148
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• 1996

We have estimated a metal abundance of [Fe/H]= -0.48 $\pm$ 0.14 dex, a reddening of E(B- V)= 0.30 mag, an age of 2.0 $\pm$ 0.4 Gyr, and a distance of 7.9 $\pm$ 0.8 kpc for Tombaugh 2 using the Washington filter system.

• 천문학회지
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• 제29권spc1호
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• pp.123-124
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• 1996

Snapshots of eight SA and standard fields from low to high galactic latitudes were made using the KPNO 0.9m 2K $\times$ 2K CCD with a limiting magnitude from 19 to 22.5. The purpose of this study is to determine the vertical distribution of stars with respect to Galactic latitude and z-distance in comparison with the model simulation between intermediate population to the 'thick disk' component of scale height of a few kpc. Comparison of the preliminary results between observed and model simulation for 3 of the S fields shows good agreement both in V-mag and B- V color distributions. A bimodal distribution in B- V at high galactic latitude seems to be represented by a halo and 'thick disk' dwarf in the blue and by a normal disk dwarf population in the red.

• 천문학회보
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• 제35권2호
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• pp.83.1-83.1
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• 2010

Recent observations of Sloan Digital Sky Survey (SDSS) for the ugriz filters have provided the largest and the most homogeneous photometric database. Especially, the ugriz systems have been used in many telescopes, such as SDSS, CFHT, and Gemini, and will be applied next generation large telescopes. In addition, many stellar evolution models, like as PADOVA, BaSTI and DSEP, have introduced theoretical isochrones in ugriz system, to apply the isochrones into the photometry of stars in globular clusters. In this study, we transformed Yonsei-Yale($Y^2$) isochrones to ugriz photometric system and fit the isochrones to the (g-r, r), (g-i, r), and (r-i, r) CMDs of 13 globular clusters (Chun et al. 2009, Clem et al. 2008, An et al. 2008). We found that the derived ages from $Y^2$-isochrones are 1~3Gyr younger and the estimated distance moduli are 0.3mag larger than the values inferred from the other isochrones in r-band. Also, the E(B-V) are 0.02~0.04mag less than those estimated from the other models. The ages of each globular cluster estimated from $Y^2$-isochrones are 12~14Gyr and distance moduli show good agreement with previous studies. From this result, we confirmed the availability of the $Y^2$-isochrones in gri filters. However, it is a problem which will improve that E(B-V) values obtained from $Y^2$-isochrones are too small. Finally, the result of this study is expected to be used research of globular cluster in ugirz photometric system.

• 대한전자공학회논문지SD
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• 제38권6호
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• pp.383-389
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• 2001

본 논문에서는 밀리미터파 대역에서 응용 가능한 AIGaAs/InGaAs PHEMT를 제작하고 특성을 분석하였다. 제작에 사용된 PHEMT 웨이퍼는 ATLAS 시뮬레이터를 이용하여 DC 및 RF 특성을 최적화 하였다. 게이트 길이가 0.35 ㎛이고 서로 다른 게이트 폭과 게이트 핑거 수를 갖는 PHEMT를 전자빔 노광장치를 이용하여 제작하였다. 제작된 소자의 게이트 길이와 핑거수에 따른 RF 특성변화를 측정 분석하였다. 게이트 핑거 수가 2개인 PHEMT의 DC 특성으로 1.2 V의 무릎 전압, -1.5 V의 핀치-오프 전압, 275 ㎃/㎜의 드레인 전류 밀도 및 260.17 ㎳/㎜의 최대 전달컨덕턴스를 얻었다. 또한 RF 특성으로 35 ㎓에서 3.6 ㏈의 S/sub 21/ 이득, 11.15 ㏈의 MAG와 약 45 ㎓의 전류 이득 차단 주파수 그리고 약 100 ㎓의 최대 공진주파수를 얻었다.

• 천문학회보
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• 제44권2호
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• pp.79.2-79.2
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• 2019

We introduce Maemi Dual Field Telescope System (MDFTS) which is newly installed at Kyung Hee Astronomical Observatory (KHAO). MDFTS consists of two telescope tubes (40cm and 10cm), whose observing fields are aligned with different field of view, 15' x 11' and 83' x 63' respectively. We present the specification of instruments (telescope, mount, camera, and filter system) and the observation environment of KHAO. We expect that MDFTS can be used for transient survey e.g. Intensive Monitoring Survey of Nearby Galaxies (IMSNG). Based on observations conducted so far, the limiting magnitude of 40cm telescope in B-band is B_lim ~ 16 mag at 5-σ detection with 150 seconds total integration time under dark and clear observing condition. Also the integrated observing software for MDFTS, KAOS40 is now under developing.