• 천문학회보
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• 제35권2호
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• pp.79.1-79.1
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• 2010

세종 산개성단 탐사관측 연구의 일환으로 중년 산개성단 NGC 2353에 대한 UBVI CCD 측광을 수행하였다. 측광학적인 방법으로 성단 내의 구성원을 선정하였으며, 이로부터 이 성단의 성간소광과 거리를 각각 E(B-V)=$0.10\pm0.02mag$와 $d=1.17\pm0.04\;kpc$으로 얻었다. 성단 구성원의 공간적인 분포를 통해서 성단의 형태가 북서 방향에서 남동 방향을 잇는 축을 중심으로 타원의 형태를 띠고 있는 것을 발견하였다. Padova 그룹이 제시한 이론적인 등연령 곡선을 관측한 색등급도에 맞춤으로써 이 성단의 나이를 1억 3천만년으로 추정하였으며, 이는 기존 연구보다 나이가 많은 것으로 나타났다. 구성원의 거리지수 분포에서 이 성단의 거리지수보다 밝은 곳에 나타나는 쌍성의 분포를 Gaussian 분포와 맞추어 $46\pm4%$ 정도의 최소 쌍성비율을 추정하였다. 마지막으로 광도함수와 질량함수를 유도하였고, 질량함수의 기울기는 $\Gamma=-1.4\pm0.2$를 얻었다.

• 천문학회보
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• 제35권2호
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• pp.81.1-81.1
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• 2010

We present a study of five open clusters (Alessi 53, Berkeley 49, Berkeley 84, Czernik 5, Pfleiderer 3) based on ugriz images of the Sloan Digital Sky Survey (SDSS). Physical properties of these clusters are not yet well known. The center and size of these clusters are determined using the radial number density profile. Using the proper motion data, we select the members of the target clusters. We estimate physical parameters of the clusters based on the isochrone fitting in the Color-Magnitude Diagram (CMD) : reddening, distance, and age. The foreground reddening is determined to be E(B-V)=0.71-1.55 mag. The distances to target clusters are derived to be 2.0-4.4 kpc, corresponding to the galactocentric distances of 7.5-11.9 kpc. Their ages are in the range of 280 to 1000 Myr. Their spatial distribution in our Galaxy is similar to that of other intermediate-age open clusters. We find ten blue straggler star candidates in Berkeley 49. This number of blue stragglers is a typical value for the age of Berkeley 49.

• 한국자기학회지
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• 제2권1호
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• pp.44-49
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• 1992

단롤법 급속응고기술을 이용하여 $Nd_{12}Fe_{80}B_{6}(Nb,\;M)$ (M=Ti/Cu/Ga) 리본을 제작하고 이의 자기특성 및 미세조작에 관한 연구를 하였다. X-선 회절 및 TEM을 이용한 미세조직 조사 결과, 리본의 이방화에 Ga이 효과적이며, 디스크표면속도 17.9 m/s로 제작한 $Nd_{12}Fe_{80}B_{6}(Nb,\;Ca)$ 리본은 약 30 nm의 미세한 결정립으로 구성되고 자유표면이 이방화된 조직으로 형성됨을 알았다. 이 리본을 분쇄하여 자장중에서 정렬시킨 분말의 잔류자속밀도는 0.87 T의 높은 값을 보였으며, 분쇄하기전 리본의 잔류자속밀도에 비하여 약 5% 정도 높았다. 이상의 결과로 부터 리본의 자유표면은 이방화가 되고 나머지 부분은 HIREM 특성을 나타내는 새로운 형태의 고특성 급속응고리본의 제조가 가능할 것으로 사료된다.

• 대한전자공학회:학술대회논문집
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• 대한전자공학회 2000년도 하계종합학술대회 논문집(2)
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• pp.12-15
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• 2000

In this paper, we have fabricated the PHEMT's with AlGaAs/InGaAs/GaAs and measured characteristics of DC and frequencies. The PHEMT's has a 0.35$\mu\textrm{m}$ gate length, gate width of 60$\mu\textrm{m}$ and 80$\mu\textrm{m}$, and fingers of 2 and 4. From the measurements results for the 60$\mu\textrm{m}$ ${\times}$ 2 PHEMT's, we obtained 1.2V of Vk, -3.5V of Vp, 46mA of Idss, 221mS/mmof gm, and 3.6dB of S$\sub$21/ gain, 45GHz of f$\sub$T,/ 100GHz of fmax. And, in case of 80$\mu\textrm{m}$ ${\times}$ 4 PHEMT's, we obtained 1.2V of Vk, -4.5V of Vp, 125mA of Idss, 198mS/mm of gm, and 2.0dB of S$\sub$21/ gain. 44GHz of f$\sub$T/, 70GHz of fmax at 35GHz frequency. Also, MAG are decreased as a number of finger are Increased.

• Journal of Astronomy and Space Sciences
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• 제16권2호
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• pp.91-104
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• 1999

We use BV CCD images to investigate the reality of the color gradient within a King type globular cluster NGC 7089. Surface photometry shows that there is a strong radial color gradient in the central region of the cluster in the sense of bluer center with the amplitude of ~0.39 $\pm$ 0.07 mag/$arcsec^2$ in (B - V). In the outer region of the cluster, however, the radial color gradient shows a reverse case, i.e., redder toward the center. (B - V) color profile which was derived from resolved stars in VGC 7089 field also shows a significant color gradient in the central region of the clusters, indicating that lights from the combination of red giant stars and blue horizontal branch stars cause the radial color gradient. Color gradient of the outer region of NGC 7089 may be due to the unresolved background of the cluster. Similar color gradients in the central area of clusters have been previously observed exserved exclusively in highly concentrated systems classified as post core collapse clusters. We caution, however, to confirm the reality of the color gradient from resolved stars, we need more accurate imaging data of the cluster with exceptional seeing condition because the effect of completeness correlates with local density of stars.

• 천문학회지
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• 제29권1호
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• pp.43-51
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• 1996

We present test results of time-series CCD photometry to investigate the photometric precision of the BOAO (Bohyunsan Optical Astronomy Observatory) 1.8m telescope. A well-known field of the old open cluster M67, which includes two pulsating blue stragglers and two W UMa type binaries, was monitored for 3.5 hours on February 22, 1996. We have collected 148 V frames and 3 B frames. Photometric noises which consist mainly of photon noise and scintillation noise, were lowered down to about 1.9 mmag for stars of $10.\;^m5$ in M67 with exposure time of 20 seconds. From the C-M diagram for M67, a number of observational properties were derived; E(B-V) = 0.03, (V-Mv)o = 9.6, Age = 4 Gyr. We obtained light curves for four known variable stars and confirmed their variational characteristics. The pulsating blue stragglers show a low amplitude (about 0.01 mag) of light variation.

• Mass Spectrometry Letters
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• 제2권1호
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• pp.8-11
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• 2011

Two types of glycerolipids [monoacylglycerols (MAG) and cyclitols] were isolated by reversed phase high-performance liquid chromatography from the methanol extracts of a marine sponge, and analyzed by fast atom bombardment mass spectrometry (FAB-MS) in positive-ion mode. FAB mass spectra of these compounds yielded protonated molecules $[M + H]^+$ and abundant sodiated molecules $[M + Na]^+$ from a mixture of 3-nitrobenzyl alcohol and NaI. The structures of these compounds were elucidated by FAB-collisional-induced dissociation (CID)-tandem mass spectrometry. We carried out collision-indused dissociation (CID) of these lipids in B/E-linked scan mode. The CID B/E-linked scan of $[M + H]^+$ and $[M + Na]^+$ precursor ions resulted in the formation of numerous characteristic product ions through a series of dissociative processes. The product ions formed by charge-remote fragmentation (CRF) provided important information for the identification of the acyl chain structure substituted at the glycerol backbone. Some of the product the ions were diagnostic for the presence of a glycerol backbone or acyl chain structure.

• 한국자기학회지
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• 제5권4호
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• pp.261-268
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• 1995

비대칭 자화 반전 효과의 원인을 조사하기 위하여 ${(Fe_{1-x}Co_{x})}_{75}Si_{10}B_{15}$계 비정질 자성 합금 리본을 부자장 중에서 열처리 온도 $380^{\circ}C$로 하여 16시간 동안 열처리한 후 합금 조성에 따른 자기 이력 곡선의 변화에 대하여 연구하였다. Fe나 Co만을 함유하고 있는 하금의 경우보다 이들 두 금속을 모두 함유하고 있는 비정질 합금 리본의 경우가 무자장 열처리에 의해서 자구벽내에 더 큰 유도 자기 이방성을 형성함으로써 보다 뚜렷한 비대칭 자화 반전 효과를 얻을 수 있었다. 또한 영자왜 조성에 가까운 비정질 합금의 경우에서 보다 뚜렷한 비대칭 자화 반전 효과를 얻을 수 있었는데, 두가지 금속 모두를 함유하는 특히 서로 비슷한 함량을 함유 하는 조성을 가질수록 뚜렷한 효과를 얻을 수 있다는 사실과 복합적으로 적용하였다.

• 천문학회보
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• 제36권1호
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• pp.63.2-63.2
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• 2011

We present a photometric study of star clusters in three nearby barred spiral galaxies NGC 1300, NGC 1672 and NGC 6217. We use the Hubble Heritage CCD images taken with Advanced Camera for Surveys (ACS) of Hubble Space Telescope (HST) in several filters. We have selected hundreds of star clusters with V $\leq$ 24 mag in each galaxy, based on the morphological parameters and visual inspection. Most of the blue star clusters with B-V $\leq$ 0.5 are strongly concentrated in spiral arms. A significant fraction of these star clusters are distributed in ansae (the joint between spiral arms and bar structure). Some of the blue star clusters are also found in the nuclear starburst region, especially in NGC 1672. A small number of star clusters are found in the bar region. In contrast, the red star clusters with B-V < 0.5 are relatively uniformly located over the entire field of galaxy, and show some central concentration around the bulge. We discuss the physical properties of these star clusters with the expected results from simulations.

• 천문학회보
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• 제45권1호
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• pp.60.2-60.2
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• 2020

In the hierarchical framework, galaxies grow through mergers and accretion. Those mechanisms leave faint features, such as stellar streams, shells and smooth stellar halos in the outskirts of galaxies. In order to search for those features in the nearby galaxies, we are conducting a KMTNet Nearby Galaxy Survey using the Korea Microlensing Telescope Network. We present a deep and wide-field imaging of NGC 5236, a barred spiral galaxy. In one-dimensional surface brightness profiles, we reach 28, 29 mag/arcsec2 in the R- and B-band, respectively. We find that the outer disk of NGC 5236 can be well described with a single exponential profile up to 17 kpc (~3.8 Reff) indicating that the excess light due to the stellar halo is not clearly detected. B-R color gradually increases towards the outskirts of the galaxy. It may reveal that stellar properties in the outskirts are marginally distinctive from those in the central part.