• 천문학회지
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• 제56권1호
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• pp.97-115
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• 2023

We present the deep homogeneous UBV RI photometric data of 135,071 stars down to V ~ 23 mag and I ~ 22 mag toward the Carina Nebula. These stars are cross-matched with those from the previous surveys in the X-ray, near-infrared, and mid-infrared wavelengths as well as the Gaia Early Data Release 3 (EDR3). This master catalog allows us to select reliable members and determine the fundamental parameters distance, size, stellar density of stellar clusters in this star-forming region. We revisit the reddening toward the nebula using the optical and the near-infrared colors of early-type stars. The foreground reddening [E(B-V)_fg] is determined to be 0.35 ± 0.02, and it seems to follow the standard reddening law. On the other hand, the total-to-selective extinction ratio of the intracluster medium (R_V,cl) decreases from the central region (Trumpler 14 and 16, R_V,cl ~ 4.5) to the northern region (Trumpler 15, R_V,cl ~ 3.4). It implies that the central region is more dusty than the northern region. We find that the distance modulus of the Carina Nebula to be 11.9 ± 0.3 mag (d = 2.4 ± 0.35 kpc) using a zero-age main-sequence fitting method, which is in good agreement with that derived from the Gaia EDR3 parallaxes. We also present the catalog of 3,331 pre-main-sequence (PMS) members and 14,974 PMS candidates down to V ~ 22 mag based on spectrophotometric properties of young stars at infrared, optical, and X-ray wavelengths. From the spatial distribution of PMS members and PMS candidates, we confirm that the member selection is very reliable down to faint stars. Our data will have a legacy value for follow-up studies with different scientific purposes.

• 한국전기전자재료학회:학술대회논문집
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• 한국전기전자재료학회 2003년도 춘계학술대회 논문집 유기절연재료 방전 플라즈마연구회
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• pp.81-84
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• 2003

유도결합형 플라즈마(Inductively coupled plasma)는 조명기술 분야에서도 효과적인 방전 소스로 이용되고 있다. 이중 무전극 램프에서의 유도결합형 플라즈마의 이용은 장수명은 물론 높은 효율과 넓은 동작 온도특성, 전원 인가시와 동시에 방전이 개시되는 등 여러 가지 장점을 가지고 있다. 본 논문에서는 Re-entr-ant Type QL-lamp에 사용되어진 페라이트의 형태에 변화를 주어 이에 따른 전자계 특성을 살펴보았다. 먼저 페라이트 코어의 특성에 따른 임의의 영역에서의 자속 및 자속밀도 그리고 자계강도 등을 고려하였으며, 시뮬레이션을 통한 페라이트 크기의 변화에 따른 전자계 분포 특성을 조사하였다.

• 핵의학기술
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• 제20권1호
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• pp.59-65
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• 2016

동적신장검사는 신장기능을 영상화하는 대표적인 방법이다. 동적신장검사에서 저선량 방사성의약품의 사용으로 기존 동적신장검사와 저선량을 사용한 신장검사의 비교를 통한 동적신장검사의 재현성을 평가해 보기로 했다. 본 비교실험을 통해 재현성이 우수할 경우 환자에 투여하는 방사선량을 줄인 동적신장검사법을 활용하고 환자의 피폭을 줄이고자 한다. 감마카메라 장비로는 Orbiter, SymbiaE (Siemens, Germany)를 사용하였고, 2013년 1월부터 2014년 2월까지 370 Mbq (10mCi)을 사용한 환자와 동일 환자 중 2014년 3월부터 2015년 7월까지 185 Mbq (5 mCi)을 사용한 환자를 대상으로 $^{99m}Tc-DTPA$사용 검사 21명과 $^{99m}Tc-MAG_3$사용 검사 20명 총 41명을 대상으로 데이터를 선별하였다. 결과 영상의 Renogram에서 Peak 지점의 프레임을 선택하여 신장의 관심영역과 배후방사능의 관심영역을 설정하고 K/B ratio를 구하여 비교하였다. $^{99m}Tc-DTPA$를 사용한 검사에서 370 Mbq을 사용하였을 때의 K/B ratio는 평균 $5.67{\pm}0.8$이었고, 185 Mbq을 사용하였을 때는 평균 $5.62{\pm}0.87$로 큰 차이를 보이지 않았다. $^{99m}Tc-MAG_3$를 사용한 검사에서도 신장/배후방사능 비는 370 Mbq을 사용 시 평균 $14.95{\pm}2.58$과 185 Mbq을 사용 시 평균 $14.56{\pm}2.02$로 큰 차이를 보이지 않았다. Paired sample t-test결과 p-value는 $^{99m}Tc-DTPA$ 0.566, $^{99m}Tc-MAG_3$ 0.363로 같은 비교집단 간 차이점이 없음을 확인하였다. 동일 환자를 대상으로 선량을 370 Mbq에서 185 Mbq로 줄였을 때의 동적신장검사의 재현성은 우수한 것으로 확인 되었다. 저선량 동적신장검사는 기존 감마카메라의 성능 개선 없이 재현성이 우수한 결과를 얻을 수 있고 환자의 피폭 또한 줄일 수 있을 것으로 사료된다.

• 천문학회지
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• 제40권1호
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• pp.17-28
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• 2007

We present wide-field $JHK_s$-band photometric observations of the three compact H II regions G48.9-0.3, G49.0-0.3, and G49.2-0.3 in the active star-forming region W51B. The star clusters inside the three compact H II regions show the excess number of stars in the $J-K_s$ histograms compared with reference fields. While the mean color excess ratio $(E_{J-H}/E_{H-K_s})$ of the three compact H II regions are similar to ${\sim}2.07$, the visual extinctions toward them are somewhat different: ${\sim}17$ mag for G48.9-0.3 and G49.0-0.3; ${\sim}23$ mag for G49.2-0.3. Based on their sizes and brightnesses, we suggest that the age of each compact H II region is ${\leq}2\;Myr$. The inferred total stellar mass, ${\sim}1.4{\times}10^4M_{\odot}$, of W51B makes it one of the most active star forming regions in the Galaxy with the star formation efficiency of ${\sim}10%$.

• 대한전자공학회논문지TC
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• 제47권10호
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• pp.74-79
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• 2010

본 논문에서는 70 nm mHEMT MMIC 기술을 이용한 고이득 W-band 증폭기를 제시한다. W-band에서 고이득 특성을 얻기 위하여 공통 소스 FET의 소스 피드백 라인의 길이를 조절하면 설계 주파수에서 이득이 최대가 되도록 하였다. 이 라인의 길이를 조절하여 94 GHz에서 MAG를 0.8 dB 향상 시킬 수 있음을 시뮬레이션에서 확인하였다. 뿐만 아니라, 이 소스 피드백 라인은 FET의 입력 임피던스도 변화시켜 입력 정합을 용이하게 한다. 이 현상을 이용하여 공통 소스 FET 4단으로 이루어진 w-band 증폭기를 CPW로 설계하였다. 제작된 W-band 증폭기는 측정 결과 70~103 GHz에서 22.0 dB 이상의 아주 우수한 이득 특성을 보였다.

• 천문학회보
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• 제40권2호
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• pp.43.2-43.2
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• 2015

The RGB Bayer filter system consists of a mosaic of R, G, and B filters on the grid of the photo sensors which typical commercial DSLR (Digital Single Lens Reflex) cameras and CCD cameras are equipped with. Lot of unique astronomical data obtained using an RGB Bayer filter system are available, including transient objects, e.g. supernovae, variable stars, and solar system bodies. The utilization of such data in scientific research requires that reliable photometric transformation methods are available between the systems. In this work, we develop a series of equations to convert the observed magnitudes in the RGB Bayer filter system (RB, GB, and BB) into the Johnson-Cousins BVR filter system (BJ, VJ, and RC). The new transformation equations derive the calculated magnitudes in the Johnson-Cousins filters (BJcal, VJcal, and RCcal) as functions of RGB magnitudes and colors. The mean differences between the transformed magnitudes and original magnitudes, i.e. the residuals, are (BJ - BJcal) = 0.064 mag, (VJ - VJcal) = 0.041 mag, and (RC - RCcal) = 0.039 mag. The calculated Johnson-Cousins magnitudes from the transformation equations show a good linear correlation with the observed Johnson-Cousins magnitudes.

• 천문학회보
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• 제41권1호
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• pp.53.2-53.2
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• 2016

We present surface photometry results of the dwarf galaxies in the nearby NGC 2784 galaxy group. We newly detected about 30 dwarf galaxy candidates at about 30 square degree area around the nearby NGC 2784 galaxy (D~10 Mpc and MV=-20.5) applying a visual inspection technique on the wide-field optical images taken by the KMTNet Supernova Program (KSP). Surface brightnesses of the objects estimated from the stacked-images with total exposure time of about 6 hours reach approximately ${\mu}V$ ~28.5 mag/arcsec2 around $3{\sigma}$ above sky background. The central surface brightness and the total absolute magnitude for the faintest candidate dwarf galaxy among about 40 galaxies including the previously known ones is ${\mu}0$, V~26.1 mag/arcsec2 and MV~-9.5 mag, respectively. The effective radii of the candidates are larger than ~200 pc. The radial number density of the dwarf galaxy candidates from the center of NGC 2784 is decreasing. The mean color (<(B-V)0>~0.7) and $S{\acute{e}}rsic$ structure parameters of the dwarfs, assuming them to be located in the NGC 2784 group, are well consistent with those of the dwarf galaxies in other groups (e.g. M83 group and the Local Group (LG)). The faint-end slope of the cumulative luminosity function (CLF) of the galaxies in NGC 2784 group is about ${\alpha}=-1.2$, which is steeper than that of the LG galaxies, but is much flatter than that of the CLF expected by a ${\Lambda}CDM$ model.

• 천문학회지
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• 제41권5호
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• pp.121-137
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• 2008

We present optical and near-infrared imaging and long-slit spectroscopy for the blue compact dwarf galaxy (BCD) Mrk 49 in the Virgo Cluster. The surface brightness distribution analysis shows that Mrk 49 consists of an off-centered blue bright compact core of r = 10" and a red faint outer exponential envelope. The $H_{\alpha}$ image and color difference suggest that these two components have different stellar populations: a high surface brightness population of massive young stars and an underlying low surface brightness population of older stars. The redder near-infrared colors of the inner most region suggest that the near-infrared flux of Mrk 49 originates from evolved massive stars associated with the current star-forming activity. The total apparent magnitude is $B_T\;=\;14.32$ mag and the mean effective surface brightness is ${\mu}_{eff}(B)\;=\;21.56$ mag $arcsec^{-2}$. Long-slit spectroscopy shows that Mrk 49 rotates apparently as a solid body within r = 10" in a plane at position angle 55 degrees with an amplitude of about $20\;km\;sec^{-1}$. The measured radial velocity of Mrk 49 was derived as $1,535\;km\;sec^{-1}$; and the total mass of stars and gases is in the range of 3 to $6\;{\times}\;10^9\;M_{\odot}$. The mass-to-light ratios for the central region of Mrk 49 in I and B band are estimated 1.0 and 0.5, respectively. The upper limit of the dark matter to visible matter ratio seems to be < 5. The oxygen abundance is $12\;+\;\log(O/H)\;=\;8.21\;{\pm}\; 0.1$ which is about one quarter of the solar value while the relative helium abundance appears to be similar to that of the sun.

• 천문학회보
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• 제36권2호
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• pp.143.1-143.1
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• 2011

Deep Ca,b,y images obtained from the CTIO 4m Blaco telescope are used to investigate the multiple stellar populations of red giant branch (RGB) and sub-giant branch (SGB) in Galactic globular clusters NGC 6656 and NGC 6723. For NGC 6656, confirming the result of Lee et al. (2009), we find two discrete populations of the RGB stars of which mean color separation is about 0.2 mag in hk[=(Ca-b)-(b-y)] index. Furthermore, we also find the bimodel distribution of the SGB stars in (hk, y) color-magnitude diagram. A new finding is that the (hk, y) color-magnitude diagram of NGC 6723 shows two distinct RGB stars with different calcium abundances of which mean color separation is about 0.12 mag in hk index. This multiple stellar feature has not been observed in previous observation, suggesting that NGC 6723 may also be a possible relic of dwarf galaxies that merged into the Milky Way in the past. Thus our result adds further constraints to the merging scenario of the Galaxy formation. Unfortunately, the split of SGB stars in NGC 6723 is not obvious. We will present some statistical results to compare properties of two populations in two clusters.

• 대한의생명과학회지
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• 제10권4호
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• pp.421-427
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• 2004

The possible mechanisms of decreased monoamine oxidase (MAO) A and B activities in cholestatic rat liver were studied. Hepatic and serum MAG activities were determined from the experimental rats with common bile duct ligation (CBDL). The Michaelis-Menten constants in these hepatic enzymes were also measured. The activities of mitochondrial MAO A and B, and mircosomal MAO B as well as their Vmax values were found to be decreased significantly in CBDL plus taurocholic acid (TCA) injected group than in the control group, such as CBDL alone groups. However, their Km values in the experimental groups did not vary. Serum MAO activity increased significantly in the CBDL plus TCA injected group than in the control group. The above results suggest that TCA represses biosynthesis of the MAO in the liver. The elevated activity of the serum MAO is believed to be caused by the increment of membrane permeability ofhepatocytes upon TCA mediated liver cell necrosis.