• 한국진공학회지
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• 제10권1호
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• pp.98-103
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• 2001

차세대 평판 디스플레이로서 플라즈마표시기(Plasma Display Pannel, PDP)는 현재 350 $\textrm{cd/cm}^2$의 휘도와 l lm/W 정도의 효율을 갖는 AC형 PDP가 개발되어 있으나, 음극선관(CRT)의 피크 휘도가 700 $\textrm{cd/cm}^2$, 효율이 수 1 m/W인 것을 감안하면 음극선관을 대체할 수 있는 표시기가 되기 위해서는 PDP의 휘도와 효율을 더욱 개선시킬 필요가 있다. 반사형 AC-PDP셀 내에서 가스 방전으로 발생된 진공 자외선(Vacuum Utraviolet, VUV) 중 배면판 쪽으로 진행되는 부분은 형광체를 여기시켜 가시광을 발생시키게 되지만, 전면판 쪽으로 진행되는 부분은 발광에 사용되지 못하고 있다. 본 연구에서는 PDP 셀 전면판의 유전체와 보호막 사이에 VUV를 반사시킬 수 있는 다이크로익 미러(Dichroic mirror)를 증착함으로써 셀 내의 VUV 이용 효율을 증가시켜 휘도와 효율을 향상시킬 수 있는 방법을 제안하였다. 다이크로익 미러를 정확하게 설계하기 위해서 미러에 사용되는 $MgF_2$, $LaF_3$, MgO 박막의 VUV 영역에서의 광학 계수(Optical Constant)를 실험과 시뮬레이션을 이용한 광도 측정법(Photometric method)을 통해서 구하였다 (1). 이 값들을 이용해서 플라즈마 표시기의 패널 방전에서 방출되는 빛의 휘도를 결정짓는 가장 중요한 요소인 147nm 부근의 진공자외선을 반사시킬 수 있는 다이크로익 미러를 설계하였다. 다이크로익 미러는 전자빔 증착기 (I-beam evaporator)를 이용하여 증착되었고, 박막의 광학 계수 결정을 위한 반사도(Reflectance), 투과도(Transmittance) 측정과 다이크로익 미러의 반사도 측정은 Reflectometer를 이용해 측정하였다. 패널 실험은 동일한 패널 내에 반쪽 면에만 다이크로익 미러를 증착시켜 방전 전압에 따른 휘도와 효율을 미러가 없는 면과 동일 조건하에 비교 측정하였다. 여러 방전 조건하에서 다이크로익 미러를 AC-PDP에 적용한 경우가 그렇지 않은 경우보다 휘도와 효율이 약 20-30% 정도 증가함을 확인하였다.

• 천문학회보
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• 제43권1호
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• pp.41.1-41.1
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• 2018

We introduce a current status and future plans of Korea Microlensing Telescope Network (KMTNet) microlensing experiments, which include an observational strategy, pipeline, event-finder, and collaborations with Spitzer. The KMTNet experiments were initiated in 2015. From 2016, KMTNet observes 27 fields including 6 main fields and 21 subfields. In 2017, we have finished the DIA photometry for all 2016 and 2017 data. Thus, it is possible to do a real-time DIA photometry from 2018. The DIA photometric data is used for finding events from the KMTNet event-finder. The KMTNet event-finder has been improved relative to the previous version, which already found 857 events in 4 main fields of 2015. We have applied the improved version to all 2016 data. As a result, we find that 2597 events are found, and out of them, 265 are found in KMTNet-K2C9 overlapping fields. For increasing the detection efficiency of event-finder, we are working on filtering false events out by machine-learning method. In 2018, we plan to measure event detection efficiency of KMTNet by injecting fake events into the pipeline near the image level. Thanks to high-cadence observations, KMTNet found fruitful interesting events including exoplanets and brown dwarfs, which were not found by other groups. Masses of such exoplanets and brown dwarfs are measured from collaborations with Spitzer and other groups. Especially, KMTNet has been closely cooperating with Spitzer from 2015. Thus, KMTNet observes Spitzer fields. As a result, we could measure the microlens parallaxes for many events. Also, the automated KMTNet PySIS pipeline was developed before the 2017 Spitzer season and it played a very important role in selecting the Spitzer target. For the 2018 Spitzer season, we will improve the PySIS pipeline to obtain better photometric results.

• Journal of Astronomy and Space Sciences
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• 제11권2호
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• pp.185-195
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• 1994

우리는 충북대학교가 보유하고 었는 $1024\times1024$ pixel의 CCD 카메라를 이용하여 식변광성 U Cep를 1993년 1월 11-12일에 측광관측하였다. 이날 얻은 총 62개의 관측점을 가지고 제1극심 부근의 광도곡선을 완성하여 JD Hel 2448999.7274의 극심 시각을 결정하였다. 한편 1993년 10월 21-22일에 미국 네브라스카 대학의 Behlen 천문대에서 변광성 GW Cep와 V700 Cyg를 CCD 측광관측하여 총 168개의 관측점을 만들었다. 이들 자료를 가지고 광도곡선들을 완성하였고, GW Cep의 광도극심 시각 JD Hel 2449282.8485와 V700 Cyg의 광도극심 시각 JD Hel 2449282.7979을 각각 결정하였다. Behlen천문대의 CCD 관측방법과 충북대의 관측방법의 장단점을 비교하고 충북대 관측 방법의 개선을 위해 노출후 램에 기억되어 있는 CCD화상으로부터 직접 필요한 부분의 밝기만을 측정하고 이를 저장하는 방식의 개념을 제시하였다.

• 한국광학회지
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• 제15권2호
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• pp.137-141
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• 2004

조도단위계로부터 전광선속의 단위계를 실현하기 위해서 전광선속 측정장치를 제작하여 광도측정의 단위계를 복사선 측정의 기준으로 변환하였다. 제작된 전광선속 측정장치는 광원으로부터 전 방향으로 발산하는 광속을 측정하고, 광원 주위의 가상구면을 적분함으로서 전광선속을 측정하였다. 광검출기로 LMT사의 조명도계를 사용하여 광원의 중심과 조명도 기준면까지의 거리가 약 1.693 m인 가상의 구면의 조명도를 측정하였다. 제작된 고니오광도계의 전광선속은 95% 신뢰수준에서 측정불확도는 1%이다.

• 천문학회보
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• 제39권2호
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• pp.111-111
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• 2014

Intensity interferometry, based on the Hanbury Brown--Twiss effect, is a simple and inexpensive method for optical interferometry at microarcsecond angular resolutions. Motivated by recent technical developments, we argue that the sensitivity of large modern intensity interferometers can be improved by factors up to approximately 25,000, corresponding to 11 photometric magnitudes, compared to the pioneering Narrabri Stellar Interferometer of the 1970s when resolving. Our approach, based on spectrally resolved light, permits the construction of large optical interferometers at the cost of (very) long-baseline radio interferometers. Realistic intensity interferometers are able to spatially resolve main-sequence O-type stars in the Magellanic Clouds. Multi-channel intensity interferometers can address a wide variety of science cases: (i) linear radii, effective temperatures, and luminosities of stars; (ii) mass-radius relationships of compact stellar remnants; (iii) stellar rotation; (iv) stellar convection and the interaction of stellar photospheres and magnetic fields; (v) the structure and evolution of multiple stars; (vi) direct measurements of interstellar distances; (vii) the physics of gas accretion onto supermassive black holes; and (viii) calibration of amplitude interferometers by providing a sample of calibrator stars.

• 천문학회보
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• 제41권2호
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• pp.43.1-43.1
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• 2016

The duration of star formation activity is a key to understanding the formation process of star clusters. Although a number of astronomers have attempted to derive the underlying age spread in photometric diagrams with a variety of stellar evolutionary models, the resultant findings are subject to uncertainties due to intrinsic variability of pre-main sequence (PMS) stars, observational errors, difficulties in reddening correction, and systematic differences in adopted stellar evolutionary models. The distribution of Li abundance for PMS stars in a cluster could, on the other hand, provide an alternative way to estimate the age spread. In this study, a total of 134 PMS stars in NGC 2264 are observed with the high resolution multi-object spectrogragh Hectochelle attached to the 6.5m Multi Mirror Telescope. We have successfully detected Li ${\lambda}6708$ resonance doublet for 86 low-mass PMS stars. The Li abundance of the stars is derived from their equivalent width using a curves of growth method. After correction for non-LTE effects, the underlying age spread of 3 - 4 Myr is inferred from the Li abundance distribution of low-mass PMS stars. We suggest that NGC 2264 formed on a timescale shorter than 5 Myr given the presence of embedded populations.

• 천문학회보
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• 제42권2호
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• pp.78.1-78.1
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• 2017

We present a noble method to determine BH mass of many AGNs directly through reverberation mapping using a small telescope with wide-field of view. In 2017 August we installed five medium-band filters to a 0.25m diameter $5deg^2$ FOV telescope at the McDonald observatory. The width of these filters (FWHM ~ 50nm) are matched to the broad line width of type-1 AGNs at various redshifts. From recently obtained data, about r ~ 19 magnitude AGNs can be detected in line component with 150s exposure. With this magnitude limit, about 20~30 AGNs can be studied in one field. We plan to carry out at one day cadence observation over 20~30 fields, enabling us to monitor up to ~1000 AGNs over a wide range of variability. This poster presents out plan and early results from test observation.

• 천문학회보
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• 제42권1호
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• pp.52.2-53
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• 2017

We develop a methodology to use the redshift dependence of the galaxy 2-point correlation function (2pCF) as a probe of cosmological parameters. The positions of galaxies in comoving Cartesian space varies under different cosmological parameter choices, inducing a redshift-dependent scaling in the galaxy distribution. This geometrical distortion can be observed as a redshift-dependent rescaling in the measured 2pCF. The shape of the 2pCF exhibits a significant redshift evolution when the galaxy sample is analyzed under a cosmology differing from the true, simulated one. Other contributions, including the gravitational growth of structure, galaxy bias, and the redshift space distortions, do not produce large redshift evolution in the shape. We show that one can make use of this geometrical distortion to constrain the values of cosmological parameters governing the expansion history of the universe. This method could be applicable to future large scale structure surveys, especially photometric surveys such as DES, LSST, to derive tight cosmological constraints. This work is a continuation of our previous works as a strategy to constrain cosmological parameters using redshift-invariant physical quantities.

• KSII Transactions on Internet and Information Systems (TIIS)
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• 제14권10호
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• pp.4042-4059
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• 2020

The development of new multimedia techniques such as 3D printing is increasingly attracting the public's attention towards 3D objects. An optimized robust and imperceptible watermarking method based on Ant Colony Optimization (ACO) and Weber Law is proposed for 3D polygonal models. The proposed approach partitions the host model into smaller sub meshes and generates a secret watermark from the sub meshes using Weber Law. ACO based optimized strength factor is identified for embedding the watermark. The secret watermark is embedded and extracted on the wavelet domain. The proposed scheme is robust against geometric and photometric attacks that overcomes the synchronization problem and authenticates the secret watermark from the distorted models. The primary characteristic of the proposed system is the flexibility achieved in data embedding capacity due to the optimized strength factor. Extensive simulation results shows enhanced performance of the recommended framework and robustness towards the most common attacks like geometric transformations, noise, cropping, mesh smoothening, and the combination of such attacks.

• 천문학논총
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• 제30권2호
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• pp.443-445
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• 2015

We provide results of near-infrared (NIR) spectroscopic observations of 83 nearby (0.002< z <0.48) and bright (K <14 mag) type 1 active galactic nuclei (AGNs). For the observations, we used the Infrared Camera (IRC) on AKARI allowing us to obtain the spectrum in the rarely studied spectral range of $2.5-5.0{\mu}m$. The $2.5-5.0{\mu}m$ spectral region suffers less dust extinction than ultra violet (UV) or optical wavelength ranges, and contains several important emission lines such as $Br{\beta}$ ($2.63{\mu}m$), $Br{\alpha}$ ($4.05{\mu}m$), and polycyclic aromatic hydrocarbon (PAH; $3.3{\mu}m$). The sample is selected from the bright quasar surveys of Palomar Green and SNUQSO, and AGNs with black hole (BH) masses estimated from reverberation mapping method. We measure the Brackett line properties for 11 AGNs, which enable us to derive BH mass estimators and investigate circum-nuclear environments. Moreover, we perform spectral modeling to fit the hot and warm dust components by adding photometric data from SDSS, 2MASS, WISE, and ISO to the AKARI spectra, and estimate hot and warm dust temperatures of ~1100K and ~220 K, respectively.