• Journal of Astronomy and Space Sciences
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• 제29권1호
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• pp.79-84
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• 2012

After a visit by Peter Waddell from the University of Strathclyde, Glasgow, UK in 1991, Robert H. Koch launched a program at the University of Pennsylvania to build lightweight pneumatic membrane mirrors, initially for balloon flight observations where weight is at a premium. Mirror cells were fabricated from sizes 0.18 m to 1.77 m, and experiments conducted to characterize the mirror figure and stability. Most of the work stopped after Prof. Koch's retirement in 1996 until 2006 when the authors expressed an interest in building an array of medium-aperture portable telescopes. The program restarted in earnest at Gravic, Inc. in Malvern, PA in 2008 with Koch using his extensive observational astronomy experience to guide the fabrication of a fully operational 1.07 m membrane mirror telescope with an optical tube assembly weighing under 45 Kg. Residual wavefront aberrations remediation resulted in Koch and the authors investigating membrane tensioning techniques with different cell designs, active secondary wavefront correction, photometric algorithms for aberrated images, and the use of additional lightweight mirror substrates from the Alt-Az Initiative Group, such as foamed glass. The best result for the lightweight mirrors was a point spread function spot size of several arc seconds. A lightweight 1.6 m cast aluminum cell alt-az telescope was subsequently designed by Koch and the authors for prime focus use.

• 대한의용생체공학회:학술대회논문집
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• 대한의용생체공학회 1985년도 춘계학술대회
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• pp.22-25
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• 1985

본고에서, "나선형 주사 방법에 의한 고속 NMR 영상화" 방법을 제안하고 그에 따른 실험 결과를 보였다. 이것은 2차원 FID 영역을 나선형 궤적으로 스캐닝하며 데이타를 받을 수 있도록 경사 자계 파형 (gradient pulse)을 가하여 빠른 시간에 (수십 msec - 수초)내에 영상 정보를 얻어낸 후, 재구성 알고리즘을 씀으로써 영상을 얻어내는 방법이다. 이 방법의 장점은 첫째로 $T_2$ 감쇄에 의한 PSF (Point Spread Function)가 윈형 대칭으로 주어지므로 영상화 했을때 물체의 구조 식별이 기존의 EPI (Echo Planar Imaging) 방법에 비해서 선명하며, 둘째로 나선형 궤적을 구현하기 의한 경사 자계 파형에서 불연속 점을 없앰과 동시에 파형의 세기가 점차로 증가하는 형태이므로, 기존의, 파형 왜곡에 의해 영상에 미치는 영향을 최소화 할 수가 있으며, 세째로 나선형 스캔을 사이 사이에 끼워 넣는 방법을 씀으로써 해상도를 향상시킬 수가 있다.

• 천문학회보
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• 제41권2호
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• pp.66.1-66.1
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• 2016

We developed an observation control software for the IGRINS (Immersion Grating Infrared Spectrograph) silt-viewing camera module, which points the astronomical target onto the spectroscopy slit and sends tracking feedbacks to the telescope control system. The point spread function (PSF) is not always symmetric. In addition, bright targets are easily saturated and shown as a donut shape. It is not trivial to define and find the center of the asymmetric PSF especially on a slit mask. We made a center balancing algorithm (CBA) following the concept of median. The CBA derives the expected center position along the slit-width axis by referencing the stray flux ratios of both upper and lower sides of the slit. We compared efficiencies of the CBA and those of a two-dimensional Gaussian fitting (2DGA) through simulations from observation images in order to evaluate the center finding algorithms. Both of the algorithms are now applied in observation and users can select the algorithm.

• 천문학회보
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• 제41권2호
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• pp.55.3-55.3
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• 2016

By comparing MIRIS Paschen-${\alpha}$ ($Pa{\alpha}$) Galactic Plane Survey (MIPAPS) data with Anderson's H II region catalog (the most complete Galactic H II region catalog up to date), we confirmed $Pa{\alpha}$ detections from ~50% of the H II region candidates in Cepheus (Galactic longitude from $+96^{\circ}$ to $116^{\circ}$). The detection of the hydrogen recombination line identifies these candidates as clear H II regions. If we extend this result to the whole plane, more than 1000 candidates are expected to be identified as H II regions. In this contribution, we present the results of quantitative estimations (brightness, size, etc.) for the $Pa{\alpha}$ blobs detected in Cepheus. To obtain intensity of $Pa{\alpha}$ emission line, we perform background and point spread function (PSF) matching between two filter images (line and continuum filters) as well as flux calibration.

• 대한전자공학회논문지SP
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• 제47권5호
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• pp.145-152
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• 2010

본 논문에서는 초점 열화를 제거하기 위해서 반복적 Unsharp mask (UM) 필터를 이용한 디지털 자동초점 기법을 제안한다. 제안한 디지털 자동초점 기술은 영상열화를 추정하기 위해서 점확산함수를 추정하지 않고 단순한 필터를 사용하기 때문에 계산량이 적은 장점을 갖는다. 본 기법은 반복적 필터 구조로 영상을 복원하기 때문에 사용자의 주관적 기준 및 영상의 객관적 지표를 사용하여 필터링의 반복 회수를 제한할 수 있다. 또한 반복적 UM 기반의 영상개선 방법이 기존의 반복적 영상복원 기술과 등가임을 보인다. 마지막으로 본 논문에서 제안한 알고리듬의 성능평가를 위해서 기존의 영상복원 기반의 디지털 자동초점 기술과의 비교 실험을 수행하였고, 이를 통하여 제안한 디지털 자동초점 기법이 주관적으로나 객관적으로 우수함을 보였다.

• 한국가시화정보학회지
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• 제3권1호
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• pp.3-19
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• 2005

Novel optical techniques are presented for three-dimensional tracking of nanoparticles; Optical Serial Sectioning Microscopy (OSSM) and Ratiometric Total Internal Reflection Fluorescent Microscopy (R-TIRFM). OSSM measures optically diffracted particle images, the so-called Point Spread Function (PSF), and dotermines the defocusing or line-of-sight location of the imaged particle measured from the focal plane. The line-of-sight Brownian motion detection using the OSSM technique is proposed in lieu of the more cumbersome two-dimensional Brownian motion tracking on the imaging plane as a potentially more effective tool to nonintrusively map the temperature fields for nanoparticle suspension fluids. On the other hand, R-TIRFM is presented to experimentally examine the classic theory on the near-wall hindered Brownian diffusive motion. An evanescent wave field from the total internal reflection of a 488-nm bandwidth of an argon-ion laser is used to provide a thin illumination field of an order of a few hundred nanometers from the wall. The experimental results show good agreement with the lateral hindrance theory, but show discrepancies from the normal hindrance theory. It is conjectured that the discrepancies can be attributed to the additional hindering effects, including electrostatic and electro-osmotic interactions between the negatively charged tracer particles and the glass surface.

• 천문학회보
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• 제35권2호
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• pp.34.1-34.1
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• 2010

Studies suggest that activities in luminous AGNs, residing mostly in early-type galaxies, are triggered by merging. However, the observational evidence for the connection between mergers and AGN activity is not clear yet because tracer of the past merging activities such as tidal tail, shell are often too faint. To see if we can reveal the merging features with a small telescope, we observed an AGN, MARK 478, at z=0.077 with long exposure time (7550 seconds) in V filter at Maidanak observatory. Our 2-D fitting analysis shows that the host galaxy of MARK 478 has the bulge to the total luminosity ratio of 0.3. And the residual image, after subtracting point spread function (PSF), bulge and disk components, shows that the host galaxy has an arm-like feature that could be a spiral arm or a feature from minor merging. We also show that the structural parameters obtained from our 2-D fitting match well with those derived from HST image. The promising result suggests that studies of low redshift AGN host galaxies are possible with data from a small telescope. In order to allow a statistical analysis, we hope to expand our sample size in future.

• 한국정보처리학회:학술대회논문집
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• 한국정보처리학회 2005년도 춘계학술발표대회
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• pp.781-784
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• 2005

홍채 인식은 동공과 흰자위 사이에 존재하는 도넛 모양의 홍채 패턴(Iris pattern)을 이용하여 자신인지 타인인지 판별하는 매우 신뢰도가 높은 생체인식기술 가운데 하나이다. 홍채 인식은 홍채 영상의 홍채 패턴으로부터 홍채 코드(Iris code)를 추출하여 인식하기 때문에 좋은 질의 홍채영상을 취득하는 것은 정확한 홍채 인식을 위해서 매우 중요하다. 이러한 홍채 영상의 질을 결정하는 중요한 요소 가운데 하나가 초점(focus)이다. 초점이 맞지 않아 흐려진(blurring) 영상은 홍채 인식에서 자신임에도 불구하고 타인으로 인식하는 FRR(false reject error)를 증가시킨다. 홍채 인식 시스템의 카메라는 고정 초점 방식과 가변 초점 방식이 있다. 고정 초점 방식은 초점렌즈가 고정되어 있어서 초점이 맞지 않는 영상을 취득할 경우 사용자에게 다시 요구하여 입력받도록 한다. 이는 사용자에게 불편을 초래한다. 가변 초점 방식은 사용자와의 거리를 측정하여 초점렌즈를 움직여서 초점이 잘 맞은 선명한 영상을 얻는다. 하지만, 초점렌즈를 움직이기 위해서 사용자와의 거리를 측정하는 센서와 초점렌즈를 움직이는 모터등과 같은 부가 장비가 필요하다. 따라서 카메라의 부피가 커지고, 가격이 상승하게 되는 문제점이 있다. 그리므로 본 논문은 고정 초점 카메라를 사용하여 부가 장비 없이 홍채 영상 복원 알고리즘을 사용하여 소프트웨어적으로 초점이 맞지 않아 흐려진 영상을 처리하는 방법을 제안한다. 본 논문은 초점값을 이용하여 열화(degradation)의 정도를 판단하였으며, 초점값(focus value)에 따라 점확산함수(point spread function)를 설계하여 홍채영상을 복원하였다.

• 천문학회지
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• 제26권1호
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• pp.33-45
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• 1993

We have conducted surface photometry of a spiral galaxy NGC4419, by making use of photographic plates in U, B, V and R-bands taken by 105cm Schmidt Camera at Kiso Observatory. Two dimensional surface brightness distributions as well as luminosity profiles along the major axis are examined in detail to decipher the morphological properties of the galaxy. Analysis of the color distributions of NGC4419 shows that B-V and U-B colors remain constant throughout the galaxy with a weak trend of blue bulge in B-V color. The blue bulge might indicate an active star formation in the nucleus of NGC4419. For a quantitative analysis of the luminosity distribution of NGC4419, the observed luminosity profiles are decomposed into bulge and disk components, assuming the bulge component to follow de Vaucouleurs $\gamma^{1/4}-law$ while the disk component is assumed to be exponential. The fitting generally fails at the central part and at the shoulder near r = 15' where bulge and disk components overlap. The failure at the central part cannot be attributed wholly by the seeing disk since the core-radius of the central plateau is much larger than the width of point spread function. The failure at shoulder could be due to the luminosities from the spiral arms.

• 천문학회보
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• 제37권2호
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• pp.91-91
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• 2012

We present high-resolution near-infrared host galaxy spectra of low-z quasars, PG0844+349 (z=0.064), PG1226+023 (z=0.158), and PG1426+015 (z=0.086). The observation was done by using the near-IR high resolution echelle spectrometer, IRCS, at the SUBARU 8.2 m telescope. The full width at half maximum of the point spread function was about 0.3 arcsec by using an Adaptive Optics system, which can effectively resolve the quasar spectra from the host galaxy spectra. The signal-to-noise ratios are increased by the total exposure time up to several hours per targets and the development of data reduction method. We compare our results to the stellar spectra library and sample spectra from Dasyra et al. (2007) and Watson et al. (2008). The identified spectral lines will be used to study the physical mechanism of quasars, and the velocity dispersions of the stars in the bulge of the host galaxy.