• 대한전자공학회논문지SP
• /
• 제48권6호
• /
• pp.27-34
• /
• 2011

본 논문에서는 스마트폰 단말기에 장착되어있는 카메라와 플래시를 이용한 photometric stereo 기반의 능동적 3차원 형상 취득 기법을 제안한다. 조명의 위치 변화에 따라 여러 장의 입력 영상을 취득하기 위헤 고정된 위치에서 영상을 취득하는 스마트폰 한 대와 위치를 변화시키며 조명을 투사하는 스마트폰 한 대를 이용하여 시스템을 구성한다. 우선 카메라 렌즈의 왜곡과 카메라 센서의 비선형성 반응함수에 의한 3차원 형상 취득의 오차를 줄이기 위해 카메라 보정을 수행한다. 또한 스마트폰 카메라간의 자세를 추정하기 위해 5-point 알고리즘을 적용한 후 이를 이용하여 광원의 방향 벡터를 추정한다. 그 후 취득된 영상과 추정된 광원의 방향 벡터를 이용하여 photometric stereo기법으로 3차원 형상을 취득한다. 실험결과 본 논문에서 제안하는 기법을 통하여 스마트폰이 저비용 고품질의 소형화된 3차원 카메라의 역할을 수행할 수 있는 것을 확인할 수 있다.

• 천문학회지
• /
• 제10권1호
• /
• pp.31-38
• /
• 1977

To reduce the instrumental and calibration errors in the photoelectric photometry as much as possible it is necessary to select the optimum photocell voltage and energy attenaution and to observe as many standard stars as possible over the wide range of color, spectral type and air mass.

• 천문학회지
• /
• 제20권2호
• /
• pp.63-94
• /
• 1987

Using many homogeneous data of DDO and UBV colors for all luminosity classes and physical quantities known from spectroscopic observations, new calibration schemes with DDO photometric parameters are presented for metal abundance, effective temperature and surface gravity of stars. And an intrinsic color relation is derived for the reddening estimate.

• Journal of Astronomy and Space Sciences
• /
• 제30권3호
• /
• pp.179-185
• /
• 2013

Photometric observation is one of the most effective techniques for determining the physical characteristics of unknown space objects and space debris. In this research, we examine the change in brightness of the Communication, Ocean, Meteorological Satellite-1 (COMS-1) Geostationary Orbit Satellite (GEO), and compare it to our estimate model. First, we calculate the maximum brightness time using our calculation method and then derive the light curve shape using our rendering model. The maximum brightness is then calculated using the induced equation from Pogson's formula. For a comparison with our estimation, we carried out photometric observation using an optical telescope. The variation in brightness and the shape of the light curve are similar to the calculations achieved using our model, but the maximum brightness shows a slightly different value from our calculation result depending on the input parameters. This paper examines the photometric phenomenon of the variation in brightness of a GEO satellite, and the implementation of our approach to understanding the characteristics of space objects.

• Journal of Astronomy and Space Sciences
• /
• 제20권4호
• /
• pp.249-260
• /
• 2003

1998년 12월부터 1999년 5월까지 총 10일간 W UMa형 접촉쌍성 AH Cnc를 소백산천문대의 61cm 망원경과 PM512 CCD 카메라, 그리고 BVI 필터를 사용하여 CCD 측광을 수행하였다. 새롭게 얻은 BVI 광도곡선을 Wilson-Devinney 쌍성모델의 Mode 3(접촉형)으로 분석해서 측광해를 구하고 Roche 모형을 얻었다. 지금까지 발표된 모든 극심시각들과 이번 관측자료를 사용하여 얻은 (O-C)도를 분석해서 영년주기 증가율와 질량이동률을 계산하였다.

• Journal of Astronomy and Space Sciences
• /
• 제30권4호
• /
• pp.213-221
• /
• 2013

We present the first BVRI CCD photometric observations of V345 Cas made on 22 nights during the observing seasons in 2007-2008. Our light curves, resembling those of EB-type binary stars, are analyzed with the 2003 version of the Wilson-Devinney binary code. The photometric study shows that V345 Cas is a typical semi-detached binary system with the primary star being about ${\Delta}T$ = 2400 K hotter, two times more massive, but only 17% larger than the secondary star being filled with it's Roche-lobe. The orbit has a relatively large inclination of about $88^{\circ}$. A cool spot on the secondary component is modeled to explain a small light curve asymmetry. Absolute dimensions and related radiometric parameters of the eclipsing pair are calculated and their evolutionary states are discussed with the HR diagrams of mass-radius and temperature-luminosity. A period analysis of all available times of minima, including our measurements, indicates that the orbital period may vary in a cyclical way, unfortunately the secondary period for the variation can not be uniquely determined because of lack of present timing data.

• 조명전기설비학회논문지
• /
• 제28권5호
• /
• pp.1-14
• /
• 2014

This study has found out appropriate scopes of correlated color temperature and illuminance value with regard to general diffused lighting and work in the kitchen. It also has presented appropriate photometric quantity control speed for behavioral change with the following results. 1)For general diffused lighting, the appropriate photometric quantity has turned out to be 4,000 to 4,500K in color temperature and illuminance value of 300 to 400lx. And 300lx at 4,500K has proven to be the most comfortable, behavior-appropriate, and preferred pair. 2)As far as appropriate photometric quantity for work is concerned, color temperature of 4,000 to 5,000K and illuminance value of 600 to 800lx are appropriate, while 700lx at 4,500 to 5,000K are the most comfortable, behavior-appropriate, and preferred set. 3)As for appropriate photometric quantity control speed in behavioral change, 3 to 5 seconds has proven the most comfortable, appropriate, and preferred for behavioral change from entry to general areas and 1 to 3 seconds for change from general to work.

• 천문학논총
• /
• 제30권2호
• /
• pp.265-266
• /
• 2015

A search for luminous white dwarfs (WDs) in several nearby Galactic globular clusters (GCs) was carried out using the deep and homogeneous photometric catalog of Galactic GCs taken with the ACS/WFC aboard the Hubble Space Telescope (HST) by Sarajedini et al. and Anderson et al- It resulted in the identification of luminous WD candidates in the GCs M13 (NGC 6205) and M22 (NGC 6656). The purpose of the present study is to identify luminous WDs in the deep and homogeneous V versus V - I color-magnitude diagrams (CMDs) of several nearby Galactic GCs taken with the ACS/WFC aboard the HST. Using photometric data for the GCs M13 and M22 that are now in the public domain, the V versus V - I CMDs of the GCs M13 and M22 were constructed. Many spurious detections in the CMDs were removed using the photometric quality parameters qfit(V) and qfit(I), and a radial restriction was applied to the CMDs to remove the central stars with higher photometric errors due to central crowding. From each resultant V versus V - I CMD of the GCs M13 and M22, a dozen or so luminous WD candidates were identified. They were confirmed as stellar objects in the accompanying ACS/WFC images and their positions in the CMDs were in the bright part of the DA WD cooling curve. Therefore, the luminous WD candidates in the GCs M13 and M22 seem to be true luminous WDs, and spectroscopic observations are needed to confirm their true identity.

• 천문학회보
• /
• 제40권2호
• /
• pp.41.2-41.2
• /
• 2015

We have performed deep wide-field CCD photometry of the young open cluster IC 1805 in the famous star forming region W4, and obtained photometric data for more than 91,000 stars in the field of IC 1805 based on observations with the 3.6m CFHT and the AZT-22 1.5m telescope at Maidanak Astronomical Observatory in Uzbekistan. The photometric data cover an area $43^{\prime}{\times}45^{\prime}$ which is far larger and far deeper than any other optical observations made for the cluster. In order to select the young stellar objects with mid-IR excess emission, we have performed mid-IR photometry of the cluster using the archival images obtained with the Spitzer Space Telescope IRAC and MIPS instruments. From a preliminary analysis of the data, we determined the reddening law ($R_V=3.02{\pm}0.05$), distance modulus ($V_0-M_V=11.9{\pm}0.2$), and the spatial distribution of members.

• 천문학회보
• /
• 제40권2호
• /
• pp.50.4-51
• /
• 2015

Current and planned deep multicolor wide-area cosmological surveys will map in detail the spatial distribution of galaxies and quasars over unprecedented volumes, and provide a number of objects with photometric redshifts more than an order of magnitude bigger than that of spectroscopic redshifts. Photometric information is statistically more significant for studying cosmological evolution, dark energy, and the expansion history of the universe at a fraction of the cost of a full spectroscopic survey, but intrinsically carries a bias due to noise in the distance estimates. We provide convolution- and deconvolution-based algorithms capable of removing this bias -- thus able to exploit the full cosmological information -- in order to reconstruct intrinsic distributions and correlations between distance-dependent quantities. We then show some direct applications of our techniques to the VIMOS Public Extragalactic Redshift Survey (VIPERS) and the Sloan Digital Sky Survey (SDSS) datasets. Our methods impact a broader range of studies, when at least one distance-dependent quantity is involved; hence, they will be useful for upcoming large-volume surveys, some of which will only have photometric information.