• 조명전기설비학회논문지
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• 제27권10호
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• pp.1-8
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• 2013

Wireless Visible Light Communication is the technology that enables communication using LED illumination Infrastructure instead of existing illumination such as incandescent lamp or fluorescent light. Because VLC uses light for communication, it has no problem of frequency permission and is harmless to human body. It is also possible to check the communication through eye. So VLC can be used as a supplement to the Radio Frequency communication, Infrared in indoor environment. So far, researchers on the LED Visible light communication have focused on the increasing transmission speed, transmission distance, modulation method. However, there is few research of main factors that influence on system performance. System performance has been mainly predicted through simulation. In this paper, I recognized that these factors such as outside light noise, obstacle, LED panel position or emitted angle have a great impact on wireless communication system. So I experimented VLC system by changing distance and position to discover location suitable for BER regulation.

• The Journal of Korean Physical Therapy
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• 제13권3호
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• pp.561-567
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• 2001

IR classified by wavelength three parts NIR, MIR. FIR. There is FIR which is radiated from healthy human body the wave length is 8-14m. The Sun's ray is composed of Infared(49%), Visible light(40%) and Ultra violet(11%), however the ray getting to the earth is FIR(60%), IR(20%), and UV(20%). Human beings has utilized FIR already from time immemorial. Hershel found out Infrared for the first time, in the Industrial Revolution the Infrared and FIR had been begun to use making products. FIR with low temperature can deeply penetrate on the human body composed things without troublesome, since FIR has effectively operated on the human body at low temperature (35-40 $^{\circ}$C). In this study, we experimented in the specific temperature FlR radiation intensity. water consumption rate, feed consumption rate. survival rate and mean of weight balance with FlR radiation instrument. According to the results, the FlR radiation to the mice assisted to increase the survival rate.

• 대한전기학회:학술대회논문집
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• 대한전기학회 2004년도 하계학술대회 논문집 C
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• pp.1721-1723
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• 2004

우리는 황토 조명등을 제작하여 원 적외선 발생 실험을 하였다. 실험에는 백열전구 200W, 실내온도 21도, 습도 38%의 조건에서 열화상실험과 TF-IR(적외선 분광방사 측정장치)에 의한 원적외선 방사한도를 측정하였으며, 그 결과 방사율 0.914와 방사에너지 $6.23{\times}10^2\;(w/m^2{\cdot}{\mu}m)$ 가 얻어졌다. 이와 같은 결과로 황토조명등에서 원적외선이 발생한 것을 확인하였다.

• 천문학회보
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• 제37권1호
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• pp.101.1-101.1
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• 2012

Interplanetary dust particles are observable as zodiacal light, which is the sunlight scattered by the interplanetary dust particles. The origins of interplanetary dust particles are still in question because they are eroded by Poynting-Robertson photon drag and mutual collisions among dust particles. The small-scale structures in the zodiacal light provided a clue to specify their origins. Asteroidal debris were detected as band-like structures (dust bands), and the cometary large particles were detected as narrow trails (dust trails). However, little is confirmative about their detailed origins and mineralogical compositions because of the lack of observational data particularly in the optical wavelength. We made a high-resolution optical zodiacal light map based on the CCD observations at Mauna Kea, Hawaii. We analyzed data taken on November 12, 2004. After the data reduction, such as flat fielding and subtraction of airglow emissions, we succeeded in the construction of the zodiacal light map with the spatial resolution of 3' in the solar elongation between 45 degree and 180 degree. This is the highest resolution map in the visible wavelength so far. In this map, we confirmed the dust bands structures near the ecliptic plane. We will discuss about the similarities and the differences between optical and infrared dust bands.

• 천문학회보
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• 제37권1호
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• pp.42-42
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• 2012

The First stars (Pop.III stars) in the universe are expected to be formed between the recombination era at z - 1100 and the most distant quasar (z - 8). They have never been directly detected due to its faintness so far, but can be observed as a background radiation at around 1${\mu}m$ which is called the Cosmic Near-Infrared Background (CNB). Main part of the CNB is thought to be redshifted Lyman-alpha from gas clouds surrounding the Pop.III stars. Until now, the COBE (COsmic Background Explorer) and the IRTS (Infrared Telescope in Space) observed excess emission over the background due to galaxies. To confirm the COBE and the IRTS results and pursue more observational evidences, we carried out the sounding rocket experiment named the Cosmic Infrared Background ExpeRiment (CIBER). The CIBER is successfully launched on July 10, 2010 at White Sands Missile Range, New Mexico, USA. It consists of three kinds of instruments. We report the results obtained by LRS (Low Resolution Spectrometer) which is developed to fill the uncovered spectrum around 1${\mu}m$. LRS is a refractive telescope of 5.5 cm aperture with spectral resolution of 20 - 30 and wavelength coverage of 0.7 to 2.0${\mu}m$. After subtracting foreground components (zodiacal light, integrated star light and diffuse galactic light) from the sky brightness of observed five fields, there remained significant residual emission (even for the lower limit case) consistent with the IRTS and the COBE results. In addition, there exists a clear gap at 0.7 - 0.8${\mu}m$ in the CNB spectrum over the background due to galaxies according to recent results (Matsuoka et al. 2011; Mattila et al. 2011). The origin of the excess emission could be ascribed to the Pop.III stars with its active era of z = 7 - 10.

• 천문학회보
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• 제35권2호
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• pp.54-54
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• 2010

Interplanetary space is filled with dust particles originating mainly from comets and asteroids. Such interplanetary dust particles lose their angular momentum by olar radiation pressure, causing the dust grains to slowly spiral inward Poynting-Robertson effect). As dust particles move into the Sun under the influence of Poynting-Robertson drag force, they may encounter regions of resonance just outside planetary orbits, and be trapped by their gravities, forming the density enhancements in the dust cloud (circumsolar resonance ring). The circumsolar resonance ring near the Earth orbit was detected in the zodiacal cloud through observations of infrared space telescopes. So far, there is no observational evidence other than Earth because of the detection difficulty from Earth bounded orbit. A Venus Climate Orbiter, AKATSUKI, will provide a unique opportunity to study the Venusian resonance ring. It equips a near-infrared camera for the observations of the zodiacal light during the cruising phase. Here we consider whether Venus gravity produces the circumsolar resonance ring around the orbit. We thus perform the dynamical simulation of micron-sized dust particles released outside the Earth orbit. We consider solar radiation pressure, solar gravity, and planetary perturbations. It is found that about 40 % of the dust particles passing through the Venus orbit are trapped by the gravity. Based on the simulation, we estimate the brightness of the Venusian resonance ring from AKATSUKI's locations.

• 천문학회보
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• 제44권1호
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• pp.62.2-62.2
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• 2019

The ADF-S (AKARI Deep Field - South) toward South Ecliptic Pole is one of the deep survey fields designed for the study of Extragalactic Background Light (EBL). The deep extragalactic survey was initiated by AKARI far-infrared deep observations. Other space missions (e.g., Euclid, NISS, SPHEREx) will perform the deep observations in the ADF-S. Based upon the recent optical survey with KMTNet, we can identify the optical counterparts for dusty star-forming galaxies such as ULIRG, DOG, SMG. Among them, the Dust-Obscured Galaxies (hereafter DOGs with f(24um)/f(R) > 1,000) in the heavily obscured system are expected to play an important role in the formation of most massive galaxies. We have newly discovered ~100 DOGs in ~12 sq. deg. of the ADF-S from our optical survey with KMTNet. We also confirmed that some of DOGs host the most luminous AGN for their black hole masses through the near-infrared spectroscopic follow-ups. Here, we report the properties of high-z hyperluminous DOGs in the ADF-S.

• 한국멀티미디어학회논문지
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• 제14권9호
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• pp.1125-1137
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• 2011

최근, 휴대성과 이동성이 뛰어난 모바일 단말기 환경에 홍채 인식 기술을 도입하여 신원을 확인하는 연구가 진행 되었는데, 이러한 모바일 홍채 인식 시스템은 취득된 홍채 영상 품질에 따라 인식률이 좌우된다. 홍채 영상은 취득 시 조명환경에 영향을 많이 받게 되는데, 기존의 시스템은 태양광이 없는 실내에서는 높은 인식률을 보이나, 실외 태양광 환경에서는 외부태양광이 홍채 영역에 투사되어 입력 영상 내에서 홍채 패턴의 그레이 레벨 변화, 고스트(Ghost region) 및 속눈썹 그림자(Eyelash shading region) 발생 등의 요인으로 인식 성능 저하를 초래하는 문제가 있었다. 이를 해결하기 위하여, 본 연구에서는 850nm 근적외선 조명과 850nm 대역 밴드 패스 필터를 장착한 홍채 카메라 시스템을 제안한다. 성능 평가를 위해 기존의 홍채 인식시스템과 제안하는 홍채 인식 시스템을 사용하여 실내 및 실외 태양광 환경에서 취득한 홍채 영상으로부터 홍채코드를 추출한 후 타인 수락률(False Acceptance Rate), 본인 거부율 (False Rejection Rate)을 통한 균등 에러율(EER, Equal Error Rate)을 측정하였다. 실험 결과 기존의 시스템 보다 제안하는 시스템의 EER이 실내 정면 조명일 때 약 0.96%, 실외 정면 조명일 때 약 4.94%, 실외 측면 조명일 때 약 9.24%, 실외 후면 조명일 때 약 7% 낮아지는 개선된 성능을 보였다.

• 한국컴퓨터산업학회논문지
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• 제2권4호
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• pp.565-572
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• 2001

최근 고체 레이저 출력측에 비선형 광학재료를 설치하여 적외선에서 자외선에 이르기까지 넓은 대역의 파장을 가진 레이저광이 요구된다. 비선형 광학소자는 고조파발생기와 파라메터 발생기와 같은 레이저원을 이용한 주파수 전 영역까지 확장 할 수가 있다. 주파수 변환은 고전력 레이저를 이용한 확장기술에 많이 이용하고있다. 새로운 각 주파수 대역에서 광학 매개체의 비선형 광학의 응답 등을 이용할 수가 있다. 이러한 과정들은 자외선영역에서 적외선까지 고전력 방사발생을 이용할 수가 있다. 광학 파라메터발생기와 증폭기는 저주파수에서 2가지 파장 등을 발생한다. 싱글 주파수원으로부터 발생하여 몇몇의 경우에는 가시광선 영역에서 거의 자외선 영역까지 이용할 수가 있다. 결과적으로 녹색광을 얻기 위해서, 펄스형Nd:YAG 레이저는 다단펄스 포밍회로를 이용하였고 비선형광학(KTP)소자를 채택하여 적용하였다. 따라서 본 연구에서는 펄스 중첩법을 이용하여 기본파로서 직접 설계 제작 후 SHG 장치를 장착하여 녹색광을 얻고 각 중첩 메쉬에 같은 에너지를 인가했을 때의 레이저 출력과 녹색광 출력간의 상관관계와 메쉬 수에 따른 변환효율을 조사하였다.

• 한국염색가공학회지
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• 제23권3호
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• pp.187-194
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• 2011

This study used Jeju scoria to dye cotton fabric and measured its dyeability, colorfastness, antibacterial activity, deodorization efficiency, ultraviolet protection, and far-infrared emission. The cotton fabric was colored to yellowish red and optimal dyeing can be achieved at a temperature of $80^{\circ}C$ for a dyeing time of 120 minutes with a colorant concentration of 25%(o.w.b). The colorfastness to light, rubbing, perspiration, and washing was 8, 5, 5, and 4~5 ratings respectively, where the wash colorfastness remained after 15 wash cycles. The cotton fabric dyed with Jeju scoria demonstrated excellent antimicrobial activity to Staphylococcus aureus and high deodorization efficiency. Ultraviolet protection factor was as high as 50+. The Jeju scoria can be used as a new colorant for the natural dyeing of silk.