Experiments designed to measure the effect of LED (light–emitting diode) light wavelength on the growth of fingerling rockfishes (Sebastes inermis) were conducted. Fingerling rockfishes (average body weight of individual: 1.13g) were divided into two groups by wavelength of the LED light [light power: 1,620 mW; wavelength: 518 nm (green color), 622 nm (red color)]. Triplicate groups of 180 individuals were reared over 7 weeks. Lighting duration was 14 hours from 06:00 to 20:00. A water tank exposed on the natural light in a room through the windows was used as a control. At results of the first experiment [initial average body weight (BW) of individual: 1.13 g; standard deviation (SD): 0.13 g], the final individual BW exposed on the green color was increased 0.39 g than the red color, and decreased 0.12 g than the natural light in the room. At results of the second (initial individual BW: 5.07 g; SD: 0.70 g) and the third experiment (initial individual BW: 10.67 g; SD: 0.67 g), the final individual BW exposed on the green color was increased 1.07 g and 2.55 g than the red color, respectively, and increased 0.57 g and 0.84 g than the natural light, respectively. The relative growth rate of the green color was higher about 8% significantly (p<0.05) than the natural light. In the case of the red color the relative growth rate was lower significantly (p<0.05) than the natural light.

Recently, studies have been actively conducted on light sources which can affect the growth rate of plants by using monochromatic lights which have light wavelength or combining them into mixed lights. The studies measure Photosynthetic Photon Flux Density (PPFD) according to the change of light quality of LED light source and research on the acceleration of plant growth. With red, blue, green and white mono-chromatic lights, this study fabricated 6 mixed lights. Then, with 3 mono-chromatic lights and 6 fabricated mixed light source, the study conducted comparison analysis on what effect optical properties and PPFD have on (the growth of) a plant (radish sprouts). As the result of analysis, in the same PPFD, it turned out that the speed of plant growth was faster in red mono-chromatic lights while the speed was similar in blue and white mono-chromatic lights and mixed lights.

PURPOSES : Recently, attempts have been made to evaluate tire-pavement noise based on a measure of Mean Profile Depth (MPD). However, equivalent values of MPD appear to correspond to different levels of tire-pavement noise, which indicates that other factors such as texture wavelength need to be included to improve the accuracy of noise prediction. A single index to represent texture wavelength is proposed in this study. A consistent relationship between tire-pavement noise and texture wavelength on asphalt concrete pavement is observed. METHODS: Profile data and tire-pavement noise data were collected from a number of expressway sections in Korea. In addition, texture wavelength was defined by a Peak Number (PN), which was calculated using profile data. Statistical analysis was performed to find the relationship between the PN and tire-pavement noise. RESULTS: As a result of this study, a linear relationship between PN and tire-pavement noise is observed on asphalt concrete pavement. CONCLUSIONS: Tire-pavement noise on asphalt concrete pavement can be predicted from PN information.

양송이버섯 재배지에서 LED 광원의 파장에 따른 큰검 점버섯파리(Lycoriella ingenua)의 유인력을 조사하였다. 시험은 용인과 부여의 양송이 재배지에서 수행되었으며, LED 광원은 백색광, 녹색광, 적색광, 청색광, 황색광을 이 용하였다. LED 광원 파장별 버섯파리 유인수는 용인과 부여에서 백색광 132.9마리, 3,272.5마리, 녹색광 120.3마 리, 3,109.5마리, 적색광 105.5마리, 1,910.1마리, 청색광 88.3마리, 2,708.3마리, 황색광 46.7마리, 2,465.6마리였다. LED 광원들은 무처리와 비교하여 2.7~3.5배 더 많은 큰 검정버섯파리가 유인되었다.

In order to identify peculiar X-ray sources, we select 442 sources with no counterparts in other wavelength bands (as of the year 1999) from the ROSAT All-Sky Survey Bright Source Catalog. We cross- correlate this initial list with the NASA/IPAC Extragalactic Database, the USNO and WISE catalogs, and the HEASARC XRAY Master Catalog. Eventually, we are left with four unidentified sources with no counterparts in other wavelength bands. We present these four sources and their X-ray properties in this paper.

레이저 주사 공초점 현미경은 비접촉, 비파괴적인 방법으로 수백 ㎚ 크기의 물질의 이미지를 관찰할 수 있다. 본 연구에서는 공초점 현미경을 이용하여 V₂O5 박막의 표면에 성장된 수백 ㎚ 크기의 나노로드를 관찰하였으며, 공초점 현미경의 파장 의존성을 확인하기 위해 동일한 위치에 대해 짧은 파장대인 405 ㎚와 긴 파장대의 633 ㎚의 레이저 광원을 사용하여 이미지를 구현하였다. 실험결과, 긴 파장인 633㎚의 광원을 사용한 이미지에서는 번짐 현상이 심해져 명암대비가 작아지고 나노로드의 경계를 명확하게 분해하지 못하였지만, 짧은 파장인 405 ㎚의 광원을 사용하면 명암대비가 커지고 나노로드의 이미지를 명확하게 분해할 수 있었다. 따라서 짧은 파장의 광원을 사용한 공초점 현미경은 주사전자현미경(SEM)을 대신한 새로운 나노구조의 측정방법으로 이용될 수 있을 것으로 기대된다.

본 연구는 단색광, 혼합광, 광조사 주기에 대해 총 14가지 실험구를 설치하여 적치마 상추의 생육특성 안토시아닌 및 비타민 C 함량에 대해 조사하였다. 그 결과, 단색광 처리에서 적색광은 초장, 엽수, 지상부 생체중, 청 색광은 근장과 엽폭을 증대 시키는 것으로 나타났다. 따라서 적색광은 상추의 지상부, 생육에 청색광은 지하부 생육에 많은 영향을 미치는 것으로 판단된다. 혼합광의 경우 적색광과 백색광 혼합광에서 초장, 엽수, 엽폭, 지상부와 지하부의 생체중 및 건물중이 가장 높게 나타났다. 이는 백색광이 LED광원에 비해 광파장 대역이 다양하기 때문에 생육이 좋은 것으로 판단된다. 근장과 엽록소 함량에 대해서는 적색광과 청색광의 비율이 7 : 3에서 가장 양호한 결과를 보였다. 광조사 시간에 따른 생육특 성은 광주기가 15/09h에서 가장 효과적인 반응을 보였다. 안토시아닌 함량의 경우, 단색광에서는 463nm의 청색 광 처리에서 가장 높았고, 혼합광에서는 적색광과 청색광의 비율이 7 : 3일 때 가장 높게 나타났다. 또한 광조 사 주기에 따른 실험에서는 광주기 18/06h의 처리구에서 안토시아니 함량이 가장 높았다. 비타민 C 함량은 적색 광과 청색광의 비율이 8 : 2일 때 1.77mg · L−1로 가장 높게 나타났으며, 백색광에서 1.26mg · L−1로 가장 적은 함량을 보였다.

표고 톱밥재배시 LED광파장에 따른 생육특성을 분석한 결과, 파장이 긴 적색광과 황색광에서 대길이가 길어지고 갓색이 연해지며, 파장이 짧은 청색광과녹색광에서는 대길이가 짧아지고 갓색이 진해지는현상을 보였다. 자실체 항산화활성은 광파장에 따른큰 차이를 보이지 않았으며, 2주기까지 배지당 자실체 수량은 녹색에서 159g으로 형광등 121g 대비31% 증수효과가 있었다.

국화생육에 있어서 LED광이 미치는 영향을 구명하기 위해서 국화 'Shinma'를 대상으로 단일광 적색광(Red) 650nm, 647nm, 622nm, 청색광(Blue) 463nm, 450nm, 백색광(White)과 혼합광(적색광(Red) :청색광(Blue)-(9 : 1, 8 : 2, 7 : 3, 6 : 4, 5 : 5), 적색광(Red) :백색광(White)-(7 : 3) 그리고 광원의 조사시간에 따른 LED효과를 구명하고자 광원 비율 적색광(Red) : 청색광(Blue)-(8 : 2)의 컨트롤 베드를 3개로 구성하고, 대조구(태양광)를 포함하여 총 15개의 컨트롤 베드를 구성하여 수행하였다. 광 조사시간에 따른 생육에서는 6/6(on/off)에서 초장, 엽수, 생체 중, 엽면적이 높게 나타났지만, 전체적으로 통계적인 유의성은 인정되지 않았다. 단일광원의 경우 청색광(Blue) 450nm에서 초장과 엽면적이 가장 크게 나타났고, 근장에서는 적색광(Red) 650nm에서 가장 높게 나타났다. 그 외의 측정항목에서는 대조구(태양광)와 백색광(White)에서 높게 나타나, 단일광원에 대한 영향도 있지만, 다양한 파장대의 광원도 작물 생육에 필요한 것으로 판단된다. 혼합광의 경우 단일광과 달리 대조구(태양광)를 제외하고 적색광(Red)의 비율이 가장 높은 적색광(Red) :청색광(Blue)-(9 : 1)에서 초장이 가장 높게 나타났으며, 생체중과 건물중에서는 적색광(Red) : 백색광(White)-(7 : 3)에서 가장 높게 나타났다. 그 다음으로는 대조구(태양광)에서 높게 나타났으며, 엽면적에 있어 대조구(태양광)가 가장 높게 나타났다. 국화생육에 있어서 LED광이 미치는 영향을 구명한 결과 국화의 생장 및 형태형성에 분명히 영향을 미치는 것으로 보였으며, 단일광과 혼합광에 대해 적절한 광원의 선택은 보광의 목적이나 고품질 국화생산을 위해 필요하다고 판단된다.

Using extensive mid-IR datasets from AKARI, i.e. 9-band photometry covering the wavelength range from 2μm to 24μm and the unbiased spectroscopic survey for sources with Sν(9μm)>0.3 mJy, we study starburst galaxies specifically at the redshift of z ~ 0.5, whose mid-IR spectra are clearly dominated by the PAH emission features. PAH-selected galaxies, selected with extremely red mid-IR colour due to PAHs, have high rest-frame PAH-to-stellar luminosity ratios, comparable to those in the most active regions in nearby starburst galaxies. Thus, they seem to have active starburst regions spreading over the whole body. Furthermore, some of PAH-selected galaxies are found to have peculiar rest-frame 11-to- 8μm flux ratios, which is systematically smaller than nearby starburst/AGN spectral templates. This may indicate a systematic difference in the physical condition of ISM between nearby and distant starburst galaxies.

AKARI's all-sky survey resolves the far-infrared emission in many thousands of nearby galaxies, providing essential local benchmarks against which the evolution of high-redshift populations can be measured. This review presents some recent results in the resolved galaxy populations, covering some well-known nearby targets, as well as samples from major legacy surveys such as the Herschel Reference Survey and the JCMT Nearby Galaxies Survey. This review also discusses the prospects for higher redshifts surveys, including strong gravitational lens clusters and the AKARI NEP field.

An overview of the North Ecliptic Pole (NEP) deep multi-wavelength survey covering from X-ray to radio wavelengths is presented. The main science objective of this multi-wavelength project is to unveil the star-formation and AGN activities obscured by dust in the violent epoch of the Universe (z=0.5-2), when the star formation and black-hole evolution activities were much stronger than the present. The NEP deep survey with AKARI/IRC consists of two survey projects: shallow wide (8.2 sq. deg, NEP-Wide) and the deep one (0.6 sq. deg, NEP-Deep). The NEP-Deep provides us with a 15 μm or 18 μm selected sample of several thousands of galaxies, the largest sample ever made at these wavelengths. A continuous filter coverage at mid-IR wavelengths (7, 9, 11, 15, 18, and 24 μ m ) is unique and vital to diagnose the contribution from starbursts and AGNs in the galaxies at the violent epoch. The recent updates of the ancillary data are also provided: optical/near-IR magnitudes (Subaru, CFHT), X-ray (Chandra), FUV/NUV (GALEX), radio (WSRT, GMRT), optical spectra (Keck/DEIMOS etc.), Subaru/FMOS, Herschel/SPIRE, and JCMT/SCUBA-2.

We present a 1.1mm emission map of the OMC1 region observed with AzTEC, a new large-format array composed of 144 silicon-nitride micromesh bolometers, that was in use at the James Clerk Maxwell Telescope (JCMT). These AzTEC observations reveal dozens of cloud cores and a tail of filaments in a manner that is almost identical to the submillimeter continuum emission of the entire OMC1 region at 450 and 850 μm. We perform Fourier analysis of the image with a modified periodogram and the density power spectrum, which provides the distribution of the length scale of the structures, is determined. The expected value of the periodogram converges to the resulting power spectrum in the mean squared sense. The present analysis reveals that the power spectrum steepens at relatively smaller scales. At larger scales, the spectrum flattens and the power law becomes shallower. The power spectra of the 1.1mm emission show clear deviations from a single power law. We find that at least three components of power law might be fitted to the calculated power spectrum of the 1.1mm emission. The slope of the best fit power law, γ≈−2.7 is similar to those values found in numerical simulations. The effects of beam size and the noise spectrum on the shape and slope of the power spectrum are also included in the present analysis. The slope of the power law changes significantly at higher spatial frequency as the beam size increases.