근적외선 흡수 물질은 근적외선 이미징에 사용가능한 물질이며 최근에는 바이오 이미징, 유기태양전지 효율 향상을 목적으로 활용 범위가 확장되고 있다. 근적외선 흡수 물질은 π-conjugation system을 가지고 있으며 전자가 비편재화 되어 밴드갭이 작을수록 장가장 빛을 흡수한다. 주요 물질군으로는 유기 단분자 물질인 Polymethine, Phthalocyanine, Porphyrin 계 물질과 고분자인 Poly(thiophene), Poly(selenophene) 이 있으며, 유기 단분자 소재는 용매에 잘 녹으며 흡수 밴드가 Sharp 하고 고분자 소재는 용매에 잘 녹지 않으며 흡수 밴드가 Broad 한 특징이 있다. 최근 근적외선 응용 관련 분야의 대표적인 선도 연구로는 세포 이미징, 세포치료, 유기태양전지가 있다.

We report a search for fluctuations of the sky brightness toward the North Ecliptic Pole with AKARI, at 2.4, 3.2, and 4.1 μm . The stacked images with a diameter of 10 arcminutes of the AKARI-Monitor Field show a spatial structure on the scale of a few hundred arcseconds. A power spectrum analysis shows that there is a significant excess fluctuation at angular scales larger than 100 arcseconds that cannot be explained by zodiacal light, diffuse Galactic light, shot noise of faint galaxies, or clustering of low-redshift galaxies. These findings indicate that the detected fluctuation could be attributed to the first stars of the universe, i.e., Population III stars.

We present the result of our near infrared J- (λ=1.25μm), H- (λ=1.63μm), and Ks-band (λ=2.14μm) imaging of ultraluminous (LI > 1012L⊙) and uminous(LIR=1011−12L⊙) infrared galaxies (ULIRGs and LIRGs), to investigate their relationship through properties of their host galaxies. We find that (1) for single-nucleus ULIRGs and LIRGs, their spheroidal host galaxies have similar properties, but ULIRGs display a substantially higher level of nuclear activity than LIRGs, suggesting that their infrared luminosity difference comes primarily from the different level of current nuclear activity. We infer that LIRGs and ULIRGs have similar progenitor galaxies, follow similar evolutionary processes, and may evolve into optically-selected QSOs. (2) Largely-separated multiple-nuclei ULIRGs have significantly brighter host galaxies than single-nucleus ULIRGs and LIRGs in Ks-band, indicating that multiple-nuclei ULIRGs have a bias towards mergers of intrinsically large progenitor galaxies, in order to produce high infrared luminosity (LIR > 102L⊙) even at the early merging stage. (3) We derive dust extinction of host galaxies of ULIRGs and LIRGs to be AV ~ 14 mag in the optical or quivalently AK ~ 0.8 mag in the near-infrared Ks-band, based on the comparison of host galaxy's uminosities in the J-, H-, and Ks-bands.

We provide a new physical insight on the hot molecular clouds near the nucleus of the heavily obscured AGN IRAS 01250+2832, based on the results of near-infrared high-resolution spectroscopy of gaseous CO ro-vibrational absorption lines with Subaru/IRCS. The detected CO absorption lines up to highly excited rotational levels reveal that hot dense molecular clouds exist around the AGN under the peculiar physical conditions.

We present the properties of dust and the near-infrared spectral features in nearby early-type galaxies. The properties of dust are obtained from the AKARI far-infrared all-sky survey diffuse map. The AKARI/IRC is used for the near-infrared spectra. We improve spectral data with the new dark subtraction method on the basis of the knowledge acquired in our laboratory experiments of the engineering-model detector for the IRC. We have succeeded in fitting the continuum by a power-law function and detecting CO and SiO absorption features in early-type galaxy spectra. Comparing the properties of dust and near-infrared spectral features, we find that the power-law slope depends on dust temperature, but not on the dust mass, which suggests that low-luminosity AGNs may contribute to the changes in the power-law slope and dust temperature.

With AKARI, we carried out near-infrared spectroscopy of the nearby barred spiral galaxy, NGC 1097, categorized as Seyfert 1 with a circumnuclear starburst ring. Our observations mapped the galactic center region. As a result, we obtain the spatial distributions of the polycyclic aromatic hydrocarbon 3.3μm and the aliphatic hydrocarbon 3.4−3.6 μm emission. The former is detected from all the observed regions and the latter is enhanced near the bar connecting the ring with the nucleus. In addition, we detect absorption features due to H2O ice and CO/SiO at the ring and the galactic center, while we detect the hydrogen recombination line Brα only from the ring. Hence the observed spectra change dramatically within the central 1 kpc region.

We present the results of the near-infrared (NIR) to mid-infrared (MIR) slit spectroscopic observations of the diffuse emission toward nine positions in the nearby irregular galaxy Large Magellanic Cloud (LMC) with the Infrared Camera (IRC) on board AKARI. The unique characteristic of AKARI/IRC provides a great opportunity to analyze variations in the unidentified infrared (UIR) bands based on continuous spectra from 2.5 to 13.4 μm of the same slit area. The observed variation of I3.3 / I11.3 suggests destruction of small-sized UIR band carriers, polycyclic aromatic hydrocarbons (PAHs) in harsh environments. This result demonstrates that the UIR 3.3 μm band provides us powerful information on the excitation conditions and/or the size distribution of PAHs, which is of importance for understanding the evolutionary process of hydrocarbon grains in the Universe. It also suggests a new diagnostic diagram of two band ratios, such as I3.3 / I11.3 versus I7.7 / I11.3 , for the interstellar radiation conditions. We discuss on the applicability of the diagnostic diagram to other astronomical objects, comparing the LMC results with those observed in other galaxies such as NGC 6946, NGC 1313, and M51.

We performed a spectroscopic survey for cometary volatiles with the Infrared Camera onboard the Japanese infrared satellite AKARI. The observations were carried out in the near-infrared wavelength range in the period from 2008 June to 2010 January. In this paper, we summarize the observations and results of the AKARI survey for the mixing ratios of major volatiles in comets. We derived the 2.5 − 5 μm spectra of 18 comets including both Oort cloud comets and Jupiter-family comets. Prominent emission bands in the observed spectra are the fundamental vibrational bands of water ( H2O ) at 2.7 μm and carbon dioxide ( CO2 ) at 4.3 μm . The fundamental vibrational band of carbon monoxide (CO) at 4.7 μm and the broad emission feature probably related to C-H bearing molecules can also be recognized around the 3.4 − 3.5 μm region in some comets. We detect CO2 in 17 out of 18 comets, and derived gas production rate ratios of CO2 with respect to H2O in 17 comets. We detect a reliable CO emission band only in three of the comets. Our data set provides the largest homogeneous database of CO2 / H2O ratios in comets obtained so far.

본 연구는 근적외선분광법의 현장 이용성 및 이탈리안 라이그라스 원물 사일리지의 신속한품질평가를 위한 근적외선 검량식을 개발하기 위하여 전국에서 이탈리안 라이그라스 사일리지 약 450여 점을 수집하였다. 각각의 시료는근적외선 분광기를 이용하여 스펙트럼을 측정한 후 측정된 스펙트럼과 실험실 분석값 간에상관관계를 이용한 다변량회귀분석법을 통하여검량식을 유도한 다음 각 성분별로 예측 정확성을 평가하였다. 이탈리안 라이그라스 원물사일리지의 수분 함량에 대한 검량식 개발 결과는 검량식 작성시 표준오차(SEC)가 0.94%(R2=0.99)로 매우 우수한 정확성을 보였으며 개발된 검량식의 상호검증(SECV) 결과는 1.27%(R2=0.98)로 나타났다. ADF, NDF 및 조단백질함량 평가를 위해 개발된 검량식의 상호검증(SECV) 결과는 각각 1.26% (R2=0.88), 2.0%(R2=0.84) 및 0.96% (R2=0.93)으로 나타났으며조회분함량 평가에 대한 검량식 개발 결과는다소 낮은 정확성(SECV 0.72%, R2=0.62)을 나타내었다. 사일리지의 발효품질의 주요 평가항목인 pH와 젖산함량 평가에 대한 검량식 개발결과(SEC)는 각각 0.41 (R2=0.85), 0.18% (R2=0.92)로 나타났으며 개발된 검량식의 상호검증결과(SECV)는 각각 0.56 (R2=0.78), 0.31%(0.81)로 나타났다.

본 연구는 최근 조사료의 신속한 품질평가 방법으로 근적외선 분광법의 이용성이 확대되고 있는 시점에 근적외선 분광기의 현장 적용성을 평가하기 위하여 수행되었다. 실험실용 근적외선분광기와 소형 근적외선분광기의 조사료 품질평가의 예측 정확성을 평가하기 위하여 전남지역에서 이탈리안 라이그라스 사일리지 67점을 수집하여 각각의 근적외선 분광기를 이용하여 스펙트럼을 측정한 후 사료가치의 실험실 분석값과 다변량회귀분석을 통하여 검량식을 유도하여 예측 정확성을 평가하

본 연구는 춘파용 사초의 사료가치를 신속하고 정확하게 측정할 수 있는 습식분석의 대안을 모색하기 위하여 수행하였다. 근적외선분광 분석법을 이용한 사초의 분석 가능성을 타진하기 위해 2009년에 생산된 사초 175점을 시료로 사용하였다. 시료는 이탈리안 라이그라스와 보리, 그리고 완두를 혼파한 것으로 NIR System으로 400~2,400nm 사이의 파장을 얻었다. 그리고 수분, 조단백질, 조회분, NDF, ADF를 분석한 다음, 파장과 습식분석치를 이