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AKARI OBSERVATIONS OF DUSTY TORI OF ACTIVE GALACTIC NUCLEI
SHINKI OYABU,HIDEHIRO KANEDA,Masaya Izuhara,Keisuke Tomita,DAISUKE ISHIHARA,Kimiaki Kawara,Yoshiki Matsuoka 한국천문학회 2017 天文學論叢 Vol.32 No.1
The dusty torus of Active Galactic Nuclei (AGNs) is one of theimportant components for theunification theory of AGNs. The geometry and properties ofthe dusty torus are key factors in understanding the nature of AGNs aswell as the formation and evolution of AGNs. However, they are stillunder discussion. Infrared observation is useful for understanding the dustytorus as thermal emission from hot dust with the dust sublimationtemperature ($\sim$ 1500 K) has been observed in the infrared. We have analyzed infrared spectroscopic data of low-redshift andhigh-redshift quasars, which are luminous AGNs. For the low-redshift quasars, we constructed the spectral energydistributions (SEDs) with AKARI near-infrared and Spitzer mid-infraredspectra and decomposed the SEDs into a power-lawcomponent from the nuclei, silicate features, and blackbody components withdifferent temperatures from the dusty torus. From the decomposition,the temperature of the innermost dusty torus shows the range between900-2000 K. For the high-redshiftquasars, AKARI traced rest-frameoptical and near-infrared spectra of AGNs. Combining with WISE data,we havefound that the temperature of the innermost dusty torus in high redshift quasarsis lower than that in typical quasars. The hydrogen H$\alpha$ emission line from the braod emission line region in thequasars also shows narrow full widthat half maximumof 3000$-$4000 km s$^{-1}$. These results indicatethat the dusty torus and the broad emission line region are more extendedthan those of typical quasars.
miniTAO/ANIR Paα SURVEY OF LOCAL LIRGs
Tateuchi, Ken,Motohara, Kentaro,Konishi, Masahiro,Takahashi, Hidenori,Kato, Natsuko,Uchimoto, Yuka K.,Toshikawa, Koji,Ohsawa, Ryou,Kitagawa, Yutaro,Yoshii, Yuzuru,Doi, Mamoru,Kohno, Kotaro,Kawara, Kim The Korean Astronomical Society 2012 天文學論叢 Vol.27 No.4
ANIR (Atacama Near InfraRed camera) is a near infrared camera for the University of Tokyo Atacama 1m telescope, installed at the summit of Co. Chajnantor (5,640 m altitude) in northern Chile. The high altitude and extremely low water vapor (PWV = 0.5 mm) of the site enable us to perform observation of hydrogen $Pa{\alpha}$ emission line at $1.8751{\mu}m$. Since its first light observation in June 2009, we have been carrying out a $Pa{\alpha}$ narrow-band imaging survey of nearby luminous infrared galaxies (LIRGs), and have obtained $Pa{\alpha}$ for 38 nearby LIRGs listed in AKARI/FIS-PSC at the velocity of recession between 2,800 km/s and 8,100 km/s. LIRGs are affected by a large amount of dust extinction ($A_V$~ 3 mag), produced by their active star formation activities. Because $Pa{\alpha}$ is the strongest hydrogen recombination line in the infrared wavelength ranges, it is a good and direct tracer of dust-enshrouded star forming regions, and enables us to probe the star formation activities in LIRGs. We find that LIRGs have two star-forming modes. The origin of the two modes probably come from differences between merging stage and/or star-forming process.