<P>We present 2.5-5.0 mu m spectra of 83 nearby (0.002 <z <0.48) and bright (K <14 mag) type-1 active galactic nuclei (AGNs) taken with the Infrared Camera on board AKARI. The 2.5-5.0 mu m spectral region contains emission lines such as...
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https://www.riss.kr/link?id=A107514920
2015
-
SCI,SCIE,SCOPUS
학술저널
17
0
상세조회0
다운로드다국어 초록 (Multilingual Abstract)
<P>We present 2.5-5.0 mu m spectra of 83 nearby (0.002 <z <0.48) and bright (K <14 mag) type-1 active galactic nuclei (AGNs) taken with the Infrared Camera on board AKARI. The 2.5-5.0 mu m spectral region contains emission lines such as...
<P>We present 2.5-5.0 mu m spectra of 83 nearby (0.002 <z <0.48) and bright (K <14 mag) type-1 active galactic nuclei (AGNs) taken with the Infrared Camera on board AKARI. The 2.5-5.0 mu m spectral region contains emission lines such as Br alpha (2.63 mu m), Bra (4.05 mu m), and polycyclic aromatic hydrocarbons (3.3 mu m), which can be used for studying the black hole (BH) masses and star formation activity in the host galaxies of AGNs. The spectral region also suffers less dust extinction than in the ultra violet (UV) or optical wavelengths, which may provide an unobscured view of dusty AGNs. Our sample is selected from bright quasar surveys of Palomar-Green and SNUQSO, and AGNs with reverberation-mapped BH masses from Peterson et al. Using 11 AGNs with reliable detection of Brackett lines, we derive the Brackett-line-based BH mass estimators. We also find that the observed Brackett line ratios can be explained with the commonly adopted physical conditions of the broad line region. Moreover, we fit the hot and warm dust components of the dust torus by adding photometric data of SDSS, 2MASS, WISE, and ISO to the AKARI spectra, finding hot and warm dust temperatures of similar to 1100K and similar to 220 K, respectively, rather than the commonly cited hot dust temperature of 1500 K.</P>