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BLACK HOLE MASS MEASUREMENTS WITH REST-FRAME OPTICAL QUASAR SPECTRA AT 3<z<
Jun, Hyunsung David,Im, Myungshin,Lee, Hyung Mok,AKARI QSONG team, AKARI QSONG team The Korean Astronomical Society 2012 天文學論叢 Vol.27 No.4
We summarize the progress on the rest-frame optical spectroscopy of quasars at 3<z<6, from the AKARI QSONG program. QSONG (Quasar Spectroscopic Observations with NIR Grism) is an AKARI space telescope mission program which utilizes the unique spectroscopic capability in the wavelength range of $2.5-5{\mu}m$. This spectral window has been utilized for detecting redshifted $H{\alpha}$ emission lines of our high redshift subsample of quasars. From the calculated emission line widths and luminosities we measured supermassive black hole masses using well calibrated optical mass estimators. Science topics regarding optical based black hole masses at high-z are discussed.
The Most Massive Active Galactic Nuclei at 1 ≲<i>z</i>≲ 2
Jun, Hyunsung D.,Im, Myungshin,Kim, Dohyeong,Stern, Daniel American Astronomical Society 2017 The Astrophysical journal Vol.838 No.1
<P>We obtained near-infrared spectra of 26 Sloan Digital Sky Survey quasars at 0.7 < z < 2.5 with reported rest-frame ultraviolet M-BH similar to 10(10) M-circle dot to critically examine the systematic effects involved with their mass estimations. We find that active galactic nuclei (AGNs) heavier than 10(10) M-circle dot often display double-peaked H alpha emission, extremely broad Fe II complex emission around Mg II, and highly blueshifted and broadened C IV emission. The weight of this evidence, combined with previous studies, cautions against the use of M-BH values based on any emission line with a width over 8000 km s(-1). Also, the M-BH estimations are not positively biased by the presence of ionized narrow line outflows, anisotropic radiation, or the use of line FWHM instead of sigma for our sample, and unbiased with variability, scatter in broad line equivalent width, or obscuration for general type-1 quasars. Removing the systematically uncertain M-BH values, similar to 10(10) M-circle dot black holes (BHs) in 1 less than or similar to z less than or similar to 2 Ns can still be explained by anisotropic motion of the broad line region from similar to 10(9.5) M-circle dot BHs, although current observations support that they are intrinsically most massive, and overmassive to the host's bulge mass.</P>