Optically Adaptive System for Imaging Spectroscopy (OASIS) 3D data of the Canada-France-Hawaii Telescope in the central 10''.48''.3 (2.92.3 kpc2) region of the Seyfert 2 galaxy NGC 1358 were analyzed. Emission line maps for H at 6563 Å and H at 4861 Å were obtained from the OASIS spectra in the 4800-5500 and 6220-6990 Å wavelength regions. Density distribution, as indicated by the H/H flux ratio, is 105.5 cm3 at the center and 104.4-106.0 cm3 surrounding the center. An elliptical region with a density of 105.5-105.8 cm-3 (perpendicular to the bar's position angle, PA) was discovered at symmetrical locations approximately 1.2-2.0 arcsec and 1.1-1.9 arcsec south east (SE) and north west (NW), respectively, of the center along the bar (PA=130o) axis. A lower-density region (appearing as a void) also existed between the center and this symmetrical structure. The high F(H)/F(H) flux ratio values and the distribution of line widths suggest a region with high-density neutral hydrogen gas. The H flux image and linewidth, and F(H)/F(H) flux ratio image maps suggest presence of a substructure associated with a supermassive black hole at the galactic center, as well as independent structures with relatively strong fluxes in the SE and NW regions. The SE structure is delineated as one substantial substructure, whereas the NW substructure appears broken, or is potentially two separate structures, due to dust shielding. The regions have an independent boundary layer with a density exceeding 106.0cm3 toward the center, likely resulting from collision of the structure flowing along the bar with the Inner Lindblad resonance zone.

We analyze the spatially resolved kinematics of gas and stars for a sample of ten hidden type 1 AGNs in order to investigate the nature of their central sources and the scaling relation with host galaxy stellar velocity dispersion. We select our sample from a large number of hidden type 1 AGNs, which are identified based on the presence of a broad (full width at half maximum ≳1000 kms-1) component in the Hα line profile and which are frequently mis-classified as type 2 AGNs because AGN continuum and broad emission lines are weak or obscured in the optical spectral range. We used the Blue Channel Spectrograph at the 6.5-m Multiple Mirror Telescope to obtain long-slit data with a spatial scale of 0.3 arcsec pixel-1. We detected broad Hβ lines for only two targets; however, the presence of strong broad Hα lines indicates that the AGNs we selected are all low-luminosity type 1 AGNs. We measured the velocity, velocity dispersion, and ux of stellar continuum and gas emission lines (i.e., Hβ and [OIII]) as a function of distance from the center. The spatially resolved gas kinematics traced by Hβ or [OIII] are generally similar to the stellar kinematics except for the inner center, where signatures of gas out ows are detected. We compare the luminosity-weighted effective stellar velocity dispersions with the black hole masses and find that our hidden type 1 AGNs, which have relatively low back hole masses, follow the same scaling relation as reverberation-mapped type 1 AGN and more massive inactive galaxies.

While the reverberation mapping technique is the best available method for measuring black hole mass in active galactic nuclei (AGNs) beyond the local volume, this method has been mainly applied to relatively low-to-moderate luminosity AGNs at low redshift. We present the strategy of the Seoul National University AGN Monitoring Project, which aims at measuring the time delay of the Hβ line emission with respect to AGN continuum, using a sample of relatively high luminosity AGNs out to redshift z ∼ 0.5. We present simulated cross correlation results based on a number of mock light curves, in order to optimally determine monitoring duration and cadence. We describe our campaign strategy based on the simulation results and the availability of observing facilities. We present the sample selection, and the properties of the selected 100 AGNs, including the optical luminosity, expected time lag, black hole mass, and Eddington ratio.