Search

We present mid-infrared (mid-IR) spectra of the Compton-thick Seyfert 2 galaxy NGC 3281, obtained with the Thermal-Region Camera Spectrograph at the Gemini-South telescope. The spectra present a very deep silicate absorption at 9.7 µm, and [S IV] 10.5 µm and [Ne II] 12.7 µm ionic lines, but no evidence of polycyclic aromatic hydrocarbon emission. We find that the nuclear optical extinction is in the range 24 mag ⩽ Av ⩽ 83 mag. A temperature T = 300 K was found for the blackbody dust continuum component of the unresolved 65 pc nucleus and the region at 130 pc SE, while the region at 130 pc NW reveals a colder temperature (200 K). We describe the nuclear spectrum of NGC 3281 using a clumpy torus model that suggests that the nucleus of this galaxy hosts a dusty toroidai structure. According to this model, the ratio between the inner and outer radius of the torus in NGC 3281 is R0/Rd = 20, with 14 clouds in the equatorial radius with optical depth of πv = 40 mag. We would be looking in the direction of the torus equatorial radius (i = 60°), which has outer radius of R0 ~ 11 pc. The column density is NH ≈ 1.2 x 1024cm-2 and the iron Kα equivalent width (≈0.5-1.2 keV) is used to check the toms geometry. Our findings indicate that the X-ray absorbing column density, which classifies NGC 3281 as a Compton-thick source, may also be responsible for the absorption at 9.7µm providing strong evidence that the silicate dust responsible for this absorption can be located in the active galactic nucleus toms. [ABSTRACT FROM AUTHOR]

In recent observations by the Hubble Space Telescope (HST) as part of a campaign to discover locations and kinematics of AGN outflows, we found that Mrk 509 contains a 3″ (∼2100 pc) linear filament in its central region. Visible in both optical continuum and [O III] imaging, this feature resembles a “check mark” of several knots of emission that travel northwest to southeast before jutting toward the nucleus from the southwest. Space Telescope Imaging Spectrograph (STIS/HST) observations along the inner portion of the filament reveal redshifted velocities, indicating that the filament is inflowing. We present further observations of the nucleus in Mrk 509 using the Gemini Near-Infrared Integral Field Spectrograph, from which we conclude that this structure cannot be related to previously studied, typical narrow line region outflows and instead embodies the remains of an ongoing minor merger with a gas-rich dwarf galaxy, therefore providing a great opportunity to study the fueling of an AGN by a minor merger in progress. [ABSTRACT FROM AUTHOR]