SIMBAD references

2011ApJ...740...94D - Astrophys. J., 740, 94 (2011/October-3)

A view of the narrow-line region in the infrared: active galactic nuclei with resolved fine-structure lines in the Spitzer archive.

DASYRA K.M., HO L.C., NETZER H., COMBES F., TRAKHTENBROT B., STURM E., ARMUS L. and ELBAZ D.

Abstract (from CDS):

We queried the Spitzer archive for high-resolution observations with the Infrared Spectrograph of optically selected active galactic nuclei (AGNs) for the purpose of identifying sources with resolved fine-structure lines that would enable studies of the narrow-line region (NLR) at mid-infrared wavelengths. By combining 298 Spitzer spectra with 6 Infrared Space Observatory spectra, we present kinematic information of the NLR for 81, z ≲ 0.3 AGNs. We used the [Ne V], [O IV], [Ne III], and [S IV] lines, whose fluxes correlate well with each other, to probe gas photoionized by the AGN. We found that the widths of the lines are, on average, increasing with the ionization potential of the species that emit them. No correlation of the line width with the critical density of the corresponding transition was found. The velocity dispersion of the gas, σ, is systematically higher than that of the stars, σ*, in the AGN host galaxy, and it scales with the mass of the central black hole, MBH. Further correlations between the line widths and luminosities L, and between L and MBH, are suggestive of a three-dimensional plane connecting to a linear combination of log (σ) and log (L). Such a plane can be understood within the context of gas motions that are driven by AGN feedback mechanisms, or virialized gas motions with a power-law dependence of the NLR radius on the AGN luminosity. The MBHestimates obtained for 35 type 2 AGNs from this plane are consistent with those obtained from the relation.

Abstract Copyright:

Journal keyword(s): galaxies: active - galaxies: kinematics and dynamics - galaxies: nuclei - galaxies: Seyfert - infrared: galaxies - quasars: emission lines

Simbad objects: 85

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2021.06.14-02:16:57

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