Physical Conditions in the Inner Narrow Line Region of the Seyfert 2 Galaxy Markarian 573

TL;DR

This study investigates the physical conditions of the inner narrow-line region in Seyfert 2 galaxy Mrk 573 using optical spectra and photoionization models, revealing complex ionization structures and spatial distributions.

Contribution

It provides a detailed three-component photoionization model for the NLR of Mrk 573, linking emission lines to spatially distinct ionization zones and comparing with other Seyfert galaxies.

Findings

[Fe X] is broader and blue-shifted compared to less ionized lines.

The AGN in Mrk 573 is radiating at or above its Eddington Luminosity.

The ionized components are approximately 55 parsecs from the AGN.

Abstract

We have examined the physical conditions within a bright emission-line knot in the inner narrow-line region (NLR) of the Seyfert 2 galaxy Mrk 573 using optical spectra and photoionization models. The spectra were obtained with the Hubble Space Telescope/Space Telescope Imaging Spectrograph with the G430L and G750M gratings. Comparing the spatial emission-line profiles, we found [Fe X] 6734 barely resolved, [O III] 5007 centrally peaked, but broader than [Fe X], and [O II] 3727 the most extended. The spectra reveal that [Fe X] is broader in velocity width and blue-shifted compared with lines from less ionized species. Our estimate of the bolometric luminosity indicates that the active galactic nucleus (AGN) is radiating at or above its Eddington Luminosity, which is consistent with its identification as a hidden Narrow-Line Seyfert 1. We were able to successfully match the observed emission line ratios with a three-component photoionization model. Two components, one to account for the [O III] emission and another in which the [Fe X] arises, are directly ionized by the AGN, while [O II] forms in a third component, which is ionized by a heavily absorbed continuum. Based on our assumed ionizing continuum and the model parameters, we determined that the two directly-ionized components are ~ 55 pc from the AGN. We have found similar radial distances for the central knots in the Seyfert 2 galaxies Mrk 3 and NGC 1068, but much smaller radial distances for the inner NLR in the Seyfert 1 galaxies NGC 4151 and NGC 5548. Although in general agreement with the unified model, these results suggest that the obscuring material in Seyfert galaxies extends out to at least tens of parsecs from the AGN.