The Mid-Infrared Continua of Seyfert Galaxies

TL;DR

This study analyzes mid-infrared spectra of Seyfert galaxies, distinguishing starburst and active nuclear contributions, revealing differences between types and identifying a common warm dust emission feature.

Contribution

It introduces a method to separate starburst and nuclear components in Seyfert spectra and compares spectral features across Seyfert types, revealing new insights into their dust emission.

Findings

Type 2 Seyferts have weaker short-wavelength nuclear continua than Type 1.

A spectral bump between 15-20 microns indicates warm dust emission (~200 K).

PAH-dominated Seyferts show similar spectra to Seyfert 1.8/1.9 types after starburst subtraction.

Abstract

An analysis of archival mid-infrared (mid-IR) spectra of Seyfert galaxies from the Spitzer Space Telescope observations is presented. We characterize the nature of the mid-IR active nuclear continuum by subtracting a template starburst spectrum from the Seyfert spectra. The long wavelength part of the spectrum contains a strong contribution from the starburst-heated cool dust; this is used to effectively separate starburst-dominated Seyferts from those dominated by the active nuclear continuum. Within the latter category, the strength of the active nuclear continuum drops rapidly beyond ~ 20 micron. On average, type 2 Seyferts have weaker short-wavelength active nuclear continua as compared to type 1 Seyferts. Type 2 Seyferts can be divided into two types, those with strong poly-cyclic aromatic hydrocarbon (PAH) bands and those without. The latter type show polarized broad emission lines in their optical spectra. The PAH-dominated type 2 Seyferts and Seyfert 1.8/1.9s show very similar mid-IR spectra. However, after the subtraction of the starburst component, there is a striking similarity in the active nuclear continuum of all Seyfert optical types. PAH-dominated Seyfert 2s and Seyfert 1.8/1.9s tend to show weak active nuclear continua in general. A few type 2 Seyferts with weak/absent PAH bands show a bump in the spectrum between 15 and 20 micron. We suggest that this bump is the peak of a warm (~200 K) blackbody dust emission, which becomes clearly visible when the short-wavelength continuum is weaker. This warm blackbody emission is also observed in other Seyfert optical subtypes, suggesting a common origin in these active galactic nuclei.