Hot Graphite Dust and the Infrared Spectral Energy Distribution of Active Galactic Nuclei

TL;DR

This study models the infrared spectral energy distribution of active galactic nuclei using a three-component approach, revealing similarities in mid-IR emission between different Seyfert types and characterizing hot graphite dust properties.

Contribution

It introduces a detailed three-component model including hot graphite dust, with a focus on the hot dust's temperature distribution and emission lines, advancing understanding of AGN IR emission.

Findings

Hot dust covering factor is 0.15-0.35, anti-correlated with luminosity.

Mid-IR emission of NLS1s and BLS1s are very similar.

Hot dust continuum fits near-IR spectra well.

Abstract

We present a detailed investigation of the near-to-far infrared (IR) spectral energy distribution (SED) of a large sample of Spitzer-observed active galactic nuclei (AGN). We fitted the spectra of 51 narrow line Seyfert 1 galaxies (NLS1s) and 64 broad line Seyfert 1 galaxies (BLS1s) using a three component model: a clumpy torus, a dusty narrow line region (NLR) and hot pure-graphite dust located in the outer part of the broad line region (BLR). The fitting is performed on star formation (SF) subtracted SEDs using SF templates that take into account the entire range of possible host galaxy properties. We find that the mid-IR intrinsic emission of NLS1s and BLS1s are very similar, regardless of the AGN luminosity, with long wavelength downturn at around 20-25 um. We present a detailed model of the hot dust component that takes into account the distribution of dust temperature within the clouds and their emission line spectrum. The hot dust continuum provides a very good fit to the observed near-IR continuum spectrum. Most line emission in this component is dramatically suppressed, except MgII(2798A) and HeI lines that are still contributing significantly to the total BLR spectrum. We calculate the covering factors of all the AGN components and show that the covering factor of the hot-dust clouds is about 0.15-0.35, similar to the covering factor of the torus, and is anti-correlated with the source luminosity and the normalized accretion rate.