The FeII emission in active galactic nuclei: excitation mechanisms and location of the emitting region

TL;DR

This study investigates FeII emission in 25 AGNs, revealing that Lyman-alpha fluorescence significantly contributes to FeII production and that FeII originates from a region roughly twice as far from the nucleus as Paschen-beta, with implications for AGN physics.

Contribution

It provides new insights into the excitation mechanisms and spatial origin of FeII emission in AGNs, emphasizing the role of Lyman-alpha fluorescence and detailed emission region localization.

Findings

Lyman-alpha fluorescence contributes at least 18% to optical FeII.

FeII emission region is approximately twice as far from the nucleus as Paschen-beta.

FeII, OI, and CaII lines have similar widths, narrower than Paschen-beta.

Abstract

We present a study of FeII emission in the near-infrared region (NIR) for 25 active galactic nuclei (AGNs) to obtain information about the excitation mechanisms that power it and the location where it is formed. We employ a NIR FeII template derived in the literature and found that it successfully reproduces the observed FeII spectrum. The FeII bump at 9200 Angstroms detected in all objects studied confirms that Lyman-alpha fluorescence is always present in AGNs. The The correlation found between the flux of the 9200 Angstroms bump, the 1 micron lines and the optical FeII imply that Lyman-alpha fluorescence plays an important role in the FeII production. We determined that at least 18% of the optical FeII is due to this process while collisional excitation dominates the production of the observed FeII. The line profiles of FeII 10502, OI 11287, CaII 8664 and Paschen-beta were compared to gather information about the most likely location where they are emitted. We found that FeII, OI and CaII have similar widths and are, on average, 30% narrower than Paschen-beta. Assuming that the clouds emitting the lines are virialized, we show that the FeII is emitted in a region twice as far from the central source than Paschen-beta. The distance though strongly varies: from 8.5 light-days for NGC4051 to 198.2 light-days for Mrk509. Our results reinforce the importance of the FeII in the NIR to constrain critical parameters that drive its physics and the underlying AGN kinematics as well as more accurate models aimed at reproducing this complex emission.