AGN-Driven Biconical Outflows as the Origin of the Double-Peaked [O~{\sc iii}] doublet in SDSS J134733.36+121724.27

TL;DR

This study confirms that the double-peaked [O III] emission lines in SDSS J134733.36+121724.27 are caused by AGN-driven biconical outflows, providing insights into the kinematic processes in this Type-1.9 AGN.

Contribution

The paper demonstrates that double-peaked [O III] lines can originate from AGN-driven outflows rather than alternative scenarios like dual AGN or rotation.

Findings

Double-peaked [O III] lines are best modeled by two Gaussian components.

The source is classified as a Type-1.9 AGN based on spectral features.

Outflows are the likely cause of the double-peaked emission profiles.

Abstract

In this manuscript, we recheck the spectroscopic properties of SDSS J134733.36+121724.27 (4C+12.50), confirming the presence of the double-peaked [O~{\sc iii}]$\lambda\lambda4959,5007$\AA\ doublet and a broad H$\alpha$. The former likely results from AGN-driven biconical outflows, while the absence of a broad H$\beta$ supports a classification of the source as a Type-1.9 AGN. We analyze its high-quality Sloan Digital Sky Survey (SDSS) optical spectrum after robustly subtracting host galaxy and AGN continuum contributions through a simple stellar population fitting method employing 39 templates and a power-law continuum. Each narrow line of the [O~{\sc iii}]$\lambda\lambda4959,5007$\AA\ doublet is better described by two Gaussian components (blue-shifted and red-shifted) than by a single Gaussian, as confirmed by the F-test. Broad components are included for both H$\alpha$ and H$\beta$, but only H$\alpha$ reveals a significant detection, further supported by a comparison between the SDSS spectrum and that previously reported. These results support that the object is highly consistent with a Type-1.9 AGN classification, and the double-peaked [O~{\sc iii}] profiles are most likely produced by AGN-driven biconical outflows rather than by a rotating narrow-line region or a dual AGN merger system. Additional observations are still needed to strengthen these conclusions.