Discovery of Relativistic Outflow in the Seyfert Galaxy Ark 564

TL;DR

This paper reports the first unambiguous detection of ultra-high velocity relativistic outflows in the soft X-ray spectrum of the Seyfert galaxy Ark 564, challenging existing models of AGN outflows.

Contribution

It presents the identification of relativistic outflow lines at ~0.1c in a Seyfert galaxy's X-ray spectrum, supported by photoionization modeling, marking a novel discovery in AGN research.

Findings

Detection of absorption lines at ~0.1c velocities.

Significant improvement in spectral fit with ultra-high velocity components.

Implications for AGN outflow models and driving mechanisms.

Abstract

We present \chandra high energy transmission grating spectra of the narrow-line Seyfert-1 galaxy Ark 564. The spectrum shows numerous absorption lines which are well modeled with low velocity outflow components usually observed in Seyfert galaxies \citep{Gupta2013}. There are, however, some residual absorption lines which are not accounted for by low-velocity outflows. Here we present identifications of the strongest lines as $K\alpha$ transitions of \oviin (two lines) and \ovin at outflow velocities of $\sim 0.1c$. These lines are detected at $6.9\sigma$, $6.2\sigma$, and $4.7\sigma$ respectively and cannot be due to chance statistical fluctuations. Photoionization models with ultra-high velocity components improves the spectral fit significantly, providing further support for the presence of relativistic outflow in this source. Without knowing the location of the absorber, its mass and energy outflow rates cannot be well constrained; we find $\dot{E}(outflow)/L_{bol}$ lower limit of $\geq 0.006$% assuming a bi-conical wind geometry. This is the first time that absorption lines with ultra-high velocities are unambiguously detected in the soft X-ray band. The presence of outflows with relativistic velocities in AGNs with Seyfert-type luminosities is hard to understand and provides valuable constraints to models of AGN outflows. Radiation pressure is unlikely to be the driving mechanism for such outflows and magneto-hydrodynamic may be involved.