# Relativistic components of the Ultra-Fast Outflow in the Quasar PDS 456 from Chandra/HETGS, NuSTAR and XMM-Newton observations

## TL;DR

This study analyzes multi-epoch X-ray observations of quasar PDS 456, revealing a persistent ultra-fast outflow with relativistic velocities and a new faster component, providing insights into AGN feedback mechanisms.

## Contribution

First detection of a relativistic outflow component at -0.48c in PDS 456 across multiple epochs, with detailed photoionization modeling of the outflow properties.

## Key findings

- Confirmed persistent ultra-fast outflow at -0.24 to -0.29c
- Detected an additional faster outflow component at -0.48c
- Outflows are powerful enough to influence host galaxy evolution

## Abstract

We present the spectral analysis of Chandra/HETGS and NuSTAR observations of the quasar PDS 456 from 2015, and XMM-Newton and NuSTAR archival data from 2013-2014, together with Chandra/HETGS data from 2003. We analyzed these three different epochs in a consistent way, looking for absorption features corresponding to highly ionized blueshifted absorption lines from H-like and He-like ions of iron (and nickel), as well as of other elements (O, Ne, Si, and S) in the soft band. We confirm the presence of a persistent ultra-fast outflow (UFO) with a velocity of v_out=-0.24 - -0.29c, previously detected. We also report the detection of an additional faster component of the UFO with a relativistic velocity of v_out=-0.48c. We implemented photoionization modeling, using XSTAR analytic model warmabs, to characterize the physical properties of the different kinematic components of the ultra-fast outflow and of the partial covering absorber detected in PDS 456. These two relativistic components of the ultra-fast outflow observed in the three epochs analyzed in this paper are powerful enough to impact the host galaxy of PDS 456 through AGN feedback.