Multi-layered Fast Wind observed in XMM-Newton snapshot of Seyfert 1 Markarian 877

TL;DR

This study analyzes an XMM-Newton snapshot of Seyfert 1 galaxy Mrk 877, revealing three distinct ultra-fast outflow components with velocities up to 0.1c, indicating complex multi-phase winds driven by radiation and magnetic forces.

Contribution

First detailed multi-component UFO analysis in Mrk 877, showing diverse velocities and ionization states, and suggesting combined radiative and magnetic driving mechanisms.

Findings

Detected three UFO components with velocities up to 0.1c.

Fastest component exceeds 5% of Eddington luminosity, capable of galaxy feedback.

Soft X-ray UFO shares velocity with higher-ionization component, indicating a two-phase medium.

Abstract

Ultra Fast Outflows (UFOs) are powerful, highly ionized winds launched from the innermost regions of Active Galactic Nuclei (AGNs), reaching velocities of 0.03 -- 0.3 c and playing a key role in AGN feedback. We present a photoionization analysis of an 18 ks \xmm\ snapshot of the Seyfert 1 AGN Mrk 877, revealing three distinct UFO components with line-of-sight velocities of $0.10^{+0.005}_{-0.005}~c$ , $ 0.04^{+0.005}_{-0.004}~c$ , and $0.05^{+0.005}_{-0.004}~c$. These components span a broad range of ionization parameters and column densities, producing absorption features across both soft and hard X-ray bands. Even under the most conservative assumption for the volume filling factor, the fastest component exceeds $5\%$ of the Eddington luminosity, making it capable of driving strong galaxy-scale feedback. The soft X-ray UFO component, despite its lower ionization, shares a similar velocity as a higher-ionization component, hinting at a two-phase medium likely shaped by clumpiness or interactions with ambient material. The density profile inferred from the Absorption Measurement Distributions (AMD) and the positive trend between outflow momentum rate and radiation momentum flux suggest that wind is powered by a combination of radiative and magnetic driving.