Xmm-newton Reveals Multi-layered Fast Wind in Markarian 877, Reaching 0.03, 0.3c Velocity

Powerful, highly ionized winds, known as Ultra Fast Outflows, significantly influence the evolution of galaxies by transferring energy and momentum from supermassive black holes, and a new investigation into the Seyfert 1 galaxy Markarian 877 reveals an unexpectedly complex outflow structure. Xin Xiang, Jon M. Miller, and Ehud Behar, alongside colleagues including W. N. Brandt and Luigi Gallo, analysed data from the XMM-Newton space telescope and discovered not one, but three distinct outflow components, each travelling at a substantial fraction of the speed of light. This multi-layered fast wind exhibits a wide range of properties, with the fastest component possessing enough energy to drive significant feedback throughout the host galaxy, and the observation of multiple velocity components suggests a complex, potentially clumpy, outflow medium shaped by both radiation and magnetic forces. The team’s findings, which also include analysis of absorption patterns across different X-ray wavelengths, provide crucial insights into the mechanisms driving these powerful outflows and their impact on galaxy evolution.

Outflows in Active Galactic Nuclei Revealed

This research investigates the powerful outflows emanating from Active Galactic Nuclei, or AGN, which are supermassive black holes actively accreting matter at the centers of galaxies. Scientists are studying these outflows to understand their properties and how they impact the surrounding galactic environment. By meticulously analyzing absorption features in both soft and hard X-ray bands, scientists determined the velocity, ionization, and density of each component.

They calculated launching radii using two independent methods, suggesting a common origin for the outflows. Calculations reveal mass outflow rates reaching up to 880 solar masses per year for the fastest component, and kinetic power exceeding 21x 10⁴⁶ erg s⁻¹. Even after conservative estimates, the inferred mass outflow rates remained substantial. The study demonstrates that the innermost wind component exceeds the threshold required to initiate significant galaxy-scale feedback, establishing it as a strong candidate for driving substantial changes in the host galaxy. By calculating both outflow momentum rate and radiation momentum flux, the team demonstrated that the wind is likely powered by a combination of radiative and magnetic forces.

Measurements confirm a positive correlation between these two forces, indicating their combined influence on the outflow. This research builds upon previous studies of Mrk 877, revealing a complex structure of ionized winds. Their modeling demonstrates that the fastest component exceeds 10% of the Eddington luminosity, indicating its potential to significantly influence galaxy-scale feedback processes. Scientists identified three distinct outflow components, each travelling at a substantial fraction of the speed of light, and characterized by differing ionization states and absorption features across the X-ray spectrum. These observations demonstrate that powerful winds are launched from close to the supermassive black hole, capable of influencing the surrounding galactic environment through feedback mechanisms. The study infers that these outflows likely originate within or near the broad line region surrounding the black hole, and that their combined mass loss may even exceed the rate of material falling into the black hole itself.

While the data suggest a contribution from radiation pressure in driving these winds, the team acknowledges that magnetic forces likely play a crucial role, particularly for the fastest components. Researchers note that the observed winds are likely clumpy and intermittent in nature, reducing the total mass carried by the flow. Future high-resolution observations are needed to confirm the origin of the outflows and to better constrain the contribution of different driving mechanisms. Despite these limitations, this work provides valuable insights into the dynamics of active galactic nuclei and the powerful feedback processes that shape galaxy evolution.