Exploring accretion disc physics and black hole growth with regular monitoring of ultrafast AGN winds

TL;DR

This study uses 15 years of XMM-Newton data to analyze ultra-fast winds in AGN, linking wind properties to accretion physics and black hole growth, and highlights the potential of targeted future observations.

Contribution

It demonstrates that Eddington-limited accretion models predict wind velocities and ionization consistent with observations, and emphasizes the importance of long-term monitoring for understanding SMBH evolution.

Findings

Ultra-fast winds are common in radio-quiet AGN.

Observed wind velocities (~0.1c) match theoretical predictions.

Extended observations reveal complex wind flow patterns.

Abstract

15 years of XMM-Newton observations have established that ultra-fast, highly ionized winds are common in radio-quiet AGN. A simple theory of Eddington-limited accretion correctly predicts the typical velocity (~0.1c) and high ionization of such winds, with observed flow energy capable of ejecting star-forming gas. With a recent extended XMM-Newton observation of the archetypal UFO, PG1211+143, revealing a more complex flow pattern, we suggest that targetted observations over the next decade offer unique potential for probing the inner accretion disc structure and SMBH growth.