Mechanisms and Impact of Fast Disk Winds in Active Galactic Nuclei

Determine the launching mechanisms of fast accretion disk winds in active galactic nuclei (including ultra-fast outflows, UFOs), quantify the mass, momentum, and energy transported by these winds, identify the evolutionary stage toward the quasar phase at which they become prominent, and establish their role in active galactic nucleus (AGN) feedback on the host galaxy.

Background

The paper reports XRISM observations of the ULIRG IRAS 05189−2524, revealing multiple ultra-fast outflow (UFO) components and a P Cygni profile in the Fe-K band. In the broader context of AGN–galaxy co-evolution, fast disk winds such as UFOs are a key proposed mechanism for AGN feedback that may suppress star formation and drive evolutionary transitions toward the quasar phase.

Despite observational progress, the introduction emphasizes that core aspects of fast disk winds remain unresolved: how they are launched, how much mass/momentum/energy they carry, when in the evolutionary sequence they become prominent, and how they affect the host galaxy. The paper positions these as central, outstanding questions in AGN research, motivating the detailed spectroscopic analysis presented.

References

However, the launching mechanisms of fast disk winds, the amount of mass, momentum, and energy they carry, the evolutionary stage toward the quasar phase in which they become prominent, and their role in AGN feedback remain poorly understood, constituting one of the most important open questions in AGN research.

— Discovery of Powerful Multi-Velocity Ultra-Fast Outflows in the Starburst Merger Galaxy IRAS 05189$-$2524 with XRISM  (2510.18027 - Noda et al., 20 Oct 2025) in Section 1 (Introduction)

Understanding how powerful X-ray winds launched from the inner accretion disc transfer their energy and momentum to the host galaxy remains a key open question in AGN feedback.

— AGN winds and outflows: from accretion-disc scales to the host galaxy  (2609.29758 - Porquet, 24 Sep 2026) in Section 3, “From accretion-disc winds to galaxy-scale outflows”

However, both the acceleration mechanism of UFOs and the formation mechanism of clumps remain unknown.

— Radiation Pressure Instability-Driven Variability of Line-Driven Disk Winds in AGNs: Connection to Periodic Luminosity Variations and UFO Appearance  (2609.16636 - Kuroda et al., 15 Sep 2026) in Section 1, Introduction

However, the origin of absorption lines remains unknown.

— A relativistic inflow candidate in a quasar at cosmic noon  (2610.10267 - Xu et al., 7 Oct 2026) in Section 2, Analysis and Results

Despite this evidence, whether the inflow originates in a chaotic cold accretion cascade, a magnetically guided channel, or the fallback of material that fails to escape the gravitational potential remains an open question.

— Multi-epoch Detection of an Ultra-fast Inflow in ESP 39607: Evidence for an Accretion Cascade  (2609.03019 - Peca et al., 2 Sep 2026) in Section 7, Summary and Conclusions; discussion of the cascade scenario in Section 6.5

A dusty wind could potentially contribute to the reddening, but the present data do not establish its role in obscuring the nucleus or clearing the host.

— A dust-reddened quasar in a [C II]-luminous host at z=6.55  (2610.13758 - Yang et al., 9 Oct 2026) in Section 4.3, “Connection to lower-redshift red quasars”