Speaker
Description
Outflows in galaxies play a crucial role in AGN feedback by transporting mass and energy from the nucleus to larger scales through winds and jets, as observed across multiple wavelengths. Theoretical models suggest that quasar feedback originates from sub-relativistic Ultra Fast Outflows (UFOs) ($\sim$10$^4$ km/s) launched at accretion disk scales, which interact with the ISM, slowing down and cooling as they propagate outward. This process results in less ionized outflows at larger scales, observed in the optical and molecular phases. The presence of energy-conserving winds can be tested by comparing the X-ray, ionized, and molecular gas phases.
IRAS 17020+4544, a Narrow Line Seyfert 1 and LIRG, is an ideal target for such a study, as it hosts a multi-component X-ray UFO, a molecular outflow resolved with NOEMA, and an elongated VLBI radio jet that may induce shocks in the ISM. Using MEGARA/GTC data, we characterize the ionized outflow over $\sim$140 kpc$^2$, covering the region where the powerful molecular outflow is resolved. By deriving its kinematics and energetics (velocity, mass, kinetic power, momentum, etc.), we aim to assess the energy budget of the outflow and compare it with the molecular and X-ray phases. This work will provide key insights into AGN feedback efficiency and the conditions under which outflows retain their energy as they expand ("energy-conserving" regime).
