The XMM-Newton and NuSTAR View of IRASF11119+3257. I Detection of Multiple Ultra Fast Outflow Components and a Very Cold Corona

IRASF11119+3257 is an ultra-luminous infrared galaxy with a post-merger morphology, hosting a type-1 quasar at z=0.189. It shows a prominent ultra-fast outflow (UFO) absorption feature ($ in its 2013 spectrum. This is the first system in which the energy released by the UFO was compared to that of the known galaxy-scale molecular outflow to investigate the mechanism driving active galactic nuclei (AGN) feedback. In 2021, we obtained the first long look of the target, coordinated with a simultaneous observation, with the goal of constraining the broad band continuum and the nuclear wind physical properties and energetics with an unprecedented accuracy. The new high-quality data allowed us to clearly detect at a confidence level $P>99.8$ multiple absorption features associated with the known UFO at the 9.1 and 11.0 keV rest frames. Furthermore, an emission plus absorption feature at $1.1-1.3$ keV reveals the presence of a blueshifted P-Cygni profile in the soft band. We associate the two hard band features with blends of FeXXV and FeXXVI and line pairs and infer a large column ($ $ cmsq ) of highly ionized ($log gas outflowing at $ The 1.3 keV absorption line can be associated with a blend of Fe and Ne transitions, produced by a lower column ($ $ cmsq ) and ionization ($log gas component outflowing at the same speed. Using a radiative-transfer disk wind model to fit the highly ionized UFO, we derive a mass outflow rate comparable with the mass accretion rate and the Eddington limit ($ macc and $ medd ), and kinetic energy ($ and $ and momentum flux ($ among the highest reported in the literature. We measured an extremely low high-energy cutoff ($ keV). This and several other cases in the literature suggest that a steep X-ray continuum may be related to the formation of powerful winds. We also analyzed the ionized OIII component of the large-scale outflow through optical spectroscopy and derived a large outflow velocity ($ km/s) and energetics comparable with the large-scale molecular outflows. Finally, we observe a trend of decreasing outflow velocity from forbidden optical emission lines of decreasing ionization levels, interpreted as the outflow decelerating at large distances from the ionizing source. The lack of a significant momentum boost between the nuclear UFO and the different phases of the large-scale outflow, observed in IRASF11119 and in a growing number of similar sources, can be explained by (i) a momentum-driven expansion, (ii) an inefficient coupling of the UFO with the host interstellar medium, or (iii) by repeated energy-driven expansion episodes with a low duty cycle, that average out on long timescales to produce the observed large-scale outflow.