NuSTAR view of the black hole wind in the galaxy merger IRAS F11119$+$3257

Galactic winds driven by active galactic nuclei (AGN) have been invoked to play a fundamental role in the co-evolution between supermassive black holes and their host galaxies. Finding observational evidence of such feedback mechanisms is of crucial importance and it requires a multi-wavelength approach in order to compare winds at different scales and phases. In Tombesi et al. (2015) we reported the detection of a powerful ultra-fast outflow (UFO) in the Suzaku X-ray spectrum of the ultra-luminous infrared galaxy IRAS F11119$+$3257. The comparison with a galaxy-scale OH molecular outflow observed with Herschel in the same source supported the energy-conserving scenario for AGN feedback. The main objective of this work is to perform an independent check of the Suzaku results using the higher sensitivity and wider X-ray continuum coverage of NuSTAR. We clearly detect a highly ionized Fe K UFO in the 100ks NuSTAR spectrum with parameters $N_H=(3.2\pm 1.5)\times {10}^{24}$ cm${}^{-2}$, log$\xi$$=$$4.0_{-0.3}^{+1.2}$ erg s${}^{-1}$ cm, and $v_{$\text{out}$} = 0.253^{+0.061}{-0.118}$c\mathrm{.}Thelaunchingradiusislikelyatadistanceof$r \ge 16$ $r_s$ from the black hole. The mass outflow rate is in the range ${\dot{M}}_{out}$$\simeq$0.5-2 $M_{\odot }$ yr${}^{-1}$. The UFO momentum rate and power are ${\dot{P}}_{out}\simeq$0.5-2 $L_{AGN}\mathrm{/}c$ and $\dot{E}{out} \simeq$7-27\mathrm{\%}$L_{AGN}$, respectively. The UFO parameters are consistent between the 2013 Suzaku and the 2015 NuSTAR observations. Only the column density is found to be variable, possibly suggesting a clumpy wind. The comparison with the energetics of molecular outflows estimated in infrared and millimeter wavelengths support a connection between the nuclear and galaxy-scale winds in luminous AGN.