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

Abstract

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 $v_{\text{out}}=0.253_{-0.118}^{+0.061}$ c. The launching radius is likely at a distance of $r\ge 16$ $r_s$ 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 $L_{AGN}/c$ and ${\dot{E}}_{out}\simeq$7-27\% $L_{AGN}$, 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.

Accepted for publication in ApJ

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