The typical value of the mass outflow rate for sources accreting below or close to the Eddington limit is $\dot{M}_{\rm out} \gtrsim 5\!-\!10{{\ \rm per\ cent}} \,\dot{M}_{\rm acc}$, for both UFOs and non-UFOs (Tombesi et al. 2012). In this scenario, even for the UFOs with the lowest allowed velocity, the mechanical power is enough to exercise a significant feedback impact on the surrounding environment. Looking at the comparison between mass accretion rate and mass outflow rate for our source (see Table 3), the upper limit on the mass outflow rate for Wind 1 is extremely high, but the values for Wind 2 and Wind 3 are still comparable with the values of quasars and Seyfert galaxies (Tombesi et al. 2012). If we consider the lower limits instead, their values are well below the average. Theoretical works (Di Matteo, Springel & Hernquist 2005; King 2010; Ostriker et al. 2010; Debuhr, Quataert & Ma 2011) showed that, in order to have a significant feedback impact in the environment surrounding an AGN, it is required a minimum ratio between the mechanical power of the outflow and the bolometric luminosity of ${\sim}0.5{{\ \rm per\ cent}}$. Tombesi et al. (2012) showed that actually the lower limit of this value for UFOs is ${\sim}0.3{{\ \rm per\ cent}}$ and for non-UFOs is ${\sim}0.02 \!-\! 0.8{{\ \rm per\ cent}}$. According to what found for the ratio between the mass outflow rate and the mass accretion rate, looking at the upper limits on $\dot{K}/L_{\rm b,out}$ of our source, i.e. multiphase and multiscale X-ray winds, IRAS 04416+1215 fits well in this scenario in which the outflowing winds can impress a feedback. Indeed, the upper limits on $\dot{K}/L_{\rm b,out}$ is comparable with the kinetic coupling efficiency, defined as the ratio of the kinetic luminosity of outflows to the AGN radiative luminosity (Eout/Lrad), calculated with the feedback model for hyper-Eddington accretion by Takeo, Inayoshi & Mineshige (2020), using the outflow velocities and the $\dot{M}/\dot{M}_{\rm acc}$ values of IRAS 04416+1215. Instead, the lower limits are below the minimum value required to generate at least a weak feedback. Considering only the values derived from the lower limits on the distance, i.e. the situation in which the X-ray winds are cospatial, we would be in a scenario in which the source loses much luminosity due to advection inside the disc, resulting in a much lower efficiency for wind production as most of the radiation remains trapped inside the disc. This deduction is supported also by the results of the lower limits on the ratio between the momentum rate of the outflows and the momentum of the radiation. Outflows accelerated through the continuum radiation pressure are expected to have a $\dot{p}_{\rm out}/\dot{p}_{\rm rad}\sim 1$ (King & Pounds 2015). The median value of this ratio for UFOs is ∼0.96 after the relativistic correction and ∼0.64 without the relativistic corrections (Luminari et al. 2020). The values we found for the lower limits on $\dot{p}_{\rm out}/\dot{p}_{\rm rad}$ of IRAS 04416+1215 are again well below the median. Thus, the outcoming luminosity of the source is not enough to accelerate the material to the escape velocity, which is required for a wind to leave the system, suggesting that likely in the scenario of the cospatial winds the outflows observed in IRAS 04416+1215 could be accelerated by other mechanisms such as magnetohydrodynamic processes.
Citation: Di Matteo, Springel & Hernquist 2005
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