Location and energetics of the ultra-fast outflow in PG 1448+273
  Ultra-fast outflows (UFOs) play a key role in the AGN feedback mechanism. It
is therefore important to fully characterize their location and energetics. We
study the UFO in the latest XMM-Newton archival observation of the NLSy1 galaxy
PG 1448+273 by means of a novel modeling tool, that is, the Wind in the Ionized
Nuclear Environment model (WINE). Our detection of the UFO in PG 1448+273 is
very robust. The outflowing material is highly ionized, $\log\xi =
5.53_{-0.05}^{+0.04}$ erg s$^{-1}$ cm, has a large column density,
$N_\mathrm{H} = 4.5_{-1.1}^{+0.8} \times 10^{23}$ cm$^{-2}$, is ejected with a
maximum velocity $v_0 = 0.24^{+0.08}_{-0.06}\,c$ (90% c.l. errors), and attains
an average velocity $v_\mathrm{avg} = 0.152\,c$. WINE succeeds remarkably well
to constrain a launching radius of $r_0=77_{-19}^{+31} \, r_\mathrm{S}$ from
the black hole. We also derive a lower limit on both the opening angle of the
wind ($\theta > 72^{\circ}$) and the covering factor ($C_\mathrm{f} > 0.69$).
We find a mass outflow rate $\dot{M}_\mathrm{out}=0.65^{+0.44}_{-0.33}\,M_\odot
\mathrm{yr}^{-1} = 2.0^{+1.3}_{-1.0}\, \dot{M}_\mathrm{acc}$ and a large
instantaneous outflow kinetic power $\dot{E}_\mathrm{out}=4.4^{+4.4}_{-3.6}
\times 10^{44}$ erg s$^{-1}$ = 24% $L_\mathrm{bol}$ = 18% $L_\mathrm{Edd}$ ($1
\sigma$ errors). We find that a major error contribution on the energetics is
due to $r_0$, stressing the importance of an accurate determination through a
proper spectral modeling, as done with WINE. Using 20 Swift (UVOT and XRT)
observations and the simultaneous OM data from XMM-Newton, we also find that
$\alpha_\mathrm{ox}$ undergoes large variations, with a maximum excursion of
$\Delta\alpha_\mathrm{ox} =-0.7$, after the UFO is detected, leading to a
remarkable X-ray weakness. This may point towards a starving of the inner
accretion disk due to the removal of matter through the wind.
