Location and energetics of the ultra-fast outflow in PG 1448+273. (arXiv:2011.08212v2 [astro-ph.HE] UPDATED)

Location and energetics of the ultra-fast outflow in PG 1448+273. (arXiv:2011.08212v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Laurenti_M/0/1/0/all/0/1">M. Laurenti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Luminari_A/0/1/0/all/0/1">A. Luminari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tombesi_F/0/1/0/all/0/1">F. Tombesi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vagnetti_F/0/1/0/all/0/1">F. Vagnetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Middei_R/0/1/0/all/0/1">R. Middei</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piconcelli_E/0/1/0/all/0/1">E. Piconcelli</a>

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, $logxi =
5.53_{-0.05}^{+0.04}$ 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
$Deltaalpha_mathrm{ox} =-0.7$, 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.

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, $logxi =
5.53_{-0.05}^{+0.04}$ 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
$Deltaalpha_mathrm{ox} =-0.7$, 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.

http://arxiv.org/icons/sfx.gif