论文标题
PG 1448+273中超快速流出的位置和能量学
Location and energetics of the ultra-fast outflow in PG 1448+273
论文作者
论文摘要
超快速流出（UFO）在AGN反馈机制中起关键作用。因此，重要的是要充分表征其位置和能量学。我们通过一种新型的建模工具（即电离核环境模型（Wine）中的风）研究了NLSY1 Galaxy PG 1448+273的最新XMM-Newton档案观察中的UFO。我们在PG 1448+273中对UFO的检测非常强大。流出的材料高度离子化，$ \logξ= 5.53 _ { - 0.05}^{+0.04} $ erg s $^{ - 1} $ cm，具有较大的柱密度，$ n_ \ m atrm {h} = 4.5 _ { - 1.1}以最大速度$ v_0 = 0.24^{+0.08} _ { - 0.06} \，c $（90％c.l. errors）弹出，并达到平均速度$ v_ \ mathrm {avg} = 0.152 \ \，c $。葡萄酒的成功率非常好，以限制$ r_0 = 77 _ { - 19}^{+31} \，r_ \ mathrm {s} $的发射半径。我们还在风的开头（$θ> 72^{\ circ} $）和覆盖因子（$ c_ \ mathrm {f}> 0.69 $）上得出了下限。我们发现质量流出率$ \ dot {m} _ \ mathrm {out} = 0.65^{+0.44} _ { - 0.33} \，m_ \ odot \ odot \ odot \ mathrm {yr} \ dot {m} _ \ Mathrm {acc} $和一个大的瞬时流动动力$ \ dot {e} _ \ Mathrm {out} = 4.4^{+4.4} {+4.4} _ { - 3.6} $ L_ \ MATHRM {BOL} $ = 18％$ L_ \ MATHRM {EDD} $（$1σ$错误）。我们发现，对能量学的主要错误贡献是由于$ r_0 $引起的，这强调了通过适当的光谱建模的准确确定的重要性，就像葡萄酒所做的那样。使用20个Swift（UVOT和XRT）观察结果以及来自XMM-Newton的同时OM数据，我们还发现$α_\ Mathrm {ox} $经历了较大的变化，在UFO中最大的差异为$Δα__\ Mathrm {ox} = -0.7 $，在UFO之后，UFO被检测到了XM的差异。这可能指向由于通过风清除物质而导致内部积聚盘的饥饿。
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, $\logξ= 5.53_{-0.05}^{+0.04}$ 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 ($θ> 72^{\circ}$) 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% $L_\mathrm{Edd}$ ($1 σ$ 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 $α_\mathrm{ox}$ undergoes large variations, with a maximum excursion of $Δα_\mathrm{ox} =-0.7$, 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.
