论文标题
类星体SDSS J163345.22+512748.4中的宽发射和吸收线流出
Broad Emission and Absorption Line Outflows in the Quasar SDSS J163345.22+512748.4
论文作者
论文摘要
我们介绍了类星体SDSS J163345.22+512748.4的光学和NIR发射和吸收线光谱的详细研究。我们在新获得的NIR光谱上发现了高度元稳定的中性中性氦宽吸收线（BAL）\ Heiozetz \，其宽度为$ \ sim $ 2000 \ kmps \，在Velocity空间中的$ \ sim $ \ sim $ 7000 \ kmps \ blueshift。在\ mgii \和\ heiteen中也可以显着检测到BAL系统。我们估计$（5.0 \ pm 1.7）\ times 10^{14} $ cm $^{ - 2} $的times*（2〜 $^3 $ s）水平，并推断出$ u_ {a} = 10^{-1.9 \ pm 0.2} $的电离参数，以适用于bal fort Forth a Bal fort Fulte for A Bal fort Fulf Fulf Fulf Fulf Futf for A forth Fulf Fulf Fulf Fulf Fulf Fulf Fulf Flow。 BAL流出的总列密度在范围内约束N $ \ rm _ {h} $ $ \ sim $ 10 $^{21} $ -10 $^{21.4} $ cm $^{ - 2} $。我们还发现，MGII和UV FEII的大部分以及H $α$宽发射线（BELS）都以$ \ sim $ 2200 \ kmps \相对于类星体的系统性红色速度而蓝光。我们认为Blueshifted Bel区域具有覆盖因子$ C_ {F} \大约16 \％$，一个密度N $ \ rm _ {H} $ $ \ sim $ \ sim $ \ sim $ 10 $^{10.6} $ -10 $^{11.3} $ CM $^{ - 3} $ cm $^{ - 3} $ 10^{23} $ cm $^{ - 2} $和电离参数$ u_ {e} \ sim 10^{ - 2.1} -10^{ - 1.5} $。流出气体位于$ \ sim $ 0.1 PC距中央电离源，比例可与BLR相当。如果BALS观察到的，则提出了一个玩具动力学模型，以便以径向速度为径向速度，并以径向速度的流出轴对称几何形状来重现MGII BEL的曲线。
We present a detailed study of the optical and NIR emission and absorption line spectrum of the quasar SDSS J163345.22+512748.4. We discovered on the newly acquired NIR spectrum a highly meta-stable neutral helium broad absorption line (BAL) \heiozetz\ with a width of $\sim$ 2000 \kmps\ and a blueshift of $\sim$ 7000 \kmps\ in the velocity space. The BAL system is also significantly detected in \mgii\ and \heiteen. We estimate a column density of $(5.0 \pm 1.7) \times 10^{14}$ cm$^{-2}$ for the HeI*(2~$^3$S) level, and infer an ionization parameter of $U_{A} = 10^{-1.9\pm 0.2}$ for the BAL outflow assuming that the BAL region is thick enough for a full development of an ionization front. The total column density of the BAL outflow is constrained in the range N$\rm _{H}$ $\sim$ 10$^{21}$-10$^{21.4}$ cm$^{-2}$. We also found that the bulk of both MgII and UV FeII, as well as H$α$ broad emission lines (BELs) are blueshifted with a velocity of $\sim$ 2200 \kmps\ with respect to the quasar systemic redshift. We constrain that the blueshifted BEL region has a covering factor $C_{f}\approx 16\%$, a density n$\rm _{H}$ $\sim $ 10$^{10.6}$-10$^{11.3}$ cm$^{-3}$, a column density N$\rm _{H}\gtrsim 10^{23}$ cm$^{-2}$, and an ionization parameter $U_{E}\sim 10^{-2.1}-10^{-1.5}$. The outflow gas is located at $\sim$0.1 pc away from the central ionization source, at a scale comparable to the BLR. A toy kinetic model has been proposed to reproduce the profile of MgII BEL well if assuming a partial obscured axisymmetric geometry of the outflow with a radial velocity as observed by the BALs.
