IRAS 13349+2438的电离吸收体和核环境：来自协调的Chandra HETGS、HST STIS、HET和Spitzer IRS的多波长见解
The Ionized Absorber and Nuclear Environment of IRAS 13349+2438: Multi-wavelength insights from coordinated Chandra HETGS, HST STIS, HET, and Spitzer IRS
摘要：
我们提出的结果，从协调IR到X射线光谱活动的类星体IRAS 13349+2438。光谱显示极端的本征矢量-1特性，但H-β线宽反对NLS 1分类;我们根据[O III]改进z=0.10853。我们使用两种独立的方法（H-β线宽和SED拟合）估计BH质量=10^9 Msun。蓝移吸收（-950km/s和-75km/s）首次出现在Ly-alpha，NV和CIV的STIS紫外光谱中。较高速度的紫外线与较低电离度（xi~1.6）的X射线暖吸收线重合。需要一个蓝移700- 900 km/s的尘埃多重电离吸收体来拟合X射线数据。比较不同电离SED的理论模型揭示了包含UV的（即，吸积盘）电离连续体强烈影响热吸收体的热力学稳定性的结论。具体到IRAS 13349，一个X射线-紫外电离SED有利于连续分布的电离状态在一个光滑的流动（本文），而不是离散的云在压力平衡（工作的其他人，其中紫外线被省略）。直接灰尘检测可见于IR：PAH发射（7.7和11.3）微米，其也可能与镁橄榄石混合，和（10和18）微米硅酸盐发射，以及X射线：铁粉，其中灰尘与气体的比率> 90%。我们发展了一个几何模型，通过一个模糊的环面的高层大气中看到的类星体核区。这条视线被灰尘遮挡，阻挡了紫外线/光发射区域的直接视野，但由于气体被电离，因此在X射线中基本上是透明的。在我们的模型中，20%的固有UV/光学连续谱被散射到我们的视线中的模糊环面的远壁。另外2.4%的直射光，可能占紫外线发射的主导地位，被另一个高度电离气体的离面成分散射到我们的视线中。
英文摘要：
We present results from a coordinated IR-to-X-ray spectral campaign of the QSO IRAS 13349+2438. Optical spectra reveal extreme Eigenvector-1 characteristics, but the H-beta line width argues against a NLS1 classification; we refine z=0.10853 based on [O III]. We estimate a BH mass=10^9 Msun using 2 independent methods (H-beta line width & SED fits). Blue-shifted absorption (-950km/s & -75km/s) is seen for the 1st time in STIS UV spectra from Ly-alpha, NV, & CIV. The higher velocity UV lines are coincident with the lower-ionisation (xi~1.6) X-ray warm absorber lines. A dusty multiple ionization absorber blueshifted by 700-900km/s is required to fit the X-ray data. Theoretical models comparing different ionising SEDs reveal that a UV-inclusive (i.e., the accretion disc) ionising continuum strongly impacts conclusions for the thermodynamic stability of the warm absorber. Specific to IRAS13349, an Xray-UV ionising SED favors a continuous distribution of ionisation states in a smooth flow (this paper), versus discrete clouds in pressure equilibrium (work by others where UV is omitted). Direct dust detections are seen in both the IR: PAH emission at (7.7 & 11.3)micron which may also be blended with forsterite, and (10 & 18)micron silicate emission, and X-rays: iron dust with a dust-to-gas ratio > 90%. We develop a geometrical model whereby the QSO nuclear region is viewed through the upper atmosphere of an obscuring torus. This sight line is obscured by dust that blocks a direct view of the UV/optical emission region but is largely transparent in X-rays since the gas is ionised. In our model, 20% of the intrinsic UV/optical continuum is scattered into our sight line by the far wall of an obscuring torus. An additional 2.4% of the direct light, which likely dominates the UV emission, is Thomson-scattered into our line-of-sight by another off-plane component of highly ionized gas.
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