窄线塞弗特1星系WPVS 007中宽吸收线外流的出现
Emergence of a Broad-Absorption-Line Outflow in the Narrow-line Seyfert 1 Galaxy WPVS 007
摘要：
我们报告的结果，从2003年FUSE的观察，并重新分析1996年HST观察不寻常的X射线瞬态窄线塞弗特1星系WPVS 007。HST FOS光谱显示了最大速度约为900 km s^-1、半高宽约为550 km s^-1的小型BALs。FUSE谱显示，出现了V_max ~ 6000 km s^-1和FWHM ~ 3400 km s^-1的附加BAL外流。WPVS 007是一个低光度的天体，在它里面不会有如此高速的外流，因此它是M_V/V_max关系的一个异常值。模板光谱拟合产生了明显的离子柱，多云分析表明，PV的存在需要高电离参数log（U）>= 0和高柱密度log（N_H）>= 23，假设太阳丰度和低光度NLS 1的标称SED，α_ox=-1.28。最近的一次长时间Swift观测揭示了第一个硬X射线探测和内在（未吸收）α_ox ~-1.9$。在我们的分析中使用该SED产生了较低的柱密度约束（对于Z=1，log（N_H）>= 22.2，或者如果Z=5，log（N_H）>= 21.6）。X射线弱连续谱，结合与紫外线一致的X射线吸收，为观测到的斯威夫特X射线光谱提供了最好的解释。在任何一种情况下，紫外线数据所暗示的大柱密度和速度都可能对辐射加速造成问题。我们还指出，由于所观察到的PV吸收可以解释为较低的总柱密度使用一个固有的X射线弱光谱，我们可能会期望找到PV吸收优先更频繁（或更强）的类星体，本质上是X射线弱。
英文摘要：
We report results from a 2003 FUSE observation, and reanalysis of a 1996 HST observation of the unusual X-ray transient Narrow-line Seyfert 1 galaxy WPVS 007. The HST FOS spectrum revealed mini-BALs with V_max ~ 900 km s^-1 and FWHM ~ 550 km s^-1. The FUSE spectrum showed that an additional BAL outflow with V_max ~ 6000 km s^-1 and FWHM ~ 3400 km s^-1 had appeared. WPVS 007 is a low-luminosity object in which such a high velocity outflow is not expected; therefore, it is an outlier on the M_V/V_max relationship. Template spectral fitting yielded apparent ionic columns, and a Cloudy analysis showed that the presence of PV requires a high ionization parameter log(U) >= 0 and high column density log(N_H) >= 23 assuming solar abundances and a nominal SED for low-luminosity NLS1s with alpha_ox=-1.28. A recent long Swift observation revealed the first hard X-ray detection and an intrinsic (unabsorbed) alpha_ox ~ -1.9$. Using this SED in our analysis yielded lower column density constraints (log(N_H) >= 22.2 for Z=1, or log(N_H) >= 21.6 if Z=5). The X-ray weak continuum, combined with X-ray absorption consistent with the UV lines, provides the best explanation for the observed Swift X-ray spectrum. The large column densities and velocities implied by the UV data in any of these scenarios could be problematic for radiative acceleration. We also point out that since the observed PV absorption can be explained by lower total column densities using an intrinsically X-ray weak spectrum, we might expect to find PV absorption preferentially more often (or stronger) in quasars that are intrinsically X-ray weak.
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