首款HeI *λ10830 BALQSO
The First HeI*λ10830 BALQSO
摘要：
报道了第一个HeI λ10830宽吸收线类星体FBQS J1151+3822的发现。使用新的红外光谱和光学光谱，以及SDSS光谱，我们提取的表观光学深度剖面作为3889 A和10830 A HeI* 吸收线的速度的函数。由于这些线具有相同的较低水平，因此可以使用非均匀吸收模型提取平均真实HeI* 柱密度;该数字的对数为14.9。使用Cloudy模型获得总氢柱密度。允许一系列电离参数和密度，电离参数的下限log U=-1.4由有足够HeI* 的要求确定，密度的上限log n=8由缺乏Balmer吸收确定。模拟紫外光谱表明，原则上可以使用低电离线和高电离线（如Mg II和PV）的组合进一步限制电离参数，但预测可观察到且未显著混合的唯一密度敏感线是CIIIλ1176。我们估算了流出率和动能，发现它们是一致的，但与其他物体的分析相比偏高。假设辐射线驱动是加速机制，建立了力倍增器模型。使用模型结果的动力学参数强烈约束密度为log n >= ~7。因此，氢柱密度的对数被限制在21.7 ~ 22.9之间，质量流出率被限制在11 ~ 56个太阳质量/年之间，质量流出率与吸积率之比被限制在1.2 ~ 5.8之间，动能被限制在1 ~ 5 x 10^44 erg/s之间。我们讨论了使用HeI* 来检测高柱密度BALQSO和测量它们的属性的优点。（节录）
英文摘要：
We report the discovery of the first HeI*λ10830 broad absorption line quasar FBQS J1151+3822. Using new infrared and optical spectra, as well as the SDSS spectrum, we extracted the apparent optical depth profiles as a function of velocity of the 3889A and 10830A HeI* absorption lines. Since these lines have the same lower levels, inhomogeneous absorption models could be used to extract the average true HeI* column density; the log of that number was 14.9. The total hydrogen column density was obtained using Cloudy models. A range of ionization parameters and densities were allowed, with the lower limit on the ionization parameter of log U=-1.4 determined by the requirement that there be sufficient HeI*, and the upper limit on the density of log n=8 determined by the lack of Balmer absorption. Simulated UV spectra showed that the ionization parameter could be further constrained in principle using a combination of low and high ionization lines (such as MgII and PV), but the only density-sensitive line predicted to be observable and not significantly blended was CIIIλ1176. We estimated the outflow rate and kinetic energy, finding them to be consistent but on the high side compared with analysis of other objects. Assuming that radiative line driving is the responsible acceleration mechanism, a force multipler model was constructed. A dynamical argument using the model results strongly constrained the density to be log n >= ~7. Consequently, the log hydrogen column density is constrained to be between 21.7 and 22.9, the mass outflow rate to be between 11 and 56 solar masses per year, the ratio of the mass outflow rate to the accretion rate to be between 1.2 and 5.8, and the kinetic energy to be between 1 and 5 x 10^44 erg/s. We discuss the advantages of using HeI* to detect high-column-density BALQSOs and and measure their properties. (Abridged)
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