The Physical Properties of Low-redshift FeLoBAL Quasars. III. The Location and Geometry of the Outflows
The Physical Properties of Low-redshift FeLoBAL Quasars. III. The Location and Geometry of the Outflows
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DOI：
10.3847/1538-4357/ac854c
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发表时间：
2022-08
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影响因子：
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通讯作者：
Hyunseop 현섭 Choi 최;K. Leighly;C. Dabbieri;D. Terndrup;S. Gallagher;G. Richards
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作者：
Hyunseop 현섭 Choi 최;K. Leighly;C. Dabbieri;D. Terndrup;S. Gallagher;G. Richards
我们提出了一个低红移铁低电离宽吸收线类星体（FeLoBALQs）的样本的继续分析。Choi等人介绍了对50个天体的宽吸收线（BAL）流出的SimBAL光谱分析。Leighly等人分析了这50个天体中的30个天体的光学发射谱线，发现它们要么具有高吸积率（L Bol/L Edd > 0.3），要么具有低吸积率（0.03 < L Bol/L Edd < 0.3）。我们报告说，外流速度是负相关的BAL位置之间的高吸积率的对象，在秒差距尺度的外流观察到的最高速度。相比之下，低爱丁顿比率的对象显示出相反的趋势。我们证实了已知的流出速度和L Bol/L Edd之间的关系，并发现散射可能起源于低（高）吸积率物体的力乘数（发射半径）。在大多数流出物中发现对数体积填充因子在-6和-4之间，但对于低速致密流出物高达-1。我们调查了观测到的[O III]排放量和预测的BAL气体之间的关系。我们发现，如果发射线覆盖分数取决于塞弗特类型和BAL位置，这些可以调和。预测和观察到的[O III]光度之间的差异与流出速度，这表明[O III]发射在高爱丁顿比对象可能是广泛的，隐藏在Fe II的排放。我们认为，流出的物理性质的差异作为类星体和吸积率的位置的函数指向不同的形成，加速和约束机制的两个FeLoBALQ类型。
We present continued analysis of a sample of low-redshift iron low-ionization broad-absorption-line quasars (FeLoBALQs). Choi et al. presented SimBAL spectral analysis of broad-absorption-line (BAL) outflows in 50 objects. Leighly et al. analyzed the optical emission lines of 30 of those 50 objects and found that they are characterized by either a high accretion rate (L Bol/L Edd > 0.3) or low accretion rate (0.03 < L Bol/L Edd < 0.3). We report that the outflow velocity is inversely correlated with the BAL location among the high-accretion-rate objects, with the highest velocities observed in parsec-scale outflows. In contrast, the low-Eddington-ratio objects showed the opposite trend. We confirmed the known relationship between the outflow velocity and L Bol/L Edd and found that the scatter plausibly originates in the force multiplier (launch radius) in the low(high)-accretion-rate objects. A log volume filling factor between −6 and −4 was found in most outflows but was as high as −1 for low-velocity compact outflows. We investigated the relationship between the observed [O iii] emission and that predicted from the BAL gas. We found that these could be reconciled if the emission-line covering fraction depends on the Seyfert type and BAL location. The difference between the predicted and observed [O iii] luminosity is correlated with the outflow velocity, suggesting that [O iii] emission in high-Eddington-ratio objects may be broad and hidden under Fe ii emission. We suggest that the physical differences in the outflow properties as a function of location in the quasar and accretion rate point to different formation, acceleration, and confinement mechanisms for the two FeLoBALQ types.