We report on the discovery of unusual broad absorption lines (BALs) in the bright quasar SDSS J075133.35+134548.3 at z ∼ 1, using archival and newly obtained optical and NIR spectroscopic data. The BALs are detected reliably in He i* λ3889, He i* λ10830 and tentatively in Al iii, Mg ii. These BALs show complex velocity structures consisting of two major components: a high-velocity component (HV), with a blueshifted velocity range of Δv _HV ∼ −9300 − −3500 km s⁻¹, which can be reliably detected in He i* λ10830, and tentatively in Al iii and Mg ii, whereas it is undetectable in He i* λ3889 and a low-velocity component (LV), with Δ v _LV ∼ −3500 − −1800 km s⁻¹, is only detected in He i* and He i* λ10830. With the BALs from different ions, the HV outflowing gas can be constrained to have a density of n _H ∼10^10.3–10^11.4 cm⁻³, a column density of N _H ∼ 10²¹ cm⁻² and an ionization parameter of U ∼10^−1.83–10^−1.72; inferring a distance of R _HV∼0.5 pc from the central continuum source with a monochromatic luminosity λ L_λ (5100) = 7.010⁴⁵ erg s⁻¹ at 5100 . This distance is remarkably similar to that of the normal broad line region (BLR) estimated from reverberation experiments, suggesting association of the BLR and the HV BAL outflowing gas. Interestingly, a blueshifted component is also detected in Al iii and Mg ii broad emission lines (BELs), and the Al iii/Mg ii of such a BEL component can be reproduced by the physical parameters inferred from the HV BAL gas. The LV BAL gas likely has a larger column density, a higher ionization level and hence a smaller distance than the HV BAL gas. Further spectroscopy with a high S/N ratio and broader wavelength coverage is needed to confirm this to shed new light on the possible connection between BALs and BELs.

我们使用档案和新获得的光学和近红外光谱数据报告了在z ∼ 1处明亮的类星体 SDSS J075133.35+134548.3 中发现不寻常的宽吸收线 (BAL) 。在 He i * λ 3889、He i * λ 10830中可靠地检测到 BAL ，并在 Al iii、Mg ii中暂时检测到 BAL 。这些 BAL 显示了由两个主要分量组成的复杂速度结构：高速分量 (HV)，蓝移速度范围为 Δ v _HV ∼ -9300 - -3500 km s ^-1，可以在 He i *中可靠地检测到λ 10830，暂定为 Aliii和 Mg ii，而在 He i * λ 3889 和低速分量 (LV) 中无法检测到，Δ v _LV ∼ -3500 - -1800 km s ^-1仅在 He i * 和 He i中检测到* λ 10830. 使用不同离子的 BAL，可以将 HV 流出气体的密度限制为n _H ∼10 ^10.3 –10 ^11.4 cm ^-3，柱密度N _H ∼ 10 ²¹ cm ^-2和电离U ∼10的参数^-1.83 –10 ^-1.72；推断距离中心连续谱源R _HV ∼0.5 pc 的距离，在 5100 处具有单色光度λ L _λ (5100) = 7.010 ⁴⁵ erg s ^-1。这个距离与从混响实验估计的正常宽线区域 (BLR) 非常相似，表明 BLR 和 HV BAL 流出气体的关联。有趣的是，在 Al iii和 Mg ii宽发射线 (BEL) 和 Al iii /Mg ii中也检测到了蓝移成分可以通过从 HV BAL 气体推断出的物理参数来再现这种 BEL 分量。与 HV BAL 气体相比，LV BAL 气体可能具有更大的柱密度、更高的电离水平并因此具有更小的距离。需要具有高信噪比和更宽波长覆盖范围的进一步光谱来证实这一点，以揭示 BAL 和 BEL 之间可能的联系。