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首页> 外文期刊>The Astrophysical journal >THE ULTRAVIOLET SPECTRUM OF THE GRAVITATIONAL LENS CANDIDATE UM 425 = QSO 1120 + 019: EVIDENCE FOR BROAD ABSORPTION LINE (BAL) STRUCTURE
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THE ULTRAVIOLET SPECTRUM OF THE GRAVITATIONAL LENS CANDIDATE UM 425 = QSO 1120 + 019: EVIDENCE FOR BROAD ABSORPTION LINE (BAL) STRUCTURE

机译：候选重力透镜的紫外光谱UM 425 = QSO 1120 + 019：宽带吸收线（BAL）结构的证据

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摘要

The UV line profile structure of high-ionization resonance lines found with the International Ultraviolet Explorer (WE) in the brightest of four multiply imaged sources (image-A) in the candidate gravitational lens UM 425 = QSO 1120+019 indicates broad absorption line (BAL) structure. The deep-broad trough associated with the O Ⅵ line extends to velocities ～ -12,000 km s~(-1), and contains discrete features that suggest multicomponent velocity structure. This structure may include contributions from C Ⅳ absorption from the early-type galaxy that is believed to lens UM 425. A strong absorption feature in the blue wing of the Lyman-α λ1216 emission line may be a Lyman-α absorption system at a z_(Lyα) = 1.437 ± 0.003, or it may be formed by the superposition of the broad N v λλ1238, 1242 absorption trough on the extended blue emission wing of the QSO Lyman-α line. We obtained a redshift of z_(Qso) = 1.471 ± 0.003 from Lyman-α λ1215, consistent with the redshift found by Meylan and Djorgovski in the optical. The Lyman-α line appears unusually weak due to the presence of N v λ1240 BAL absorption. A Lyman-limit absorption system at λ912 was not observed in the QSO rest frame. The detection of BAL structure in the other weaker ground-state resonance lines of N Ⅱ (1) and S Ⅳ (1) was not found, suggesting these lines are formed in a region that is distinct from the BAL component. Detection of BAL structure in the other fainter images in this system with HST instrumentation, similar to structure observed here in image A, could provide evidence that UM 425 is a gravitational lens.
机译：在候选重力透镜UM 425 = QSO 1120 + 019的四个多重成像源（image-A）中最亮的情况下，使用国际紫外线探测器（WE）发现的高电离共振线的UV线轮廓结构表示宽吸收线（ BAL）结构。与OⅥ线有关的深槽延伸到速度〜-12,000 km s〜（-1），并具有表明多分量速度结构的离散特征。这种结构可能包括来自早期类型星系的CⅣ吸收的贡献，该星系被认为是对UM 425透镜的影响。Lyman-αλ1216发射线的蓝翼中的强大吸收特征可能是z_处的Lyman-α吸收系统。 （Lyα）= 1.437±0.003，或者它可以由宽阔的N v λλ1238、1242吸收槽叠加在QSOLyman-α谱线的扩展蓝色发射翼上形成。我们从Lyman-αλ1215获得了z_（Qso）= 1.471±0.003的红移，与Meylan和Djorgovski在光学中发现的红移一致。由于存在N vλ1240BAL吸收，Lyman-α谱线显得异常弱。在QSO静止框架中未观察到λ912的莱曼极限吸收系统。在NⅡ（1）和SⅣ（1）的其他较弱的基态共振线中未发现BAL结构，表明这些线形成在与BAL成分不同的区域。使用HST仪器对该系统中其他较暗的图像中的BAL结构进行检测，类似于图像A中观察到的结构，可以提供UM 425是重力透镜的证据。

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