GEMINI 3D spectroscopy of BAL + IR + Fe ii QSOs – I. Decoupling the BAL, QSO, starburst, NLR, supergiant bubbles and galactic wind in Mrk 231
GEMINI 3D spectroscopy of BAL + IR + Fe ii QSOs – I. Decoupling the BAL, QSO, starburst, NLR, supergiant bubbles and galactic wind in Mrk 231
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BAL + IR + Fe ii QSO 的 GEMINI 3D 光谱 – I. 对 Mrk 231 中的 BAL、QSO、星暴、NLR、超巨气泡和银河风进行解耦
DOI：
10.1111/j.1365-2966.2008.14148.x
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发表时间：
2006
影响因子：
4.8
通讯作者：
K. Jahnke
中科院分区：
文献类型：
--
作者：
S. Lípari;S. Sánchez;M. Bergmann;R. Terlevich;B. García;B. Punsly;E. Mediavilla;Y. Taniguchi;M. Ajiki;W. Zheng;J. Acosta;K. Jahnke
在本文中，我们提出的第一个研究结果的BAL类星体（在低和高红移），非常深的双子座GMOS积分场光谱的基础上。特别是，最近的BAL IR-QSO Mrk 231获得的结果。
对于Mrk 231的核区域，利用一种新的三维谱解耦技术，模拟了类星体和宿主星系的成分。从这项研究中，发现了以下主要结果：（一）在纯宿主星系光谱中，在蓝色波长处清楚地观察到极端的核星爆成分，作为流量的非常强烈的增加;（二）在宿主星系的光谱中观察到BAL系统I;（三）在干净/纯类星体发射光谱中，只检测到宽线。3D GMOS个别光谱（特别是在近红外Ca ii三重态）和地图证实了一个极端和年轻的核恒星爆发（8 <年龄<1500万年）的存在，它被发现在一个半径r= 0.3 arcsec <$200 pc的环或环中，围绕着核的核心。极端连续的蓝色成分只在核心的南部被探测到。这个区域与我们先前提出的银河风正在清理核尘埃的区域相一致。
非常深的3D光谱和地图清楚地表明，BAL系统I和II -在强“吸收线”Na iDλ5889-95和Ca ii Kλ3933中-被扩展（达到1.4-1.6角秒，距核1.2-1.3千秒差距），并在靠近射电喷流PA的位置角（PA）处明显拉长，这表明BAL系统I和II都与射电喷流有关。
利用GMOS三维谱图分析了四个膨胀核泡的物理性质。特别是，我们发现了强大的多LINER/OF发射线系统和沃尔夫-拉叶功能的主要结的更外部的超级气泡S1（r= 3.0千秒差距）。这些结的运动学-以及内部气泡-表明它们与壳S1的破裂区域（在西南部）有关。此外，在更内部的超级气泡S4中，靠近核的核心（r < 0.7 arcsec <$0.6 kpc），检测到两个类似的窄发射线系统，具有强的[S ii]和[O i]发射，ΔV −200 km s−1。这些结果表明，核NLR的一个重要组成部分是由OF过程和相关的低速电离冲击。
最后，复合BAL系统的性质和非常扩展的OF过程-50千秒差距-在Mrk 231（和类似的类星体）进行了讨论。此外，我们还提出了巨Lyα团起源的“复合超风假设”（已经为巴尔斯提出）。讨论了研究Mrk 231以及类似演化椭圆星系和类星体（即星系遗迹）终相的重要性。
In this paper we present the first results of a study of BAL QSOs (at low and high redshift), based on very deep Gemini GMOS integral field spectroscopy. In particular, the results obtained for the nearest BAL IR–QSO Mrk 231 are presented.
For the nuclear region of Mrk 231, the QSO and host galaxy components were modelled, using a new technique of decoupling 3D spectra. From this study, the following main results were found: (i) in the pure host galaxy spectrum an extreme nuclear starburst component was clearly observed, as a very strong increase in the flux, at the blue wavelengths; (ii) the BAL system I is observed in the spectrum of the host galaxy; (iii) in the clean/pure QSO emission spectrum, only broad lines were detected. 3D GMOS individual spectra (specially in the near-infrared Ca ii triplet) and maps confirm the presence of an extreme and young nuclear starburst (8 < age < 15 Myr), which was detected in a ring or toroid with a radius r= 0.3 arcsec ∼ 200 pc, around the core of the nucleus. The extreme continuum blue component was detected only to the south of the core of the nucleus. This area is coincident with the region where we previously suggested that the galactic wind is cleaning the nuclear dust.
Very deep 3D spectra and maps clearly show that the BAL systems I and II – in the strong ‘absorption lines’ Na iDλ5889–95 and Ca ii Kλ3933 – are extended (reaching ∼1.4–1.6 arcsec ∼ 1.2–1.3 kpc, from the nucleus) and clearly elongated at the position angle (PA) close to the radio jet PA, which suggest that the BAL systems I and II are ‘both’ associated with the radio jet.
The physical properties of the four expanding nuclear bubbles were analysed, using the GMOS 3D spectra and maps. In particular, we found strong multiple LINER/OF emission-line systems and Wolf–Rayet features in the main knots of the more external super bubble S1 (r= 3.0 kpc). The kinematics of these knots – and the internal bubbles – suggest that they are associated with an area of rupture of the shell S1 (at the south-west). In addition, in the more internal superbubble S4 and close to the core of the nucleus (for r < 0.7 arcsec ∼ 0.6 kpc), two similar narrow emission-line systems were detected, with strong [S ii] and [O i] emission and ΔV∼−200 km s−1. These results suggest that an important part of the nuclear NLR is generated by the OF process and the associated low-velocity ionizing shocks.
Finally, the nature of the composite BAL systems and very extended OF process – of 50 kpc – in Mrk 231 (and similar QSOs) are discussed. In addition, the ‘composite hyperwind scenario’ (already proposed for BALs) is suggested for the origin of giant Lyα blobs. The importance of study the end phases of Mrk 231, and similar evolving elliptical galaxies and QSOs (i.e. galaxy remnants) is discussed.