SDSS J163459.82+204936.0 is a local (z?=?0.1293) infrared-luminous quasar with L IR?=?1011.91 . We present a detailed multiwavelength study of both the host galaxy and the nucleus. The host galaxy, appearing as an early-type galaxy in the optical images and spectra, demonstrates violent, obscured star formation activities with SFR?≈?140 yr?1, estimated from either the polycyclic aromatic hydrocarbon emission or IR luminosity. The optical to NIR spectra exhibit a blueshifted narrow cuspy component in Hβ, He i λλ5876, 10830, and other emission lines consistently with an offset velocity of ≈900 , as well as additional blueshifting phenomena in high-ionization lines (e.g., a blueshifted broad component of He i λ10830 and the bulk blueshifting of [O iii]λ5007), while there exist blueshifted broad absorption lines (BALs) in Na i?D and He i λλ3889, 10830, indicative of the active galactic nucleus outflows producing BALs and emission lines. Constrained mutually by the several BALs in the photoionization simulations with Cloudy, the physical properties of the absorption line outflow are derived as follows: density 104??n H 105 cm?3, ionization parameter 10?1.3 U 10?0.7 , and column density 1022.5 N H 1022.9 cm?2, which are similar to those derived for the emission line outflows. This similarity suggests a common origin. Taking advantages of both the absorption lines and outflowing emission lines, we find that the outflow gas is located at a distance of ~48–65 pc from the nucleus and that the kinetic luminosity of the outflow is 1044–1046 . J1634+2049 has a off-centered galactic ring on the scale of ~30?kpc that is proved to be formed by a recent head-on collision by a nearby galaxy for which we spectroscopically measure the redshift. Thus, this quasar is a valuable object in the transitional phase emerging out of dust enshrouding as depicted by the co-evolution scenario invoking galaxy merger (or violent interaction) and quasar feedback. Its proximity enables our further observational investigations in detail (or tests) of the co-evolution paradigm.
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机译：SDSS J163459.82 + 204936.0是局部的（z≥＝ 0.1293）红外发光类星体，L IR≥1011.91。我们提出了对宿主星系和细胞核的详细的多波长研究。宿主星系在光学图像和光谱中以早期星系的形式出现，表现出剧烈的，模糊的恒星形成活动，SFR≈≈140yr？1，由多环芳烃发射或红外发光度估算得出。光学光谱到NIR光谱在Hβ，He i λλ5876、10830和其他发射谱线中均表现出蓝移的窄尖角分量，其偏移速度始终约为≈900，并且在高电离谱线中还存在其他蓝移现象（例如，蓝移宽He iλ10830的组成部分和[O iii]λ5007的整体蓝移），而Na i？D和He iλλ3889，10830中存在蓝移的宽吸收线（BAL），指示产生BAL和发射的活跃银河核流出。线。在Cloudy光电离模拟中，受几个BAL相互约束，得出吸收线流出物的物理特性如下：密度104？<？n H 105 cm？3，电离参数10？1.3 U 10？0.7，柱密度为1022.5 NH 1022.9 cm？2，这与排放管线流出的密度相似。这种相似性暗示了一个共同的起源。利用吸收线和流出发射线两者的优势，我们发现流出气体与原子核的距离约为〜48–65 pc，流出的动力学光度为1044–1046。 J1634 + 2049有一个偏心的银河系环，范围约为30kkpc，这被证明是由附近的一个星系最近发生的正面碰撞所形成的，我们用光谱法测量了它的红移。因此，这个类星体是过渡阶段的一个有价值的对象，这是由尘埃掩盖引起的，如协同演化场景所描绘的那样，它们调用了星系合并（或剧烈的相互作用）和类星体反馈。它的接近性使我们能够进一步深入地观察研究（或测试）协同进化范例。
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