Understanding the Nature of an Unusual Post-starburst Quasar with Exceptionally Strong Ne v Emission
Understanding the Nature of an Unusual Post-starburst Quasar with Exceptionally Strong Ne v Emission
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DOI：
10.3847/1538-4357/ac5c2c
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发表时间：
2022-03
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通讯作者：
Cameren N. Swiggum;C. Tremonti;S. Perrotta;A. Schaefer;R. Hickox;A. Coil;P. Sell;A. Diamond-Stanic;Jalyn N. Krause;G. Mosby
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作者：
Cameren N. Swiggum;C. Tremonti;S. Perrotta;A. Schaefer;R. Hickox;A. Coil;P. Sell;A. Diamond-Stanic;Jalyn N. Krause;G. Mosby
我们提出了一个z = 0.94的类星体，SDSS J004846.45-004611.9，发现于斯隆数字巡天III（SDSS-III）BOSS调查。对该光谱的视觉分析显示出高度加宽和蓝移的窄发射线，特别是[Ne v] λ3426和[O iii] λ5007，流出速度为4000 km s−1，沿着具有异常大的[Ne v] λ3426/[Ne iii] λ3869比值。气体在更高的流出速度下表现出更高的电离，这表明强大的流出和高电离线的不寻常强度之间存在联系。源的光谱能量分布和i-W3颜色显示它很可能是一个核心极红类星体（ERQ）;一个年轻的活动星系核（AGN）的候选群体，正在猛烈地从它们的中心喷出气体和尘埃。宿主星系光在其光谱中的主导地位及其在SDSS S82区域的偶然位置使我们能够测量其星星形成历史，并首次在ERQ中调查变化。我们的分析表明，SDSS J004846.45-004611.9在4亿年前经历了一个短暂的星爆阶段，随后被淬灭，这可能表明星星形成淬灭和活动星系核活动开始之间存在时滞。我们还发现，强烈的灭绝可以独特地归因于活动星系核，并不坚持在宿主星系，矛盾的情况下，源最近已经从一个尘埃亚毫米星系过渡。在我们相对较浅的光度数据中，在静止坐标系中，源在0.24-2.4 μm处似乎没有变化，很可能是由于宿主星系星光在这些波长处的主要贡献。
We present a z = 0.94 quasar, SDSS J004846.45-004611.9, discovered in the Sloan Digital Sky Survey III (SDSS-III) BOSS survey. A visual analysis of this spectrum reveals highly broadened and blueshifted narrow emission lines, in particular, [Ne v] λ3426 and [O iii] λ5007, with outflow velocities of 4000 km s−1, along with unusually large [Ne v] λ3426/[Ne iii] λ3869 ratios. The gas shows higher ionization at higher outflow velocities, indicating a connection between the powerful outflow and the unusual strength of the high ionization lines. The spectral energy distribution and the i − W3 color of the source reveal that it is likely a core extremely red quasar (ERQ); a candidate population of young active galactic nuclei (AGN) that are violently blowing out gas and dust from their centers. The dominance of host galaxy light in its spectrum and its fortuitous position in the SDSS S82 region allows us to measure its star formation history and investigate variability for the first time in an ERQ. Our analysis indicates that SDSS J004846.45-004611.9 underwent a short-lived starburst phase 400 Myr ago and was subsequently quenched, possibly indicating a time lag between star formation quenching and the onset of AGN activity. We also find that the strong extinction can be uniquely attributed to the AGN and does not persist in the host galaxy, contradicting a scenario where the source has recently transitioned from being a dusty submillimeter galaxy. In our relatively shallow photometric data, the source does not appear to be variable at 0.24–2.4 μm in the rest frame, most likely due to the dominant contribution of host galaxy starlight at these wavelengths.