High Excitation Emission Line Nebula associated with an Ultra Luminous X-ray Source at $z=$ 0.027 in the \textit{AKARI} North Ecliptic Pole Deep Field
High Excitation Emission Line Nebula associated with an Ultra Luminous X-ray Source at $z=$ 0.027 in the \textit{AKARI} North Ecliptic Pole Deep Field
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DOI：
10.1051/0004-6361/201730611
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发表时间：
2017-06
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通讯作者：
J. D. Tello;T. Miyaji;T. Ishigaki;M. Krumpe;Y. Ueda;H. Brunner;T. Goto;H. Hanami;Y. T. I. D. A. S. Ensenada;Universidad Nacional Autnoma de M'exico;Mexico Physics Section;Faculty of Computer Science;Engineering;Iwate University Leibniz Institut fur Astrophysik Potsda Astronomy-Iwate-University-Leibniz-Institut-fur-Astrophysik-102690840;Kyoto University Max-Planck-Institut fur extraterrestris Astronomy-Kyoto-University-Max-Planck-Institut-fur-Astronomy-102802481;Astrophysics
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作者：
J. D. Tello;T. Miyaji;T. Ishigaki;M. Krumpe;Y. Ueda;H. Brunner;T. Goto;H. Hanami;Y. T. I. D. A. S. Ensenada;Universidad Nacional Autnoma de M'exico;Mexico Physics Section;Faculty of Computer Science;Engineering;Iwate University Leibniz Institut fur Astrophysik Potsda Astronomy-Iwate-University-Leibniz-Institut-fur-Astrophysik-102690840;Kyoto University Max-Planck-Institut fur extraterrestris Astronomy-Kyoto-University-Max-Planck-Institut-fur-Astronomy-102802481;Astrophysics
目标。我们报告了在 $z=$0.027 处与超亮 X 射线源 (ULX) 相关的高激发发射线星云的发现，这是我们在 AKARI 北黄道极 (NEP) 深场的钱德拉观测中发现的。方法。我们对 ULX 斑点进行了钱德拉 X 射线和加那利大望远镜 (GTC) 光谱分析。我们通过使用线比诊断图研究发射线星云的性质，并通过光谱能量分布（SED）拟合估计其物理特性。结果。该 ULX 斑点的光谱显示了位于 [OIII]/H$\beta$-[OI]/H$\alpha$、[OIII]/H$\beta$-[SII]/H$\alpha$ 和 [OIII]/H$\beta$-[OIII]/[OII] 诊断图中恒星形成和 Seyfert 区域之间边界的发射线比率。这些与使用相同狭缝观察到的附近斑点的结果形成鲜明对比，后者占据了 HII 区域。这一结果表明，除了斑点中的恒星形成活动之外，与 ULX 相关的发射线星云的电离很大程度上还受到来自 ULX 吸积功率的能量输入的贡献，这表明 ULX 中存在吸积盘，发射 UV 辐射或施加冲击波。
Aims. We report our finding of a high excitation emission line nebula associated with an Ultra Luminous X-ray source (ULX) at $z=$ 0.027, which we found in our Chandra observation of the AKARI North Ecliptic Pole (NEP) Deep Field. Methods. We present a Chandra X-ray and Gran Telescopio Canarias (GTC) optical spectral analysis of the ULX blob. We investigate the nature of the emission line nebula by using line ratio diagnostic diagrams, and its physical properties estimated from Spectral Energy Distribution (SED) fitting. Results. The optical spectrum of this ULX blob shows emission line ratios that are located on the borderlines between star-formation and Seyfert regimes in [OIII]/H$\beta$-[OI]/H$\alpha$, [OIII]/H$\beta$-[SII]/H$\alpha$ and [OIII]/H$\beta$-[OIII]/[OII] diagnostic diagrams. These are in contrast with those of a nearby blob observed with the same slit, which occupy the HII regimes. This result suggests that the ionization of the emission line nebula associated with the ULX is significantly contributed by energy input from the accretion power of the ULX, in addition to the star formation activity in the blob, suggesting the existence of an accretion disk in the ULX emitting UV radiation, or exerting shock waves.