Bubble in the Whale: Identifying the Optical Counterparts and Extended Nebula for the Ultraluminous X-Ray Sources in NGC 4631

被引:2
作者
Guo, Jing [1 ]
Wu, Jianfeng [1 ]
Feng, Hua [2 ,3 ]
Cai, Zheng [2 ]
Zhou, Ping [4 ,5 ]
Zhou, Changxing [3 ]
Zhang, Shiwu [2 ]
Wang, Junfeng [1 ]
Sun, Mouyuan [1 ]
Gu, Wei-Min [1 ]
Weng, Shan-Shan [6 ,7 ]
Liu, Jifeng [8 ,9 ,10 ]
机构
[1] Xiamen Univ, Dept Astron, Xiamen 361005, Fujian, Peoples R China
[2] Tsinghua Univ, Dept Astron, Beijing 100084, Peoples R China
[3] Tsinghua Univ, Dept Engn Phys, Beijing 100084, Peoples R China
[4] Nanjing Univ, Sch Astron & Space Sci, 163 Xianlin Ave, Nanjing 210023, Peoples R China
[5] Nanjing Univ, Key Lab Modern Astron & Astrophys, Minist Educ, Nanjing 210023, Peoples R China
[6] Nanjing Normal Univ, Dept Phys, Nanjing 210023, Peoples R China
[7] Nanjing Normal Univ, Inst Theoret Phys, Nanjing 210023, Peoples R China
[8] Chinese Acad Sci, Key Lab Opt Astron, Natl Astron Observ, Beijing 100101, Peoples R China
[9] Univ Chinese Acad Sci, Sch Astron & Space Sci, Beijing 100049, Peoples R China
[10] Wuhan Univ, WHU NAOC Joint Ctr Astron, Wuhan 430072, Hubei, Peoples R China
基金
中国国家自然科学基金;
关键词
HOLMBERG IX X-1; MASS BLACK-HOLE; XMM-NEWTON; COHERENT PULSATIONS; SOLAR MASSES; ACCRETION; STELLAR; PULSAR; DISCOVERY; GALAXIES;
D O I
10.3847/1538-4357/acaddd
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present a deep optical imaging campaign on the starburst galaxy NGC 4631 with CFHT/MegaCam. By supplementing the HST/ACS and Chandra/ACIS archival data, we search for the optical counterpart candidates of the five brightest X-ray sources in this galaxy, four of which are identified as ultraluminous X-ray sources (ULXs). The stellar environments of the X-ray sources are analyzed using the extinction-corrected color-magnitude diagrams and the isochrone models. We discover a highly asymmetric bubble nebula around X4 that exhibits different morphology in the H alpha and [O iii] images. The [O iii]/H alpha ratio map shows that the H alpha-bright bubble may be formed mainly via the shock ionization by the one-sided jet/outflow, while the more compact [O iii] structure is photoionized by the ULX. We constrain the bubble expansion velocity and interstellar medium density with the MAPPINGS V code and hence estimate the mechanical power injected into the bubble as P (w) similar to 5 x 10(40) erg s(-1) and the corresponding bubble age as similar to 7 x 10(5) yr. Relativistic jets are needed to provide such a level of mechanical power with a mass-loss rate of similar to 10(-7) M (circle dot) yr(-1). Besides the accretion, the black hole spin is likely an additional energy source for the super-Eddington jet power.
引用
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页数:13
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