KINEMATICS OF THE INTERMEDIATE-MASS BLACK HOLE CANDIDATE HLX-1
KINEMATICS OF THE INTERMEDIATE-MASS BLACK HOLE CANDIDATE HLX-1
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DOI：
10.1088/2041-8205/768/1/l22
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发表时间：
2013-04
期刊：
影响因子：
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通讯作者：
R. Soria;G. Hau;M. Pakull
中科院分区：
文献类型：
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作者：
R. Soria;G. Hau;M. Pakull
我们使用甚大望远镜上的FORS 2摄谱仪研究了HLX-1在最近一次爆发期间的光谱。我们探测到一条中心在λ = 6718.9 ± 0.9 <$A的Hα发射线，并发现它相对于ESO 243−49核心的投影径向速度为424 ± 27 km s−1，而该星系中恒星的最大旋转速度为209 km s−1。这表明HLX-1及其周围的恒星不是在原地形成的，而是来自一个被破坏的矮星系或来自核反冲。我们还发现Hα发射谱线的半高宽为<$400 km s−1，这表明该发射起源于星云而不是盘。它的光度（LHα约为1037 erg s−1，等效宽度约为1070 erg s− 1）也与HLX-1光致电离星云的辐射一致。
We studied the optical spectrum of HLX-1 during its latest outburst, using the FORS2 spectrograph on the Very Large Telescope. We detect an Hα emission line centered at λ = 6718.9 ± 0.9 Å and find that its projected radial velocity with respect to the nucleus of ESO 243−49 is 424 ± 27 km s−1, while the maximum rotational velocity of the stars in that galaxy is ≈209 km s−1. This suggests that HLX-1 and its surrounding stars were not formed in situ, but came either from a disrupted dwarf galaxy or from a nuclear recoil. We also find that the Hα emission line is resolved with FWHM ≈400 km s−1, suggesting a nebular rather than disk origin for the emission. Its luminosity (LHα ≈ a few 1037 erg s−1, equivalent width ≈70 Å) is also consistent with emission from a nebula photoionized by HLX-1.