Kinematics of the intermediate mass black hole candidate HLX-1Report as inadecuate



 Kinematics of the intermediate mass black hole candidate HLX-1


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We studied the optical spectrum of HLX-1 during its latest outburst, using the FORS2 spectrograph on the Very Large Telescope. We detect an Halpha emission line centered at lambda = 6718.9 +- 0.9 Ang and find that its projected radial velocity with respect to the nucleus of ESO243-49 is 424 +- 27 km-s, while the maximum rotational velocity of the stars in that galaxy is ~209 km-s. 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 Halpha emission line is resolved with full width at half maximum ~400 km-s, suggesting a nebular rather than disk origin for the emission. Its luminosity L {Halpha} ~ a few 10^{37} erg-s, equivalent width ~70 Ang is also consistent with emission from a nebula photo-ionized by HLX-1.



Author: Roberto Soria; George K. T. Hau; Manfred W. Pakull

Source: https://archive.org/







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