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dc.contributor.authorSoria, Roberto
dc.contributor.authorHau, G.
dc.contributor.authorPakull, M.
dc.identifier.citationSoria, Roberto and Hau, George K.T. and Pakull, Manfred W. 2013. Kinematics of the intermediate-mass black hole candidate HLX-1. The Astrophysical Journal Letters. 768 (1): pp. 1-5.

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 (L Hα = a few 1037 erg s–1, equivalent width = 70 Å) is also consistent with emission from a nebula photoionized by HLX-1.

dc.publisherInstitute of Physics Publishing
dc.subjectindividual (Abell 2877)
dc.subjectgalaxies: clusters
dc.subjectgalaxies: individual (ESO 243–49)
dc.subjectaccretion disks
dc.subjectblack hole physics
dc.titleKinematics of the intermediate-mass black hole candidate HLX-1
dc.typeJournal Article
dcterms.source.titleAstrophysical Journal Letters

Copyright © 2013 The American Astronomical Society

curtin.accessStatusOpen access

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