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    Kinematics of the intermediate-mass black hole candidate HLX-1

    193282_97473_Astro_Journal-2041-8205_768_1_L22_1_-Soria.pdf (444.1Kb)
    Access Status
    Open access
    Authors
    Soria, Roberto
    Hau, G.
    Pakull, M.
    Date
    2013
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Soria, 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.
    Source Title
    Astrophysical Journal Letters
    DOI
    10.1088/2041-8205/768/1/L22
    ISSN
    2041-8205
    Remarks

    Copyright © 2013 The American Astronomical Society

    URI
    http://hdl.handle.net/20.500.11937/19722
    Collection
    • Curtin Research Publications
    Abstract

    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.

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