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    The slim-disk state of the ultraluminous X-ray source in M83

    238108_238108.pdf (521.3Kb)
    Access Status
    Open access
    Authors
    Soria, Roberto
    Kuntz, K.
    Long, K.
    Blair, W.
    Plucinsky, P.
    Winkler, P.
    Date
    2015
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Soria, R. and Kuntz, K. and Long, K. and Blair, W. and Plucinsky, P. and Winkler, P. 2015. The slim-disk state of the ultraluminous X-ray source in M83. Astrophysical Journal. 799 (2).
    Source Title
    Astrophysical Journal
    DOI
    10.1088/0004-637X/799/2/140
    ISSN
    0004-637X
    School
    Department of Physics and Astronomy
    Remarks

    This is an author-created, un-copy edited version of an article accepted for publication in Astrophysical Journal. The publisher is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at http://doi.org/10.1088/0004-637X/799/2/140

    URI
    http://hdl.handle.net/20.500.11937/33376
    Collection
    • Curtin Research Publications
    Abstract

    The transient ULX in M83 that went into outburst in, or shortly before, 2010 is still active. Our new XMM-Newton spectra show that it has a curved spectrum typical of the upper end of the high/soft state or slim-disk state. It appears to be spanning the gap between Galactic stellar-mass black holes (BHs) and the ultraluminous state, at X-ray luminosities of ≈1-3 × 1039 erg s–1 (a factor of two lower than in the 2010 and 2011 Chandra observations). From its broadened disk-like spectral shape at that luminosity, and from the fitted inner-disk radius and temperature, we argue that the accreting object is an ordinary stellar-mass BH with M ~ 10-20 M ☉. We suggest that in the 2010 and 2011 Chandra observations, the source was seen at a higher accretion rate, resulting in a power-law-dominated spectrum with a soft excess at large radii.

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