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    Multiband counterparts of two eclipsing ultraluminous X-ray sources in M51

    265475.pdf (3.835Mb)
    Access Status
    Open access
    Authors
    Urquhart, Ryan
    Soria, Roberto
    Johnston, H.
    Pakull, M.
    Motch, C.
    Schwope, A.
    Miller-Jones, James
    Anderson, Gemma
    Date
    2018
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Urquhart, R. and Soria, R. and Johnston, H. and Pakull, M. and Motch, C. and Schwope, A. and Miller-Jones, J. et al. 2018. Multiband counterparts of two eclipsing ultraluminous X-ray sources in M51. Monthly Notices of the Royal Astronomical Society. 475 (3): pp. 3561-3576.
    Source Title
    Monthly Notices of the Royal Astronomical Society
    DOI
    10.1093/mnras/sty014
    ISSN
    0035-8711
    School
    Curtin Institute of Radio Astronomy (Physics)
    Funding and Sponsorship
    http://purl.org/au-research/grants/arc/FT140101082
    Remarks

    This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

    URI
    http://hdl.handle.net/20.500.11937/66814
    Collection
    • Curtin Research Publications
    Abstract

    We present the discovery and interpretation of ionized nebulae around two ultraluminous X-ray sources in M 51; both sources share the rare property of showing X-ray eclipses by their companion stars and are therefore prime targets for follow-up studies. Using archival Hubble Space Telescope images, we found an elongated, 100-pc-long emission-line structure associated with one X-ray source (CXOM51 J132940.0+471237; ULX-1 for simplicity), and a more circular, ionized nebula at the location of the second source (CXOM51 J132939.5+471244; ULX-2 for simplicity). We observed both nebulae with the Large Binocular Telescope’s Multi-Object Double Spectrograph. From our analysis of the optical spectra, we argue that the gas in the ULX-1 bubble is shock-ionized, consistent with the effect of a jet with a kinetic power of ≈2 × 1039 erg s−1. Additional X-ray photoionization may also be present, to explain the strength of high-ionization lines such as He II λ4686 and [Ne V] λ3426. On the other hand, the emission lines from the ULX-2 bubble are typical for photoionization by normal O stars suggesting that the nebula is actually an H II region not physically related to the ULX but is simply a chance alignment. From archival Very Large Array data, we also detect spatially extended, steep-spectrum radio emission at the location of the ULX-1 bubble (consistent with its jet origin), but no radio counterpart for ULX-2 (consistent with the lack of shock-ionized gas around that source).

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