Middleton, Matthew J. and Miller-Jones, James C. A. and Markoff, Sera and Fender, Rob and Henze, Martin and Hurley-Walker, Natasha and Scaife, Anna M. M. and Roberts, Timothy P. and Walton, Dominic and Carpenter, John and Macquart, Jean-Pierre and Bower, Geoffrey C. and Gurwell, Mark and Pietsch, Wolfgang and Haberl, Frank and Harris, Jonathan and Daniel, Michael and Miah, Junayd and Done, Chris and Morgan, John S. and Dickinson, Hugh and Charles, Phil and Burwitz, Vadim and Della Valle, Massimo and Freyberg, Michael and Greiner, Jochen and Hernanz, Margarita and Hartmann, Dieter H. and Hatzidimitriou, Despina and Riffeser, Arno and Sala, Gloria and Seitz, Stella and Reig, Pablo and Rau, Arne and Orio, Marina and Titterington, David and Grainge, Keith (2013) 'Bright radio emission from an ultraluminous stellar-mass microquasar in M 31.', Nature., 493 (7431). pp. 187-190.
A subset of ultraluminous X-ray sources (those with luminosities of less than 1040 erg s−1; ref. 1) are thought to be powered by the accretion of gas onto black holes with masses of ~5–20 , probably by means of an accretion disk2, 3. The X-ray and radio emission are coupled in such Galactic sources; the radio emission originates in a relativistic jet thought to be launched from the innermost regions near the black hole4, 5, with the most powerful emission occurring when the rate of infalling matter approaches a theoretical maximum (the Eddington limit). Only four such maximal sources are known in the Milky Way6, and the absorption of soft X-rays in the interstellar medium hinders the determination of the causal sequence of events that leads to the ejection of the jet. Here we report radio and X-ray observations of a bright new X-ray source in the nearby galaxy M 31, whose peak luminosity exceeded 1039 erg s−1. The radio luminosity is extremely high and shows variability on a timescale of tens of minutes, arguing that the source is highly compact and powered by accretion close to the Eddington limit onto a black hole of stellar mass. Continued radio and X-ray monitoring of such sources should reveal the causal relationship between the accretion flow and the powerful jet emission.
|Full text:||(AM) Accepted Manuscript|
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|Publisher Web site:||http://dx.doi.org/10.1038/nature11697|
|Date accepted:||No date available|
|Date deposited:||09 January 2014|
|Date of first online publication:||January 2013|
|Date first made open access:||No date available|
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