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Bright radio emission from an ultraluminous stellar-mass microquasar in M 31

Middleton, Matthew J. and Walton, Dominic and Carpenter, John (2013) Bright radio emission from an ultraluminous stellar-mass microquasar in M 31. Nature, 493 (7431). pp. 187-190. ISSN 0028-0836. doi:10.1038/nature11697.

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A subset of ultraluminous X-ray sources (those with luminosities of less than 10^(40 ) erg s^(−1); ref. 1) are thought to be powered by the accretion of gas onto black holes with masses of ~5–20 M_⊙ , probably by means of an accretion disk. 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 hole, 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 Way, 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 10^(39) 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.

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Middleton, Matthew J.0000-0002-8183-2970
Walton, Dominic0000-0001-5819-3552
Additional Information:© 2013 Macmillan Publishers Limited. Received: 10 May 2012; Accepted: 22 October 2012; Published online: 12 December 2012. We thank C. Trott and R. Soria for discussions, and C. Gough for making his code available. This work was supported by a Science and Technology Facilities Council (STFC) standard grant (M.J.M.), Netherlands Organization for Scientific Research Vidi Fellowship (S.M.), European Research Council partial funding (R.F.) and grant number BMWI/DLR, FKZ 50 OR 1010 (M. Henze). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.Wethank the staff of the Mullard Radio AstronomyObservatory for their assistance in the commissioning and operation of AMI, which is supported by Cambridge University and the STFC. This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This research has also made use of data obtained from NASA’s Swift and Chandra satellites. Author Contributions: M.J.M. wrote the manuscript with comments from all authors. J.C.A.M.-J. designed and analysed the VLA and VLBA observations. N.H.-W. and A.M.M.S. analysed the AMI-LA observations. J.-P.M. and J.C.A.M.-J. conducted the scintillation analysis. S.M., R.F. and M. Henze made significant contributions to the overall science case and manuscript. J.C., G.C.B. and M.G. provided support and analysis for the CARMA observations. The remaining authors either assisted with various aspects of the science case or are contributing members of the M 31 group.
Group:Space Radiation Laboratory
Funding AgencyGrant Number
Science and Technology Facilities Council (STFC)UNSPECIFIED
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)UNSPECIFIED
European Research Council (ERC)UNSPECIFIED
Bundesministerium für Wirtschaft und Energie (BMWi)FKZ 50 OR 1010
Deutsches Zentrum für Luft- und Raumfahrt (DLR)UNSPECIFIED
Subject Keywords:High-energy astrophysics
Issue or Number:7431
Record Number:CaltechAUTHORS:20130208-131926131
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:36824
Deposited On:11 Feb 2013 21:07
Last Modified:09 Nov 2021 23:24

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