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

A new ultraluminous X-ray source has been discovered in M 31, whose variability and associated bright, compact radio emission identify it as a stellar-mass black hole accreting close to the Eddington limit. The ULX factor in the Andromeda galaxy Ultra-luminous X-ray sources, or ULXs, are a subject o...

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Published inNature (London) Vol. 493; no. 7431; pp. 187 - 190
Main Authors Middleton, Matthew J., Miller-Jones, James C. A., Markoff, Sera, Fender, Rob, Henze, Martin, Hurley-Walker, Natasha, Scaife, Anna M. M., Roberts, Timothy P., Walton, Dominic, Carpenter, John, Macquart, Jean-Pierre, Bower, Geoffrey C., Gurwell, Mark, Pietsch, Wolfgang, Haberl, Frank, Harris, Jonathan, Daniel, Michael, Miah, Junayd, Done, Chris, Morgan, John S., Dickinson, Hugh, Charles, Phil, Burwitz, Vadim, Valle, Massimo Della, Freyberg, Michael, Greiner, Jochen, Hernanz, Margarita, Hartmann, Dieter H., Hatzidimitriou, Despina, Riffeser, Arno, Sala, Gloria, Seitz, Stella, Reig, Pablo, Rau, Arne, Orio, Marina, Titterington, David, Grainge, Keith
Format Journal Article
LanguageEnglish
Published London Nature Publishing Group UK 10.01.2013
Nature Publishing Group
Subjects
639/33/34/864
639/624/400/1106
Accretion
Astronomy
Astrophysics
Black holes
Black holes (astronomy)
Emissions
Environmental aspects
Humanities and Social Sciences
letter
Luminosity
Luminosity (Astronomy)
Microquasars
multidisciplinary
Observations
Radio
Radio emission
Science
Stars & galaxies
X-ray sources
X-rays
Australia
United Kingdom
Netherlands
Online AccessGet full text

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Abstract A new ultraluminous X-ray source has been discovered in M 31, whose variability and associated bright, compact radio emission identify it as a stellar-mass black hole accreting close to the Eddington limit. The ULX factor in the Andromeda galaxy Ultra-luminous X-ray sources, or ULXs, are a subject of controversy as their extreme luminosities have not yet been satisfactorily explained. Here Matthew Middleton et al . report radio and X-ray observations of a bright new X-ray source in the nearby M31 Andromeda galaxy. Its radio luminosity is extremely high and variable on a timescale of tens of minutes, implying a highly compact source powered by accretion onto a stellar-mass black hole at close to the Eddington limit, the theoretical maximum rate of matter infall. The authors speculate that using the latest highly sensitive radio telescopes, future observations of transient ULX systems in nearby galaxies will reveal the causal relationship between the accretion flow and the powerful jet emission. 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 , probably by means of an accretion disk 2 , 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 hole 4 , 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 Way 6 , 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.
AbstractList A subset of ultraluminous X-ray sources (those with luminosities of less than 10 super(40)ergs super(-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 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 super(39)ergs super(-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.
A new ultraluminous X-ray source has been discovered in M 31, whose variability and associated bright, compact radio emission identify it as a stellar-mass black hole accreting close to the Eddington limit. The ULX factor in the Andromeda galaxy Ultra-luminous X-ray sources, or ULXs, are a subject of controversy as their extreme luminosities have not yet been satisfactorily explained. Here Matthew Middleton et al . report radio and X-ray observations of a bright new X-ray source in the nearby M31 Andromeda galaxy. Its radio luminosity is extremely high and variable on a timescale of tens of minutes, implying a highly compact source powered by accretion onto a stellar-mass black hole at close to the Eddington limit, the theoretical maximum rate of matter infall. The authors speculate that using the latest highly sensitive radio telescopes, future observations of transient ULX systems in nearby galaxies will reveal the causal relationship between the accretion flow and the powerful jet emission. 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 , probably by means of an accretion disk 2 , 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 hole 4 , 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 Way 6 , 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.
A subset of ultraluminous X-ray sources (those with luminosities of less than 10^sup 40^ erg s^sup -1^; ref. 1) are thought to be powered by the accretion of gas onto black holes with masses of 5-20M^sub *^, 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 softX-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^sup 39^ erg s^sup -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. [PUBLICATION ABSTRACT]
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 ∼5-20M cicled dot, 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.
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 ∼5-20M cicled dot, 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.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 ∼5-20M cicled dot, 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.
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 similar to 5-20M(circle dot), probably by means of an accretion disk(2,3). 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 hole(4,5), 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 Way(6), 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.
Audience Academic
Author Miah, Junayd
Greiner, Jochen
Scaife, Anna M. M.
Riffeser, Arno
Done, Chris
Morgan, John S.
Titterington, David
Reig, Pablo
Harris, Jonathan
Henze, Martin
Haberl, Frank
Roberts, Timothy P.
Gurwell, Mark
Carpenter, John
Macquart, Jean-Pierre
Burwitz, Vadim
Hatzidimitriou, Despina
Middleton, Matthew J.
Freyberg, Michael
Hernanz, Margarita
Markoff, Sera
Fender, Rob
Valle, Massimo Della
Pietsch, Wolfgang
Hurley-Walker, Natasha
Orio, Marina
Daniel, Michael
Charles, Phil
Sala, Gloria
Rau, Arne
Dickinson, Hugh
Grainge, Keith
Hartmann, Dieter H.
Walton, Dominic
Seitz, Stella
Miller-Jones, James C. A.
Bower, Geoffrey C.
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  organization: Physics Department, University of Durham, Durham DH1 3LE, UK, Astronomical Institute Anton Pannekoek, Science Park 904, 1098 XH Amsterdam, The Netherlands
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https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-87696$$DView record from Swedish Publication Index
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Snippet A new ultraluminous X-ray source has been discovered in M 31, whose variability and associated bright, compact radio emission identify it as a stellar-mass...
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...
A subset of ultraluminous X-ray sources (those with luminosities of less than 10^sup 40^ erg s^sup -1^; ref. 1) are thought to be powered by the accretion of...
A subset of ultraluminous X-ray sources (those with luminosities of less than 10 super(40)ergs super(-1); ref. 1) are thought to be powered by the accretion of...
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...
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SubjectTerms 639/33/34/864
639/624/400/1106
Accretion
Astronomy
Astrophysics
Black holes
Black holes (astronomy)
Emissions
Environmental aspects
Humanities and Social Sciences
letter
Luminosity
Luminosity (Astronomy)
Microquasars
multidisciplinary
Observations
Radio
Radio emission
Science
Stars & galaxies
X-ray sources
X-rays
Title Bright radio emission from an ultraluminous stellar-mass microquasar in M 31
URI https://link.springer.com/article/10.1038/nature11697
https://www.ncbi.nlm.nih.gov/pubmed/23235823
https://www.proquest.com/docview/1285241936
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Volume 493
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