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

被引：112

作者：

Middleton, Matthew J. ^{[1
,2
]}

Miller-Jones, James C. A. ^{[3
]}

Markoff, Sera ^{[2
]}

Fender, Rob ^{[4
]}

Henze, Martin ^{[5
]}

Hurley-Walker, Natasha ^{[3
]}

Scaife, Anna M. M. ^{[4
]}

Roberts, Timothy P. ^{[1
]}

Walton, Dominic ^{[6
,7
]}

Carpenter, John ^{[7
]}

Macquart, Jean-Pierre ^{[3
,8
]}

Bower, Geoffrey C. ^{[9
]}

Gurwell, Mark ^{[10
]}

Pietsch, Wolfgang ^{[5
]}

Haberl, Frank ^{[5
]}

Harris, Jonathan ^{[1
]}

Daniel, Michael ^{[1
]}

Miah, Junayd ^{[1
]}

Done, Chris ^{[1
]}

Morgan, John S. ^{[3
]}

Dickinson, Hugh ^{[11
]}

Charles, Phil ^{[4
,12
]}

Burwitz, Vadim ^{[5
]}

Della Valle, Massimo ^{[13
,14
]}

Freyberg, Michael ^{[5
]}

Greiner, Jochen ^{[5
]}

Hernanz, Margarita ^{[15
]}

Hartmann, Dieter H. ^{[16
]}

Hatzidimitriou, Despina ^{[17
]}

Riffeser, Arno ^{[18
]}

Sala, Gloria ^{[19
]}

Seitz, Stella ^{[18
]}

Reig, Pablo ^{[20
]}

Rau, Arne ^{[5
]}

Orio, Marina ^{[21
]}

Titterington, David ^{[22
]}

Grainge, Keith ^{[22
]}

机构：

[1] Univ Durham, Dept Phys, Durham DH1 3LE, England

[2] Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands

[3] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia

[4] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England

[5] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

[6] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England

[7] CALTECH, Dept Astron, Pasadena, CA 91125 USA

[8] Curtin Univ Technol, ARC Ctr Excellence All Sky Astrophys CAASTRO, Perth, WA 6845, Australia

[9] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[10] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[11] Stockholm Univ, Oskar Klein Ctr, AlbaNova, SE-10691 Stockholm, Sweden

[12] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa

[13] Osserv Astron Capodimonte, INAF, I-80131 Naples, Italy

[14] Int Ctr Relativist Astrophys, I-65122 Pescara, Italy

[15] Fac Ciencies, Inst Space Sci CSIC IEEC, Barcelona 08193, Spain

[16] Clemson Univ, Dept Phys & Astron, Kinard Lab 118, Clemson, SC 29631 USA

[17] Univ Athens, Fac Phys, Dept Astrophys Astron & Mech, Athens 15784, Greece

[18] Univ Munich, Univ Observ Munich, D-81679 Munich, Germany

[19] EUETIB UPC IEEC, Dept Phys & Nucl Engn, Barcelona 08036, Spain

[20] Fdn Res & Technol Hellas, Iraklion 71110, Crete, Greece

[21] Osserv Astron Padova, I-35122 Padua, Italy

[22] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England

来源：

NATURE | 2013年 / 493卷 / 7431期

基金：

美国国家科学基金会; 欧洲研究理事会; 英国科学技术设施理事会;

关键词：

X-RAY SOURCE; BLACK-HOLE BINARIES; SUPERLUMINAL SOURCE; GRS 1915+105; J1819.3-2525; EVOLUTION; SYSTEMS; CHANDRA; GALAXY; MODEL;

D O I：

10.1038/nature11697

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

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.

引用

页码：187 / 190

页数：4

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