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dc.contributor.authorRussell, T.
dc.contributor.authorDegenaar, N.
dc.contributor.authorWijnands, R.
dc.contributor.authorEijnden, J.
dc.contributor.authorGusinskaia, N.
dc.contributor.authorHessels, J.
dc.contributor.authorMiller-Jones, James
dc.identifier.citationRussell, T. and Degenaar, N. and Wijnands, R. and Eijnden, J. and Gusinskaia, N. and Hessels, J. and Miller-Jones, J. 2018. The Radio-bright Accreting Millisecond X-Ray Pulsar IGR J17591-2342. Astrophysical Journal Letters. 869 (1): pp. 1-6.

IGR J17591-2342 is a 527 Hz accreting millisecond X-ray pulsar that was discovered in outburst in 2018 August. In this Letter, we present quasi-simultaneous radio and X-ray monitoring of this source during the early part of the outburst. IGR J17591-2342 is highly absorbed in X-rays, with an equivalent hydrogen absorption along the line of sight, NH, of 4.4-1022 cm-2, where the Galactic column density is expected to be 1-2-1022 cm-2. The high absorption suggests that the source is either relatively distant (6 kpc), or that the X-ray emission is strongly absorbed by material local to the system. Radio emission detected by the Australia Telescope Compact Array shows that, for a given X-ray luminosity and for distances greater than 3 kpc, this source was exceptionally radio-loud when compared to other accreting neutron stars in outburst (LX1033 erg s-1). For most reasonable distances, IGR J17591-2342 appeared as radio luminous as actively accreting, stellar-mass black hole X-ray binaries.

dc.publisherInstitute of Physics Publishing
dc.titleThe Radio-bright Accreting Millisecond X-Ray Pulsar IGR J17591-2342
dc.typeJournal Article
dcterms.source.titleAstrophysical Journal Letters
curtin.departmentCurtin Institute of Radio Astronomy (Physics)
curtin.accessStatusFulltext not available

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