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Identification of a Likely Radio Counterpart to the Rapid Burster

Moore, Christopher B. and Rutledge, Robert E. and Fox, Derek W. and Guerriero, Robert A. and Lewin, Walter H. G. and Fender, Robert and van Paradijs, Jan (2000) Identification of a Likely Radio Counterpart to the Rapid Burster. Astrophysical Journal, 532 (2). pp. 1181-1191. ISSN 0004-637X. doi:10.1086/308589.

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We have identified a likely radio counterpart to the low-mass X-ray binary MXB 1730-335 (the Rapid Burster). The counterpart has shown 8.4 GHz radio on/off behavior correlated with the X-ray on/off behavior as observed by the RXTE/ASM during six VLA observations. The probability of an unrelated, randomly varying background source duplicating this behavior is 1%-3% depending on the correlation timescale. The location of the radio source is R.A. 17^h33^m24^s.61, decl. -33°23'19".8 (J2000), ±0".1. We do not detect 8.4 GHz radio emission coincident with type II (accretion-driven) X-ray bursts. The ratio of radio to X-ray emission during such bursts is constrained to be below the ratio observed during X-ray-persistent emission at the 2.9 σ level. Synchrotron bubble models of the radio emission can provide a reasonable fit to the full data set, collected over several outbursts, assuming that the radio evolution is the same from outburst to outburst but given the physical constraints the emission is more likely to be due to ~1 hr radio flares such as have been observed from the X-ray binary GRS 1915+105.

Item Type:Article
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Fox, Derek W.0000-0002-3714-672X
Additional Information:© 2000. The American Astronomical Society. Received 1998 December 21; accepted 1999 November 10. We are grateful to Evan Smith, Jean Swank, and the XTE Science Operations Facility staff for their efficient processing of the several XTE TOO observations covered in this work. We are also indebted to VLA observers and staff Phillip Hicks, Robert Hjellming, Rick Perley, Michael Rupen, and Ken Sowinski, who graciously gave us time to perform observations of the RB, to Barry Clark, who worked on short notice to help find the time to make observations during critical periods, to Tasso Tzioumis, who performed the observations at ATCA, and to Ian Robson, who made possible the observations at the JCMT. We are grateful to M. van der Klis and the anonymous referee for their detailed and helpful comments on the manuscript. This work has been supported under NASA Grant NAG5-7481. J. v. P. acknowledges the support of NASA under grant NAG5-7414. R. P. F. was supported during the period of this research initially by ASTRON grant 781-76-017 and subsequently by the EC Marie Curie Fellowship ERBFMBICT 972436. C. B. M. thanks the University of Groningen for its support in the form of a Kapteyn Institute Postdoctoral Fellowship. R. E. R. thanks his host J. Trümper of Max-Planck-Institut für Extreterrestrische Physik, where this work began, and his host Lars Bildsten of University of California, Berkeley, where this work was completed.
Group:Space Radiation Laboratory
Funding AgencyGrant Number
Marie Curie FellowshipERBFMBICT 972436
University of GroningenUNSPECIFIED
Subject Keywords:radiation mechanisms: non-thermal; radio continuum: stars; stars: individual (MXB 1730–335); X-rays: stars
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Other Numbering System NameOther Numbering System ID
Space Radiation Laboratory2000-04
Issue or Number:2
Record Number:CaltechAUTHORS:20150219-083952540
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:54988
Deposited By: Deborah Miles
Deposited On:24 Feb 2015 20:12
Last Modified:10 Nov 2021 20:40

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