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Infrared Counterpart of the Microquasar GRS 1758−258

Rothstein, D. M. and Eikenberry, S. S. and Chatterjee, S. and Egami, E. and Djorgovski, S. G. and Heindl, W. A. (2002) Infrared Counterpart of the Microquasar GRS 1758−258. Astrophysical Journal, 580 (1). L61-L63. ISSN 0004-637X. doi:10.1086/345546.

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We present revised infrared (2.2 μm) astrometry of the field containing the Galactic microquasar GRS 1758-258, using observations at the Keck I 10 m telescope. We find three candidates for the microquasar within a 3 σ error circle but none within 2 σ. We show that if the 18.4 day X-ray period of GRS 1758-258 is due to a binary orbit, then only one of the three candidates, an early K-type giant, is large enough to power the microquasar via Roche lobe overflow. We therefore identify this star as the infrared counterpart of GRS 1758-258, which we classify as a low-mass X-ray binary. Long-term infrared monitoring of this source should provide further information about the microquasar system, including a confirmation of the X-ray period and an estimate of the compact object's mass.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Chatterjee, S.0000-0002-2878-1502
Djorgovski, S. G.0000-0002-0603-3087
Additional Information:© 2002 The American Astronomical Society. Received 2002 June 14; accepted 2002 October 15; published 2002 October 23. This Letter is based in part on observations obtained at the W. M. Keck Observatory, which is operated by the California Association for Research in Astronomy, a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The VLA is a facility of the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The authors thank L. Armus and R. Gal for help in obtaining the CCD images at Palomar Observatory. We also thank the staff at Palomar and Keck Observatories for their expert help during our observing runs. D. M. R. is supported in part by a National Science Foundation Graduate Research Fellowship. S. S. E. and D. M. R. are supported in part by an NSF CAREER award (NSF-9983830).
Funding AgencyGrant Number
NSF Graduate Research FellowshipUNSPECIFIED
Subject Keywords:black hole physics—infrared: stars—stars: individual (GRS 1758-258)—X-rays: stars
Issue or Number:1
Record Number:CaltechAUTHORS:20190924-090846820
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Official Citation:D. M. Rothstein et al 2002 ApJ 580 L61
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:98823
Deposited By: Tony Diaz
Deposited On:24 Sep 2019 16:23
Last Modified:16 Nov 2021 17:41

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