Identification of the Optical Counterpart of LMC X-1

Details Identification of the Optical Counterpart of LMC X-1 Identification of the Optical Counterpart of LMC X-1

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aas...18510206a&link_type=abstract

American Astronomical Society, 185th AAS Meeting, #102.06; Bulletin of the American Astronomical Society, Vol. 26, p.1484

Astronomy and Astrophysics

Astronomy

Scientific paper

LMC X-1 is one of the most luminous and highly variable X-ray sources in the LMC. However, there has been a long standing uncertainty about its optical identification. The Einstein--HRI position lay between the early-type supergiant R148 and a peculiar O7 III star, known as Star #32 (Cowley et al. 1978), which has a resolved He II nebula surrounding it (Pakull & Angebualt 1986). The system is of particular interest since it appears to contain a black hole. A new X-ray position for LMC X-1 has been derived using 23 ROSAT--HRI observations. Corrections for a small field rotation (Kuerster 1993) and an optical-X-ray offset (Schmidtke et al. 1994) have been applied. The resulting position is ~ 1('') from Star #32, confirming its identification with LMC X-1. In addition, quasi-periodic oscillations (QPO) have been found in some of the data. They show a centroid frequency of 0.0718 Hz, slightly lower than the frequency detected by Ebisawa et al. (1989) using Ginga data.

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