Optical identification of the LMC supersoft source RX J0527.8-6954 from MACHO project photometry

We identify the likely optical counterpart to the Large Magellanic Cloud (LMC) supersoft X-ray source RX J0527.8–6954, and hence recover HV 2554. This identification is based on an analysis of ~ 4 yr of optical photometry obtained serendipitously via the MACHO project. We see a steady fading of the...

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Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society 1997-10, Vol.291 (1), p.L13-L16
Main Authors: Alcock, C., Allsman, R. A., Alves, D. R., Axelrod, T. S., Bennett, D. P., Charles, P. A., Cook, K. H., Freeman, K. C., Griest, K., Lehner, M. J., Livio, M., Marshall, S. L., Minniti, D., Peterson, B. A., Pratt, M. R., Quinn, P. J., Rodgers, A. W., Southwell, K. A., Stubbs, C. W., Sutherland, W.
Format: Article
Language:English
Subjects:
accretion
accretion discs
binaries: close
binaries: spectroscopic
stars: individual: RX J0527.8-6954
X-rays: stars
Citations: Items that cite this one
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Summary:We identify the likely optical counterpart to the Large Magellanic Cloud (LMC) supersoft X-ray source RX J0527.8–6954, and hence recover HV 2554. This identification is based on an analysis of ~ 4 yr of optical photometry obtained serendipitously via the MACHO project. We see a steady fading of the star of ~0.5 mag over the duration of the observations. Evidence is also presented for an orbital modulation of ~0.05-mag semi-amplitude on a period of P = 0.39262 ± 0.00015 d. Our optical observations are consistent with the suggestion that the X-ray decline in this system is caused by cooling after a weak shell flash.
ISSN:0035-8711
1365-2966
DOI:10.1093/mnras/291.1.L13