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Multiwavelength monitoring of BD+53 2790, the optical counterpart to 4U~2206+54

  • Blay, P.
  • Negueruela, I.
  • Reig, P.
  • Coe, M. J.
  • Corbet, R. H. D.
  • Fabregat, J.
  • Tarasov, A. E.
Publication Date
Oct 13, 2005
Submission Date
Oct 13, 2005
DOI: 10.1051/0004-6361:20053951
arXiv ID: astro-ph/0510400
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We present the results of our long-term monitoring of BD+53 2790, the optical counterpart to the X-ray source 4U~2206+54. Unlike previous studies that classify the source as a Be/X-ray binary, we find that its optical and infrared properties differ from those of typical Be stars: the variability of the V/R ratio is not cyclical; there are variations in the shape and strength of the H$\alpha$ emission line on timescales less than 1 day; and no correlation between the EW and the IR magnitudes or colors is seen. Our observations suggest that BD+53 2790 is very likely a peculiar O9.5V star. In spite of exhaustive searches we cannot find any significant modulation in any emission line parameter or optical/infrared magnitudes. Spectroscopy of the source extending from the optical to the K-band confirms the peculiarity of the spectrum: not only are the He lines stronger than expected for an O9.5V star but also there is no clear pattern of variability. The possibility that BD+53 2790 is an early-type analogue to He-strong stars (like theta^1 Ori C) is discussed.


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