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Individual sheet: WR140
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Spectral type(s): WC7 + O5
Multiplicity:
Confirmed binary system
Period(s): 7.9 yr
Orbital solution: yes
Ref: Marchenko et al.(2003), Fahed et al.(2011)
Quality flag (Q): I
Comments:
The synchrotron emission region has been resolved and monitored along a significant part of the orbit (e.g. Dougherty et al. 2005).
Upper limits on the hard X-ray emission based on INTEGRAL observations have been published in De Becker et al. (2007). Sugawara et al. (2015) reported on the detection of non-thermal X-rays positionally coincident with WR140 on the basis of Suzaku observations, but the physical relation of that source with the massive binary is questioned.
For detailed information on WR140, see Peredur Williams's web page
Low-frequency measurements have been published by Benaglia et al. (2020), with a detection at 610 MHz (but not at 325 MHz).