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A new reduction and a new analysis of a rich series of high-S/N spectra of the bright star κ Sco is carried out to test the technique of spectral disentangling in the case when one of the components is a non-radial oscillator. We im- prove the orbital elements of the system and find the basic physical properties of the binary to be Teff = 24 500 K, masses of 10.7-11.9 Mand 9.6-10.7 Mand the primary radius and rotational period of 7-8 Rand 3 d .56-3 d68, respectively. This also implies log g = 3.70-3.78 (cgs). KOREL disentangling is applied and we find that it worked properly and was not misled by the complex line-profile variability of the pulsating primary. Moreover, the pulsational frequencies are detected via the period search in the line intensities and radial-velocity residuals of the primary derived by KOREL and in the time series of residual spectra in the rest frame of the primary after KOREL disentangling. This constitutes a much better starting point to interpret the complex pixel-by-pixel variations of the disentangled profiles of the primary in terms of stellar oscillations and/or additional rotational modulation than the original spectra before disentangling.

Disentangling component spectra of , a spectroscopic binary with a pulsating primary