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Analyses of multi-epoch, high-resolution (~ 50000) optical spectra of seven early-type systems provided various important new insights with respect to their multiplicity. First determinations of orbital periods were made for HD 92206C (2.022 d), HD 112244 (27.665 d), HD 164438 (10.25 d), HD 123056A (~ 1314 d) and HD 123056B (< 2 d); the orbital period of HD 318015 could be improved (23.445975 d). Concerning multiplicity, a third component was discovered for HD 92206C by means of He I line profiles. For HD 93146A, which was hitherto assumed to be SB1, lines of a secondary component could be discerned. HD 123056 turns out to be a multiple system consisting of a high-mass component A (~ O8.5) displaying a broad He II 5411 A feature with variable radial velocity, and of an inner pair B (~ B0) with double He I lines. The binary HD 164816 was revisited and some of its system parameters were improved. In particular, we determined its systemic velocity to be -7 km/s, which coincides with the radial velocity of the cluster NGC 6530. This fact, together with its distance, suggests the cluster membership of HD 164816. The OB system HD 318015 (V1082 Sco) belongs to the rare class of eclipsing binaries with a supergiant primary (B0.5/0.7). Our combined orbital and light-curve analysis suggests that the secondary resembles an O9.5III star. Our results for a limited sample corroborate the findings that many O stars are actually massive multiple systems., Comment: 16 pages, 16 figures, to appear in Astronomy and Astrophysics

Using ESO FEROS archive spectra of several southern OB-type binaries, we derived periods for three SB2 spectroscopic binaries, HD 97166, HD 115455, and HD 123590, and two SB1 systems, HD 130298 and HD 163892. It was also possible to use new FEROS spectra to improve the parameters of the known binaries, KX Vel and HD 167263. For KX Vel, we determined a dynamic mass of the primary of 16.8 M$_{\odot}$, while the evolutionary model suggests a higher value of 20.2 M$_{\odot}$. We derived an improved period for HD 167263, and in its spectra, we recognized contributions of both of its interferometric components., Comment: 9 pages, A&A accepted

Preface of Planetary Systems Beyond the Main Sequence including conference scope and summary, short overview of programme, acknowledgements of patronage, sponsors, the scientific organising committee, and the local organising committee., Comment: Part of PlanetsbeyondMS/2010 proceedings http://arxiv.org/html/1011.6606

We give here the Table of Contents page for the Proceedings of "Planetary Systems beyond the Main Sequence", held in August 2010 at Bamberg, Germany. This conference was the first to discuss the fate of a planet and its host star when the star evolves into a red giant and finally ends its life as a white dwarf. Scientists specialised in stellar evolution met experts from the exoplanet field to discuss this interplay., Comment: HTML file with clickable links to papers (if submitted to astro-ph, including the appropriate report number, and linking the submission to the index at arXiv:1011.6606)

We analyse new spectra of the multiple system SZ Cam because previous studies found different values of the primary radial velocity amplitude. The older solutions of light curves also have different ratios of secondary to primary luminosity as inferred from the observed equivalent widths of spectral lines. We therefore reanalyse the light curves of the eclipsing pair. Only the light curve derived by Wesselink has a solution that agrees with the observed equivalent width ratio. The resulting parameters of the binary are discussed. Masses of $M_1=16.6$ and $M_2=11.9$ M$_{\odot}$, and radii $R_1=9.4$ and $R_2=5.4$ R$_{\odot}$ are derived. We point out that radial velocities measured with the CCF method can be misleading when the method is applied to multiple systems with complex line blends. New radial velocities are also obtained for the visual component ADS 2984 A (HD 25639)., Comment: Astronomy and Astrophysics, accepted