Abstract.We have performed abundance analysis of two slowly rotating, late A-type stars, HD 32115 (HR 1613) and HD 37594 (HR 1940), based on obtained echelle spectra covering the spectral range 4000-9850Å. These spectra allowed us to identify an extensive line list for 31 chemical elements, the most complete to date for A-type stars. Two approaches to abundance analysis were used, namely a "manual" (interactive) and a semi-automatic procedure for comparison of synthetic and observed spectra and equivalent widths. For some elements non-LTE (NLTE) calculations were carried out and the corresponding corrections have been applied. The abundance pattern of HD 32115 was found to be very close to the solar abundance pattern, and thus may be used as an abundance standard for chemical composition studies in middle and late A stars. Further, its Hα line profile shows no coreto-wing anomaly like that found for cool Ap stars and therefore also may be used as a standard in comparative studies of the atmospheric structures of cool, slowly rotating Ap stars. HD 37594 shows a metal deficiency at the level of −0.3 dex for most elements and triangle-like cores of spectral lines. This star most probably belongs to the δ Sct group.

The laboratory gas phase spectrum recently published by Campbell et al. has reinvigorated attempts to confirm the presence of the C + 60 cation in the interstellar medium, thorough an analysis of the spectra of hot, reddened stars. This search is hindered by at least two issues that need to be addressed: (i) the wavelength range of interest is severely polluted by strong water-vapour lines coming from the Earth's atmosphere; (ii) one of the major bands attributed to C + 60 , at 9633Å, is blended with the stellar Mgii line, which is susceptible to non-local-thermodynamic equilibrium effects in hot stellar atmospheres. Both these issues are here carefully considered here for the first time, based on high-resolution and high signal-to-noise ratio echellé spectra for 19 lines of sight. The result is that the presence of C + 60 in interstellar clouds is brought into question.

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Aims. We present the results of spectroscopic-and orbit-sampled photometric observations of the faint UV-excess object PG 2200+085. Methods. The optical CCD photometry observations of this object were performed by the Russian-Turkish 1.5-m telescope RTT150 at the TUBITAK National Observatory (Turkey). The long-slit optical spectroscopy observations with 2.6 Å resolution were carried out by 6-m telescope BTA at the Special Astrophysical Observatory (Russia). Results. The photometric variations over two nights are almost sinusoidal with an amplitude ∆m V = 0. m 04 and a period of P = 0.3186 d. Such a light curve is typical of a detached close binary with an illumination effect or the ellipsoidal deformation of a secondary star. The observed spectrum clearly displays a featureless blue continuum of a hot component and a rich absorption-line and molecular band K-star spectrum. The CaII line profiles with strong emission cores are remarkably similar to those of V471 Tau. Conclusions. We tentatively classify PG 2200+085 as a pre-cataclysmic binary of the V471 Tau type.