Abstract. We present and analyse in this paper the first results of a systematic search for Galactic carbon (C) stars using the First Byurakan Spectral Sky Survey (FBS). The present surveyed area extends over ∼6140 deg 2 on the sky corresponding to ∼1/3 of the complete FBS Survey. Accurate positions, spectral classifications, approximate B and R magnitudes, and finding charts are provided for 35 objects. Identification and spectral subclasses (R or N) of those stars, belonging to the magnitude range 10.5 ≤ R ≤ 16.4, were determined by scrutinizing the Byurakan Schmidt telescope objective-prism plates. Subsequent slit-spectroscopic observations were obtained by us for 21 stars, confirming the carbon nature of them all. From this result, it is assumed that the remaining C star candidates are most likely carbon-rich stars as well. 18 of the listed objects at a Galactic latitude (|b| > 30• ) are faint enough (R > 11.0) to be considered as Faint High Latitude Carbon (FHLC) stars according to the definition of Totten & Irwin (1998). JHK magnitudes for 23 objects of our list are provided by the 2MASS database. Approximate distances are estimated from R and/or JHK data. Most of the stars are located between d 7 and d 25 kpc from the Sun while their distances z to the Galactic plane range from about 2 to 25 kpc. The most distant object of our sample is found at d 45 kpc and z 40 kpc. It is interesting to note that the rate of newly discovered FBS FHLC stars -one object per 200 deg 2 -is comparable to that achieved by other previous surveys. Consequently it is reasonable to expect that the full exploitation of the FBS plates might result in the identification of about 45 new FHLC stars.

We have studied spectra of the peculiar B[e] star HD 45677. Examination of the Balmer wings enabled us to determine a value of log g = 3.9 indicating a possibly luminosity class V. The weak Heɪ lines togetherwith the Si ɪɪ 4128 and 4130 Å doublet indicate a low rotation velocity in the order of 70 km s−1, which is much lower than the previously claimed value of 200 km s−1 by Swings & Allen (1971). We have examined high-resolution profiles of the strong He I line at 5876 Å and found on one hand that we can explain the variation of the profile by the motions of clouds, some of which accreted. The Balmer lines on the other hand show the presence of an accelerated wind plus absorption by a disk seen edge-on

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Abstract. We discuss new and archive spectroscopic and photometric observations of the Herbig Ae star V 380 Ori obtained between 1978 and 1995 and covering at different epochs the wavelength range from 1200Å to 5 µm. The coordinated JHKLM and CVF infrared observations and optical spectroscopy made at ESO of March 1985 confirm the presence of a strong IR excess due to emission from hot cicumstellar dust. The comparison with IR photometry from the literature suggests the presence of oscillations, without secular variations. The optical spectrum of V 380 Ori, observed at ESO during 1983ESO during -1985, and at OHP in January 1995, remained substatially stable, and was all the time characterized by a large number of broad (F W HM ∼ 150 km s −1 ) permitted emission lines, probably formed in a rotating optically thick disk. The strongest Fe ii lines have complex profile with a principal central emission and a blue-shifted (−140 km s −1 ) wind component, the redward component probably being occulted by the disk. The multiplet 42 lines have P Cygni absorption components shifted by −250 km s −1 which should be associated with a teneous cool wind. We remark the secular behaviour of the stellar activity probe He i 5876Å line, which is present in all our spectra as a broad emission, while in other times it was absent or in absorption. The ultraviolet (IUE) spectrum shows a short wavelength cut off at ∼ 1300Å typical of a B9-A0 star, with a rich absorption spectrum, which is thought to be produced in an optically thick stellar envelope or wind. The 2175Å interstellar band strength is consistent with a mean Send offprint requests to: C. Rossi, rossic@uniroma1.it Based on observations made with the International Ultraviolet Explorer collected at the Villafranca Satellite Tracking Station of ESA, on archive IUE data, and on observations collected at the European Southern Observatory, at the Observatoire de Haute Provence. Table 3 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.html galactic-type extinction law with an E B−V = 0.20 ± 0.05, much smaller than that derived from the visual (∼0.5), which suggests an anomalous local UV extinction. The comparison of the archive IUE data shows that during 1978-1989 there was no significant flux variation, with the possible exception of the UV Mg ii emission line.

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