%R 1999A&AS..140..261A %J-277 %A Alonso A. %A Arribas S. %A Martinez-Roger C. %T The effective temperature scale of giant stars (F0-K5). II. Empirical calibration of T_eff_ versus colours and [Fe/H]. %M ds1708 %F 1999.12.16 %B We present calibrations of the effective temperatures of giant stars versus [Fe/H] and colours (U-V), (B-V), (R-I), (V-R), (V-I), (V-K), (J-H), (J-K), (I-K), (V-L'), (b-y) and (u-b). These calibrations are based on a large sample of field and globular cluster stars which roughly cover spectral types from F0 to K5. Their effective temperatures, scaled to direct T_eff_ determinations via reliable angular diameter measurements, were derived by applying the infrared flux method. The empirical relations have been fitted to polynomials of the form {theta}_eff_ = P(colour,[Fe/H]) by using the least squares method. The precision of the fits ranges from 40K for (V-K) to 170K for (J-H). We tabulate intrinsic colours of giant stars in the ranges: 3500K<=T_eff_<=8000K; -3.0<=[Fe/H]<=+0.5. We also present the calibration of BC(V) as a function of log(T_eff_) and metallicity. Finally, we compare the resulting scale of temperatures with previous works. %K stars: fundamental parameters - stars: Population II - stars: giants - stars: atmospheres - stars: general %R 1999A&AS..140..279G %J-285 %A Ginestet N. %A Griffin R.F. %A Carquillat J.M. %A Udry S. %T Contribution a l'etude des spectres composites. VIII. HD 174016-7, une etoile Ap associee a une geante G Contribution to the study of composite spectra VIII. HD 174016-7, an Ap star with a giant G. %M ds1769 %F 1999.12.16 %B HD 174016-7, listed by Hynek (1938CoPer...1...10H) as a star having a composite spectrum, was on our observing programmes of such objects carried out both at the Cambridge Observatories and at the Observatoire Midi-Pyrenees. Most of the observations were made with the CORAVEL spectrovelocimeter of the Swiss telescope at the Observatoire de Haute-Provence. We find that this star is a long-period spectroscopic binary with two correlation dips; we obtain the following orbital elements: P=3097.9days; T=JD2450605.2; {omega}=204.8{deg}; e=0.600; K_1_=12.95km/s; K_2_=15.14km/s; V_0_=-1.65km/s; a_1_sini=441.1Gm; a_2_sini=516.0Gm; M_1_sin^3^i=1.967M_{sun}_; M_2_sin^3^i=1.681M_{sun}_. The primary is a giant star of spectral type near G6III, and the hot dwarf secondary is found to be a peculiar A star of type A0p Sr, Cr, Eu, Si; so HD 174016-7 is, to our knowledge, the second discovered composite-spectrum binary with a Ap-type hot component. A confrontation with Hipparcos data suggests M_v1_=0 and m_v_=0.6mag. On the basis of very accurate masses of main sequence stars by Andersen (1991) we estimate the mass, M_1_=2.8M_{sun}_, of the giant primary, the orbital inclination, i=63{deg}, and the mean linear separation of the components, a=7.2AU. The evolutionary status of the system is discussed using Schaller et al. (1992) M_bol_/T_eff_ diagram for stars of solar metallicity. Theoretical masses suggested by this diagram confirm the proposed model. %K stars: individual: \objS{HD 174016}{HD 174016-7} - binaries: spectroscopic; symbiotic - stars: fundamental parameters %R 1999A&AS..140..287B %J-292 %A Balega I.I. %A Balega Y.Y. %A Maksimov A.F. %A Pluzhnik E.A. %A Shkhagosheva Z.U. %A Vasyuk V.A. %T Binary star speckle measurements during 1992-1997 from the SAO 6-m and 1-m telescopes in Zelenchuk. %M ds1776 %F 1999.12.16 %B We present the results of speckle interferometric measurements of binary stars made with the television photon-counting camera at the 6-m Big Azimuthal Telescope (BTA) and 1-m telescope of the Special Astrophysical Observatory (SAO) between August 1992 and May 1997. The data contain 89 observations of 62 star systems on the large telescope and 21 on the smaller one. For the 6-m aperture 18 systems remained unresolved. The measured angular separation ranged from 39mas, two times above the BTA diffraction limit, to 1593mas. %K stars: binaries: visual - techniques interferometric - catalogs %R 1999A&AS..140..293G %J-307 %A Guertler J. %A Friedemann C. %A Reimann H.-G. %A Splittgerber E. %A Rudolph E. %T A comparative study of the long-term light variations of six young irregular variables. %M h0993 %F 1999.12.16 %B We investigated the long-term light variations of six young irregular variables, all of them UX Orionis stars or related objects. For this aim we determined new photographic magnitudes for the five stars VX Cas, BH Cep, BO Cep, SV Cep, and RZ Psc and made use of similar data for WW Vul published independently. The magnitudes were derived from Argelander brightness estimates performed on plates of the Harvard College Observatory and Sonneberg Observatory plate collections. The data cover a period of about 100 years and are available at the Centre des Donnees Stellaires, Strasbourg. The new data were supplemented by multicolour photoelectric measurements taken from the literature and visual estimates collected by the AAVSO. The resulting lightcurves are displayed and discussed. Algol-like minima are observed with all the stars. Their properties are discussed under the presumption that they are caused by circumstellar dust clouds orbiting the stars. Parameters of the circumstellar dust shells are derived from modelling the observed infrared excess radiation and compared with constraints from the light variations. %K stars: individual: VX Cas, BH Cep, BO Cep, SV Cep, RZ Psc, WW Vul - stars: variables: general - circumstellar matter %R 1999A&AS..140..309F %J-326 %A Fabrika S. %A Sholukhova O. %T A survey of blue - H{alpha} objects in the galaxy M33. %M ds1746 %F 1999.12.16 %B For the purposes of a search for SS433 type objects, LBV stars and hypergiants in M33, we have carried out a photometry of blue stars in H{alpha} images of this galaxy. From 2332 listed OB stars, we have isolated 549 objects, which have H{alpha} excess over stars of the same V magnitude. Among them 81 emission stars (s) have been selected. About 60% of isolated objects found to be extended in H{alpha}, among them 154 diffuse (d) and 180 bubble-type (b) nebulae. 117 objects are compact (c) and faint H{alpha} sources. These groups are different in colour indices, H{alpha} fluxes, surface brightness and sizes. The most probable size of the H{alpha} nebulae is FWHM=10-14pc. There is evidence that their properties and location in the galaxy are defined by interstellar gas pressure and related to spiral arms. The d objects are HII regions with an embedded star. The b objects are probably envelopes around WR stars or SN remnants. Among s-type objects we isolated a group of 20 brightest stars, which in their average properties fit well to the parameters of blue hypergiants or LBV-type stars. The stars of intermediate brightness follow very well to blue Ia supergiants. The interstellar absorption derived from brightest H{alpha} stars is A_ V_=0.93mag+/-0.05mag . We classify the faintest stars as blue Ib supergiants, their average absorption is A_V_=~0.6mag . They are restricted in number by the limiting stellar magnitude in the original sample. %K nearby galaxies: stellar content: individual (M33) - stars: early type - H{alpha} excess %R 1999A&AS..140..327M %J-344 %A Mueller K.R. %A Wegner G. %A Raychaudhury S. %A Freudling W. %T Fundamental plane distances to early-type field galaxies in the South Equatorial Strip. I. The spectroscopic data. %M ds8990 %F 1999.12.16 %B Radial velocities and central velocity dispersions are derived for 238 E/S0 galaxies from medium-resolution spectroscopy. New spectroscopic data have been obtained as part of a study of the Fundamental Plane distances and peculiar motions of early-type galaxies in three selected directions of the South Equatorial Strip, undertaken in order to investigate the reality of large-scale streaming motion; results of this study have been reported in Mueller et al. (1998ApJ...507L.105M ). The new APM South Equatorial Strip Catalog (-17.5deg<{delta}<+2.5deg) was used to select the sample of field galaxies in three directions: (1) 15h10-16h10; (2) 20h30-21h50; (3) 00h10-01h30. The spectra obtained have a median S/N per {AA} of 23, an instrumental resolution (FWHM) of ~4{AA}, and the spectrograph resolution (dispersion) is ~100km/s. The Fourier cross-correlation method was used to derive the radial velocities and velocity dispersions. The velocity dispersions have been corrected for the size of the aperture and for the galaxy effective radius. Comparisons of the derived radial velocities with data from the literature show that our values are accurate to 40 km.s^-1^. A comparison with results from Jorgensen et al. (1995MNRAS.276.1341J) shows that the derived central velocity dispersion have an rms scatter of 0.036 in log{sigma}. There is no offset relative to the velocity dispersions of Davies et al. (1987ApJS...64..581D). %K techniques: spectroscopic - galaxies: distances and redshifts - galaxies: elliptical and lenticular, cD - galaxies: fundamental parameters %R 1999A&AS..140..345D %J-349 %A Della Prugna F. %T Visual measurements and spectral survey of night sky brightness in Venezuela and Italy. %M ds8880 %F 1999.12.16 %B This paper reports measurements of zenith night sky brightness and a spectral survey carried out at selected places in Venezuela and Italy. These range from large cities (Caracas and Florence) and towns (Merida and Siena), to dark sites, such as the Venezuelan Astronomical Observatory and the Alps. Measurements were carried out visually by means of a simple photometer and spectra from 4100 to 6400{AA}, were obtained by a small spectrograph. From the results obtained at the sites tested in Italy, the sky brightness increase since 1973 is given. Since in both countries there are effective regulations to fight light pollution, and more are foreseen in the near future, it is the purpose of this paper to stress the importance, and also the need, of night sky quality monitoring over time to assess the efficacy of these legal tools. %K site testing - techniques: photometric - techniques: spectroscopic %R 1999A&AS..140..351L %J-353 %A La Franca F. %A Lissandrini C. %A Cristiani S. %A Miller L. %A Hawkins M.R.S. %A McGillivray H.T. %T A survey of UV-excess AGNs in the South Galactic Pole. A sample for the analysis of the QSO clustering. %M h1644 %F 1999.12.16 %B Spectra, position, magnitudes and colors are presented for 485 faint (B_J_<20.5) emission line objects selected with the ultraviolet-excess (UVX) criterion on a area of 24.6deg^2^ in the South Galactic Pole. The objects were selected from the analysis of pixel-to-pixel stacking of COSMOS scans of UKST U J and R plates. The candidates were observed with the Meudon-ESO Fiber Optics System (MEFOS) at the ESO 3.6 m telescope. 429 type 1 AGNs have been identified (373 in the redshift range 0.3