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Pulkovo compilation of radial velocities for 35495 stars in a common system.
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| Hipparcos red stars in the HpV_T2 and V I_C systems
For Hipparcos M, S, and C spectral type stars, we provide calibratedinstantaneous (epoch) Cousins V - I color indices using newly derivedHpV_T2 photometry. Three new sets of ground-based Cousins V I data havebeen obtained for more than 170 carbon and red M giants. These datasetsin combination with the published sources of V I photometry served toobtain the calibration curves linking Hipparcos/Tycho Hp-V_T2 with theCousins V - I index. In total, 321 carbon stars and 4464 M- and S-typestars have new V - I indices. The standard error of the mean V - I isabout 0.1 mag or better down to Hp~9 although it deteriorates rapidly atfainter magnitudes. These V - I indices can be used to verify thepublished Hipparcos V - I color indices. Thus, we have identified ahandful of new cases where, instead of the real target, a random fieldstar has been observed. A considerable fraction of the DMSA/C and DMSA/Vsolutions for red stars appear not to be warranted. Most likely suchspurious solutions may originate from usage of a heavily biased color inthe astrometric processing.Based on observations from the Hipparcos astrometric satellite operatedby the European Space Agency (ESA 1997).}\fnmsep\thanks{Table 7 is onlyavailable in electronic form at the CDS via anonymous ftp tocdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/397/997
| Vitesses radiales. Catalogue WEB: Wilson Evans Batten. Subtittle: Radial velocities: The Wilson-Evans-Batten catalogue.
We give a common version of the two catalogues of Mean Radial Velocitiesby Wilson (1963) and Evans (1978) to which we have added the catalogueof spectroscopic binary systems (Batten et al. 1989). For each star,when possible, we give: 1) an acronym to enter SIMBAD (Set ofIdentifications Measurements and Bibliography for Astronomical Data) ofthe CDS (Centre de Donnees Astronomiques de Strasbourg). 2) the numberHIC of the HIPPARCOS catalogue (Turon 1992). 3) the CCDM number(Catalogue des Composantes des etoiles Doubles et Multiples) byDommanget & Nys (1994). For the cluster stars, a precise study hasbeen done, on the identificator numbers. Numerous remarks point out theproblems we have had to deal with.
| CCD uvbyβ photometry of faint stars. I. Observations and reductions.
An observational programme involving simultaneous CCD- and photoelectricuvbyβ photometry has been carried out using the two Danishtelescopes at La Silla. In order to derive reliable astrophysicalparameters for F dwarfs at distances of several kpc final accuraciesbetter than 0.015mag for each magnitude are needed for faint stars. Highaccuracy requires careful preprocessing and data handling and therequested accuracy is now obtained for stars as faint as V=~18mag usingthe procedure described in this paper. A common robust CCD instrumentalsystem is established and the subsequent transformation to the standardsystem is performed using a set of faint secondary standards observed inthe photoelectric programme. Photoelectric photometry for a number ofcalibration stars in the CCD frames is also published. These stars haveup to 11 observations each and may be included in the preliminary sampleof secondary standards that has emerged from the combined programme.
| UBVRI photometry of FKSZ stars. II
The results of UBVRI photometry for 169 stars of the Faint FundamentalStars Catalog (Zverev, 1957) in the declination zone lambda of between-30 and -60 deg are presented. Observations were obtained between May1984 and February 1987 using the 50-cm ESO telescope at La Silla.Tabular data presented include the number of the star in the E-regions,the V magnitude, the (B-V), (U-B), (V-R), and (R-I) colors, and thespectral types.
| A photoelectric UBV sequence in SA 184
A photometric sequence in SA 184 is presented. A total of 135 UBVobservations have been made for 27 sequence stars. They range in B from7.1 to 20.2 and in B-V from +0.2 to +1.6. The resulting accuracy ofmagnitudes and colours should internally as well as externally be aroundor better than 0.02 magnitude for most of the data presented. Accuratecoordinates are given together with identification maps. The resultingUBV data are plotted in a two-colour diagram. Some results arediscussed.
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