%R 1997A&AS..121..405P %J-406 %A Prieto C. %T Micrometer measurements of southern double stars made at the Observatory of Llano del Hato at Merida (Venezuela). %M DS1228 %F 1997.02.07 %B We present 93 micrometer measurements of 46 double stars observed with the 65 cm refractor at the Llano del Hato Observatory (Merida, Venezuela). %K binaries: visual - astrometry %R 1997A&AS..121..407L %J-438 %A Leisy P., Dennefeld M., Alard C., Guibert J. %T Accurate positions and finding charts of known planetary nebulae in the Large Magellanic Cloud. %M DS1072 %F 1997.02.07 %B We present identifications and accurate positions for about 280 planetary nebulae (PNe) in the Large Magellanic Cloud (LMC). These positions are needed for follow-up ground or space observations. Entire Schmidt plates have been scanned with the MAMA micro-densitometer, and PPM stars used for the astrometric reduction. The precision achieved is always better than 0.5", and better than 0.3" for most of the objects not located close to the border of the plates. Photometry in the B band is provided with an accuracy of about 0.2-magnitude, except in too crowded zones where the background cannot be determined. Cross-identifications with IRAS sources have also been tabulated and discussed. %K planetary nebulae: general - galaxies: Magellanic Clouds - galaxies: ISM; stellar content -- astrometry %R 1997A&AS..121..439K %J-450 %A Kharchenko N., Scholz R.-D., Lehmann I. %T Membership and structural parameters of the globular cluster M 5 from Schmidt plates. %M DS5139 %F 1997.02.07 %B Using absolute proper motions derived from APM measurements of Tautenburg, Palomar and UK Schmidt plates (cf. Scholz et al. 1996MNRAS.278..251S) we determined membership probabilities of the globular cluster M 5 in a four-dimensional space of proper motions and coordinates. The solution for 19 unknown parameters was obtained by the maximum likelyhood method. Different mean absolute proper motions and dispersions were found for three distribution functions of the cluster stars, near field stars and distant field stars. In addition to the four-dimensional distribution functions, we also investigated two-dimensional distribution functions including either only the proper motions or only the coordinates. We compared the results with the colour-magnitude diagram obtained from a B,V photographic photometry using two of the Tautenburg plates and with the membership determination of Rees (1993AJ....106.1524R). In comparison to the last work based on observations with larger epoch differences and better astrometric scale, our results are less accurate but extend the membership investigation of M 5 to fainter stars (B=19) and to the outer regions of the cluster. The full APM scans of the different Schmidt plates were also used for star counts applying a crowding correction in the central cluster region based on the area of crowded images and on the stellar luminosity function in the outer cluster region. The tidal radii from fitting King profiles to the counts of all objects on the plates and of the cluster members are discussed. From the deep counts of the full scans we found an indication of a tidal tail around M 5 (cf. Grillmair et al. 1995). However, this effect was not confirmed by the member counts. %K astrometry - methods: statistical - globular clusters: individual: M 5 - stars: kinematics %R 1997A&AS..121..451G %J-454 %A Guarnieri M.D., Carraro G. %T VI photometry of the galactic cluster Berkeley 66. %M DS5212 %F 1997.02.07 %B A colour magnitude diagram (CMD) extending to V=~19mag is given for 444 stars in the region of the galactic cluster Berkeley 66. The V and I photometry of a nearby field is also reported. This object appears very faint, highly contaminated by foreground stars and very reddened. The apparent distance modulus (m-M) and the colour excess E_V-I_ are guessed to be 17.5 and 1.1, respectively, with an uncertainty of at least 30%. Adopting these values the comparison of the CMD with theoretical isochrones from the Padova group provides an age around 1.0Gyr. %K open clusters: individual: Cl Berkeley 66 - HR diagram %R 1997A&AS..121..455K %J-460 %A Kaluzny J. %T CCD photometry of distant open clusters. III. Berkeley 18. %M DS5190 %F 1997.02.07 %B We present CCD BVI photometry for Berkeley 18, a rich open cluster located in the Galactic anticenter. The cluster age is similar to, or mariginally lower than age of M 67. Its distance is estimated at 5.8kpc and the reddening E(B-V) is probably higher than 0.46. Our data indicate that Be 18 is one of the most populous objects in the whole sample of known galactic open clusters. The angular diameter of the cluster is estimated at 26arcmin, which corresponds to a linear size of about 44pc. The horizontal branch of Be 18 exhibits a large width in comparison with other old open clusters. %K open clusters and associations: individual: Cl Berkeley 18 - HR diagram %R 1997A&AS..121..461R %J-487 %A Recondo-Gonzalez M.C., Wamsteker W., Clavel J., Rodriguez-Pascual P.M., Vio R., Wang T.-G., Santos-Lleo M., Makino F. %T Ultraviolet variability of the Seyfert 1 galaxy Fairall 9. %M DS1182 %F 1997.02.07 %B The large amplitude of the variations of the Seyfert I Galaxy Fairall-9 between 1978 and 1991 make this Active Galaxy especially suitable for a combined study in terms of reverberation analysis and photoionization modeling over the velocity field of the broad lines of its ultraviolet spectrum. We have combined our ultraviolet data with those available at other wavelengths to derive the intrinsic ionizing continuum and to compare the predictions of the photoionization models with the observations. The UV continuum varies with a factor of 33 +/- 4 on a characteristic time scale of 182 days. The intrinsic spectral index UV-optical is {alpha}=-0.07 +/-0.02 and the optical variations do not lag behind the UV variations at the mean sampling interval of 96 days. In the near IR, the J band flux presents a direct extension of the UV-optical continuum ( {alpha}_J-UV_=-0.07 +/- 0.05). Only at low flux levels is the 2-10 keV flux proportional to the UV continuum, at higher UV flux levels proportionality between the X-rays and the UV brightness breaks down. The continuum spectral energy distribution (SED) of the nucleus supports the previously reported FIR-NIR excess associated with 0.02 M_{sun}_ dust at a distance of some 400 +/-100 light-days, as well as a soft X-ray excess, possibly associated with the reprocessing on an accretion disk of the hard X-rays emitted from a region above the disk. The presence of strong Fe K {alpha} line in the GINGA spectra of this galaxy does lend support to this model. Line profile variability has been used to isolate four gaussian line components, which are sufficient to describe all lines at all levels of brightness in a consistent way: one narrow (i.e. unresolved at the IUE resolution), and three broad components: a central (velocity same as the narrow line), a red shifted (v=3300 km.s^-1^) and a blue shifted (v =-3600 km.s^-1^) one. The three broad components are strongly correlated with the UV continuum, indicating that photoionization is the dominant mechanism in the BLR. Correlation analysis shows different delays between the broad components and the UV continuum: respectively, 400 +/-100, -4 +/-70 and 230 +/-95 days for the central, red and blue one. Only the red component of Ly{alpha}{lambda}1216 and CIV{lambda}1549 appear to vary linearly with the continuum and give significant transfer functions. The resulting transfer functions are peaked at zero days delay and are unresolved at the average time resolution (96 days) of our data. The photoionization models (CLOUDY) applied to the line ratios in these components, indicate that the Broad-Line-Region (BLR) is situated between 50-250 light-days from the ionizing source, with an hydrogen density of 10^12-10^ cm^-3^, a column density of 10^23-26^ cm^-2^ and a covering factor of 12-2%, with an ionization parameter between 0.003 and 0.089. However, no optically thick model reproduces the Ly{alpha}/CIV and Ly{alpha}/NV ratios. From these results we propose a model for the structure and dynamics of the BLR: the mass of the central compact object is M =~2x10^8^ M_{sun}_. Around this exist two distinct gas zones within the BLR: the gas producing the central component at =~200 light-days and gas, emitting the red and the blue components, at =~80 light-days moving inward to a central source. These results require that both these gas zones be localized along the line-of-sight or, alternatively, that the continuum emission must be strongly anisotropic. Besides, the gas emitting the central component is most likely mixed with the dust and the central gas to dust mass ratio is Mass (central gas)/mass(dust) = 100 - 750. %K galaxies: individual (Fairall 9) - galaxies: Seyfert - ultraviolet: spectra %R 1997A&AS..121..489P %J-497 %A Piironen J., Magnusson P., Lagerkvist C.-I., Williams I.P., Buontempo M.E., Morrison L.V. %T Physical studies of asteroids. XXXI. Asteroid photometric observations with the Carlsberg Automatic Meridian Circle. %M DSH0094 %F 1997.02.07 %B Photometric observations of 74 asteroids obtained with the Carlsberg Automatic Meridian Circle between January 1990 and December 1993 are presented. The data from individual asteroid apparitions have been fitted by phase curves based on the standard HG magnitude system. Statistics on mean G-values for different types of asteroids are presented. A few new determinations of asteroid rotation periods are presented. In addition, we analyse magnitude-aspect relations, and derive ellipsoidal shape models for some asteroids. %K minor planets - photometry %R 1997A&AS..121..499B %J-505 %A Borissova J., Markov H., Spassova N. %T CCD photometry of the globular cluster Palomar 13. %M DS1164 %F 1997.02.07 %B A new CCD photometry of the halo cluster Palomar 13 is used to construct a color-magnitude diagram in the Thuan-Gunn and the B, V photometric systems. The color-magnitude diagram of the cluster shows as already noted by Ortolani et al. (1985AJ.....90..473O) an extremely poor red horizontal branch and a very sparsely populated giant branch. Seven BSS candidates are identified in the field of Palomar 13. The age of the cluster determined by fitting with the isochrones of Proffitt & Vanden Berg (1991ApJS...77..473P) and Bergbusch & Vanden Berg (1992ApJS...81..163B) and by a differential comparison of the color-magnitude diagram with that of Pal 5 is 12+/-2Gyr. %K globular clusters: individual: Palomar 13 - Hertzprung - Russel diagram %R 1997A&AS..121..507B %J-551 %A Boselli A., Tuffs R.J., Gavazzi G., Hippelein H., Pierini D. %T Near infrared surface photometry of late-type Virgo cluster galaxies. %M DS1135 %F 1997.02.07 %B Near Infrared (K' band) surface photometry has been obtained for 102 (88 late-type) Virgo cluster galaxies. A subset of 20 galaxies was also imaged in the H band. Magnitudes and diameters within the 21.5 and 22.0mag/arcsec^2^ isophote, concentration indices and total H and K' magnitudes are derived. Basic statistical properties of a complete sample of spiral galaxies spanning the range 6.3