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Abundance analysis of targets for the COROT/MONS asteroseismology missions. I. Semi-automatic abundance analysis of the gamma Dor star HD 49434
One of the goals of the ground-based support program for the COROT andMONS/Römer satellite missions is to select and characterisesuitable target stars for the part of the missions dedicated toasteroseismology. While the global atmospheric parameters may bedetermined with good accuracy from the Strömgren indices, carefulabundance analysis must be made for the proposed main targets. This is atime consuming process considering the long list of primary andsecondary targets. We have therefore developed new software called VWAfor this task. The VWA automatically selects the least blended linesfrom the atomic line database VALD, and consequently adjusts theabundance in order to find the best match between the calculated andobserved spectra. The variability of HD 49434 was discovered as part ofCOROT ground-based support observations. Here we present a detailedabundance analysis of HD 49434 using VWA. For most elements we findabundances somewhat below the Solar values, in particular we find [Fe/H]= -0.13 +/- 0.14. We also present the results from the study of thevariability that is seen in spectroscopic and photometric time seriesobservations. From the characteristics of the variation seen inphotometry and in the line profiles we propose that HD 49434 is avariable star of the gamma Doradus type. Based on observations obtainedat Observatoire d'Haute Provence, France and at the Observatory ofSierra Nevada, Granada, Spain.
| Mesures de vitesses radiales. VIII. Accompagnement AU sol DU programme d'observation DU satellite HIPPARCOS
We publish 1879 radial velocities of stars distributed in 105 fields of4^{\circ} \times 4^{\circ}. We continue the PPO series \cite[(Fehrenbachet al. 1987;]{Feh87} \cite[Duflot et al. 1990, 1992 and 1995),]{Du90}using the Fehrenbach objective prism method. Table 1 only available inelectronic form at CDS via to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html
| Far-ultraviolet stellar photometry - A field in Monoceros
FUV photometry of stars in a field in Monoceros in the wavelength rangefrom 1230 to 1600 A has been carried out using data from anelectrographic Schmidt camera carried on a sounding rocket. Ultravioletmagnitudes were extracted for 602 objects in the field. Fifty-eightpercent were tentatively identified with visible stars using the SIMBADdata base while another 25 percent are blends of objects too closetogether to separate with our resolution. Eleven of the UV objectscoincide with parts of the star clusters NGC 2169, NGC 2244, and NGC2264 in which individual stars cannot be resolved. As in previousstudies, the majority of the identified ultraviolet sources areidentified with early-stars. However, there are a significant number forwhich no such identification was possible, and we suggest that many ofthese are nearby white dwarfs.
| Hyades and Sirius supercluster members brighter than magnitude (V) 7.1. II - Right ascension six to twelve hours
The present star sample is contained in the Bright Star Catalogue andits Supplement, augmented with a further supplement of 788 stars foundduring various observing programs over the past 40 years. Accurate,four-color and H-beta, or (RI), photometry is available for most of thesupercluster members. The criteria for membership are the comparisons ofthe proper motion, radial velocity, and luminosity obtained from thesupercluster parameters with the observed motions and the luminosityderived from the photometric parameters. New proper motions, based onall available catalogs, have been derived for the additional 788 starsdiscussed here, as well as all supercluster members.
| Stellar Spectra in Milky way Regions. V.A Region in Monoceros.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1956ApJS....2..271M&db_key=AST
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Dades d'Observació i Astrometria
| Constel·lació: | Monoceros |
| Ascensió Recta: | 06h45m50.05s |
| Declinació: | -00°42'59.3" |
| Magnitud Aparent: | 6.768 |
| Distancia: | 201.613 parsecs |
| Moviment propi RA: | -6.1 |
| Moviment propi Dec: | -4.3 |
| B-T magnitude: | 6.736 |
| V-T magnitude: | 6.766 |
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