========================================================================== J/A+A/448/171 BV photometry of 3 globular clusters (Hilker+, 2006) The following files can be converted to FITS (extension .fit .fgz or .fiZ) tablea?.dat ========================================================================== Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/A+A/448/171 ==========================================================================
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Beginning of ReadMe : J/A+A/448/171 BV photometry of 3 globular clusters (Hilker+, 2006) ================================================================================ Probable member stars of the gravitational theory-testing globular clusters AM 1, Pal 3 and Pal 14. Hilker M. <Astron. Astrophys., 448, 171-180 (2006)> =2006A&A...448..171H ================================================================================ ADC_Keywords: Clusters, globular ; Photometry, UBV Keywords: Galaxy: globular clusters: individual: AM 1, Pal 3, Pal 14 - astrometry - Galaxy: kinematics and dynamics Abstract: Some of the Galactic outer halo globular clusters are excellent tools to probe gravitational theories in the regime of weak accelerations. The measurement of the line-of-sight velocity dispersion among stars in these clusters will differentiate between the validity of Newtonian dynamics (low velocity dispersion) and the possibility of modified Newtonian dynamics (MOND) or dark matter dominated globular clusters (high velocity dispersion). In this paper, the properties of probable member stars of the three best-case gravitational theory-testing clusters AM 1, Pal 3 and Pal 14 are presented. The member selection is based on VLT photometry in Johnson BV. The positions of the stars were determined with an accuracy of the order of <=0.2", allowing their direct use for follow-up spectroscopy. The distance, reddening, age and metallicities of the clusters were estimated from isochrone fitting. Furthermore, improved structural parameters, like central coordinates, ellipticity, half-light radius, King model core and tidal radius, are presented. Description: The observations were performed in February 2005 with the VLT/UT1 at Paranal (ESO), Chile. The instrument in use was the FORS2 camera with a 4x4 k MIT CCD array attached. The data were read out with a 2x2 binning, resulting in a spatial scale of 0.25"/pixel and a field of view of 6.8'x6.8'. Objects: ---------------------------------------------------------- RA (2000) DE Designation(s) (file) ---------------------------------------------------------- 03 55 02.7 -49 36 52 Cl AM 1 = ESO 201- 10 (tablea1) 10 05 31.0 +00 04 15 Cl Pal 3 = UGC 5439 (tablea2) 16 10 59.0 +14 57 42 Cl Pal 14 = GCl 38 (tablea3) ----------------------------------------------------------