========================================================================== J/AJ/132/714 QUEST RR Lyrae survey. II. Halo overdensities (Vivas+, 2006) The following files can be converted to FITS (extension .fit .fgz or .fiZ) table2.dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/AJ/132/714 ==========================================================================
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Beginning of ReadMe : J/AJ/132/714 QUEST RR Lyrae survey. II. Halo overdensities (Vivas+, 2006) ================================================================================ The QUEST RR Lyrae survey. II. The halo overdensities in the first catalog. Vivas A.K., Zinn R. <Astron. J., 132, 714-728 (2006)> =2006AJ....132..714V ================================================================================ ADC_Keywords: Stars, variable ; Positional data ; Stars, distances Keywords: Galaxy: halo - Galaxy: structure - stars: variables: other Abstract: The first catalog of the RR Lyrae stars (RRLSs) in the Galactic halo by the Quasar Equatorial Survey Team (QUEST) has been searched for significant overdensities that may be debris from disrupted dwarf galaxies or globular clusters. These RRLSs are contained in a band 23 wide in declination that spans 165deg in right ascension and lie 4 to 60kpc from the Sun. Away from the major overdensities, the distribution of these stars is adequately fitted by a smooth halo model, in which the flattening of the halo decreases with increasing galactocentric distance (as reported by Preston et al., 1991ApJ...375..121P). This model was used to estimate the background of RRLSs on which the halo overdensities are overlaid. A procedure was developed for recognizing groups of stars that constitute significant overdensities with respect to this background. To test this procedure, a Monte Carlo routine was used to make artificial RRLS surveys that follow the smooth halo model but with Poissondistributed noise in the numbers of RRLSs and, within limits, random variations in the positions and magnitudes of the artificial stars. The 104 artificial surveys created by this routine were examined for significant groups in exactly the same way as the QUEST survey.