Two populations among the metal-poor field RR Lyrae stars

We compute the spatial velocity components and the galactic orbital elements for 209 metal-poor ((Fe/H) < −1.0) RRLyrae (ab) variable stars in the solar neighborhood using proper motions, radial velocities, and photometric distances avail- able in the literature. The computed orbital elements and published heavy element abundances are used to study relationships between the chemical, spatial, and kinematical characteristics of nearby field RR Lyrae variables. We observe abrupt changes in the stellar spatial and kinematical characteristics when the peculiar velocities relative to the local standard of rest cross the threshold value, Vpec ≈ 280 kms −1 . This provides evidence that the general population of metal-poor RRLyrae stars is not uniform, and includes two spherical subsystems occupying different volumes in the Galaxy. Based on the agreement between typical parameters of corresponding subsystems of field RRLyrae stars and of the globular clusters, studied by us earlier, we conclude that metal-poor stars and globular clusters can be subdivided into two populations, but using different criteria for stars and clusters. We suppose that field stars with velocities below the threshold value and clusters with extremely blue horizontal branches form the spherical, slowly rotating subsystem of the proto-disk halo (related by its origin to the Galactic thick disk). It has a negligible, but non-zero, vertical metallicity gradient. Field stars with fast motion and clusters with redder horizontal branches constitute the spheroidal subsystem of the accreted outer halo, which is approximately two times larger in size than the first subsystem. It has absolutely no metallicity gradients, most of its stars have eccentric orbits, many stars display retrograde motion in the Galaxy, and their ages are comparatively low, supporting the hypothesis that the objects in this subsystem have an extragalactic origin. The presence of two different populations with separate histo- ries in the metal-poor halo was suggested by Hartwick (1987). He showed that model of the dynamics of RR Lyrae variables with metallicities (Fe/H) < −1.0 required two components: one sphericaland a somewhatflattened componentthat is dom- inant at galactocentricdistances less than the radius of the solar circle. The idea that there are two subsystems in the metal-poor halo has already been addressed in several investigations fo- cused on globular clusters. It turned out that globular clusters present a distinctive inner feature (the morphologyof their hor- izontal branches), which makes it possible to distinguish the individual metal-poor clusters in terms of different halo sub- systems. It was found that halo clusters that have redder hor- izontal branches for a given metallicity (i.e. with horizontal branches showing a considerable number of stars on the low- temperature side of the Schwarzschild gap), are predominantly outside the solar circle. Furthermore, they exhibit larger veloc- ity dispersion, slower circular velocity (a significant number having retrograde orbits), and are, on average, younger than clusters with extremely blue horizontal branches, which are