Abstract
The spatial metallicity distribution in the Galaxy, as depicted by the globular cluster system, is analyzed. Two metallicity maps (on the omega-Zeta-vertical plane) corresponding to the halo and disk subsamples (Zinn 1985) have been obtained. The resulting pictures reveal the existence of a highly structured abundance pattern for the two subsystems. Variations of the metallicity with omega as well as with Zeta-vertical are clearly evidenced in both maps. However, the slope of these variations is very dependent on the direction chosen to estimate the gradient. This effect is particularly pronounced for the halo sample of globular clusters. Our results indicate that the metallicity distribution of the halo subsystem does not allow a simple description in terms of a single, direction independent gradient and that, possibly, this is the main cause of the long-standing controversy generated around the search for such a gradient. Superposed on this large-scale structure is the clearly visible presence of several metallicity patches of variable size. The most striking of them is a low-metallicity spot located at the solar galactocentric radius, which extends up to 6 kpc away from the Galactic plane.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
