Hostname: page-component-8448b6f56d-qsmjn Total loading time: 0 Render date: 2024-04-19T19:47:41.587Z Has data issue: false hasContentIssue false
  • English
  • Français

Vertical Metallicity Gradient of the Galaxy Based on UBV Starcount Data

Published online by Cambridge University Press:  26 July 2016

T. Yamagata  and
Y. Yoshii
T. Yamagata
Affiliation:
Elementary and Secondary Education Bureau, Ministry of Education, Science and Culture, Kasumigaseki, Chiyoda, Tokyo 100, Japan
Y. Yoshii
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181, Japan

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The spatial distribution of metal abundance in the Galaxy has been analyzed using the UBV starcount data recently obtained in two high-latitude regions of the North Galactic Pole (NGP) and Selected Area 54 (SA54).

A least-squares analysis was performed to determine the vertical metallicity gradient for each of the thin and thick disk components that gives a reasonable fit to the observed U-B and B-V colour distributions to V = 18 mag. The most probable value of the vertical gradient is obtained as d[Fe/H]/dz = −0.5 kpc−1 for the thin disk, and −0.1 kpc−1 for the thick disk.

Type
Part Nine: Galactic Structure
Information
Symposium - International Astronomical Union , Volume 161: Astronomy from Wide-Field Imaging , 1994 , pp. 420 - 422
Copyright
Copyright © Kluwer 1994 

References

Stobie, R.S. and Ishida, K., 1987. Astron. J., 93, 624.Google Scholar
Yamagata, T. and Yoshii, Y., 1992. Astron. J., 103, 117.Google Scholar
Yamagata, T. and Yoshii, Y., 1994. In preparation.Google Scholar
Yoshii, Y., Ishida, K. and Stobie, R.S., 1987. Astron. J., 93, 323.Google Scholar