English
 
Help Privacy Policy Disclaimer
  Advanced SearchBrowse
  1. View item / 
  2. Item Summary

Item

ITEM ACTIONSEXPORT
Add to Basket
  Local TagsRelease HistoryDetailsSummary

Released
Conference Paper

Star Formation History of the WLM dIrr

MPS-Authors

Hughes,  Joanne D.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Stetson,  Peter B.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Leaman,  Ryan
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Wallerstein,  George
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Cook,  Zalia
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

External Resource

https://ui.adsabs.harvard.edu/abs/2019AAS...23344902H
(Any fulltext)

Fulltext (restricted access)
There are currently no full texts shared for your IP range.
Fulltext (public)
There are no public fulltexts stored in PuRe
Supplementary Material (public)
There is no public supplementary material available
Citation

Hughes, J. D., Stetson, P. B., Leaman, R., Wallerstein, G., & Cook, Z. (2019). Star Formation History of the WLM dIrr. In American Astronomical Society Meeting Abstracts #233.


Cite as: https://hdl.handle.net/21.11116/0000-0005-D0E2-0
Abstract
The HI-gas-rich, WLM dwarf irregular galaxy has been forming stars for at least 11 Gyr. It is one of the nearest examples of isolated, metal- poor star formation in the Local Group, and contains a single globular cluster. We explore the spatial distribution, ages, and chemical evolution of its stellar population, particularly in the metal-poor halo, compared to the rotating bulge/disk system. We present an extensive imaging survey in BVRI filters (based largely on archival data) as a supplement to previous spectroscopy of a limited sample of giants and supergiants. In addition, a Washington-C survey has been carried out along the rotation (minor) axis into the halo, where the Washington color, C-T1(where the R-filter can be used) can be up to 3 times more sensitive to metallicity than V-I for giant-branch populations.