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Structure in the Milky Way

Published online by Cambridge University Press:  02 August 2018

Trey V. Wenger ,
Dana S. Balser ,
L. D. Anderson  and
T. M. Bania
Trey V. Wenger
Affiliation:
Astronomy Department, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325, USA National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903-2475, USA
Dana S. Balser
Affiliation:
National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903-2475, USA
L. D. Anderson
Affiliation:
Department of Physics and Astronomy, West Virginia University, Morgantown, WV 26506, USA
T. M. Bania
Affiliation:
Department of Astronomy, Boston University, 725 Commonwealth Avenue, Boston, MA 02215, USA
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Abstract

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The morphological and chemical structure of the Milky Way today is an important constraint on models of the formation and evolution of the Galaxy. We use H ii regions, the sites of recent massive star formation, to probe both the Galactic spiral structure and the Galactic metallicity structure. H ii regions are the brightest objects in the Galaxy at radio wavelengths and are detected across the entire Galactic disk. We derive the distances to H ii regions using parallax measurements or by deriving kinematic distances. Here we summarize ongoing work to assess the accuracy of kinematic distances and to complete the census of Galactic H ii regions in the Southern sky.

Keywords

Galaxy: structureISM: H ii regionsradio lines: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S334: Rediscovering our Galaxy , July 2017 , pp. 381 - 382
Copyright
Copyright © International Astronomical Union 2018 

References

Anderson, L. D., Bania, T. M., Balser, D. S., & Rood, R. T., 2011, ApJS, 194, 32Google Scholar
Bania, T. M., Anderson, L. D., Balser, D. S., & Rood, R. T., 2010, ApJL, 718, L106Google Scholar
Brand, J., & Blitz, L., 1993, A&A, 275, 67Google Scholar
Brown, C., Jordan, C., Dickey, J. M., et al. 2017, AJ, 154, 23Google Scholar
Reid, M. J., Menten, K. M., Brunthaler, A., et al. 2014, APJ, 783, 130Google Scholar