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What is 4He from H II regions? What needs to be done to better understand the systematic errors?

Published online by Cambridge University Press:  23 April 2010

Gary J. Ferland ,
Yuri Izotov ,
Antonio Peimbert ,
Manuel Peimbert ,
Ryan L. Porter ,
Evan Skillman  and
Gary Steigman
Gary J. Ferland
Affiliation:
Physics, University of Kentucky, Lexington KY 40506, USA, email: gary@pa.uky.edu
Yuri Izotov
Affiliation:
Main Astronomical Observatory, 27 Acad. Zabolotnoho St, UA Kyiv 03680Ukraine email: izotov@mao.kiev.ua
Antonio Peimbert
Affiliation:
Instituto de Astronomia, UNAM Apartado Postal 70-264 Mexico 04510, D.F., Mexico, email: antonio@astroscu.unam.mx, peimbert@astroscu.unam.mx
Manuel Peimbert
Affiliation:
Instituto de Astronomia, UNAM Apartado Postal 70-264 Mexico 04510, D.F., Mexico, email: antonio@astroscu.unam.mx, peimbert@astroscu.unam.mx
Ryan L. Porter
Affiliation:
Astronomy, University of Michigan, Ann Arbor, MI USA email: ryanlporter@gmail.com
Evan Skillman
Affiliation:
Dept. of Astronomy, U of Minnesota, 116 Church St. SE, Minneapolis, MN 55455 email: skillman@astro.umn.edu
Gary Steigman
Affiliation:
Depts. of Physics and Astronomy, The Ohio State University, Columbus, OH 43210.USA email: steigman.1@osu.edu
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Abstract

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Here we summarize the discussion that took place after the presentation of papers discussing measurement of abundances from emission lines in H II regions. A cosmological test using 4He is harder than those using the other light elements due to the small dynamic range over which He/H varies for cosmologically interesting parameters. A precision of much better than 1% is needed. This precision challenges both observations and theory. Several of the major uncertainties were identified and methods of improving the accuracy were described.

Keywords

ISM: abundancesHII regionsGalaxy: abundances

Information

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S268: Light Elements in the Universe , November 2009 , pp. 163 - 167
Copyright
Copyright © International Astronomical Union 2010

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