Hostname: page-component-cb9f654ff-nr592 Total loading time: 0 Render date: 2025-09-03T11:30:13.115Z Has data issue: false hasContentIssue false
  • English
  • Français

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
Rights & Permissions [Opens in a new window]

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.

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

References

Benjamin, Robert A., Skillman, Evan D., Smits, , & Derck, P. 1999, ApJ, 514, 307CrossRefGoogle Scholar
Davidson, K. & Kinman, T. D. 1985, ApJS, 58, 321CrossRefGoogle Scholar
Gonzalez Delgado, R. M., Cervio, M., Martins, L. P., Leitherer, C., & Hauschildt, P. H. 2005, MNRAS, 357, 945CrossRefGoogle Scholar
Izotov, Y., Thuan, T., & Stasinska, G. 2007, ApJ, 662, 15CrossRefGoogle Scholar
Osterbrock, D. E. & Ferland, G. J. 2006 The Astrophysics of Gaseous Nebulae and Active Galactic Nuclei, 2nd Edition (Mill Valley; University Science Press) (ANG3)Google Scholar
Osterbrock, D. E. & Rogerson, J. B. 1961, PASP, 73, 129CrossRefGoogle Scholar
Osterbrock, D. E., 2009, in Finding the Big Bang, Peebles, P. J. E., Page, L. A. & Partridge, R. B. eds (Cambridge; Cambridge University Press), p. 86Google Scholar
Peimbert, Manuel, Luridiana, Valentina & Peimbert, Antonio 2007, ApJ, 666, 636CrossRefGoogle Scholar
Peimbert, Manuel, Peimbert, Antonio, Luridiana, Valentina, & Ruiz, Maria Teresa 2003, ASPC, 297, 81Google Scholar
Porter, R. L., Bauman, R. P., Ferland, G. J., & MacAdam, K. B. 2005, ApJ, 622, L73CrossRefGoogle Scholar
Porter, R. L., Ferland, G. J., & MacAdam, K. B. 2007, ApJ, 657, 327CrossRefGoogle Scholar
Porter, R. L., Ferland, G. J., MacAdam, K. B., & Storey, P. J. 2009, MNRAS, 393L, 36CrossRefGoogle Scholar