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HII radiative transfer revealed by ionization parameter mapping

Published online by Cambridge University Press:  05 March 2015

M. S. Oey ,
E. W. Pellegrini ,
P. F. Winkler ,
S. D. Points ,
R. C. Smith ,
A. E. Jaskot  and
J. Zastrow
M. S. Oey
Affiliation:
Astronomy Department, University of Michigan, Ann Arbor, MI 48109-1042, USA
E. W. Pellegrini*
Affiliation:
Astronomy Department, University of Michigan, Ann Arbor, MI 48109-1042, USA
P. F. Winkler
Affiliation:
Department of Physics, Middlebury College, Middlebury, VT 05753, USA
S. D. Points
Affiliation:
Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile
R. C. Smith
Affiliation:
Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile
A. E. Jaskot
Affiliation:
Astronomy Department, University of Michigan, Ann Arbor, MI 48109-1042, USA
J. Zastrow
Affiliation:
Astronomy Department, University of Michigan, Ann Arbor, MI 48109-1042, USA
*
†Present address: Dept of Physics & Astronomy, University of Toledo, Toledo, OH 43606-3390
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Abstract

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We develop the technique of ionization parameter mapping (IPM) to probe the optical depth of Hii regions, applying our method to the Magellanic Clouds. Our results dramatically clarify the radiative transfer in these galaxies. Based on Sii, Oiii, and Hα imaging from the Magellanic Clouds Emission Line Survey, we find that the frequency of optically thin objects correlates strongly with Hα luminosity and correlates inversely with Hi column density. The aggregate escape fraction for the Lyman continuum is sufficient to ionize the diffuse, warm ionized medium, but the galactic escape fraction is dominated by the few largest Hii regions. The quantitative trends are similar in both the LMC and SMC in spite of their different star formation and Hi properties.

Keywords

radiative transferstars: early-typeHii regionsgalaxies: ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Highlights H16: Highlights of Astronomy , August 2012 , pp. 587 - 589
Copyright
Copyright © International Astronomical Union 2015 

References

Arthur, S. J., Henney, W. J., & Mellema, G., et al. 2011, MNRAS 414, 1747Google Scholar
Beckman, J. E., Rozas, M., Zurita, A., Watson, R. A., & Knapen, J. H. 2000, AJ 119, 2728Google Scholar
Castellanos, M., Díaz, A. I., & Tenorio-Tagle, G. 2002, ApJ (Letters) 565, L79CrossRefGoogle Scholar
Hanish, D. J., Oey, M. S., Rigby, J. R., de Mello, D. F., & Lee, J. C. 2010, ApJ 725, 2029CrossRefGoogle Scholar
Hoopes, C. G. & Walterbos, R. A. M. 2000, ApJ 541, 597Google Scholar
Oey, M. S., King, N. L., & Parker, J. Wm. 2004, AJ 127, 1632CrossRefGoogle Scholar
Oey, M. S., Meurer, G. R., & Yelda, S., et al. 2007, ApJ 661, 801CrossRefGoogle Scholar
Pellegrini, E. W., Oey, M. S., Winkler, P. F., Points, S. D., Smith, R. C., Jaskot, A. E., & Zastrow, J. 2012, ApJ 755, 40; Erratum, astro-ph/1202.3334.CrossRefGoogle Scholar
Seon, K.-I. 2009, ApJ 703, 1159CrossRefGoogle Scholar
Smith, R. C., Points, S. D., & Chu, Y.-H., et al. 2005, BAAS 37, 1200Google Scholar
Voges, E. S., Oey, M. S., Walterbos, R. A. M., & Wilkinson, T. M. 2007, AJ 135, 1291Google Scholar
Wood, K. & Mathis, J. S. 2004, MNRAS 353, 1126Google Scholar
Walterbos, R. A. M. 1998, PASA 15, 99CrossRefGoogle Scholar
Zastrow, J., Oey, M. S., Veilleux, S., McDonald, M., & Martin, C. L. 2011, ApJ (Letters) 741, L17Google Scholar
Zastrow, J., Oey, M. S., & Pellegrini, E. W. 2012, ApJ, submittedGoogle Scholar