Evolution of photoionization and star formation in starbursts and H1214 II galaxies

Free access article

Issue		A&A Volume 365, Number 3, January III 2001


Page(s)		347 - 359
Section		Extragalactic astronomy
DOI		http://dx.doi.org/10.1051/0004-6361:20000045

A&A 365, 347-359 (2001)
DOI: 10.1051/0004-6361:20000045

Evolution of photoionization and star formation in starbursts and H1214 II galaxies

E. Moy¹, B. Rocca-Volmerange^{1, 2} and M. Fioc^{1, 3}

¹ Institut d'Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris, France
² Institut d'Astrophysique Spatiale, Bât. 121, Université Paris XI, 91405 Orsay Cedex, France
³ NASA/Goddard Space Flight Center, code 685, Greenbelt, MD 20771, USA

(Received 17 January 2000 / Accepted 4 September 2000)

Abstract
We analyze coherently the stellar and nebular energy distributions of starbursts and HII galaxies, using our evolutionary synthesis model, PÉGASE (Fioc & Rocca-Volmerange 1997, 2000), coupled to the photoionization code CLOUDY (Ferland 1996). The originality of this study is to relate the evolution and the metallicity of the starburst to the past star formation history of the host galaxy. Extinction and geometrical effects on emission lines and continua are computed in coherency with metallicity. We compare our model predictions to an observed sample of $\approx$ 750 HII regions and starbursts. When fitting [OIII] $_{\lambda 4363}$ /[OIII] $_{\lambda 5007}$ , [OI] $_{\lambda 6300}$ /H $\alpha$ , [SII] $_{\lambda\lambda 6716, 6731}$ /H $\alpha$ , [NII] $_{\lambda 6584}$ /H $\alpha$ and [OIII] $_{\lambda 5007}$ /H $\beta$ , the most striking feature is the decreasing spread in U with increasing metallicity Z. High-U objects systematically have a low metallicity while low levels of excitation happen at any Z. The best fits of emission line ratios are obtained with a combination of a high- and a low-ionization components. No additional source of ionizing photons - shocks or hidden AGN -is needed. The high level of excitation observed in metal-poor HII galaxies requires a very young population ( $\le 3$ Myr), while starburst nuclear galaxies (SBNGs) are consistent with a wider range of age ( $\le 5$ Myr). Colors (B-V, V-R) and equivalent widths are fitted in coherency with emission line ratios. An underlying population is needed, even for small-aperture observations. This underlying population not only reddens the continuum and dilutes the equivalent width of the emission lines, but also participates in the ionization process. Its main effect on line ratios is to maintain a high level of excitation when the burst stops. Models combining underlying populations typical of Hubble sequence galaxies and instantaneous starbursts with ages between 0 and 8 Myr agree satisfactorily with all the data.

Key words: galaxies: starburst -- galaxies: evolution -- galaxies: stellar content -- ISM: HII regions

Offprint request: E. Moy, moy@iap.fr

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