A spatially resolved study of ionized regions in galaxies at different ...

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x LIST OF TABLES 4.3 Relative observed and reddening corrected line intensities for the different observed knots of IIZw71 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 122 4.4 Relative reddening corrected line intensities for the three knots of J1657 . . . 123 4.5 Electron densities and temperatures for the knots of J1657 and IIZw71 . . . 126 4.6 Ionic and total chemical abundances for helium for the knots of J1657 . . . . 128 4.7 ICFs, ionic and total chemical abundances for the knots of J1657 . . . . . . . 130 4.8 ICFs, ionic and total chemical abundances for knots B and C of IIZw71 . . . 131 4.9 Values of the extinction, total stellar mass, and mass fraction predicted by STARLIGHT . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 145 4.10 Derived properties of the observed knots from the Hα fluxes . . . . . . . . . 146 D.1 Stellar photometry results of NGC 5471. . . . . . . . . . . . . . . . . . . . . . 187
Chapter 1 Introduction 1.1 Overview On the large scale, stars are the basic building blocks of galaxies. They are responsible for the generation of metal elements. The birth of new stars has a significant impact on the surrounding interstellar medium (ISM), the main material within galaxies. This medium is made up of several components. The more complex constituents are dust and gas. This gas is a mix of complex elements formed both during a star’s life (via nuclear processes) and during its death (supernovae). By far, the most ubiquitous components are the three forms of hydrogen. The simplest form is atomic hydrogen (H) (T ≈ 100K and n p ≈ 10 6 - 10 9 particles m −3 ), followed by molecular hydrogen (H2) (T ≈ 5 - 30K and n p > 10 9 particles m −3 ) and finally ionized hydrogen (H + ). The molecular hydrogen is the component of the ISM from which stars form. Massive young stars emit most of their radiation in the ultraviolet part of the spectrum. Some of these photons will dissociate and ionize the molecular hydrogen and will be absorbed by the surrounding gas out to considerable distance. These ionized regions are called Hii regions, very easily detectable in the sky and cradles of active star formation. Star formation is an ongoing process in the local universe, with observed rates of the order of 10 −2 M ⊙ yr −1 Mpc −3 (Madau et al., 1996). Most of the light and metals are produced in the most massive among the newly formed stars. The most extreme regions forming massive stars are often referred to as starbursts. In the local universe they account for about a quarter of all star formation (Heckman, 1997), and this fraction may be larger in the younger universe. 1
Page 1: Facultad de Ciencias Departamento d
Page 5: A Abigaíl, mi ut A mi familia, por
Page 8 and 9: La gente del grupo de Astrofísica
Page 11 and 12: Contents List of Figures List of Ta
Page 13: CONTENTS iii B •Physical conditio
Page 16 and 17: vi LIST OF FIGURES 3.12 Example of
Page 19: List of Tables 1.1 Integrated prope
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Page 25 and 26: 1.1. Overview 5 These massive star
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50 3 • IFS of a GEHR in NGC 6946
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β[H 84 3 • IFS of a GEHR in NGC
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106 4 • Long-slit spectrophotomet
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Hδ 116 4 • Long-slit spectrophot
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Table 4.4 continued SDSS J1657 Knot
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150 Conclusions and future work has
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152 Conclusions and future work oth
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154 Conclusions and future work The
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156 Conclusiones Las abundancias to
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158 Conclusiones consistentes con l
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160 Appendix A where c=0.434C. This
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162 Appendix B where R S2 = I(6717
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164 Appendix B Sulphur As in the ca
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166 Appendix B Argon For argon, the
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Appendix C Empirical calibrators In
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C • Empirical calibrators 171 One
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Appendix D Stellar photometry resul
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D • Stellar photometry results of
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190 REFERENCES Bertelli, G., Bressa
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192 REFERENCES Girardi, L. & Bertel
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194 REFERENCES Kunth, D. & Sargent,
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196 REFERENCES Pérez-Montero, E.,
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198 REFERENCES Terlevich, R., Melni
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