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

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36 2 • The star formation history of NGC 5471 19 600 20 400 m 547M 21 22 23 24 25 200 0 200 400 26 0.5 0.0 0.5 1.0 1.5 m 547M - m F675W ′ 600 400 200 0 200 400 600 600 (a) 19 600 20 400 21 200 m 547M 22 0 23 200 24 25 400 26 0.5 0.0 0.5 1.0 1.5 m 547M - m F675W ′ 600 400 200 0 200 400 600 600 (b)
2.4. Discussion 37 19 600 20 400 m 547M 21 22 23 24 25 200 0 200 400 26 0.5 0.0 0.5 1.0 1.5 m 547M - m F675W ′ 600 400 200 0 200 400 600 600 (c) 19 600 20 400 21 200 m 547M 22 0 23 200 24 25 400 26 0.5 0.0 0.5 1.0 1.5 m 547M - m F675W ′ 600 400 200 0 200 400 600 600 (d) Figure 2.11: Spatial distribution of the star formation with time. The spatial distribution of the stars within four boxes selected in the CMD are shown in the right hand side images. The images are also drawn with a circle of 15 arcsec radius, indicating the area of the integrated photometry, an ellipse delineating the core region where the present star forming event occurs, and the polygons selected for the cluster analysis. Notice how the younger stars are concentrated in the inner clusters (a) and the older stars are preferentially located in the halo (d), while intermediate age stars populate uniformly the core with some presence in the halo.
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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 and 20: List of Tables 1.1 Integrated prope
Page 21 and 22: Chapter 1 Introduction 1.1 Overview
Page 23 and 24: 1.1. Overview 3 Figure 1.1: Sample
Page 25 and 26: 1.1. Overview 5 These massive star
Page 27 and 28: 1.1. Overview 7 Figure 1.3: Color-m
Page 29: 1.2. Aims and structure of this wor
Page 32 and 33: 12 2 • The star formation history
Page 60 and 61: 40 3 • IFS of a GEHR in NGC 6946
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86 3 • IFS of a GEHR in NGC 6946
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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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