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

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76 3 • IFS of a GEHR in NGC 6946 1.0 0.8 0.6 0.4 0.2 0.0 log [OIII]5007/Hβ −0.8−0.6−0.4−0.2 −1.2 −0.8 −0.4 0.0 log [NII]6584/Hα −1.2 −0.8 −0.4 0.0 log [SII]6717,31/Hα Figure 3.19: Diagnostic diagrams derived from different line ratios. Left panel: Relation between [Oiii] λ 5007/Hβ and [Nii] λ 6584/Hα. Right panel: Relation between [Oiii] λ 5007/Hβ and [Sii] λλ 6717,6731/Hα. The solid curve represents the theoretical maximum starburst line (Kewley et al., 2001). It should be noted the variation of the [Oiii] λ 5007/Hβ ratio across the region, of about 0.8 dex. This is comparable with the spread found in Hii galaxies, as in the case of IIZw70 (Kehrig et al., 2008). On the other hand, the variation in the [Nii] λ 6584/Hα and [Sii] λλ 6717,6731/Hα ratios are lower. Numerically, the field average ratio of log([Oiii] λ 5007/- Hβ) = -0.08 ± 0.16, log([Nii] λ 6584/Hα) = -0.58 ± 0.07 and log([Sii] λλ 6717,6731/Hα) = -0.54 ± 0.10 (1σ errors). A spatial representation of these three line ratios is shown in Figure 3.20. For the sake of clarity and comparison, Hα is also included in the upper left panel, corrected for reddening. Unlike the reddening map, the structures that appear in the excitation maps are much simpler. In terms of the main four knots, particularly knot A, there is a very good correlation between the value of the intensity of Hα and the value of the ratio, being negative the sign of the correlation for ratios log([Sii] λλ 6717,6731/Hα) and log([Nii] λ 6584/Hα) and positive for the ratio log([Oiii] λ 5007/Hβ). As it was mentioned before, this is the expected behaviour if in the central zones of the Hii region the sulphur, nitrogen and, oxygen were twice ionized, while only once in the surroundings due to the increasing distance from the young stellar cluster or ionizing source.
60¡DEC (arcsec) 60¡DEC (arcsec) 60¡DEC (arcsec) 60¡DEC (arcsec) 3.4. Results 77 log([OIII]/Hβ) 2441 0.44 50 922 50 0.32 Hα 349 0.19 40 133 40 0.07 30 51 30 -0.06 20 20 20 -0.18 9 -0.31 10 4 10 -0.43 0 0 10 20 30 40 50 60 70 RA (arcsec) 3 0 0 10 20 30 40 50 60 70 RA (arcsec) -0.56 log([SII]/Hα) log([NII]/Hα) -0.32 -0.44 50 -0.41 50 -0.49 -0.50 -0.54 40 -0.59 40 -0.58 30 -0.68 30 -0.63 20 -0.77 20 -0.68 -0.86 -0.73 10 -0.95 10 -0.78 0 0 10 20 30 40 50 60 70 RA (arcsec) -1.04 0 0 10 20 30 40 50 60 70 RA (arcsec) -0.83 Figure 3.20: Upper left panel: Hα flux map (corrected for reddening). The scale bar is given in units of 10 −16 erg s −1 cm −2 . This map is included as reference for the excitation maps. Upper right panel: Flux ratio map of log([Oiii] λ 5007/Hβ). Lower left panel: Flux ratio map of log([Sii] λλ 6717,6731/Hα). Lower right panel: Flux ratio map of log([Nii] λ 6584/Hα).
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Facultad de Ciencias Departamento d
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A Abigaíl, mi ut A mi familia, por
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La gente del grupo de Astrofísica
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Contents List of Figures List of Ta
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CONTENTS iii B •Physical conditio
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vi LIST OF FIGURES 3.12 Example of
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List of Tables 1.1 Integrated prope
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Chapter 1 Introduction 1.1 Overview
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1.1. Overview 3 Figure 1.1: Sample
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1.1. Overview 5 These massive star
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1.1. Overview 7 Figure 1.3: Color-m
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1.2. Aims and structure of this wor
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12 2 • The star formation history
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Page 46 and 47: 26 2 • The star formation history
Page 60 and 61: 40 3 • IFS of a GEHR in NGC 6946
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126 4 • Long-slit spectrophotomet
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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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