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

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82 3 • IFS of a GEHR in NGC 6946 pointing for each knot. Finally, we built an integrated spectrum over the full FOV of our IFS dataset, both from the mosaic and from the one pointing data. Therefore, we ended up with ten spectra: five absolute flux calibrated spectra from the mosaic data covering the range 3700-7000 Å for the four main knots and the whole FOV, and other five spectra of the same areas coming from the blue and red first pointing covering the range 3700-10000 Å. All the fibers containing WR features were included in these integrated spectra, since the WR positions are near the peak of Hα, as shown in Figure 3.22. The spectra of the four knots (labelled from A to D) and the integrated spectrum of the whole PPak-field with some of the relevant identified emission lines are shown in Figures 3.23 (Knot A and B), 3.24 (Knot C and D) and 3.25 (PPak-field). The spectrum of each knot is split into two panels. All of them come from the blue and red first pointing. Line intensity ratios for the most relevant emission lines were measured in each spectrum using the splot task in IRAF following the procedure described in Hägele et al. (2006). A pseudo-continuum has been defined at the base of the hydrogen emission lines to measure the line intensities and minimize the errors introduced by the underlying population. As we have seen in section 3.4.1, this procedure gives the same results, within the observational errors, as fitting synthetic SSP models to the continuum. Since we had to measure auroral lines, we decided to measure manually all the lines. The statistical errors associated with the observed emission fluxes have been calculated using the same procedure as described in section 3.4.2 (see expression there). As reported in section 3.3.9, the [Siii] λ 9532 Å line is affected by strong narrow water vapour lines and therefore its value has been set to 2.44, its theoretical ratio to the weaker [Siii] λ 9069 Å. The reddening coefficient c(Hβ) has been calculated using the same procedures as described in section 3.4.4. The only difference is that an iterative method to estimate the temperature and density has been used in each case when the appropriate lines were available. To minimize the errors and to follow a similar approach as when deriving the maps, we have estimated c(Hβ) only by means of Hα and Hβ. Tables 3.4, 3.5 and 3.6 give the equivalent widths and the reddening-corrected emission line fluxes for six integrated spectra together with the reddening constant and its error, taken as the uncertainty of the least-squares fit and the reddening-corrected Hβ intensity. The adopted reddeningcurve, f(λ), normalized to Hβ, is given in column 2 of each table. The errors in the emission lines were obtained by propagating in quadrature the observational errors in the emission-line fluxes and the reddening constant uncertainties. Table 3.4 presents the results for the integrated spectra from the entire PPak FOV for the mosaic exposure (PPak field Mosaic) and for the blue and red first pointing (PPak field Mosaic). As it can be seen, the relative intensities and equivalent widths are in very good agreement, within the errors, confirming the previous assumption. Tables 3.5 and 3.6 show the results for the integrated spectra from the blue and red first
3.4. Results 83 ◦A−1 ) s−1 Flux (erg cm−2 1e−15 8 7 6 5 4 3 2 1 [OII]3727 Knot A 4000 4500 5000 5500 6000 6500 1e−15 HδHγ [OIII]4959 [OIII]5007 Hβ HeI 5876 [SII] 6717,6731 Hα ◦A−1 ) s−1 Flux (erg cm−2 4 3 2 1 HeI 7065 [ArIII] 7136 [OII] 7319,7330 0 7000 7500 8000 8500 9000 Wavelength (◦A) [SIII]9069 ◦A−1 ) s−1 Flux (erg cm−2 1e−16 8 7 Knot B 6 5 4 3 2 1 0 4000 4500 5000 5500 6000 6500 1e−16 [OII]3727 HδHγ β[OIII]4959 H [OIII]5007 HeI 5876 [SII] 6717,6731 Hα ◦A−1 ) s−1 Flux (erg cm−2 2.4 1.8 1.2 0.6 [ArIII] 7136 0.0 7000 7500 8000 8500 9000 Wavelength (◦A) [SIII]9069 Figure 3.23: Blue and red spectra for the knots A and B.
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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 52 and 53: 32 2 • The star formation history
Page 60 and 61: 40 3 • IFS of a GEHR in NGC 6946
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132 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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