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

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80 3 • IFS of a GEHR in NGC 6946 60¡DEC (arcsec) 50 40 30 20 10 0 0 10 20 30 40 50 60 70 RA (arcsec) 60¡DEC (arcsec) 50 40 30 20 10 0 0 10 20 30 40 50 60 70 RA (arcsec) Figure 3.22: Wolf-Rayet (WR) spatial distribution. The filled dark (violet) regions represent the fiber detections of the blue WR bump. On the upper panel the Hα contours are overplotted, while in the lower panel the continuum contours near the WR emission (∼ λ 4500 Å) are shown. The filled regions only represent positions of the WR stars in the field, not intensity.
3.4. Results 81 ID log L(bb) I(bb) a -EW(bb) (erg · s −1 ) Å Knot A 38.58 ± 0.04 20.3 ± 1.7 14.0 ± 1.2 Knot B 37.41 ± 0.06 27.4 ± 3.5 25.5 ± 3.3 Knot C 37.90 ± 0.05 22.7 ± 2.8 16.4 ± 2.9 Knot D · · · · · · · · · a In units of 100 · I(Hβ) Table 3.3: Luminosities, relative intensities and equivalent widths of the Wolf-Rayet features measured on the integrated spectra of four knots at 4650 Å (blue bump, bb). All quantities have been corrected for reddening. 3.4.8 Physical properties and chemical abundances from the integrated spectra In order to study the mean properties of the Hii complex, several integrated spectra were obtained from the PPak-field. As we have seen in Figure 3.14, there are four main Hα intense knots. These structures have enough signal-to-noise to perform an analysis of the physical properties of the gas and their abundances. Unfortunately, auroral lines with acceptable errors were not found in individual fibers; enough signal-to-noise to measure these weak lines was achieved only in the integrated spectrum of each knot. In section 3.3.8 we have seen that a complete mosaic of 993 spectra was accomplished for the blue range (3700-7000 Å), while for the red data (7000-10000 Å) we had only one pointing of 331 spectra, since there was a problem with the guiding and de-rotator. Therefore, in order to take advantage of all the relevant emission lines available, we had to build the integrated spectrum for each knot from the first blue and red pointing. Since the FOV for one pointing is not completely covered by all the fibers (see Figure 3.8, for example), we cannot expect to obtain absolute fluxes. Nevertheless, we can assume that the relative intensities of the lines should be similar, so that the derived properties and abundances should not be different within the errors. The spatial limits of each of the four knots were defined in the Hα map by means of visual inspection with the help of isocontour plots. The limit contour is at the 20-30% of the maximum peak. In order to have a better definition, we used the Hα map built from the mosaic (3 pointings). Then, once the knots were defined, we co-added all the fibers belonging to each knot in the mosaic exposure, obtaining four, absolute flux calibrated, integrated spectra. It is important to ensure that the integrated spectra of each knot in the one dithering exposure is built coming from exactly the same area. Performing this task is another advantage of IFU data, since each fiber is perfectly identified. From the mosaic integrated spectra we had the ID of the fibers, and therefore the fibers coming from each of the three ditherings. Thus, we co-added the fibers coming from the first blue and red
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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 50 and 51: 30 2 • The star formation history
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130 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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