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

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144 4 • Long-slit spectrophotometry of multiple knots of Hii galaxies 100 80 A 60 40 20 mass fraction (%) 0 6 7 8 9 10 80 B 60 40 20 0 6 7 8 9 10 80 C 60 40 20 0 6 7 8 9 10 log(Age) 100 80 A 60 40 20 light fraction (%) 0 80 60 40 20 6 7 8 9 10 B 0 6 7 8 9 10 80 C 60 40 20 0 6 7 8 9 10 log(Age) Figure 4.20: Histogram of the distribution in mass fraction (upper) and visual light (bottom) of the most probable stellar population models fitted by STARLIGHT for each of the observed knots of J1657.
4.4. Discussion 145 ID A(V) c(Hβ) M ∗ f(age < 10 Myr) (mag) (M ⊙ ) (%) IIZw71 Knot A 0.41 0.19 1.4×10 6 0.08 IIZw71 Knot B 0.99 0.46 8.3×10 6 0.11 IIZw71 Knot C 0.09 0.04 3.3×10 7 0.008 IIZw71 Knot D 0.54 0.25 2.9×10 6 0.013 J1657 Knot A 0.18 0.08 2.8×10 8 0.58 J1657 Knot B 0.00 0.00 1.0×10 8 0.21 J1657 Knot C 0.00 0.00 1.4×10 8 0.28 Table 4.9: Values of the extinction, total stellar mass, and fraction of the mass in stars younger than 10 Myr for each knot of IIZw71 and J1657 in the best-fit model predicted by STARLIGHT. Table 4.9 for all the knots, together with the internal extinction, represented by A(V) (as given by STARLIGHT) and the reddening constant (using the transformations of Appendix A), estimated by the model. For IIZw71, the masses were corrected using an aperture factor, which takes into account the light not collected by the slit and which was calculated as the weighted mean of the ratios of the light in the whole region as measured in the Hα image and in the regions covered by the slit. In the case of J1657, no aperture correction factors have been taken into account for the Hα luminosities, due to the compact nature of the object. Indeed, the discrepancy factors between our Hα luminosities for Knot A and those measured in the SDSS catalogue using a 3 arcsec fiber is not larger than 1.3. Although it is not expected to find the same values of extinction in the gas and the stellar population, there is a very good agreement between the values of the extinction estimated by STARLIGHT in knots C and D of IIZw71 in relation to the values obtained from the decrement of Balmer. In J1657, although the behaviour of the extinction is inverted, being larger in knot A that in B and C, the opposite from the derived values using the decrement of Balmer, the general result is consistent with low extinction. In knots A and B of IIZw71, the values are higher than those derived for the ionized gas. In these two knots the specific weight of the youngest population is higher. Since STARLIGHT assumes a common source of extinction for all the stellar populations entering the fit, the degeneracy between age and extinction tends to overestimate the extinction derived for the optimal fit. On the other hand, in knots C and D, which are probably contaminated by the light coming from the host galaxy, the contribution by the young stellar population is much lower, and the light at longer wavelengths is dominated by the older stellar population and the estimated average extinction is more representative.
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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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40 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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Page 176 and 177: 156 Conclusiones Las abundancias to
Page 178 and 179: 158 Conclusiones consistentes con l
Page 180 and 181: 160 Appendix A where c=0.434C. This
Page 182 and 183: 162 Appendix B where R S2 = I(6717
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Page 189 and 190: Appendix C Empirical calibrators In
Page 191 and 192: C • Empirical calibrators 171 One
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Page 195 and 196: D • Stellar photometry results of
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Page 210 and 211: 190 REFERENCES Bertelli, G., Bressa
Page 212 and 213: 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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