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

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28 2 • The star formation history of NGC 5471 X Y R.A. Decl. m F 547M m F 675W ′ m F 547M − m F 675W ′ ID pixel pixel (J2000) (J2000) (mag) (mag) (mag) 1 359.56 562.57 14:04:27.50 54:23:41.53 24.24 ± 0.07 23.45 ± 0.05 0.79 ± 0.09 2 324.75 512.37 14:04:27.56 54:23:47.59 24.57 ± 0.10 23.93 ± 0.07 0.65 ± 0.12 3 352.44 544.56 14:04:27.57 54:23:43.36 24.05 ± 0.07 23.95 ± 0.06 0.09 ± 0.09 4 332.62 514.12 14:04:27.61 54:23:46.96 24.59 ± 0.09 24.88 ± 0.19 -0.30 ± 0.21 5 378.56 569.56 14:04:27.62 54:23:39.79 24.04 ± 0.06 23.62 ± 0.06 0.42 ± 0.08 6 323.33 496.44 14:04:27.66 54:23:48.91 24.07 ± 0.06 24.13 ± 0.12 -0.06 ± 0.14 7 373.56 553.15 14:04:27.69 54:23:41.37 24.18 ± 0.07 23.24 ± 0.05 0.94 ± 0.09 8 293.29 455.69 14:04:27.69 54:23:53.94 23.62 ± 0.05 22.57 ± 0.03 1.05 ± 0.06 9 351.67 523.45 14:04:27.71 54:23:45.04 23.85 ± 0.07 23.87 ± 0.11 -0.02 ± 0.13 10 290.75 449.59 14:04:27.71 54:23:54.57 23.86 ± 0.06 23.02 ± 0.04 0.84 ± 0.07 11 368.80 540.45 14:04:27.74 54:23:42.65 23.14 ± 0.03 23.24 ± 0.04 -0.10 ± 0.05 12 346.68 513.49 14:04:27.74 54:23:46.12 25.26 ± 0.15 24.89 ± 0.17 0.38 ± 0.23 13 381.63 555.86 14:04:27.75 54:23:40.66 24.08 ± 0.07 24.18 ± 0.11 -0.10 ± 0.13 14 360.90 530.61 14:04:27.75 54:23:43.91 23.96 ± 0.06 24.09 ± 0.09 -0.14 ± 0.10 15 318.82 469.76 14:04:27.81 54:23:51.25 25.22 ± 0.15 25.04 ± 0.20 0.18 ± 0.26 16 312.47 461.48 14:04:27.81 54:23:52.29 23.20 ± 0.04 23.22 ± 0.04 -0.02 ± 0.05 17 291.51 435.95 14:04:27.81 54:23:55.57 25.38 ± 0.21 25.23 ± 0.19 0.16 ± 0.28 18 359.87 517.56 14:04:27.83 54:23:44.98 24.20 ± 0.09 24.26 ± 0.10 -0.06 ± 0.13 19 354.84 509.85 14:04:27.84 54:23:45.89 24.02 ± 0.06 23.67 ± 0.05 0.34 ± 0.08 20 319.56 460.53 14:04:27.88 54:23:51.91 24.45 ± 0.08 24.87 ± 0.20 -0.42 ± 0.22 Table 2.5: Stellar photometry of the first 20 stars of the resulting clean CMD of NGC 5471. (b) the field stars, panel (c) the decontaminated CMD of NGC 5471 and panel (d) the CMD of the stars rejected. Table 2.5 shows the magnitudes of the first 20 stars of the resulting clean CMD of NGC 5471 of panel (c). The complete stellar photometry table is shown in Appendix D. Isochrones To study the CMD we use the isochrone set that corresponds to the grid by Girardi et al. (2002) 4 , covering the age range 6.60 < log t < 10.25 and mass range 0.15 to 100 M ⊙ , based on the Z=0.004 (1/5 Z ⊙ ) models from Girardi et al. (2000) and Bertelli et al. (1994) that include overshooting and a simple synthetic evolution of TP-AGB (Girardi and Bertelli, 1998). Atmosphere models are from BaSeL 3.1 WLBC 99 corrected library (Westera et al., 2002) at the same metallicity as the isochrone set. The procedure is as follows: (1) we obtained the magnitudes in the HST filters for all stellar models in the atmosphere grid. (2) For each point in the isochrone we obtained the stellar flux in each of the bands by a linear interpolation in the log g − log T eff grid. (3) The final luminosity was obtained by multiplying the square radius of the star. For log g−log T eff 4 Available at http://pleiadi.pd.astro.it/
2.4. Discussion 29 19 20 NGC 5471 (m - M = 29.3) 4 Myr 16 Myr 25 Myr 50 Myr 70 Myr −11 −10 −9 21 −8 m 547M 22 23 −7 −6 M547M 24 −5 25 −4 26 −3 −0.5 0.0 0.5 1.0 1.5 m 547M−m 675W′ Figure 2.8: Final CMD corrected for field star contamination, together with five isochrones from 4 to 70 Myr. The line across the bottom shows the completeness limit at the 50% level as derived from false star tests. The right-hand side scale gives the absolute magnitudes corresponding to a distance of 7.2 Mpc. values not covered by the atmosphere grid, the boundary values have been used with a caution flag. In terms of the present work, these stars do not modify the results obtained. In Figure 2.8 we show the final CMD (corrected for field star contamination). The 50% completeness limit is also plotted, and five isochones from 4 to 70 Myr are shown in colour. The right hand side scale gives the absolute magnitude corresponding to a distance of 7.2 Mpc. 2.4 Discussion In this section we discuss the results of the photometry in terms of the integrated properties, both of the individual clusters defined in section 2.3.1 and of the whole star forming complex, and in terms of the resolved stellar photometry in the CMD. We attempt to bring all the results into a coherent picture of the past and present star formation processes in NGC 5471.
Page 1: 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
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Page 19 and 20: List of Tables 1.1 Integrated prope
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78 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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Hδ 116 4 • Long-slit spectrophot
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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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