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

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16 2 • The star formation history of NGC 5471 Figure 2.3: Color composite of HST WFPC2 images of NGC 5471. Each image has its own filter combination label, in the usual RGB (Red, Green, Blue) color sequence . North is up, and east to the left.
2.2. Observations and Data Reduction 17 Band Time (UT) Duration (s) Air mass J 04:09:00 1 × 60 1.38 H 01:03:08 3 × 15 1.11 K s 21:59:29 10 × 5 1.31 Table 2.2: Journal of TNG/ARNICA observations of NGC 5471. emission line free, broad band image (F675W ′ ). Figure 2.2 shows NGC 5471 in the four bands. An ellipse indicating the core of the region is drawn in the Hα and F675W ′ images. The five brightest components first noted by Skillman (1985) and designated as A, B, C, D and E, are distinctly observed in the Hα image. The presence of a supernova remnant (NGC 5471B) is clearly seen as an intense [SII] emission source in the B-component in the F673N image. Previous works have associated X- ray sources with supernova remnants (SNRs) in M101. Chen et al. (2002) conclude that the energetic SNR in NGC 5471B (first identified by Skillman, 1985) was very likely produced by a hypernova, an explosion one or two orders of magnitude brighter than the canonical 10 51 erg energy explosion associated with a normal SN, although this result has been questioned recently (Jenkins et al., 2004). Several color images of NGC 5471 are shown in Figure 3.1. Each image has its own filter combination label, which indicates the used filters in the composition in the usual RGB (Red, Green, Blue) color sequence. 2.2.3 Near-infrared photometry JHK s photometry was performed on 2000 April 29, using the 3.58m TNG (Telescopio Nazionale Galileo) at the Observatorio del Roque de los Muchachos in La Palma. The camera used was ARNICA (ARcetri Near Infrared CAmera), with a CCD detector NICMOS 256×256 HgCdTe and gain of 19 e − /ADU. The spatial scale was 0. ′′ 35 pixel −1 and the field of view 90×90 arcsec 2 . The details of these observations are given in Table 2.2. The flux calibration of the images has been done using 2MASS images of NGC 5471, retrieved from the 2MASS Extended Source Catalog. We first measured the integrated flux of the 2MASS images in a circle containing the region and then, we used that aperture centered in the same coordinates and covering the same area in the ARNICA images. We obtained the photometric constants comparing the calibrated 2MASS fluxes with those from ARNICA by means of the transformation equations of the two systems. In order to compare the two sets of optical and NIR data, we aligned the HST and TNG images. We degraded the WFPC2 images to the spatial scale and seeing of the IR ones, then we identified several objects in both data sets and marked them with the IRAF center routine. Next, we aligned the images with the geomap and geotran routines, using the HST
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
Page 16 and 17: vi LIST OF FIGURES 3.12 Example of
Page 19 and 20: List of Tables 1.1 Integrated prope
Page 21 and 22: Chapter 1 Introduction 1.1 Overview
Page 23 and 24: 1.1. Overview 3 Figure 1.1: Sample
Page 25 and 26: 1.1. Overview 5 These massive star
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Page 60 and 61: 40 3 • IFS of a GEHR in NGC 6946
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66 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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106 4 • Long-slit spectrophotomet
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Hδ 116 4 • Long-slit spectrophot
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Table 4.4 continued SDSS J1657 Knot
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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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