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

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110 4 • Long-slit spectrophotometry of multiple knots of Hii galaxies 1e−15 A Continuum Difference Hα 1.5 cm−2 ) Flux (erg s−1 1.0 C B 0.5 0.0 −10 0 10 20 arcsecs Figure 4.2: Spatial profile of the light distribution along the slit for the observed Hα emission (dashed red line), the adjacent continuum (thick green line), and the difference between the two (thin blue line). IIZw71 and He-Ar for J1657. The images were processed and analysed with IRAF 1 routines in the usual manner. This procedure includes the removal of cosmic rays, bias subtraction, division by a normalised flat field, and wavelength calibration. Typical wavelength fits were performed using 30-35 lines in the blue and 20-25 lines in the red and polynomials of second to third order. These fits were made at 117 different locations along the slit in each arm for the WHT-ISIS observations (beam size of 10 pixels) and at 80 different locations for the CAHA-Twin observations (beam size of 10 pixels) obtaining rms residuals between ∼0.1 and ∼0.2 pix for the WHT data and between ∼0.1 and ∼0.3 pix for the CAHA data. In the last step, the spectra were corrected for atmospheric extinction and flux-calibrated. For both arms of WHT, two standard star observations were used, allowing a good spectrophotometric calibration with an estimated accuracy of about 5%. For the CAHA data, four standard star observations were performed each night at the same time for both arms, allowing a good spectrophotometric calibration with an estimated accuracy of about 3% between the different standard star flux calibration curves. Figure 4.2 and the left panel of Figure 4.3 show the spatial distribution of the Hα flux along the slit for IIZw71 and J1657. The emission line profile in these plots have been generated by collapsing 11 pixels of the spectra in the direction of the resolution at the central 1 IRAF: the Image Reduction and Analysis Facility is distributed by the National Optical Astronomy Observatories, which is operated by the Association of Universities for Research in Astronomy, In. (AURA) under cooperative agreement with the National Science Foundation (NSF).
4.2. Observations and reduction 111 0.8 0.6 0.4 1e−15 Flux (erg s−1 cm−2 ) A B C Continuum Difference D 20 10 0 A B C 0.2 −10 D 0.0 −20 −10 0 10 20 arcsecs 1.6′ −20 −10 0 10 arcsecs Hα arcsecs Figure 4.3: In left panel, spatial profile of the light distribution along the slit for the observed Hα emission (dashed red line), the adjacent continuum (thick green line), and the difference between the two (thin blue line). The horizontal lines show the spatial pixels that have been compressed to produce the one dimensional spectra corresponding to each emission knot. In the right panel, we show the Hα image from Gil de Paz et al. (2003) with the identification of the observed knots and the regions for which the broad band magnitudes and the narrow Hα flux have been measured. In the same image, we show the position of the slit for the observations described in the text and the elliptical regions measured to correct for aperture effects in each knot. We show the R-band contours as well, as taken from the same source, which show the position of the host galaxy.
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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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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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