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

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Hδ 116 4 • Long-slit spectrophotometry of multiple knots of Hii galaxies 1e−16 ◦A−1 ) s−1 4 3 [OII]3727 Hγ J1657 - Knot C [OIII]4959 [OIII]5007 Flux (erg cm−2 2 1 [OIII]4363 Hβ ◦A−1 ) s−1 Flux (erg cm−2 0 3600 3800 4000 4200 4400 4600 4800 5000 5200 1e−16 4 3 2 1 HeI 5876 [SII] 6717,6731 Hα [SIII]9069 [SIII]9532 0 6000 6500 7000 7500 8000 8500 9000 9500 Wavelength (◦A) Figure 4.7: Blue and red spectra up to 9600 Å for the knot C of J1657. the number of pixels used in the measurement of the line flux, EW is the line equivalent width, and ∆ is the wavelength dispersion in Ångstroms per pixel. There are several lines affected by bad pixels, internal reflections or charge transfer in the CCD, telluric emission lines or atmospheric absorption lines. These cause the errors to increase, and, in some cases, they are impossible to quantify. In these cases we do not include these lines in the Tables nor in our calculations, and these lines were excluded from any subsequent analysis. In the case of IIZw71, the emission line [Siii] λ 9532 Å is affected by the strong narrow water-vapor lines present in the λ 9300 - 9500 wavelength region (Diaz et al., 1985). All physical parameters depending on its intensity were calculated using the theoretical ratio between this line and [Siii] λ 9069 Å, I(9069) ≈ 2.44 × I(9532) (Osterbrock, 1989), as we did in Chapter §3. In some cases there is an observable line (e.g., [Cliii] λλ 5517,5537, several carbon recombination lines, Balmer or Paschen lines) for which it is impossible to give a precise measurement. This might be due to a low signal to noise between the line and the surrounding continuum. This is also the case for the Balmer and Paschen jump for the CAHA data, that could not be measured even though it was observed, because it was very difficult to locate the continuum at both sides of the discontinuity with an acceptable accuracy.
4.3. Results 117 4e-15 3,5e-15 [OII] 3729 Å Flux (erg cm -2 s -1 Å -1 ) 3e-15 2,5e-15 2e-15 1,5e-15 [OII] 3726 Å 1e-15 5e-16 0 3730 3735 3740 3745 3750 3755 3760 Wavelength (Å) Figure 4.8: Deblending of the [Oii] λλ 3727, 3729 Å lines for IIZw71. Their ratio allows to put lower limits to the electron density in the observed ionized regions. A conspicuous underlying stellar population is easily appreciable in the spectra of IIZw71 by the presence of absorption features that depress the Balmer and Paschen emission lines. This effect does not allow the measurement of their fluxes with an acceptable accuracy (Diaz, 1988). To account for this, we subtracted from the four spectra of IIZw71 the best-fitting found by the spectral synthesis code STARLIGHT 2 (Cid Fernandes et al., 2004; Mateus et al., 2006). STARLIGHT fits an observed continuum spectral energy distribution using a combination of multiple simple stellar population (SSPs; also known as instantaneous burst) synthetic spectra using a χ 2 minimisation procedure. We chose for our analysis the SSP spectra from Bruzual and Charlot (2003), based on the STELIB library of Le Borgne et al. (2003), Padova (1994) evolutionary tracks, and a Chabrier (2003) initial mass function between 0.1 and 100 M ⊙ . We fixed the metallicity to Z = 0.004 (= 1/5 Z ⊙ ) for all models, which is the metallicity in the Bruzual and Charlot (2003) library closest to those corresponding to the oxygen abundances measured in knots B and C, as explained later. The code simultaneously finds the ages and the relative contributions of the different present SSPs and the average reddening. The reddening law from Cardelli et al. (1989) was used. Prior to the fitting procedure, the spectra were shifted to the rest frame, and sampled again to a resolution of 1 Å. 2 The STARLIGHT project is supported by the Brazilian agencies CNPq, CAPES and FAPESP and by the France-Brazil CAPES/Cofecub program.
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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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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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