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

More documents

Recommendations

Info

14 2 • The star formation history of NGC 5471 Filter Band Exposure (s) Observation ID F547M Strömgren y 2 × 600 U4DN030DR, U4DN030ER 2 × 100 U4DN030FR, U4DN030GR 20 U4DN030HM F675W WFPC2 R 2 × 400 U4DN0308R, U4DN0309R 2 × 50 U4DN030AR, U4DN030BR 10 U4DN030CR F656N Hα 180 U4DN0305R 2 × 600 U4DN0306R, U4DN0307R F673N [S II] 3 × 700 U4DN0301R, U4DN0302R, U4DN0303R 300 U4DN0304R Table 2.1: Journal of HST/WFPC2 observations of NGC 5471. All images were obtained on 1997 November 1 for the cycle 6 program GO-6928, with You-Hua Chu as PI. The object of study is centered in the WF3 camera. 5471, and we will only use the GALEX data to study the integrated photometry. 2.2.2 HST/WFPC2 Imaging Hubble Space Telescope (HST) Wide Field Planetary Camera 2 (WFPC2) images of NGC 5471 were retrieved from the HST archive. The images were taken on 1997 November 1 through two emission-line filters: F656N (Hα) and F673N ([S II]), and two continuum filters: F547M (Strömgren y) and F675W (WFPC2 R) (Heyer, 2004). Each camera images onto a Loral 800×800 CCD which gives a plate scale of 0. ′′ 046 pixel −1 for the PC camera and 0. ′′ 10 pixel −1 for the three WF cameras, with a readout noise of ∼5 e − and a gain of 7 e − /DN for this observations. NGC 5471 is centered in the WF3 camera in all images. The scale of the WF CCDs at NGC 5471, for which we assume a distance modulus of (m − M) = 29.3 (Stetson et al., 1998), is 3.5 pc pixel −1 . Table 2.1 lists the details concerning the WFPC2 data. The HST pipeline processed WFPC2 images were subjected to the usual processing using the IRAF 1 and STSDAS 2 software packages, following the procedures outlined in the HST Data Handbook. We used the multiple exposures to correct for the incidence of cosmic rays as well as to eliminate hotpixels and other defects on the CCD. We finally co-added the images to produce deep mosaics. Given the luminosity of NGC 5471, its Hα and [SII] emission contributes significantly 1 IRAF is distributed by the National Optical Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. 2 Space Telescope Science Data Analysis System (STSDAS) is a product of the Space Telescope Science Institute, operated by AURA for NASA.
2.2. Observations and Data Reduction 15 Figure 2.2: HST WFPC2 images of NGC 5471 in continuum corrected nebular filters Hα (F656N), [SII] (F673N), and emission line corrected continuum filters F547M and F675W ′ . The five knots from Skillman (1985) are marked in the Hα image. An ellipse indicating the core of the region is drawn in the Hα and F675W ′ images. North is up and east to the left. to the broad band (F675W) image. To eliminate the nebular contribution from the broad band and to produce continuum-free Hα and [SII] emission line images, we followed the procedure described below. First we multiplied the images by the PHOTFLAM parameter obtained by synphot to convert from count rates to flux densities, and then divided them by its time exposure. From the SYNPHOT task in STSDAS we determined the filter widths, and multiplied the flux densities found by the corresponding filter widths in order to obtain fluxes. The correct filter widths are the filter rectangular width RECTW (Luridiana et al., 2003). RECTW is defined as the width in Ångstroms of a rectangle with the same total area as the total transmission curve and a height given by the peak in the curve. We then scaled the Hα, [S II] and F675W images and performed an iterative subtraction to obtain a new,
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
Page 27 and 28: 1.1. Overview 7 Figure 1.3: Color-m
Page 29: 1.2. Aims and structure of this wor
Page 32 and 33: 12 2 • The star formation history
Page 60 and 61: 40 3 • IFS of a GEHR in NGC 6946
Page 84 and 85:
64 3 • IFS of a GEHR in NGC 6946
Page 86 and 87:
Page 88 and 89:
Page 90 and 91:
Page 92 and 93:
Page 94 and 95:
Page 96 and 97:
Page 98 and 99:
Page 100 and 101:
Page 102 and 103:
Page 104 and 105:
β[H 84 3 • IFS of a GEHR in NGC
Page 106 and 107:
Page 108 and 109:
Page 110 and 111:
Page 112 and 113:
Page 114 and 115:
Page 116 and 117:
Page 118 and 119:
Page 120 and 121:
Page 122 and 123:
Page 124 and 125:
Page 126 and 127:
106 4 • Long-slit spectrophotomet
Page 128 and 129:
Page 130 and 131:
Page 132 and 133:
Page 134 and 135:
Page 136 and 137:
Hδ 116 4 • Long-slit spectrophot
Page 138 and 139:
Page 140 and 141:
Page 142 and 143:
Page 144 and 145:
Table 4.4 continued SDSS J1657 Knot
Page 146 and 147:
Page 148 and 149:
Page 150 and 151:
Page 152 and 153:
Page 154 and 155:
Page 156 and 157:
Page 158 and 159:
Page 160 and 161:
Page 162 and 163:
Page 164 and 165:
Page 166 and 167:
Page 168 and 169:
Page 170 and 171:
150 Conclusions and future work has
Page 172 and 173:
152 Conclusions and future work oth
Page 174 and 175:
154 Conclusions and future work The
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
Page 184 and 185:
164 Appendix B Sulphur As in the ca
Page 186 and 187:
166 Appendix B Argon For argon, the
Page 189 and 190:
Appendix C Empirical calibrators In
Page 191 and 192:
C • Empirical calibrators 171 One
Page 193 and 194:
Appendix D Stellar photometry resul
Page 195 and 196:
D • Stellar photometry results of
Page 197 and 198:
Page 199 and 200:
Page 201 and 202:
Page 203 and 204:
Page 205 and 206:
Page 207:
Page 210 and 211:
190 REFERENCES Bertelli, G., Bressa
Page 212 and 213:
192 REFERENCES Girardi, L. & Bertel
Page 214 and 215:
194 REFERENCES Kunth, D. & Sargent,
Page 216 and 217:
196 REFERENCES Pérez-Montero, E.,
Page 218 and 219:
198 REFERENCES Terlevich, R., Melni
show all

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

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?