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

More documents

Recommendations

Info

172 Appendix C where x = log Ar 3 O 3 . Its standard deviation is 0.23 dex. The N 2 O 2 parameter The N 2 O 2 parameter was defined by Pérez-Montero and Díaz (2005) as: N 2 O 2 ≡ [Nii]λ6548 + [Nii]λ6584 [Oii]λ3727 + [Oii]λ3729 A tight relation exists between N 2 O 2 and log(N + /O + ), and hence, it can be used as an indicator of log(N/O). Its calibration is ( ) N log = 1.144 log O ( ) [Nii] − 0.232 [Oii] The uncertainty involved in the determination of the N/O ratio is 0.14 dex, but decreases to only 0.08 for Hii galaxies. Díaz et al. (2007) recalibrated this relation including high metallicity regions and circumnuclear star-forming regions. The data yields the expression: ( ) N log = (0.65 ± 0.02) log O ( ) [Nii] − (0.79 ± 0.01) [Oii] which is shallower than that found by Pérez-Montero and Díaz (2005).
Appendix D Stellar photometry results of NGC 5471 This Appendix includes the stellar photometry results of the NGC 5471 CMD. 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 continued on next page 173
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 34 and 35:
Page 36 and 37:
Page 38 and 39:
Page 40 and 41:
Page 42 and 43:
Page 44 and 45:
Page 46 and 47:
Page 48 and 49:
Page 50 and 51:
Page 52 and 53:
Page 54 and 55:
Page 56 and 57:
Page 58 and 59:
Page 60 and 61:
40 3 • IFS of a GEHR in NGC 6946
Page 62 and 63:
Page 64 and 65:
Page 66 and 67:
Page 68 and 69:
Page 70 and 71:
Page 72 and 73:
Page 74 and 75:
Page 76 and 77:
Page 78 and 79:
Page 80 and 81:
Page 82 and 83:
Page 84 and 85:
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: 122 4 • Long-slit spectrophotomet
Page 144 and 145: Table 4.4 continued SDSS J1657 Knot
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: C • Empirical calibrators 171 One
Page 195 and 196: D • Stellar photometry results of
Page 207: D • Stellar photometry results of
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?