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TRACING ABUNDANCES IN GALAXIES WITH
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TRACING ABUNDANCES IN GALAXIES WITH
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BIOGRAPHICAL SKETCH Shannon was bor
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ACKNOWLEDGEMENTS First and foremost
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thank my husband Ryan. The rest of
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3 Chemical Abundances and Dust in P
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LIST OF FIGURES 1.1 Diagram of the
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ditionally we find that these nebul
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seed nuclei relative to the β deca
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shape (Carollo et al., 2007). These
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Boltzmann velocity distribution cha
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etween recapture and photoionizatio
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a whole. Additionally, abundances f
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at the appropriate temperature and
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(a) 3.37 eV 1.40 eV 0.10 eV 0.04 eV
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(Iion), the radiative transition ra
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lines. For example, changing the ad
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Figure 1.4 Starburst99 synthetic sp
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Figure 1.5 Example of crystalline s
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H H H H H H H H H Anthanthrene C H
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year lifetime. Spitzer is in an Ear
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CHAPTER 2 THE SPITZER IRS INFRARED
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these elements than previous studie
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dust is seen in the spectrum. We se
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Figure 2.2 Close-ups of emission li
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2.4 Optical and UV Data We compleme
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2.5 Data Analysis Our goal is to ca
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2.5.2 Electron Density We assume an
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Table 2.6 Electron temperatures ass
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O, N, and C. The helium ionic abund
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Barlow (1994) use UV lines for impo
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is a spherical nebula with a low ma
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CHAPTER 3 CHEMICAL ABUNDANCES AND D
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essential data on important ionizat
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are members of the Bulge, (Acker et
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Table 3.2 Properties of observed GB
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nod-averaged line fluxes. Uncertain
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Table 3.3 Multiplicative scaling fa
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Table 3.4 Observed infrared line fl
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3.5 Data Analysis 3.5.1 Abundances
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Table 3.6 Comparison of the derived
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from the most reliable line(s), and
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- Page 101 and 102: towards the Galactic Center. On the
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- Page 111 and 112: expect their abundance ratio to rem
- Page 113 and 114: We extract spectra processed throug
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- Page 117 and 118: IRS slits from these WIRC observati
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- Page 121 and 122: Figure 4.3 M51 H II region Ne III/N
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- Page 133 and 134: Matsuura, M., Zijlstra, A. A., Mols
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