TRACING ABUNDANCES IN GALAXIES WITH THE SPITZER ...

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suggestions on the two papers, which indubitably made the papers fly through the review process with ease; their expertise in the subject helped immensely. Jeronimo also planned the observations on which the second paper was based. Also thanks to my other co-authors on those papers: Tom Roellig (who planned the observations on which the first paper was based), Greg Sloan (who helped with the interpretation of the dust features in the second paper), and Jim Houck (who gave me helpful comments on both papers and donated the IRS GTO time for the observations for the second paper). I also thank Daniel Devost and Terry Herter for helping me with a project to take data at Palomar, and to Thomas Jarrett for showing me how to best use the WIRC instrument there for narrow-band imaging and setting me up to use his data reduction software. Thanks to James Lloyd and Don Banfield for letting me use some of their telescope time to learn how to use the WIRC instrument before my observing run. Thanks also to the night assistant there, Jean Mueller. Also thanks to NASA for funding my research. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. Support for this work was provided by NASA through Contract Number 1257184 issued by JPL/Caltech. Additionally, I thank the members of the Ithaca Area Toastmasters Club. Their support and positive feedback have helped me improve my public speaking skills, which in turn helped me when I gave presentations on my work and talks for out- reach. I also found their friendship, cheer, and different outlook on life invaluable. Finally, I thank my family. My parents and grandparents always encouraged me to do my best, and without that encouragement I would not be here. My brother is one of my best friends, and I appreciate his support. Most of all, I vi
thank my husband Ryan. The rest of my family lives across the country. Ryan’s presence here and his love, support, and encouragement helped buoy me through the deep and sometimes turbulent waters of graduate school. vii
Page 1 and 2: TRACING ABUNDANCES IN GALAXIES WITH
Page 3 and 4: TRACING ABUNDANCES IN GALAXIES WITH
Page 5 and 6: BIOGRAPHICAL SKETCH Shannon was bor
Page 7: ACKNOWLEDGEMENTS First and foremost
Page 11 and 12: 3 Chemical Abundances and Dust in P
Page 13 and 14: LIST OF FIGURES 1.1 Diagram of the
Page 15 and 16: ditionally we find that these nebul
Page 17 and 18: seed nuclei relative to the β deca
Page 19 and 20: shape (Carollo et al., 2007). These
Page 21 and 22: Boltzmann velocity distribution cha
Page 23 and 24: etween recapture and photoionizatio
Page 25 and 26: a whole. Additionally, abundances f
Page 27 and 28: at the appropriate temperature and
Page 29 and 30: (a) 3.37 eV 1.40 eV 0.10 eV 0.04 eV
Page 31 and 32: (Iion), the radiative transition ra
Page 33 and 34: lines. For example, changing the ad
Page 35 and 36: Figure 1.4 Starburst99 synthetic sp
Page 37 and 38: Figure 1.5 Example of crystalline s
Page 39 and 40: H H H H H H H H H Anthanthrene C H
Page 41 and 42: year lifetime. Spitzer is in an Ear
Page 43 and 44: CHAPTER 2 THE SPITZER IRS INFRARED
Page 45 and 46: these elements than previous studie
Page 47 and 48: dust is seen in the spectrum. We se
Page 49 and 50: Figure 2.2 Close-ups of emission li
Page 51 and 52: 2.4 Optical and UV Data We compleme
Page 53 and 54: 2.5 Data Analysis Our goal is to ca
Page 55 and 56: 2.5.2 Electron Density We assume an
Page 57 and 58: Table 2.6 Electron temperatures ass
Page 59 and 60:
O, N, and C. The helium ionic abund
Page 61 and 62:
Barlow (1994) use UV lines for impo
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is a spherical nebula with a low ma
Page 65 and 66:
CHAPTER 3 CHEMICAL ABUNDANCES AND D
Page 67 and 68:
essential data on important ionizat
Page 69 and 70:
are members of the Bulge, (Acker et
Page 71 and 72:
Table 3.2 Properties of observed GB
Page 73 and 74:
nod-averaged line fluxes. Uncertain
Page 75 and 76:
Table 3.3 Multiplicative scaling fa
Page 77 and 78:
Table 3.4 Observed infrared line fl
Page 79 and 80:
3.5 Data Analysis 3.5.1 Abundances
Page 81 and 82:
Table 3.6 Comparison of the derived
Page 83 and 84:
from the most reliable line(s), and
Page 85 and 86:
Table 3.7 Electron temperatures and
Page 87 and 88:
Table 3.9 Ionic abundances Ion x a
Page 89 and 90:
3.5.2 Crystalline Silicates Crystal
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argon, neon, and sulfur tend to be
Page 93 and 94:
Figure 3.2 Continuum subtracted spe
Page 95 and 96:
Figure 3.3 Profiles of PAH features
Page 97 and 98:
mean argon and sulfur abundances ar
Page 99 and 100:
of two smaller than that of Simpson
Page 101 and 102:
towards the Galactic Center. On the
Page 103 and 104:
Table 3.14 Parameters of linear fit
Page 105 and 106:
models that show how a binary compa
Page 107 and 108:
y an outer dense O-rich torus, indi
Page 109 and 110:
CHAPTER 4 ABUNDANCES IN H II REGION
Page 111 and 112:
expect their abundance ratio to rem
Page 113 and 114:
We extract spectra processed throug
Page 115 and 116:
Figure 4.2 IRS spectra of H II regi
Page 117 and 118:
IRS slits from these WIRC observati
Page 119 and 120:
S IV) we employ is equal to Te(O +2
Page 121 and 122:
Figure 4.3 M51 H II region Ne III/N
Page 123 and 124:
Figure 4.4 shows a plot of the (Ne
Page 125 and 126:
James Webb Space Telescope (JWST);
Page 127 and 128:
Bernard-Salas, J. & Tielens, A. G.
Page 129 and 130:
Edgar, R. G., Nordhaus, J., Blackma
Page 131 and 132:
Hummer, D. G., Berrington, K. A., E
Page 133 and 134:
Matsuura, M., Zijlstra, A. A., Mols
Page 135 and 136:
Pradhan, A. K., Montenegro, M., Nah
Page 137:
Vassiliadis, E. & Wood, P. R. 1993,
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