TRACING ABUNDANCES IN GALAXIES WITH THE SPITZER ...

More documents

Recommendations

Info

To my husband Ryan, my parents Sharon and Norman Guiles, my brother Jason Guiles, and my grandma Frieda Maloney. iv
ACKNOWLEDGEMENTS First and foremost, I thank Jeronimo Bernard-Salas, who mentored me during my last two years of research. The work I have done with him forms the bulk of this dissertation. I am grateful to him for paying attention when I needed help, for sharing and explaining his code for calculating abundances, and for finding my mistakes and pointing me in the right direction to fix them (although of course any mistakes left in this dissertation are my fault and not his). Thanks also to Jim Houck for providing me with such a great opportunity to work on data from the Spitzer Space Telescope Infrared Spectrograph. I feel fortunate that I happened to be a graduate student when and where I had the chance to work with data from such an important instrument. Additionally, thanks to all of the other members of my special committee: Terry Herter, Saul Teukolsky, and Ira Wasserman. I thank the past and present members of the Spitzer IRS group at Cornell whom I have had the pleasure to work with (in alphabetical order): Don Barry, Jeronimo Bernard-Salas, Bernhard Brandl, Vassilis Charmandaris, Daniel Devost, Duncan Farrah, Elise Furlan, Peter Hall, Lei Hao, Terry Herter, James Higdon, Sarah Higdon, Jim Houck, Jason Marshall, Laurie McCall, Greg Sloan, Henrik Spoon, Keven Uchida, Dan Weedman, and Yanling Wu. All of them have helped me at some point, and their support has meant a lot to me. I would like to single out Don Barry who kept my computer running happily, Elise Furlan for teaching me the intricacies of SMART, Peter Hall for keeping SMART running, Laurie McCall for keeping things in the group running smoothly, Greg Sloan for answering my questions about dust, and Yanling Wu for being a kind and supportive office mate who never hesitated to answer my questions. Thanks to all of my co-authors on the two papers about planetary nebulae. Jeronimo Bernard-Salas and Stuart Pottasch gave me thorough comments and v
Page 1 and 2: TRACING ABUNDANCES IN GALAXIES WITH
Page 3 and 4: TRACING ABUNDANCES IN GALAXIES WITH
Page 5: BIOGRAPHICAL SKETCH Shannon was bor
Page 9 and 10: thank my husband Ryan. The rest of
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
Page 63 and 64:
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
Page 91 and 92:
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,
show all

TRACING ABUNDANCES IN GALAXIES WITH THE SPITZER ...

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

Delete template?

Save as template?