TRACING ABUNDANCES IN GALAXIES WITH THE SPITZER ...

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distances to more of our objects than other studies, such as van de Steene & Zijl- stra (1995) and Cahn et al. (1992). An accurate statistical distance scale for PNe is difficult to obtain, and controversies exist as to which statistical distance scales are the best: for example Bensby & Lundström (2001) find that Zhang’s distance scale is good, while Ciardullo et al. (1999) find that it is not as good. However, regardless of which statistical distances we adopt, the conclusions of the paper will remain unchanged because all of the PNe in our sample are constrained to be in the Bulge by other criteria and we include the large uncertainties that go with these statistical distances in the data analysis. We adopt the distance from the Sun to the Galactic Center, Ro, from Reid (1993) who determines the best estimate of this distance by taking a weighted average of the various determinations of Ro from different methods. Reid (1993) finds that Ro = 8.0 ± 0.5 kpc, and this value seems to agree with more current estimates of this distance (e.g. López-Corredoira et al., 2000; Eisenhauer et al., 2005; Groenewegen et al., 2008). Galactocentric distances (RGC) are then calculated assuming this Ro, and uncertainties on RGC are calculated using standard error propagation and assuming an uncertainty of 40% on the heliocentric distance (Zhang 1995 estimates the accuracy of the PN distance scale as 35-50% on average). If the distance to a PN is unknown, we assume it is within 4 kpc of the Galactic Center. Table 3.2 lists the heliocentric and galactocentric distances for each object. 61
Table 3.3 Multiplicative scaling factors for GBPNe spectra. LHn1 stands for LH nod 1, SL1n2 stands for SL order 1 nod 2, etc. PNG Number LHn1 LHn2 SHn1 SHn2 SL1n1 SL1n2 SL3n1 SL3n2 SL2n1 SL2n2 000.7+03.2 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 000.7+04.7 1.02 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 1.00 001.2+02.1 1.02 1.00 1.00 1.05 1.00 1.00 1.00 1.00 1.00 1.00 001.4+05.3 1.03 1.00 1.15 1.17 1.15 1.15 1.00 1.15 1.00 1.00 001.6-01.3 1.05 1.00 1.15 1.15 1.15 1.15 1.50 1.50 1.50 1.50 002.1+03.3 1.00 1.00 1.20 1.20 1.20 1.20 1.20 1.20 1.20 1.20 002.8+01.7 1.01 1.00 1.05 1.10 1.10 1.10 1.10 1.15 1.10 1.10 006.0-03.6 1.02 1.00 1.15 1.15 1.15 1.15 1.60 1.70 1.50 1.40 351.2+05.2 1.02 1.00 1.15 1.15 1.50 1.50 1.50 1.40 1.50 1.40 354.2+04.3 1.02 1.00 1.15 1.15 1.20 1.20 1.20 1.20 1.20 1.20 358.9+03.2 1.02 1.00 1.12 1.10 1.15 1.15 1.00 1.20 1.00 1.00 62
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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
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: nod-averaged line fluxes. Uncertain
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
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James Webb Space Telescope (JWST);
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Bernard-Salas, J. & Tielens, A. G.
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Edgar, R. G., Nordhaus, J., Blackma
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Hummer, D. G., Berrington, K. A., E
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Matsuura, M., Zijlstra, A. A., Mols
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Pradhan, A. K., Montenegro, M., Nah
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Vassiliadis, E. & Wood, P. R. 1993,
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