TRACING ABUNDANCES IN GALAXIES WITH THE SPITZER ...

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Table 2.1 Spitzer IRS observed line fluxes. All fluxes are from the high resolution modules except the lines with λ < 10 µm which are from the SL module. A less-than sign indicates a three sigma upper limit. λ(µm) Line Flux a λ(µm) Line Flux a 6.99 [Ar II]
2.4 Optical and UV Data We complement our IR line fluxes with optical and UV line fluxes in order to deter- mine abundances. The optical and UV data provide line fluxes from ions not seen in the infrared spectrum (especially carbon and nitrogen). We obtain optical line fluxes from Milingo et al. (2002b). They observed IC 2448 with the 1.5 m telescope and Cassegrain spectrograph at the Cerro Tololo Inter-American Observatory in the Spring of 1997 using a 5 ′′ x 320 ′′ slit. The slit width is about half of the diam- eter of IC 2448, and so Milingo et al. (2002b) missed some of the nebular flux. We assume that the optical lines measured in the small aperture are representative of the entire nebula of IC 2448 because IC 2448 has evenly distributed optical [N II] and [O III] line emission (Palen et al., 2002). The extinction corrected fluxes for the lines we use are listed in Table 2.2 as given by Milingo et al. (2002b). These authors report uncertainties in their line fluxes of � 10% for their strong lines (with strengths ≥ Hβ) and have flagged uncertainties of � 25% and � 50% for the weaker lines. These uncertainties are given in Table 2.2. High and low resolution large aperture International Ultraviolet Explorer (IUE) spectra of IC 2448 from the IUE Newly Extracted Spectra (<strong>IN</strong>ES) system are available on the web 2 . The high resolution spectra we use are labeled SWP19067 and LWR15096, and the low resolution spectra we use are labeled SWP03194 and LWR02756. We use SMART to measure the line fluxes from the spectra, and the results are listed in Table 2.3. Uncertainties are obtained from the gaussian fit to each line and are � 15% unless otherwise noted. The IUE large aperture (10 ′′ x 23 ′′ ellipse) is big enough to contain essentially all of the flux from IC 2448, and no aperture scaling factor needs to be applied to the spectra. 2 The IUE <strong>IN</strong>ES system archive website is http://ines.vilspa.esa.es 38
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 and 8: ACKNOWLEDGEMENTS First and foremost
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: Figure 2.2 Close-ups of emission li
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
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towards the Galactic Center. On the
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Table 3.14 Parameters of linear fit
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models that show how a binary compa
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y an outer dense O-rich torus, indi
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CHAPTER 4 ABUNDANCES IN H II REGION
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expect their abundance ratio to rem
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We extract spectra processed throug
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Figure 4.2 IRS spectra of H II regi
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IRS slits from these WIRC observati
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S IV) we employ is equal to Te(O +2
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Figure 4.3 M51 H II region Ne III/N
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Figure 4.4 shows a plot of the (Ne
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James Webb Space Telescope (JWST);
Page 127 and 128:
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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