TRACING ABUNDANCES IN GALAXIES WITH THE SPITZER ...

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LIST OF TABLES 1.1 Atomic data references . . . . . . . . . . . . . . . . . . . . . . . . . 19 2.1 Spitzer IRS observed line fluxes of IC 2448 . . . . . . . . . . . . . . 37 2.2 Extinction corrected optical line fluxes of IC 2448 . . . . . . . . . . 39 2.3 Selected observed ultraviolet line fluxes of IC 2448 . . . . . . . . . 39 2.4 Derivation of extinction coefficient from H I lines . . . . . . . . . . 41 2.5 Electron densities assuming Te = 12700 K . . . . . . . . . . . . . . 43 2.6 Electron temperatures assuming Ne = 1860 cm −3 . . . . . . . . . . 44 2.7 Ionic and elemental abundances . . . . . . . . . . . . . . . . . . . . 44 2.8 Comparison of abundances in IC 2448 to other sources . . . . . . . 45 3.1 Positions and AORkeys for observed GBPNe . . . . . . . . . . . . 57 3.2 Properties of observed GBPNe . . . . . . . . . . . . . . . . . . . . 58 3.3 Multiplicative scaling factors for GBPNe spectra . . . . . . . . . . 62 3.4 Observed infrared line fluxes . . . . . . . . . . . . . . . . . . . . . 64 3.5 Extinction corrected optical line fluxes for our GBPNe . . . . . . . 65 3.6 Comparison of the derived CHβ with the literature . . . . . . . . . 68 3.7 Electron temperatures and densities . . . . . . . . . . . . . . . . . 72 3.8 Adopted parameters for determining abundances . . . . . . . . . . 73 3.9 Ionic abundances . . . . . . . . . . . . . . . . . . . . . . . . . . . . 74 3.10 Comparison of total elemental abundances for individual GBPNe . 75 3.11 Net PAH feature fluxes . . . . . . . . . . . . . . . . . . . . . . . . 81 3.12 Comparison of mean Bulge abundances . . . . . . . . . . . . . . . 85 3.13 Abundances of PNe and H II regions across the Galaxy . . . . . . . 87 3.14 Parameters of linear fits to abundance gradients . . . . . . . . . . . 90 4.1 M51 H II region data . . . . . . . . . . . . . . . . . . . . . . . . . . 101 4.2 M51 H II region line fluxes . . . . . . . . . . . . . . . . . . . . . . 103 4.3 Abundances in M51 H II regions . . . . . . . . . . . . . . . . . . . 107 x
LIST OF FIGURES 1.1 Diagram of the structure of the Milky Way . . . . . . . . . . . . . 5 1.2 Example IRS spectrum . . . . . . . . . . . . . . . . . . . . . . . . 9 1.3 Configuration as well as Ne and Te diagnostics for S III . . . . . . . 16 1.4 Synthetic spectra of the radiation from an instantaneous starburst 22 1.5 Example of crystalline silicate features in an IRS spectrum . . . . . 24 1.6 Image of an olivine grain . . . . . . . . . . . . . . . . . . . . . . . 24 1.7 Structure of forsterite . . . . . . . . . . . . . . . . . . . . . . . . . 25 1.8 Example structures of PAH molecules . . . . . . . . . . . . . . . . 26 1.9 Example of PAH features in an IRS spectrum . . . . . . . . . . . . 27 2.1 The Spitzer IRS spectrum of IC 2448. . . . . . . . . . . . . . . . . 35 2.2 Close-ups of emission lines in the Spitzer spectrum of IC 2448 . . . 36 3.1 Spitzer IRS spectra of our GBPNe . . . . . . . . . . . . . . . . . . 63 3.2 Continuum subtracted spectra showing crystalline silicates . . . . . 80 3.3 Profiles of PAH features . . . . . . . . . . . . . . . . . . . . . . . . 82 3.4 Abundances of Bulge and Disk PNe versus galactocentric distance . 89 3.5 Comparison of mean 28 and 33 µm silicate features . . . . . . . . . 91 4.1 S<strong>IN</strong>GS Hα continuum subtracted image of M51 . . . . . . . . . . . 99 4.2 IRS spectra of H II regions in M51 . . . . . . . . . . . . . . . . . . 102 4.3 M51 H II region Ne III/Ne II flux ratio versus distance . . . . . . . 108 4.4 M51 (Ne + +Ne ++ )/(S ++ +S 3+ ) abundance ratio versus distance . . 109 xi
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: 3 Chemical Abundances and Dust in P
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
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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
Page 71 and 72:
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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Table 3.7 Electron temperatures and
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Table 3.9 Ionic abundances Ion x a
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3.5.2 Crystalline Silicates Crystal
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argon, neon, and sulfur tend to be
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Figure 3.2 Continuum subtracted spe
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Figure 3.3 Profiles of PAH features
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mean argon and sulfur abundances ar
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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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TRACING ABUNDANCES IN GALAXIES WITH THE SPITZER ...

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