TRACING ABUNDANCES IN GALAXIES WITH THE SPITZER ...

More documents

Recommendations

Info

Table 3.1 Positions and AORkeys for observed GBPNe PNG On Position a Off Position Number AORkey RA DEC AORkey 000.7+03.2 17646848 17 34 54.71 -26 35 56.9 17650176 000.7+04.7 17647616 17 29 25.97 -25 49 07.1 17650432 001.2+02.1 17648896 17 40 12.84 -26 44 21.9 17650688 001.4+05.3 17647872 17 28 37.63 -24 51 07.2 17650944 001.6-01.3 17649152 17 54 34.94 -28 12 43.3 17651200 002.1+03.3 17649408 17 37 51.14 -25 20 45.2 17651456 002.8+01.7 17649664 17 45 39.81 -25 40 00.6 17651712 006.0-03.6 17648128 18 13 16.05 -25 30 05.3 17651968 351.2+05.2 17648384 17 02 19.07 -33 10 05.0 17652224 354.2+04.3 17648640 17 14 07.02 -31 19 42.6 17652480 358.9+03.2 17647104 17 30 43.82 -28 04 06.8 17652736 a RA and DEC are in J2000.0. RA is in hours, minutes, seconds; DEC is in degrees, arcmin, arcsec. 57
Table 3.2 Properties of observed GBPNe PNG log(FHβ) a R⊙,P N b RGC c Vrad d Diam a IRAS Fluxes (Jy) e F6cm a F21cm f Number (erg cm−2 s−1 ) (kpc) (kpc) (km s−1 ) ( ′′ ) F12µm F25µm (mJy) (mJy) 000.7+03.2 -13.40 ± 0.20 7.01 1.0±2.9 -175 5.2
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 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: are members of the Bulge, (Acker et
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 ...

Create successful ePaper yourself

Delete template?

Save as template?