thesis - IRS, The Infrared Spectrograph

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36 CHAPTER 3: An ISO and IUE study of Planetary Nebula NGC 2440Table 3.2–. Infrared line intensities for NGC 2440, fluxes in units of 10 −12 erg cm −2 s −1 .λ Ident. Flux(µm) observed dereddened 1 corrected 24.051 H I Brα 3.91 4.00 6.244.527 [Ar VI] 16.8 17.2 26.85.611 [Mg V] 13.5 13.7 16.096.986 [Ar II] 3.30 3.34 5.217.654 [Ne VI] 52.0 52.7 82.27.900 [Ar V] 4.33 4.40 6.868.994 [Ar III] 9.37 9.83 15.3310.512 [S IV] 29.1 30.5 57.612.813 [Ne II] 9.18 9.36 9.3613.101 [Ar V] 4.20 4.28 4.2814.323 [Ne V] 96.4 97.8 97.815.557 [Ne III] 65.2 66.3 66.318.712 [S III] 16.7: 17.1 17.124.321 [Ne V] 121.8 123.5 123.525.896 [O IV] 297.9 301.7 301.733.479 [S III] 14.8: 14.9 14.936.017 [Ne III] 9.35 9.42 9.42: Noisy line.1 Dereddened fluxes using C Hβ =0.50.2 Aperture corrected and dereddened fluxes: only for lines below 12 µm an aperture correctionfactor of 1.56 has been applied.mally weak lines (I < 5, where I is in 10 −12 erg cm −2 s −1 ) have estimated errors of about20%, intermediate lines (5 10), havenormally less than 5% uncertainty. There are just two exceptions, the sulfur lines at 33.479and 18.712 µm. In the latter, the up and down scans differ by 40%.3.4.2 Ultraviolet spectrumIn the IUE spectra fifty lines were measured. Nitrogen, oxygen, carbon and magnesium linesare abundant (Table 3.3). The low resolution spectrum was used when deriving the physicalparameters and abundance; if not available, then the high resolution spectrum was used, and ifnot possible data from Shields et al. (1981) was used. The sum of the high resolution doubletfluxes should be the same as the unresolved low resolution, but often is not. Low–dispersionSWP spectra are preferred because they have the highest accuracy. In the high–dispersionobservations the exposures are generally much longer and thus subject to higher backgroundradiation noise. In addition, echelle order splice points and less well defined continuum levelslead to greater uncertainties in flux determination. A nominal error of ±10% was assumedfor well exposed (unsaturated) IUE low–dispersion spectra (∼ 200 DN).
Table 3.3–. IUE intensities, fluxes in units of 10 −12 erg cm −2 s −1 . The dereddened and aperture corrected fluxes in Cols. 5-6 and Cols. 11-12correspond to the low resolution spectra.λ Ident. Flux 1 Flux 2 Flux 3 λ Ident. Flux 1 Flux 2 Flux 3(nm) HR LR (nm) HR LR116.86 C IV 3.60 99.92 195.85 180.80 Si II 0.160 1.82 3.56 ∗123.92 N V 1.33 2.74 57.99 113.66 190.70 C III] 24.29 41.92 517.72 1014.73124.31 N V 1.45 190.91 C III] 17.7130.06 C III 0.39 6.95 13.62 229.80 C III 0.26 0.61 9.58 18.78132.77 C II 0.42: 6.95 13.62 232.65 C II] 1.46 3.7 21.84 42.81137.09 O V 0.55 0.32 4.79 9.39 232.81 C II] 0.65 9.67 18.95140.13 O IV] 0.78 2.74 38.54 75.53 238.66 He II 0.31 3.90 7.63140.51 O IV] 0.57 242.30 [Ne IV] 3.38 7.47 85.28 167.15140.73 O IV] 0.28 242.56 [Ne IV] 3.79148.36 N IV] 3.75 10.14 130.64 256.05 247.15 [O II] 0.56 1.04 10.76 21.09148.68 N IV] 2.38 251.24 He II 0.58 1.04 9.99 19.59154.86 C IV 11.99 27.36 349.09 684.21 273.46 He II 1.13 1.62 11.34 22.23155.12 C IV 7.24 278.42 [Mg V] 0.66: 0.87 5.86 11.48157.50 Ne V 0.630 8.05 15.78 ∗ 279.73 Mg II 0.23 1.53 3.01160.24 [Ne IV] 0.58 7.37 14.44 280.45 Mg II 0.13 0.86 1.69164.07 He II 22.36 23.43 289.73 567.86 283.00 O IV? 0.20 1.30 2.55166.10 O III] 0.44 2.96: 35.59 69.75 283.77 O III 0.72 0.59 3.82 7.48166.64 O III] 1.06 285.51 Mg I 0.31 1.98 3.883.4. Line fluxes 37
Page 1 and 2: RIJKSUNIVERSITEIT GRONINGENPhysics
Page 3 and 4: To my parents
Page 5 and 6: Contents1 Introduction 11.1 Evoluti
Page 7 and 8: CONTENTSvii5 Probing AGB nucleosynt
Page 9 and 10: 1IntroductionPLANETARY NEBULAE are
Page 11 and 12: 1.1. Evolution of low and intermedi
Page 13 and 14: 1.2. Planetary Nebulae 5Flash−Dri
Page 15 and 16: 1.3. Physics in PNe 7their whole li
Page 17 and 18: 1.3. Physics in PNe 95.35 eVO IIIλ
Page 19 and 20: 1.4. Studying PNe in the infrared 1
Page 21 and 22: 2The ISO-SWS Spectrum ofPlanetary N
Page 23 and 24: 2.3. Data reduction 15Table 2.1-. C
Page 25 and 26: 2.4. Line flux discussion 17Table 2
Page 27 and 28: 2.5. The visual and the ultraviolet
Page 29: 2.6. Analysis 21Table 2.5-. Electro
Page 32 and 33: 24 CHAPTER 2: The ISO-SWS Spectrum
Page 39 and 40: 3An ISO and IUE study of PlanetaryN
Page 41 and 42: 3.3. Corrections to line fluxes 33[
Page 43: 3.4. Line fluxes 35Table 3.1-. Comp
Page 47 and 48: 3.5. Physical parameters 393.4.3 Op
Page 49 and 50: 3.5. Physical parameters 41Table 3.
Page 51 and 52: 3.6. Chemical abundances 43Table 3.
Page 53 and 54: 3.6. Chemical abundances 45Table 3.
Page 55: 3.7. Conclusions 47Acknowledgements
Page 58 and 59: 50 CHAPTER 4: Abundances of Planeta
Page 77 and 78: 5Probing AGB nucleosynthesis viaacc
Page 79 and 80: 5.1. Introduction 71about the synth
Page 81 and 82: Table 5.2-. Radius, Zanstra tempera
Page 83 and 84: 5.3. Accurate abundances of ISO-obs
Page 85 and 86: 5.3. Accurate abundances of ISO-obs
Page 87 and 88: 5.4. Nucleosynthesis in low- and in
Page 89 and 90: 5.5. Synthetic TP-AGB calculations
Page 91 and 92: 5.6. Comparison between models and
Page 93 and 94: 5.6. Comparison between models and
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5.6. Comparison between models and
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5.7. Summary and conclusions 103Fig
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5.7. Summary and conclusions 105A s
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6Physical Conditions in PDRs around
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6.2. Observations 109are not promin
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6.4. General parameters of the PNe
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6.4. General parameters of the PNe
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Table 6.3-. Radius, Zanstra tempera
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6.6. Lines fluxes 117Figure 6.2-. S
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6.7. Physical conditions of the PDR
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6.8. PDRs versus Shocks 127Figure 6
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6.10. Atomic, ionized and molecular
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6.10. Atomic, ionized and molecular
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6.11. General discussion 133Table 6
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6.11. General discussion 135Figure
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6.12. Summary and Conclusions 137su
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7Conclusions and future workTHE res
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141• PNe with He/H > 0.14. The st
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143HERSCHEL The launch of this sate
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Nederlandse SamenvattingSTERREN wor
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Nederlandse Samenvatting 147Figuur
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Nederlandse Samenvatting 149PHOTOIO
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Nederlandse Samenvatting 151Figuur
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Nederlandse Samenvatting 153infraro
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English SummarySTARS are born, live
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English Summary 157Figure 2-. Two e
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English Summary 159PHOTOIONIZATIONR
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English Summary 161Figure 5-. Spect
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English Summary 163all) stages of i
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BibliographyAcker A., Marcout J., O
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BIBLIOGRAPHY 167Henry R.B.C., Kwitt
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BIBLIOGRAPHY 169Pottasch S.R., Bern
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List of PublicationsPublications in
Page 181 and 182:
AcknowledgementsI could easily writ
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Acknowledgements 175sense of humor,
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