thesis - IRS, The Infrared Spectrograph

58 CHAPTER 4: Abundances of Planetary Nebulae BD+30 3639 and NGC 6543Table 4.6–. Ultraviolet (IUE) line fluxes in units of 10 −12 erg cm −2 s −1 for NGC 6543. In Cols. 4and 8 the fluxes have been corrected for interstellar extinction using E B−V = 0.07 and an aperturecorrection factor of 1.3 has been used.λ (nm) Ident. Flux obs Flux corr λ (nm) Ident. Flux obs Flux corrLow ResolutionHigh Resolution124.4 s N V 57.7 140.28 137.1 s O V 2.64 5.99131.0 ? 11.9 27.83 148.3 N IV] 0.05 0.10131.7 b ? 7.30 17.01 148.7 N IV] 0.03 0.07137.6 s O V 29.9 67.66 155.2 s C IV 60.87 133.67140.9 ? 14.6 32.61 166.0 O III] 0.34 0.74155.2 s C IV 56.4 123.85 166.6 O III] 0.98 2.13164.1 s He II 17.4 37.96 174.6 N III] 0.22 0.47166.2 O III] 4.50 9.78 174.8 N III] 0.21 0.45172.1 N IV] 11.0 23.69 174.9 N III] 0.66 1.42174.5 N III] 1.90 4.08 190.6 C III] 8.34 18.19175.9 ? 2.50: 5.36 190.8 C III] 7.66 16.71181.4 [Ne III] 3.40 7.29 229.7 C III 1.41 3.25190.7 C III] 16.9 36.86 232.1 O III 0.07 0.15229.6 C III 4.90 11.30 232.5 C II] 0.71 1.61231.1 C II]+O III 7.10 16.25 232.7 C II] 1.19 2.70232.9 C II] 3.70 8.38 283.7 O IV]? 1.24 2.37241.9 [Ne IV] 2.20 4.74 302.5 O III 0.31 0.58251.0 He II 2.00 4.15 304.7 O III 0.55 1.02267.7 ? 2.30 4.52 313.3 ♮ O III 0.46 0.85279.0 [Ar V]+[Mg V] 2.10 4.04 320.3 s He II 0.28 0.51283.5 C II] 3.00 5.73292.2 † Mg V 0.70 1.32298.7 b [Ne V]? 2.20 4.12318.8 Si II, He I 2.30 4.20320.9 He II 1.50 2.73s Stellar line: ♮ Affected by reseau: b Blended: † May be present.: Noisy.4.5.1 BD+30 3639The optical and ultraviolet data have been taken from Aller & Hyung (1995) and Torres-Peimbert & Peña (1981) respectively. In Table 4.5 the ions used are listed. The dereddenedfluxes have been derived using an extinction of E B−V = 0.34, as derived from the infraredlines (see the previous section). Several lines of the same ion were sometimes used to confirmthe results of the ionic abundances.