1. IAU Symp 34 IAU Symposium 34: Planetary Nebulae Tatranska Lomnica, Czechoslovakia August 1967 C.R. O’Dell High Resolution, High S/N Spectroscopy of PNe Robert Williams Space Telescope Science Institute Collaborators: J. Baldwin (Mich. St.) E. Jenkins (Princeton) B. Sharpee (Stanford RI) Y. Zhang (Hong Kong U.)

2. PN: IC 2501 LCO Magellan 6.5m ‘MIKE’ Echelle Resolution: 12 km/s IC 2501 2D Image

3. IC2501Spectrum Tc 1 (Blue)

4. Histrogram of Line No.

5. PNe s-process abunds Sr Ba Zr Y Kr Xe Br Ar H+He Continuum ~ forbidden lines Solar Abundances (  Relative Line Strengths)

6. Kr Montage

7. Xe Montage

8. S/N=25 Ba II Montage

9. PNe s-process abunds Sr Ba Zr Y Kr Xe Br [Kr/Ar] ~ 0-0.8 [Br/Ar] ~ 0.7: [Xe/Ar] ~-0.4- 0.9 [Ba/Ar] ~ 0.2-0.6 For PNe: Ar Solar Abundances

10. Grotrian Diagram Excitation of Recombination & Forbidden Lines In PNe & H II regions, for same ions: Recombination line abundance Forbidden line abundance = 1.1  50

11. Emiss & Abs Diagram Stellar Absorption Spectrum Nebular Emission Spectrum τ i = ∫ n i dl F i = ∫ n e n i dl O+O+ O +2 (Ground-based/Optical) (HST/UV) O+O+ Abundances from Emission & Absorption Lines OoOo O +2 10 9 cm 10 15 cm

12. EmAbsPNe

13. Ions with UV Resonance & Optical Forbidden Lines IonStellar UV Resonance Absorption Neb. Optical Emission C I1277.5*, 1329.6*, 1561.4*, 1657.0*[9850], [8728], [4622] P II1152.8, 1154.0*, 1301.9, 1310.7*, 1542.3*,[7876], [4669] 1532.5 S I1270.8, 1277.2, 1295.7, 1316.5, 1425.0, 1433.3*,[7725], [4589] 1474.0, 1483.0*, 1807.3, 1820.3* Fe II1260.5, 1608.5, 1621.7*[8617], [4244], [5159], [4359] Ni II1317.2, 1370.1, 1454.8, 1709.6, 1741.5[7378], [6667] N I1199.5, 1200.2, 1200.7[5198], [10400], [3467] O I1302.2, 1304.9*, 1306.0**[6300], [5577] S II1250.6, 1253.8, 1259.5[6717], [10320], [4069] S III1190.2, 1194.1*, 1201.0*, 1201.7*[9531], [6312], [3722] UV Abs & Opt Emiss.

14. Tc 1 Abs Spectrum O I (ISM) P II ( ISM ) O I (neb) P II (neb)

15. Tc1 AlII&SiII Abs Planetary Nebula Tc 1 Al II 1670.8 Si II 1526.7 ISM Tc 1 HST/STIS ISM Tc 1 HST/STIS

16. NGC246AbsMontage

17. Ed Analysis

18. He2-138 EWs & ColDens

19. NGC 6543 Harrington & Borkowski/HST [O III] 5007 Å [O I] 6300 Å [O II] 3727 Å NGC 6543 Image

20. Temperature & Density Diagnostics Line Ratio Tc 1 He2-138 NGC 6543 T e ( o K) [O I]14,000 9,000 ---- [S II] 9,000 6,000 9,000 [O II]10,500 7,000 12,000 [N II] 8,500 6,500 10,300 [S III] 9,500 6,000 8,500 [Ar III] 9,000 ---- 8,000 [O III] 9,000 ---- 8,200 n e (cm -3 ) [N I] 400: 7,000 900: [S II] 3,000 15,000 5,000 [O II] 2,000 7,500 6,000 [Cl III] 3,000 7,500 5,000 [Ar IV] ---- ---- 4,500 Compare Emiss Abunds

21. Emission Line Abundances (log H + =12) Ion λ EM i log A i T e n e Tc 1 [O I] 6300 0.060 4.88 14300 400 6363 0.073 4.97 [S II] 6716 0.136 5.41 9000 3000 6730 0.139 5.42 4069 0.099 5.26 4076 0.084 5.20 [S III] 9068 0.990 6.25 9500 2300 6312 0.736 6.12 He2-138 [C I] 8727 0.303 5.20 8800 7000 [P II] 7875 0.088 4.81 6000 10000 [Fe II] 5158 0.460 5.56 [Ni II] 7377 0.0093 3.84 7500 7000 [O I] 6300 9.27 6.68 8800 7000 6363 10.34 6.73 [S II] 6716 8.75 6.80 6000 7000 6730 9.63 6.84 4069 10.49 6.88 4076 11.19 6.91 [S III] 9068 2.917 6.34 6000 7000 6312 2.946 6.35 NGC 6543 [N I] 5200 0.031 4.26 12000 900 5197 0.029 4.24 [O I] 6300 0.227 5.13 12000 900 6363 0.234 5.14 [S II] 6716 0.202 5.19 9000 7000 6730 0.201 5.18 [S III] 9068 5.598 6.64 8700 4800 6312 5.493 6.63 Emiss Rel Abunds

22. COMPARATIVE ION ABUNDANCES (log H + =12) (Absorption column densities have been scaled to the S + emission abundance) Tc 1 He 2-138 NGC 6543 Em Abs Em Abs Em Abs C o ---- ---- 5.20 5.29 ---- ---- N o ---- ---- ---- ---- 4.25 3.84 O o 4.89 5.38 6.68 6.81 5.13 5.00 P + ---- ---- 4.81 4.93 ---- ---- S + 5.41 5.41 6.82 6.82 5.19 5.19 S +2 6.25 6.64 6.34 6.44 6.64 6.74 Fe + ---- ---- 5.56 5.70 ---- ---- Ni + ---- ---- 3.84 4.10 ---- ---- Compare Emiss Abunds

23. EmissionDensities-Diag = density required to produce observed emission intensity given the column density of that ion (Higher em  stronger emission rel to abs) ‘Emission Density’ : Emiss Meas Col Density ∫ n e n i dl em ≡ -------------- = ∫ n i dl Conclusions: 1) Approx. agreement of em and n e for most ions. But, in 2 of 3 PNe em for neutrals is much greater than gas density. Interpretation: Dense clumps exist with small covering factor. Sometimes the narrow absorption line of sight intersects a clump (He2-138) ; other times not ( Tc 1 & NGC 6543). 2) Excellent agreement of S +2 em and n e in all 3 PNe: [S III] emission & absorption yield same abundance

24. Summary s-process lines are detected in PNe and H II regions – For PNe: Kr & Xe, from the ‘light’ & ‘heavy’ peaks, are enhanced by comparable amounts, indicating substantial neutron exposure in the progenitor AGB stars. – For H II regions: no evidence for s-process enhancements. PNe abundances derived independently from UV absorption lines and optical forbidden lines show some differences for neutral and singly ionized species, but very good agreement for S +2. – The agreement for S +2 is validation that [S III] lines---and therefore presumably other FL’s---yield correct abundances along these lines of sight. Novae spectra show distinct features that may be explained by the Quadratic Zeeman Effect – Large magnetic fields are required (B ~ 10 6 gauss)