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NGC 6567 (PK 11 --0$^{o}$ 2) was selected for study with the Hamilton Echelle Spectrograph at Lick Observatory and with the International Ultraviolet Explorer (IUE) because the level of excitation of the nebular spectrum and the appearance of the spectrum of the central star closely resembled the variable planetary nebula (PN), NGC 6572. NV, CIV, and OV and perhaps MgII all show P Cygni profiles. CIV 5801, 5812 appear as broad Wolf-Rayet lines. Unlike in NGC 6572, $\lambda$4686 HeII is definitely of nebular origin. It shows a double peaked profile similar to that of [ArIV] 4711.
We calculated models for 60,000 $<$ T$_{eff}$ $<$ 80,000K, nebular density N(H) $= 8000$/cm$^{3}$, inner shell radius $0.045$pc, outer shell radius $= 0.056$pc, R$_{\star}$ $= 0.245$R$_{\odot}$, L$_{\star}$ $= 2220$L$_{\odot}$. We found logarithmic abundances as follows: H 12.00; He 10.02; C 8.70; N 7.49; O 8.34; Ne 7.45; S 6.49; Cl 4.70, Ar 5.74; Mg 6.49; Si 6.78; K 4.23. Most spectral lines were represented reasonably well but the predicted intensities of [S III] 9531, 9069 (which are strongly affected by atmospheric extinction) were predicted too strong. The ground-based observations were supported in part by NSF grant AST 90-14333.
