Table 3: Characteristics of our program stars and their nebulae. The last column gives the references for stellar parameters and PN shape. The main-sequence (MS) mass is inferred from Weidemann's (2000) initial-final mass relation. The MS radius is estimated using Allen (1976). The future white dwarf (WD) radius is estimated from the mass-radius relation of Wood (1994). EGB 5 is not on a post-AGB evolutionary track as a result of close-binary evolution (Karl et al. 2003).
Object  T $_{\rm eff}$  log g mass MS mass radius MS radius WD radius PN shape Ref.
  [K] (cgs) [$M_\odot$] [$M_\odot$] [$R_{\odot}$] [$R_{\odot}$] [$R_{\odot}$]    
NGC 1360 97 000 5.3 0.65 2.7 0.30 2.3 0.011 elliptical A, B
Abell 36 113 000 5.6 0.60 2.7 0.21 2.3 0.012 irregular A, B
LSS 1362 114 000 5.7 0.60 2.0 0.18 1.6 0.012 ellip.ring A, C
EGB 5 34 000 5.85 0.48*   0.14     elliptical D
References: A: Traulsen et al. (2005), B: Phillips (2003), C: Heber et al. (1988), D: Lisker et al. (2004).
* Canonical mass of a hot subdwarf is assumed.

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Article Contents
1 Introduction
2 Observations and data reduction
3 Determination of the magnetic field strenghs
4 Parameters of the target stars and nebulae
5 Discussion and conclusions
References
List of tables
List of figures