Table 2.
Comparison of the best-fit luminosity (L* in log(L*/L⊙)), surface temperature (Teff in log(Teff)), and initial mass (Mi in M⊙) of the central star for the M 31 PN sample, based on CLOUDY model fitting constrained by the extinction-corrected line fluxes by GR22 (the solar metallicity of Z = 0.02 assumed for all) and us (an appropriate metallicity in the range of Z = 0.003 − 0.009 informed from abundance analyses adopted for each PN; Otsuka & Ueta, in prep.).
| GR22 |
Otsuka & Ueta |
|||||
|---|---|---|---|---|---|---|
| PN | L* | Teff | Mi | L* | Teff | Mi |
| M1687 | 3.66 | 5.06 | 1.48 | 3.87 | 5.01 | 1.9 |
| M2068 | 3.62 | 5.05 | 1.34 | 4.04 | 5.01 | 2.4 |
| M2538 | 3.65 | 5.11 | 1.56 | 4.03 | 5.07 | 2.4 |
| M50 | 3.59 | 5.13 | 1.42 | 3.88 | 5.08 | 2.0 |
| M1596 | 3.49 | 5.22 | 1.76 | 3.75 | 5.11 | 1.6 |
| M2471 | 3.50 | 5.20 | 1.70 | 3.82 | 5.10 | 1.7 |
| M2860 | 3.51 | 5.08 | 1.20 | 3.97 | 5.03 | 2.2 |
| M1074 | 3.50 | 5.03 | 1.12 | 3.76 | 5.00 | 1.4 |
| M1675 | 3.60 | 5.10 | 1.39 | 4.05 | 5.05 | 2.6 |
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