Table 2
Luminosity-specific PN numbers, α, of the SSP PNLFs.
| tage | Z | |||||
|---|---|---|---|---|---|---|
| (Gyr) | 0.0001 | 0.001 | 0.01 | 0.02 | 0.04 | 0.08 |
| 0.25 | - | 0.429 | 2.036 | 2.075 | - | - |
| 0.5 | 0.033 | 1.419 | 2.845 | 3.348 | 3.125 | 2.669 |
| 1.0 | 0.138 | 2.467 | 3.555 | 4.224 | 3.602 | 3.157 |
| 2.0 | 0.432 | 3.580 | 5.511 | 5.390 | 5.093 | 3.925 |
| 4.0 | 0.825 | 3.341 | 5.413 | 5.101 | 6.642 | 5.460 |
| 6.0 | 1.370 | 3.655 | 5.245 | 5.486 | 5.326 | 6.084 |
| 8.0 | 2.151 | 4.986 | 5.763 | 5.640 | 5.844 | 7.025 |
| 10.0 | 1.825 | 3.880 | 5.758 | 5.892 | 5.937 | 5.344 |
| 12.0 | - | - | - | 6.391 | 6.148 | 5.642 |
| 13.0 | - | - | - | - | 6.277 | 5.787 |
| α in units of 10-7 L⊙-1 | ||||||
Notes. The luminosity-specific PN numbers, α, are given in units of 10-7 L⊙-1 and are given for the brightest eight magnitudes below the typical bright-end cutoff of M(5007) = -4.5 for each SSP PNLF. Each row corresponds to the given age, tage, and each column to the given metallicity, Z. The values were computed from the constant luminosity PNLFs shown in Fig. 10 using the extincted PICS fiducial model with metallicity correction by Dopita et al. (1992), circumnebular extinction by Jacoby & Ciardullo (2025), and the same bolometric luminosity prescription by Bruzual & Charlot (2003).
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