Table 6.
Best fit abundances with respect to iron.
| 2000 | EM2 (RGS) | C | N | O | Ne | Mg | ΔC |
| 0.31 ± 0.01 | 0.67 ± 0.01 | 0.15 ± 0.01 | 0.32 ± 0.01 |  |
5200 | ||
| EM1 (PN) | Si | S | Ar | Ca | Ni | ΔC | |
| 0.47 ± 0.01 | 0.58 ± 0.02 |  |
<0.04 | <0.01 | 70 | ||
| 2014 | EMB (RGS) | C | N | O | Ne | Mg | ΔC |
| 0.27 ± 0.01 |  |
0.13 ± 0.01 | 0.30 ± 0.01 | 0.36 ± 0.01 | 10 600 | ||
| EMA (PN) | Si | S | Ar | Ca | Ni | ΔC | |
| 0.42 ± 0.01 |  |
 |
<0.01 | <0.01 | 350 | ||
Notes. Top: abundances fitted to the 2000 observation. EM2 accounts for the elements in the RGS energy range while EM1 fits those in the PN range. Bottom: abundances fitted to EMB for the RGS spectrum and EMA for PN energies in the 2014 spectrum. The abundances of the other components are coupled to these values, such that all the lines are fitted by the ions in each component, as we assume that the chemical enrichment is the same throughout the nucleus of NGC 1068.
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