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Table 5.
Wavelengths of the strongest lines (in Å) used for abundance determination in BD+18° 2647.
| C III | 977 |
|---|---|
| C IV | 1169, 1548, 1551 |
| N IV | (923), (924), (955), 1719 |
| N V | 1239, 1243 |
| O IV | 923 |
| F IV | 1060 |
| Ne V | 1721 |
| Si IV | 1067, 1122, 1128, 1394, 1403 |
| S V | 1040, 1502, 1572 |
| S VI | 933, 944, 1001, 1118 |
| Fe V | 1068, 1200–1208, 1234–1799 |
| Fe VI | 986, 1009, 1042, 1200–1210, 1228–1766 |
| Ni V | 1001, 1200–1211, 1225–1620 |
| Ni VI | 954, 971, 980, 982, 1000, 1003, 1009, 1042, 1061, |
| 1065, 1068, 1070, 1071, 1075, 1076, 1200–1211, | |
| 1227–1620 |
Notes. Lines of N IV given in parentheses, which point to a higher nitrogen abundance than given in Table 2, were heavily contaminated by interstellar lines and were not used to determine abundances.
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