Table 2
Si and C abundances.
| Object | log [Si/H] | log [C/H] | Notes | Object | log [Si/H] | log [C/H] | Notes |
|
|
|||||||
| WD 0000+171 | –8.10 (0.15) | –8.30 | WD 1102+748 | –8.50 | |||
| WD 0013-241 | –8.40 | WD 1104+602 | –8.40 | ||||
| WD 0018-339 | –8.00 | WD 1129+155 | –8.30 (0.25) | –8.10 | |||
| WD 0028-474 | –8.40 | WD 1133+293 | –7.70 (0.15) | –7.70 | |||
| WD 0047-524 | –8.40 | SDSS1228+1040 | –5.20 (0.10) | –7.60 (0.20) | *, 1, 4, 5 | ||
| WD 0059+257 | –6.50 (0.10) | –8.00 | 1 | WD 1229-013 | –8.30 | ||
| WD 0102+095 | –7.35 (0.15) | –8.00 (0.20) | WD 1230-308 | –8.10 | |||
| WD 0114-605 | –7.40 (0.20) | –8.10 (0.20) | HS1243+0132 | –7.80 (0.15) | –8.30 | ||
| WD 0124-257 | –8.20 | WD 1257+048 | –7.50 (0.15) | –7.70 (0.20) | |||
| WD 0140-392 | –7.50 (0.15) | –8.40 | WD 1310-305 | –7.70 (0.15) | –8.10 | ||
| WD 0155+069 | –8.30 | WD 1325+279 | –8.00 (0.15) | –8.20 | |||
| HS0200+2449 | –8.30 | WD 1325-089 | –8.60 (0.25) | –8.00 | |||
| WD 0242-174 | –8.20 (0.20) | –8.30 | WD 1330+473 | –8.30 | |||
| WD 0307+149 | –7.85 (0.15) | –8.30 | WD 1353+409 | –7.80 | |||
| WD 0308+188 | –8.20 | WD 1408+323 | –7.70 (0.15) | –8.30 (0.20) | |||
| HE0308-2305 | –7.80 | WD 1451+006 | –7.70 (0.20) | –8.20 | |||
| WD 0341+021 | –7.95 (0.20) | –7.55 (0.15) | WD 1459+347 | –8.20 | |||
| WD 0352+018 | –8.10 (0.15) | –8.30 | WD 1524-749 | –7.90 | |||
| HE0358-5127 | –7.80 | WD 1531-022 | –8.40 | ||||
| HE0403-4129 | –7.10 (0.15) | –7.90 | WD 1547+057 | –8.20 | |||
| HE0414-4039 | –8.20 | WD 1548+149 | –7.65 (0.15) | –7.40 (0.15) | |||
| HE0416-1034 | –7.35 (0.15) | –7.05 (0.20) | WD 1633+676 | –7.90 | |||
| HE0418-1021 | –8.20 | WD 1647+375 | –6.20 (0.10) | –5.50 (0.20) | 1 | ||
| WD 0421+162 | –7.50 (0.15) | –8.30 | WD 1713+332 | –8.30 (0.25) | –7.60 (0.20) | ||
| WD 0431+126 | –8.10 (0.15) | –8.30 | WD 1755+194 | –7.30 (0.20) | –8.10 (0.20) | ||
| HE0452-3444 | –7.60 (0.15) | –8.20 | WD 1914-598 | –8.30 (0.15) | –8.30 | ||
| HS0507+0434A | –8.40 (0.15) | –8.50 | WD 1929+012 | –4.75 (0.15) | –6.80 (0.30) | *, 1, 4 | |
| WD 0710+741 | –6.70 (0.15) | –5.90 (0.30) | *, 1, 2 | WD 1943+163 | –6.80 (0.10) | –6.60 (0.20) | 1 |
| WD 0843+516 | –5.20 (0.10) | –7.20 (0.20) | 1, 4 | WD 1953-715 | –6.70 (0.10) | –6.60 (0.20) | 1 |
| WD 0854+404 | –7.90 (0.20) | –8.10 | WD 2021-128 | –8.30 | |||
| WD 0920+363 | –7.30 (0.20) | –7.70 | WD 2032+188 | –8.20 | |||
| WD 0933+025 | –8.30 | 3 | WD 2046-220 | –7.60 (0.15) | –7.60 | ||
| HS0944+1913 | –8.40 | WD 2058+181 | –7.50 (0.10) | –6.50 (0.20) | 1 | ||
| WD 0947+325 | –8.30 | WD 2134+218 | –8.10 (0.15) | –8.10 | |||
| WD 0954+697 | –8.00 (0.20) | –8.20 | HS2210+2323 | –8.20 | |||
| WD 1005+642 | –8.20 | WD 2220+133 | –8.20 | ||||
| WD 1013+256 | –6.90 (0.10) | –6.40 (0.20) | HS2229+2335 | –6.50 (0.15) | –6.70 (0.20) | ||
| WD 1015+161 | –6.40 (0.10) | –8.00 | 1, 4 | HE2231-2647 | –8.10 (0.15) | –8.40 | |
| WD 1017+125 | –7.50 (0.15) | –7.60 | HE2238-0433 | –7.50 | |||
| WD 1034+492 | –7.55 (0.10) | –8.00 | HS2244+2103 | –7.70 (0.15) | –8.10 | ||
| WD 1038+633 | –7.90 (0.30) | –8.00 | WD 2256+249 | –6.85 (0.10) | –6.10 (0.20) | *, 1, 2 | |
| WD 1049+103 | –8.40 | 3 | WD 2257+162 | –7.40 (0.15) | –6.40 (0.20) | *, 2 | |
| WD 1049-158 | –8.40 | WD 2306+124 | –7.60 (0.10) | –8.00 (0.20) | |||
| WD 1052+273 | –8.50 | WD 2322-181 | –7.70 (0.10) | –7.70 (0.15) | |||
| WD 1058-129 | –8.30 | WD 2359-324 | –7.80 | ||||
Notes. Abundances are logarithm of the metal to hydrogen ratio by numbers. Numbers in parenthesis are estimated errors. If absent, the abundances are upper limits (Sect. 9). *: Ancillary target, not used in sample statistics; 1: additional elements detected among the following: O, Mg, Al, P, S, Ca, Fe in the ultraviolet or optical spectra; 2: post-common envelope (close) binary; 3: spatially resolved (wide) binary; 4: exhibits excess infrared emission; 5: SDSS1228 is a gas-disk DAZ with emission lines seen in the infrared Ca ii triplet near 8500 Å (Gänsicke et al. 2006) and the Mg ii doublet at ≈2800 Å (Hartmann et al. 2011). The disk emission lines are broad – in contrast, the photospheric absorption lines are narrow, and we would expect to detect any emission in Si in the high-quality COS spectra of SDSS 1228+1040. In addition, the computations of Hartmann et al. (2011) predict little emission in Si ii, and none in Si iii. We use many Si ii and Si iii in the abundance analysis and do not see a significant difference.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.