Table 4
Fitted O I properties.
| Galaxy name | log(NO I) | b | v | log(NH I) |
|---|---|---|---|---|
| [log(cm−2)] | [km s−1] | [km s−1] | [log(cm−2)] | |
| (1) | (2) | (3) | (4) | (5) |
| J0921+4509 | 15.30 ± 0.13 | 45 ± 15 | 62 ± 11 | 18.63 ± 0.19 |
| J1503+3644 | 15.55 ± 0.16 | 302 ± 98 | 102 ± 77 | 19.60 ± 0.17 |
| J0925+1409 | – | – | – | – |
| J1152+3400 | 15.43 ± 0.17 | 227 ± 129 | –102 ± 83 | 19.43 ± 0.18 |
| J1333+6246 | 15.54 ± 0.35 | 287 ± 277 | –213 ± 152 | 19.78 ± 0.37 |
| J1442–0209 | 15.62 ± 0.58 | 178 ± 145 | 82 ± 101 | 19.69 ± 0.58 |
| Tol1247–232 | 15.29 ± 0.43 | 278 ± 168 | 58 ± 143 | 19.19 ± 0.44 |
| Tol0440–381a | 15.47 ± 0.02 | 623 ± 28 | 12 ± 19 | 19.27 ± 0.10 |
| Mrk54a | 16.07 ± 0.01 | 619 ± 8 | 15 ± 6 | 19.37 ± 0.10 |
| J0926+4427 | 15.77 ± 0.02 | 118 ± 5 | –141 ± 4 | 19.76 ± 0.05 |
| J1429+0643 | 15.55 ± 0.24 | 218 ± 74 | –43 ± 98 | 19.35 ± 0.25 |
| GP0303–0759 | 15.41 ± 0.18 | 209 ± 84 | 31 ± 70 | 19.55 ± 0.19 |
| GP1244+0216 | 16.12 ± 0.14 | 157 ± 47 | –67 ± 36 | 19.95 ± 0.15 |
| GP1054+5238 | 15.73 ± 0.14 | 256 ± 72 | 39 ± 55 | 19.63 ± 0.15 |
| GP0911+1831 | 15.73 ± 0.15 | 221 ± 79 | –102 ± 67 | 19.73 ± 0.16 |
| SGAS J1226 | 16.11 ± 0.03 | 200 ± 7 | –290 ± 11 | – |
| SGAS J1527 | 15.57 ± 0.13 | 133 ± 44 | –89 ± 33 | – |
| Cosmic Eye | 20.64b ± 0.66 | 24 ± 77 | 208 ± 9 | 24.04b ± 0.67 |
Notes. Column 1: Galaxy name; Col. 2: logarithm of O I column density; Col. 3: O I Doppler b-parameter; Col. 4: velocity shift of the O I line. The O I covering fraction is fixed to the H I final value from Table 3. We did not detect the O I absorption lines in the J0925+1409 spectra. Column 5: H I column density derived from the product of (3) and 12 + log(O/H; Table 1). We cannot estimate NH I for SGAS J1226 and SGAS J1527 because they do not have a measured 12 + log(O/H). (a) Used O I 1302 Å (b) saturated O I line, hence unreliable NH I determination. From the damped Lyα profile, Quider et al. (2010) obtained NH I = (3.0 ± 0.8) × 1021 cm−2.
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