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Table 4.
Chemical enrichment, ionization properties, and Lyman continuum escape fractions of Lyα emitters presented in this study.
| ID | zspec | FHβ | FHα | log(ξion/Hz erg−1) | [O III]/[O II] | ([O II]+[O III])/Hβ | fesc(LyC) |
|---|---|---|---|---|---|---|---|
| (×10−19 cgs) | (×10−19 cgs) | (O32) | (R23) | ||||
| Deep Tier | |||||||
| 21842 | 7.982 | 3.2 ± 0.5 | − |
 |
11.5 ± 1.6 | 8.8 ± 1.1 | 0.08 ± 0.01 |
| 10013682 | 7.276 | 0.8 ± 0.2 | − |
 |
12.0 ± 2.6 | 9.5 ± 1.7 | 0.03 ± 0.01 |
| 4297 | 6.712 | 5.3 ± 0.6 | 16.2 ± 0.04 |
 |
19.8 ± 4.7 | 7.5 ± 1.4 | 0.02 ± 0.01 |
| 16625 | 6.631 | 5.9 ± 0.3 | 16.5 ± 0.2 |
 |
24.5 ± 3.0 | 4.9 ± 0.5 | 0.04 ± 0.01 |
| 18846 | 6.336 | 11.4 ± 0.2 | 30.3 ± 0.3 |
 |
25.8 ± 1.3 | 6.3 ± 0.2 | 0.07 ± 0.01 |
| 19342 | 5.974 | 4.1 ± 0.2 | 10.8 ± 0.3 |
 |
29.5 ± 1.8 | 6.4 ± 0.4 | 0.06 ± 0.01 |
| 9422 | 5.937 | 18.4 ± 0.1 | 50.0 ± 0.7 |
 |
70.6 ± 4.1 | 7.7 ± 0.3 | 0.01 ± 0.001 |
| 6002 | 5.937 | 2.8 ± 0.1 | 8.1 ± 0.2 |
 |
10.9 ± 1.1 | 7.6 ± 0.6 | 0.06 ± 0.01 |
| 19606 | 5.889 | 4.6 ± 0.4 | 13.5 ± 0.5 |
 |
21.9 ± 2.5 | 7.5 ± 0.7 | 0.06 ± 0.01 |
| 10056849 | 5.814 | 4.0 ± 0.4 | 10.9 ± 0.3 |
 |
17.22 ± 1.3 | 4.6 ± 0.3 | 0.03 ± 0.01 |
| Medium Tier | |||||||
| 12637 | 7.660 | 13.9 ± 0.5 | − |
 |
9.4 ± 0.6 | 9.7 ± 0.5 | 0.10 ± 0.01 |
| 15362 | 6.794 | 4.3 ± 0.4 | 11.8 ± 1.2 |
 |
2.7 ± 0.3 | 6.2 ± 0.6 | 0.16 ± 0.02 |
| 13607 | 6.622 | 3.6 ± 0.5 | 11.9 ± 0.9 |
 |
1.6 ± 0.1 | 11.5 ± 1.1 | 0.80 ± 0.11 |
| 14123 | 6.327 | 5.6 ± 0.9 | 15.1 ± 1.2 |
 |
12.2 ± 2.6 | 8.9 ± 2.4 | 0.04 ± 0.01 |
| 58850 | 6.263 | 26.0 ± 1.7 | 65.9 ± 2.0 |
 |
23.6 ± 4.7 | 11.2 ± 1.6 | 0.02 ± 0.01 |
| 17138 | 6.204 | 3.6 ± 3.0 (†) | 10.4 ± 1.9 |
 |
1.8 ± 0.3 | 8.1 ± 1.2 | 0.38 ± 0.10 |
| 9365 | 5.917 | 11.1 ± 1.8 | 30.8 ± 1.3 |
 |
12.3 ± 1.7 | 10.1 ± 1.2 | 0.14 ± 0.02 |
Notes. The flux units are erg s−1 cm−2 (cgs).
(†)The Hβ line was affected by a possible cosmic ray in the spectrum, and therefore, Hα flux was used to estimate Hβ flux assuming no dust.
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