Table 4
Limits of detection for LARS galaxies simulated to z ~ 2.
| ID | mrest − UV | mrest − optical | F(Lyα) | F(Hα) |
| AB | AB | erg s-1 cm-2 | erg s-1 cm-2 | |
|
|
||||
| L01lae | 28 | 26 | 8E-18 | 3E-18 |
| L02lae | 29 | 27 | 8E-18 | 1E-18 |
| L03 | 29 | 25 | 3E-18 | 3E-18 |
| L05lae | 27 | 26 | 8E-18 | 3E-18 |
| L07lae | 28 | 26 | 2E-17 | 3E-18 |
| L08lae | 28 | 25 | 8E-18 | 3E-18 |
| L09 | 28 | 27 | 5E-19 | 1E-17 |
| L10 | 28 | 25 | 5E-19 | 1E-18 |
| L11 | 28 | 26 | 3E-18 | 3E-18 |
| L12 | 26 | 26 | 3E-18 | 3E-18 |
| L13 | 28 | 27 | 8E-18 | 3E-18 |
| L14lae | 27 | 27 | 5E-17 | 1E-17 |
Notes. Almost all LARS galaxies would be detected in Lyα at a 10σ detection limit depth of 3E-18 erg s-1 cm-2. The exceptions are L09 and L10, which show strong absorption in their Lyα images (Fig. C.4). LARS-LAEs would be detected in shallower surveys. Also, the majority of LARS galaxies would be detected in Hα at a depth of 3E-18 erg s-1 cm-2.
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