Table 1
10σ detection limits applied to high-z simulated LARS images.
| F(Lyα) | m(rest-frame UV) | F(Hα) | m(rest-frame optical) |
| erg s-1 cm-2 | AB | erg s-1 cm-2 | AB |
|
|
|||
| 5E-19 | 30 | 2E-19 | 29 |
| 3E-18 | 29 | 6E-19 | 28 |
| 8E-18 | 28 | 1E-18 | 27 |
| 2E-17 | 27 | 3E-18 | 26 |
| 5E-17 | 26 | 1E-17 | 25 |
Notes. Noise corresponding to the detection limits given in the table was added to LARS continuum and line images. As LARS Lyα and Hα(rest-UV and optical continua) images are in units of flux(flux density), the image depths are given in units of erg s-1cm-2 (AB magnitudes). The MUSYC (Guaita et al. 2010; Bond et al. 2012) NB3727 survey implied a 10σ detection limit of F(Lyα) = 5E-17 erg s-1 cm-2. MUSYC U,B (HUDF V606) 10σ detection limits were about 26(29.5). Assuming a NB3727 filter width and transmission profile, a source with mAB(rest-frame UV) = 30 and EW(Lyα) = 20 Å is characterized by F(Lyα) = 5E-19 erg s-1 cm-2. mAB(rest-frame UV) = 30, 29, 28 are consistent with HUDF09, GOODS, and GEMS survey depths (Bond et al. 2009). Lee et al. (2012) survey was characterized by a 10σ detection limit of 22.9 in NB210 and 23.7 in K. CANDELS wide(deep) F160W 10σ detection limit was 25.8(26.5). Assuming a NB210 filter width, a source with mAB(rest-frame optical) = 27 and EW(Hα) = 20 Å is characterized by F(Hα) = 2E-19 erg s-1 cm-2.
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