Table 3
Expectations for lensed SNe in the multiply-imaged galaxies behind A1689 and A370 observed with JWST/NIRCam-like filters in one year.
| Filter | Nepochs |
|
|
|
|
|---|---|---|---|---|---|
| (yr) | |||||
| A370 | |||||
| F115W | 4 | 0.11 ± 0.04 | 0.02 ± 0.01 | 3.77 | 47 |
| F115W | 12 | 0.4 ± 0.1 | 0.06 ± 0.03 | 3.77 | 47 |
| F150W | 4 | 0.3 ± 0.1 | 0.02 ± 0.01 | 3.77 | 47 |
| F150W | 12 | 0.9 ± 0.5 | 0.06 ± 0.03 | 3.77 | 47 |
| A1689 | |||||
| F115W | 4 | 0.7 ± 0.3 | 0.13 ± 0.06 | 3.05 | 66 |
| F115W | 12 | 1.0 ± 0.5 | 0.17 ± 0.08 | 3.05 | 66 |
| F150W | 4 | 1.0 ± 0.5 | 0.14 ± 0.07 | 3.05 | 66 |
| F150W | 12 | 1.4 ± 0.6 | 0.17 ± 0.08 | 3.05 | 66 |
Notes. The depth of the survey in both filters is assumed to be 27.5 mag, which is the limiting 5σ depth for a 1 h exposure (Beichman et al. 2012). The separation between two epochs is set to 30 days. The errors in the NCC and NIa originate from the propagated uncertainty in the SFR. (a)The number of expected SNe in the background galaxies with resolved multiple images and secure redshifts (see Table 2). (b)The maximum redshift of the expected SNe. (c)Number of galaxies that can host observable SNe.
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