Page History
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| Cluster Name | z | Cluster | Parallel Field | HST FOV | Regions File | ||
|---|---|---|---|---|---|---|---|
| RA | Dec | RA | Dec | ||||
| Year 1: | |||||||
| Abell 2744 | 0.308 | 00:14:21.2 | -30:23:50.1 | 00:13:53.6 | -30:22:54.3 |
| regions |
| MACSJ0416.1-2403 | 0.396 | 04:16:08.9 | -24:04:28.7 | 04:16:33.1 | -24:06:48.7 | regions | |
| Year 2: | |||||||
| MACSJ0717.5+3745 | 0.545 | 07:17:34.0 | +37:44:49.0 | 07:17:17.0 | +37:49:47.3 | regions | |
| MACSJ1149.5+2223 | 0.543 | 11:49:36.3 | +22:23:58.1 | 11:49:40.5 | +22:18:02.3 | regions | |
| Year 3: | |||||||
| Abell S1063 (RXCJ2248.7-4431) | 0.348 | 22:48:44.4 | -44:31:48.5 | 22:49:17.7 | -44:32:43.8 | regions | |
| Abell 370 | 0.375 | 02:39:52.9 | -01:34:36.5 | 02:40:13.4 | -01:37:32.8 | regions | |
These were selected primarily on their predicted lensing strength*, their low/moderate zodiacal and Galactic backgrounds, their observability with ALMA and Mauna Kea, and their observability with HST and Spitzer. We've also looked at their suitability for deep radio observations, and their existing multi-wavelength data observations.
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