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 The selection of these six clusters was based 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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The parallel blank field positions are constrained by the availability of HST guide stars, which permit > 30-day windows of fixed roll-angle observations with both ACS and WFC3 at both the cluster and blank field positions. From the available locations, the final parallel field location was based primarily upon the ability to obtain very deep, high quality imaging in both HST and Spitzer. Therefore the avoidance of bright stars which would cause scattered light, saturated columns, and persistence took precedence over the avoidance of extended cluster structures.
Locations on the sky of the Frontier Fields Locationsare shown below.
