Table 3
Future telescope capabilities.
| Name | Frequency | Resolution | Filling factor | Tdetect |
| (MHz) | (h) | |||
|
|
||||
| LWA-1 | 20–80 | 9°–2° | 0.9–0.1 | ~10 |
| LOFAR-LBA | 30–90 | 2°–0.6° | ~0.1 | ~10 |
| LOFAR-HBA | 110–240 | 30′–15′ | ~0.1 | ... |
| SKA-lo | 150 | 7′ | ~0.1 | <10 |
| LRA | 100 | 10′ | ~0.9 | <10 |
Notes. Values listed are characteristic or indicative, but none of these telescopes have entered an operational state, so actual performance may vary. For LOFAR-LBA, bandwidths of 48 MHz have been assumed. LOFAR-HBAcovers a poorly explored frequency range in which the lines may become undetectable as they transition from emission at higher frequencies to absorption at lower frequencies; the same may also be true of SKA-lo. Particularly for the SKA-lo and LRA, final design parameters are yet to be determined, and these values are indicative.
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