Table 2
Comparison of some telescopes that have operated at frequencies below 200 MHz.
| Telescope | Area | Trec | Tsky | Frequencies | Bandwidth | Nbits | Beams | Transit |
| (m2) | (K) | (K) | (MHz) | (MHz) | ||||
|
|
||||||||
| Arecibo | 30 000 | 5700–5000 | 47–50 | 1 | Restricted | |||
| Cambridge 3.6 ha | 36 000 | 1400 | 81.5 | 1 | 1 | 16 | Yes | |
| DKR-1000 | 5000–8000 | 18 000–500 | 30–120 | 1–2 | Yes | |||
| Gauribidanur | 12 000 | 500 | 30 000–12 000 | 25–35 | 2 | 2 | 1 | Yes |
| GMRT | 48 000 | 295 | 276 | 151 | 16/32 | 8/4 | 2 | No |
| LOFAR (LBA) | 75 200 | 500 | 320 000–1000 | 10–90 | 48 | 16 | < 244 | No |
| LOFAR (HBA) | 57 000 | 140–180 | 630–80 | 110–240 | 48 | 16 | < 244 | No |
| LWA | 1 000 000 | 320 000–1100 | 10–88 | 19.2 | 8 | 4 | No | |
| MRT | 41 000 | 500 | 276 | ~ 150 | 2 | 2 | 1 | Yes |
| MWA | 8000 | 150 | 1400–45 | 80–300 | 32 | 5 | 16(32) | No |
| Nançay Decametric Array | 4000 | 320 000–800 | 10–100 | 32 | 14 | 1 | No | |
| LPA/BSA – Pushchino | 20 000 | 110 | 900 | 109–113 | 2.5 | 12 | 16(32) | Yes |
| UTR-2 | 150 000 | 550 000–9000 | 8–40 | 24 | 16 | 5(8) | No | |
| VLA | 13 000 | 1800 | 74 | 1.56 | 2 | 1 | No | |
| WSRT | 7000 | 400 | 650–175 | 110–180 | 8 × 2.5 | 8 | 1 | No |
Notes. Telescopes that are observing in (parts of) the same frequency range or have done so in the past are considered. The bandwidths presented are those that are used for pulsar observations and do not take into consideration what fraction may not be useful due to radio frequency interference. In the case of LOFAR pulsar observations, only a small fraction of the bandwidth requires masking (see Sect. 6). Note that the collecting area is the maximum and does not take into account efficiencies or hour angle dependent effects. The transit instruments such as the Mauritius Radio Telescope (MRT, Golap et al. 1998), Gauribidanur (Deshpande et al. 1989), and the Cambridge 3.6 ha telescope (Shrauner et al. 1998) have some tracking ability but are usually limited to observing times of a few minutes. The collecting area of Arecibo is based on an illumination equivalent to a 200 m dish. The collecting area for the UTR-2 (Abranin et al. 2001) is quoted for a frequency of 20 MHz and the 5-beam and 8-beam modes are discussed in Ryabov et al. (2010) and Abranin et al. (2001) respectively. The Murchison Widefield Array (MWA) can have 32 single polarisation beams and the area is quoted for a frequency of 200 MHz (Lonsdale et al. 2009). LOFAR can have up to a total of 244 station beams which equals the number of subbands. The Long Wavelength Array (LWA) (Ellingson et al. 2009) collecting area is quoted for a frequency of 20 MHz and decreases as λ2. We note that the LWA and MWA collecting areas are those projected for the final system and are not yet in place. For the LOFAR LBA entry, the effective area is based on using the outermost antenna configuration at a freqeuncy of 30 MHz, which maximizes collecting area. The HBA collecting area is quoted for a frequency of 150 MHz. The GMRT (Swarup et al. 1991), VLA (Cohen et al. 2007) and WSRT (Karuppusamy et al. 2011) are multiple dish interferometers. In some cases, not all parameters are available in the literature and so these entries were left blank. Tsky is an approximate value calculated on a cold piece of sky and is quoted for the full range of available frequencies at that telescope.
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