Table 4
Estimates for detecting galactic plane RRLs with LWA-1.
| ν | n | f | Nlines | DF | Tsys | Δtint |
| (MHz) | (×104 K) | (h) | ||||
|
|
||||||
| 20 | 683 | 0.92 | 10 | 0.26 | 29.5 | 50 |
| 25 | 640 | 0.87 | 8 | 0.41 | 18.3 | 28 |
| 30 | 603 | 0.76 | 12 | 0.59 | 12.4 | 6 |
| 35 | 572 | 0.63 | 10 | 0.8 | 8.9 | 5.5 |
| 40 | 548 | 0.5 | 8 | 1 | 6.7 | 7 |
| 45 | 526 | 0.4 | 6 | 1 | 5.2 | 15 |
| 50 | 508 | 0.33 | 6 | 1 | 4.1 | 23 |
| 55 | 492 | 0.27 | 10 | 1 | 3.3 | 10 |
| 60 | 478 | 0.23 | 10 | 1 | 2.7 | 14 |
| 65 | 466 | 0.2 | 8 | 1 | 2.3 | 24 |
| 70 | 454 | 0.17 | 8 | 1 | 1.9 | 32 |
| 75 | 444 | 0.15 | 6 | 1 | 1.7 | 56 |
| 80 | 434 | 0.13 | 6 | 1 | 1.4 | 72 |
Notes. Tsys is derived from the GSM sky models (de Oliveira-Costa et al. 2008). It is the average temperature along the Galactic Plane towards Galactic center (−5° < b < 5°, 340° < ℓ < 20°) after convolving the models to LWA-1 beam size and removing the pixels with the highest and lowest 2% of intensity. The dilution factor, DF, assumes 4° cloud sizes. The filling factor f is derived using the station dipole layout design (Kogan & Cohen 2009) and accounts for overlaps and edge effects. Nlines is based on two contiguous bands with roughly 2 km s-1 velocity resolution. The integration time to detect lines with optical depths of 10-4 is 100× the values listed here.
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