Table 3.
Lower limits of FARMER LP power spectra, when Δk = 0.3 Mpc−1.
| k3P(k)/2π2 ((Jy sr−1)2) | ||||
|---|---|---|---|---|
| k (Mpc−1) | 0.25–0.55 | 0.55–0.85 | 0.85–1.15 | 1.15–1.45 |
| 3.42 < z < 3.87 | 2.11×106 | 1.06×107 | 3.06×107 | 6.56×107 |
| 4.14 < z < 4.76 | 9.93×105 | 5.29×106 | 1.43×107 | 3.26×107 |
| 5.34 < z < 6.31 | 7.66×104 | 3.58×105 | 9.80×105 | 2.07×106 |
| 6.75 < z < 8.27 | 2.16×104 | 9.80×104 | 2.77×105 | 6.26×105 |
Notes. For most redshift bands this minimum model comes from Si15, with the exception of 6.75 < z < 8.27 where the minimum is m4 (Fig. 9). Due to the averaging of power spectra within these wide bins, there are slight discrepancies on clustering scales when comparing these power spectra to those with narrower bin sizes (and so higher frequency resolution).
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