Table 7.
Relative calibration between NPIPE and PR3 maps and the NPIPE gain uncertainty estimated from recovery of the injected dipole in simulated full-frequency maps.
| Frequency | 2018 gain(a) | MC gain(b) | MC bias(c) |
|---|---|---|---|
| [GHz] | [%] | [%] | [%] |
| 30..... | 99.793 | 99.975 ± 0.045 | −0.025 ± 0.005 |
| 44..... | 99.763 | 99.990 ± 0.040 | −0.010 ± 0.004 |
| 70..... | 99.959 | 99.997 ± 0.030 | −0.003 ± 0.003 |
| 100..... | 100.061 | 100.016 ± 0.023 | 0.016 ± 0.002 |
| 143..... | 100.082 | 100.016 ± 0.018 | 0.016 ± 0.002 |
| 217..... | 100.005 | 100.024 ± 0.024 | 0.024 ± 0.002 |
| 353..... | 100.463 | 100.052 ± 0.053 | 0.052 ± 0.005 |
| 545(d)..... | 115.123 | 99.586 ± 0.571 | 0.414 ± 0.057 |
Notes.
(a) Relative calibration, NPIPE / 2018, measured over 50% of the sky after adding the Solar dipole back into 2018 maps and smoothing the maps with a 1° Gaussian beam.
(b) Distribution centre and width, measured relative to the input signal.
(c) This is the average calibration error and the associated uncertainty. A 0.03% bias in calibration corresponds to about 1 μKCMB in Solar dipole amplitude.
(d) The NPIPE 545 GHz calibration is based on the orbital dipole, and does not suffer from the 10% modelling uncertainty affecting the planet-based calibration in the 2018 release. We also calibrate directly into KCMB, without needing a unit conversion factor with additional uncertainty.
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