Table 4.
Main characteristics of Planck frequency maps.
| Frequency [GHz] |
|||||||||
|---|---|---|---|---|---|---|---|---|---|
| Property | 30 | 44 | 70 | 100 | 143 | 217 | 353 | 545 | 857 |
| Frequency [GHz] (a)...... | 28.4 | 44.1 | 70.4 | 100 | 143 | 217 | 353 | 545 | 857 |
| Effective beam FWHM [arcmin] (b)...... | 32.29 | 27.94 | 13.08 | 9.66 | 7.22 | 4.90 | 4.92 | 4.67 | 4.22 |
| Temperature noise level [μKCMB deg] (c)...... | 2.5 | 2.7 | 3.5 | 1.29 | 0.55 | 0.78 | 2.56 | ||
| [kJy sr−1 deg] (c)...... | 0.78 | 0.72 | |||||||
| Polarization noise level [μKCMB deg] (c)...... | 3.5 | 4.0 | 5.0 | 1.96 | 1.17 | 1.75 | 7.31 | ||
| Dipole-based calibration uncertainty [%] (d)...... | 0.17 | 0.12 | 0.20 | 0.008 | 0.021 | 0.028 | 0.024 | ∼1 | |
| Planet submm inter-calibration accuracy [%] (e)...... | … | … | … | … | … | … | … | … | ∼3 |
| Temperature transfer function uncertainty [%] (f)...... | 0.25 | 0.11 | Ref. | Ref. | 0.12 | 0.36 | 0.78 | 4.3 | |
| Polarization calibration uncertainty [%] (g)...... | < 0.01% | < 0.01% | < 0.01% | 1.0 | 1.0 | 1.0 | … | … | … |
| Zodiacal emission monopole level [μKCMB] (h)...... | 0 | 0 | 0 | 0.43 | 0.94 | 3.8 | 34.0 | … | … |
| [MJy sr−1] (h)...... | … | … | … | … | … | … | … | 0.04 | 0.12 |
| LFI zero level uncertainty [μKCMB] (i)...... | ±0.7 | ±0.7 | ±0.6 | … | … | … | … | … | … |
| HFI Galactic emission zero level uncertainty [MJy sr−1] (j)...... | … | … | … | ±0.0008 | ±0.0010 | ±0.0024 | ±0.0067 | ±0.0165 | ±0.0147 |
| HFI CIB monopole assumption [MJy sr−1] (k)...... | ±0.0030 | ±0.0079 | 0.033 | 0.13 | 0.35 | 0.64 | |||
| HFI CIB zero level uncertainty [MJy sr−1] (l)...... | … | … | … | ±0.0031 | ±0.0057 | ±0.016 | ±0.038 | ±0.066 | ±0.077 |
Notes.
For LFI channels (30–70 GHz), this is the centre frequency. For HFI channels (100–857 GHz), it is a reference (identifier) frequency.
Estimates of noise in intensity and polarization scaled to 1° assuming that the noise is white. These levels are unchanged from 2015.
The 857 GHz channel retains the 2015 planet calibration, and the accuracy is calculated a posteriori using a model of planet emission (Planck Collaboration Int. LII 2017) and the 545 GHz data.
For LFI this is the ratio of 30 and 44 GHz half-ring cross-spectra in the range ℓ ≃ 50–850 to that of the 70 GHz cross-spectrum. For HFI it is the upper limit derived from the levels of the first three CMB acoustic peaks (ℓ ≃ 15–1000), relative to the 100 GHz channel.
Additional calibration uncertainty applicable to Q and U only. For LFI, the additional uncertainty (based on simulations) is negligible. For HFI, the dominant inaccuracy is the knowledge of the polarization efficiency, which is currently derived from the relative levels of the first three CMB acoustic peaks (ℓ ≃ 15–1000), in combination with a prediction of the best-fit TT-based cosmology. The best estimates (Planck Collaboration III 2020) indicate that a bias should be applied to the maps of 0.7, −1.7, and 1.9%, at 100, 143, and 217 GHz, respectively, with an uncertainty as indicated in this table.
Average contribution of the zodiacal emission to the monopole. As the level of this emission is dependent on the time of observation, it has been removed from the frequency maps during processing.
Estimated uncertainty in the zero levels associated with Galactic emission. The zero levels were set by fitting a model of Galactic emission that varies as the cosecant of the latitude to the maps after CMB subtraction. The levels subtracted were 11.9, −15.4, and −35.7 μKCMB at 30, 44, and 70 GHz, respectively.
The zero levels of the HFI maps are set by correlating the Galactic emission component to a map of the diffuse H I column density, as in Planck Collaboration VIII (2014). The uncertainties in the estimated zero levels are unchanged since 2013.
Once the Galactic zero level has been set, the monopole of the Béthermin et al. (2012) CIB model has been added to the frequency maps.
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