Table 6.
Best-fit power-law parameters to the angular power spectra of synchrotron (30 GHz) and thermal dust emission (353 GHz), evaluated with the XPol power spectrum estimator (Tristram et al. 2005) as detailed in Planck Collaboration XI (2020).
q [ ] |
α | |
|---|---|---|
| Thermal dust,fsky = 0.42, ℓ = 40 − 600 | ||
| Commander | ||
| EE........ | 60 ± 2 | −0.39 ± 0.03 |
| BB........ | 32 ± 1 | −0.49 ± 0.05 |
| BB/EE........ | 0.52 | |
| SMICA | ||
| EE........ | 62 ± 2 | −0.18 ± 0.04 |
| BB........ | 32 ± 1 | −0.45 ± 0.05 |
| BB/EE........ | 0.48 | |
| Frequency map cross-correlation | ||
| EE........ | 59 ± 2 | −0.28 ± 0.04 |
| BB........ | 32 ± 1 | −0.48 ± 0.06 |
| BB/EE........ | 0.50 | |
| Thermal dust,fsky = 0.78, ℓ = 40 − 600 | ||
| Commander | ||
| EE........ | 323 ± 4 | −0.40 ± 0.01 |
| BB........ | 199 ± 3 | −0.50 ± 0.02 |
| BB/EE........ | 0.57 | |
| SMICA | ||
| EE........ | 318 ± 4 | −0.34 ± 0.01 |
| BB........ | 205 ± 3 | −0.55 ± 0.02 |
| BB/EE........ | 0.54 | |
| Frequency map cross-correlation | ||
| EE........ | 313 ± 4 | −0.41 ± 0.01 |
| BB........ | 187 ± 3 | −0.50 ± 0.02 |
| BB/EE........ | 0.57 | |
| Synchrotron,fsky = 0.78, ℓ = 4 − 140 | ||
| Commander | ||
| EE........ | 2.3 ± 0.1 | −0.84 ± 0.05 |
| BB........ | 0.8 ± 0.1 | −0.76 ± 0.09 |
| BB/EE........ | 0.34 | |
| SMICA | ||
| EE........ | 2.4 ± 0.2 | −0.88 ± 0.04 |
| BB........ | 0.9 ± 0.2 | −0.75 ± 0.07 |
| BB/EE........ | 0.34 | |
Notes. Frequency cross-correlation results are derived using precisely the same methodology as in Planck Collaboration XI (2020), while Commander and SMICA results are derived using the same power spectrum estimation tools, but applied to the half-mission maps presented in this paper. Note that all uncertainties are statistical, and do not account for systematic or modelling uncertainties. Power spectrum amplitudes refer to monochromatic reference frequencies of 30 and 353 GHz for synchrotron and thermal dust emission, respectively.
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