Table 2.
Parameter fits to HM power spectra.
| Pipeline | ACMB | n | Aptsrc (μK2) | χ2 |
|---|---|---|---|---|
| TT | ||||
| Commander........ | 0.997 ± 0.002 | −0.003 ± 0.004 | 2.7 ± 0.5 | 61.6 |
| NILC........ | 0.994 ± 0.002 | −0.006 ± 0.004 | 1.9 ± 0.6 | 59.3 |
| SEVEM........ | 0.996 ± 0.002 | −0.001 ± 0.004 | 2.1 ± 0.6 | 60.3 |
| SMICA........ | 0.996 ± 0.002 | −0.001 ± 0.002 | 1.9 ± 0.5 | 58.5 |
| EE | ||||
| Commander........ | 0.985 ± 0.007 | −0.002 ± 0.009 | 0.35 ± 0.06 | 74.0 |
| NILC........ | 0.984 ± 0.007 | −0.007 ± 0.010 | 0.26 ± 0.08 | 70.3 |
| SEVEM........ | 0.983 ± 0.008 | −0.001 ± 0.010 | 0.27 ± 0.08 | 62.7 |
| SMICA........ | 0.983 ± 0.007 | −0.002 ± 0.008 | 0.30 ± 0.08 | 66.7 |
Notes. In each case, the observed spectrum is taken as the difference between the HMHS and HMHD spectra, and the model fitted reads 
, where fℓ is the transfer function shown in Fig. 11, ℓ0 = 600, and ℓps = 500. 
is the best-fit Planck 2018 ΛCDM power spectrum. Each analysis includes multipoles between ℓ = 2 and 1500. Spectra are binned with Δℓ = 20. The uncertainties within each bin are defined as the standard deviation of the observed spectrum within the bin. The number of degrees of freedom for the χ2 is nd.o.f. = 75.
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