Table 1.
Correlation coefficients between known diffuse foreground templates and each of the four component-separated CMB maps.
| Correlation coefficient |
|||||
|---|---|---|---|---|---|
| Data set | Commander | NILC | SEVEM | SMICA | |
| Intensity | |||||
| Haslam........ | 2018 | −0.037 ± 0.134 | −0.023 ± 0.135 | −0.055 ± 0.077 | −0.027 ± 0.077 |
| 2015 | −0.062 ± 0.115 | −0.051 ± 0.116 | −0.065 ± 0.115 | −0.023 ± 0.069 | |
| Hα........ | 2018 | 0.000 ± 0.032 | 0.006 ± 0.032 | 0.003 ± 0.028 | 0.004 ± 0.028 |
| 2015 | 0.010 ± 0.071 | 0.011 ± 0.071 | 0.019 ± 0.071 | 0.003 ± 0.057 | |
| CO........ | 2018 | −0.002 ± 0.019 | 0.000 ± 0.019 | 0.001 ± 0.020 | 0.001 ± 0.020 |
| 2015 | −0.004 ± 0.027 | 0.003 ± 0.027 | 0.003 ± 0.027 | −0.007 ± 0.022 | |
| 857 GHz........ | 2018 | −0.033 ± 0.097 | −0.019 ± 0.097 | −0.018 ± 0.098 | −0.019 ± 0.098 |
| 2015 | −0.043 ± 0.084 | −0.032 ± 0.084 | −0.037 ± 0.084 | −0.029 ± 0.083 | |
| Polarization | |||||
| WMAP K–Ka........ | 2018 | −0.031 ± 0.011 | −0.037 ± 0.011 | −0.039 ± 0.011 | −0.033 ± 0.011 |
| 2015 | −0.057 ± 0.026 | −0.116 ± 0.024 | −0.026 ± 0.025 | −0.027 ± 0.026 | |
Notes. The intensity templates are: (1) a 408 MHz map for synchrotron emission from Haslam et al. (1982); (2) an Hα template for free-free emission from Finkbeiner (2003); (3) a tracer of CO emission in the Galactic plane from Dame et al. (2001); and (4) the Planck 857 GHz map for thermal dust emission. For polarization, we only include the difference between the WMAP K (23 GHz) and Ka (33 GHz) frequency maps as a synchrotron tracer. All maps have been smoothed to a common resolution of 80′ FWHM prior to the fitting process, and the correlation coefficients are evaluated outside the confidence masks described in Sect. 4.2.
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