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Table 2:

Worksheet for estimating the magnitude of polconversion due to bandpass mismatch in the Planck frequency bands, over the full sky (``4$\pi $'') and over pixels outside the WMAP KQ85 mask (``Mask'').
    CMB emission Foreground emission     Polconversion ${\cal M}_{QI}I^{\rm F}$
Band Region $\sigma(I)$a $\sigma(Q,U)$a $\langle I^{\rm F} \rangle$b $\langle \sqrt{Q^2+U^2}\rangle$c $\langle \beta \rangle$b $\tilde{\beta}$b,d $\nu_0$ $\sigma(\nu_{\rm eff})$e rmsf Abs Maxf
    ($\mu$K) ($\mu$K) ($\mu$K) ($\mu$K)     (GHz) (GHz) ($\mu$K) ($\mu$K)
30 GHz $4\pi$ 85 0.94 410 13 -2.89 -2.63 28.11 0.29 28.0 1300
Mask 110 10 -2.92 -2.87 1.7 28
44 GHz $4\pi$ 89 1.31 130 4 -2.61 -2.36 43.81 0.21 4.6 210
Mask 30 3 -2.64 -2.56 0.2 2
70 GHz $4\pi$ 89 1.91 60 3 -0.46 -0.60 69.54 1.35 1.9 140
Mask 16 2 -0.46 -0.24 0.1 12

Notes.  $\langle X \rangle$denotes area-weighted mean values. Zonca et al. (2009) bandpasses were used to calculate $\nu_0$, $\nu _{\rm eff}$, and ${\cal M}_{QI}$. (a) rms after convolution with the beam; (b) foreground temperature, $I^{\rm F}$, and spectral index, $\beta $, from the Planck sky model; (c) foreground polarisation, interpolated from WMAP; (d) flux-weighted mean spectral index; (e) standard deviation of $\nu_{\rm eff}(\bar{\beta})$ over the detectors in each band; (f) rms and extreme value of the polconversion signal (mean over RCAs in each band).


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