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−  == Linear to Circular Conversion ==
 +  [[Linear to Circular Conversion]] 
−  At EOVSA’s linear feeds, in the electric field the linear polarization, X and Y, relates to RCP and LCP (R and L) as:
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−  :<math>
 +  [[Polarization Mixing Due to Feed Rotation]] ([[Polarization Mixing Correction (Old)]]) 
−  \begin{align}
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−  R = X + iY \\
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−  L = X  iY
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−  \end{align}
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−  </math>
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−   +  
−  In terms of autocorrelation powers, we have the 4 polarization products XX*, YY*, XY* and YX*, where the * denotes complex conjugation. The quantities RR* and LL* are then
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−   +  
−  :<math>
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−  \begin{align}
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−  RR^* = (X + iY)(X + iY)^* &= XX^*  iXY^* + iYX^* + YY^* \\
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−  LL^* = (X  iY)(X  iY)^* &= XX^* + iXY^*  iYX^* + YY^* \\
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−  \end{align}
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−  </math>
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−   +  
−  One problem is that there is generally a nonzero delay in Y with respect to X. This creates phase slopes in XY* and YX* from which we can determine the delay very accurately. As a check,
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−   +  
−  :<math>
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−  \begin{align}
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−  Stokes \, I &= \frac{RR^* + LL^*}{2} = XX^* + YY^* \\
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−  Stokes \, V &= \frac{RR^*  LL^*}{2} = i(XX^*  YY^*)
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−  \end{align}
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−  </math>
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−   +  
−  For completeness:
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−   +  
−  :<math>\begin{align}
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−  Stokes \, Q &= XX^*  YY^* \\
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−  Stokes \, U &= XY^*  YX^* \\
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−  P_{linear} &= \sqrt{U^2 + Q^2} \\
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−  \Theta &= \frac{1}{2}\tan^{1}{\frac{U}{Q}}
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−  \end{align}
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−  </math>
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−   +  
−  When I plot the quantities I, V, R and L as measured (Figure 1) for geosynchronous satellite Ciel2, the results look reasonable, except that there are parts of the band where R and L are misassigned, and others where they do not separate well.
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−   +  
−  The problem is that residual phase slope of Y with respect to X, caused by a difference in delay between the two channels. This can be seen in the upper panel of Figure 2, which shows the uncorrected phases of XY* and YX*. To correct the phases, the RCP phase was fit by a linear leastsquares routine, and then the phases were offset by π/2 for both XY* and YX* according to:
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−   +  
−  :<math>\begin{align}
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−  XY^{*'} &= XY^*e^{i(\phi(v) + \frac{\pi}{2})} \\
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−  YX^{*'} &= YX^*e^{ i(\phi(v) + \frac{\pi}{2})}
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−  \end{align}
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−  </math>
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−   +  
−  where φ(v) is the phase fit by the linear function. The corrected phases are shown in the lower panel of Figure 2.
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−   +  
−  When the corrected (primed) quantities are used in
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−   +  
−  :<math>\begin{align}
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−  RR^* &= XX^*  iXY^{*'} + iYX^{*'} + YY^* \\
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−  LL^* &= XX^* + iXY^{*'}  iYX^{*'} + YY^*
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−  \end{align}
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−  </math>
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−   +  
−  the resulting channel separation is shown in Figure 3, which shows pretty much perfect channel separation, with the correct polarity.
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−   +  
−  This analysis can be performed on all antennas in a completely automated way, to produce the results of Fig. 3. The curves for each antenna are very similar, except that they show differences in amplitude (gain) as a function of frequency. When the curves are scaled to have the same Stokes I levels, the result is shown in Figure 4. Here the 13 antennas are shown in different colors. It is clear that matching Stokes I also causes an excellent match in the other polarizations. Remaining mismatch is likely due to not subtracting a nosignal background prior to scaling the Stokes I curves.
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−   +  
−  Also marked in Figure 4 is the location of the beacon signal for Ciel2, which is at 12.209 GHz. The beacon signal appears in precisely the correct bin (frequency subchannel), indicating that we have precise tuning (certainly not unexpected, but nice to see).
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−   +  
−  Just to show that the approach is general, the results for a different communications satellite, Nimiq5, is shown in Figure 5.
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−   +  
−  == Polarization Mixing Correction ==
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−  Due to relative feed rotation between azal mounted antennas and equatorial mounted antennas
 +  