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Linear polarized light has been used to view the solar corona for over 150years. While the familiar Stokes representation for polarimetry is complete, itis best matched to a laboratory setting and therefore is not the mostconvenient representation either for coronal instrument design or for coronaldata analysis. Over the last 100 years of development of coronagraphs andheliospheric imagers, various representations have been used both for directmeasurement and analysis. These systems include famous representations such asthe (B, pB) system that is analogous to the Stokes system in solar observingcoordinates, and also internal representations such as in-instrument Stokesparameters with fixed or variable "vertical" direction, and brightness valuesthrough a particular polarizing optic or set thereof. Many polarimetricinstruments currently use a symmetric three-polarizer measurement andrepresentation system, which we refer to as "(M, Z, P)", to derive the (B, pB)or Stokes parameters. We present a symmetric derivation of (B, pB) and Stokesparameters from (M, Z, P), analyze the noise properties of (M, Z, P) in thecontext of instrument design, develop (M, Z, P) as a useful intermediate systemfor data analysis including background subtraction, and draw a helpful analogybetween linear polarimetric systems and the large existing body of work onphotometric colorimetry.

Three-Polarizer Treatment of Linear Polarization in Coronagraphs and Heliospheric Imagers