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In the design of Bailey & Hough (1982), the two beams emerging from the double-beam polarizer were fed to detectors of different spectral sensitivity One arm was capable of making measurements through the visual range, while the other allowed near infrared observations By using a rotating superachromatic retarder rior to the polarizer, the instrument was able to make UBVRIJHK measurements, according to the lter selection Using a rotating achromatic wave plate modulator, followed by dichroic lters, a system allowing the monitoring in eight different passbands simultaneously has been described by Kikuchi (1988) The Dollfus design of modulator was developed by Tinbergen (1972) to incorporate achromatic wave plates Tinbergen s prototype used plastic components for the compound wave plates, and the instrument, even in this primitive form, proved to be successful A further improvement was suggested by Chen (1979), which involved a Pancharatnam type wave plate with uniform retardation and no variation of reference axis orientation over the range 035 1 m Most of the early spectropolarimeters incorporated lters to achieve spectral resolution A signi cant development in terms of spectral resolution and exibility of selected passbands was made by Wolstencroft & Nandy (1971) They converted a wavelength scanning spectrometer to allow polarimetry at sequential positions in the spectrum; the single pixel nature of the photomultiplier detector, however, necessitated long observing runs to achieve data with good spectral coverage The PEM is particularly clean in that it produces an oscillating phase delay with little or no polarizance, making it very suitable for the detection and measurement of circular polarization The pioneering work of producing this device and applying it to Astronomy was undertaken by J C Kemp An early successful instrument that provided measurements of 15 objects was described by Kemp, Wolstencroft & Swedlund (1972); its development formed the basis of the production of many papers involving new astrophysical scenarios, and it was described again in Kemp & Barbour (1981) A PEM system was also used by Wolstencroft, Cormack, Campbell, et al (1983) prior to a standard spectrometer, with a photomultipler as the detector The instrument was able to explore p ( ) structure by sequential scanning through the spectrum An instrument of very high sensitivity using a PEM has recently been developed by Hough, Lucas, Bailey, et al (2006) with the aim of discovering extrasolar planets by polarimetry An early form of spectropolarimeter was devised by Nordsieck (1974) whereby fringes were imposed on the recorded spectra, their modulation carrying information on the Stokes parameters The optical system included two thick multi-order quartz wave plates, the rst 1 mm thick, the second 3 mm thick, and adjustable in orientation relative to the rst One of the best sets of data related to polarimetric structure across the Balmer lines of Be stars, and still remaining so, is that presented by McLean, Coyne, Frecker, et al (1979) Their spectropolarimeter used a Digicon as the detector, the device offering a photon counting system with 200 silicon diodes in two parallel rows, all contained in the same glass envelope The records were obtained without sequential scanning through the spectrum Unfortunately the Digicon systems had short.

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In the design of Bailey & Hough (1982), the two beams emerging from the double-beam polarizer were fed to detectors of different spectral sensitivity One arm was capable of making measurements through the visual range, while the other allowed near infrared observations By using a rotating superachromatic retarder prior to the polarizer, the instrument was able to make UBVRIJHK measurements according to the lter selection Using a rotating achromatic wave plate modulator, followed by dichroic lters, a system allowing the monitoring in eight different passbands simultaneously has been described by Kikuchi (1988) The Dollfus design of modulator was developed by Tinbergen (1972) to incorporate achromatic wave plates Tinbergen s prototype used plastic components for the compound wave plates, and the instrument, even in this primitive form, proved to be successful A further improvement was suggested by Chen (1979), which involved a Pancharatnam type wave plate with uniform retardation and no variation of reference axis orientation over the range 035 1 m Most of the early spectropolarimeters incorporated lters to achieve spectral resolution A signi cant development in terms of spectral resolution and exibility of selected passbands was made by Wolstencroft & Nandy (1971) They converted a wavelength scanning spectrometer to allow polarimetry at sequential positions in the spectrum; the single pixel nature of the photomultiplier detector, however, necessitated long observing runs to achieve data with good spectral coverage The PEM is particularly clean in that it produces an oscillating phase delay with little or no polarizance, making it very suitable for the detection and measurement of circular polarization The pioneering work of producing this device and applying it to Astronomy was undertaken by J C Kemp An early successful instrument that provided measurements of 15 objects was described by Kemp, Wolstencroft & Swedlund (1972); its development formed the basis of the production of many papers involving new astrophysical scenarios, and it was described again in Kemp & Barbour (1981) A PEM system was also used by Wolstencroft, Cormack, Campbell, et al (1983) prior to a standard spectrometer, with a photomultipler as the detector The instrument was able to explore p ( ) structure by sequential scanning through the spectrum An instrument of very high sensitivity using a PEM has recently been developed by Hough, Lucas, Bailey, et al (2006) with the aim of discovering extrasolar planets by polarimetry An early form of spectropolarimeter was devised by Nordsieck (1974) whereby fringes were imposed on the recorded spectra, their modulation carrying information on the Stokes parameters The optical system included two thick multi-order quartz wave plates, the rst 1 mm thick, the second 3 mm thick, and adjustable in orientation relative to the rst One of the best sets of data related to polarimetric structure across the Balmer lines of Be stars, and still remaining so, is that presented by McLean, Coyne, Frecker, et al (1979) Their spectropolarimeter used a Digicon as the detector, the device offering a photon counting system with 200 silicon diodes in two parallel rows, all contained in the same glass envelope The records were obtained without sequential scanning through the spectrum Unfortunately the Digicon systems had short.

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