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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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Many of the new and projected large telescopes operate with a Nasmyth focus using a tertiary mirror at 45 The problem that this introduces to polarimetry with discussion on the measures that can be taken to address the issues has been presented by Tinbergen (2007) It may be noted that an alt-azimuth mounting can be advantageous because any telescope instrumental polarization can be determined by comparing the results obtained for the same star either side of the meridian, the whole optical system suffering rotation around the observed direction as the hour angle changes sign This is common practice in radio astronomy For equatorially mounted telescopes, any polarization produced by the mirrors can be explored and eliminated by rotating the entire telescope tube together with the mirrors In the 1960s, two 2400 Cassegrain rotatable telescopes were specially designed for polarimetric use (see Hiltner & Schild, 1965), and these were instrumental in setting up set of unpolarized standard stars In the Northern Hemisphere (Yerkes Observatory), Appenzeller (1968) made use of the instrument in his survey of the galactic pole and in the Southern Hemisphere (Siding Spring in Australia), an important study was made by Serkowski, Mathewson & Ford (1975) The project established a number of nearby stars of intermediate spectral types for which no linear polarization was detectable within the limits of the measurement error It may also be noted that some of the early investigations of interstellar polarization were conducted with large refractor telescopes Again it would be expected that the circular symmetry of the collection aperture in the form of an objective lens should not introduce any spurious instrumental polarization However, Serkowski (1960) drew attention to the effects of stress birefringence that can occur in the glass material of the lenses The small phase changes that are produced effectively decrease the measured values for the degree of linear polarization Using the 26-inch refractor in Belgrade, Krzemi ski (1959) measured the polarization of 23 n stars with known interstellar 4430 band intensities Comparison with the measurements by Hiltner of the same stars showed that the values were systematically smaller, but that they were reconcilable by considering the Belgrade objective to act as a phase plate with a retardance of 1/14 of a wave According to Serkowski (1960), in view of the thickness of the lenses, such a value of phase delay is not unexpected In some cases, instrumental polarization may have components generated in the optics of the modulator itself, or in the electronic gating of the signal For example, if a rotating wave plate s employed as part of the modulator, as well as its phase delay, it also acts as a weak partial polarizer, this affecting the signal to some degree The opening and closing of gates synchronously with the modulator s position to allow sampling over sections of the oscillatory signal needs to be timed to high accuracy and be free from drift For high accuracy and precision in polarimetric observations, stability of operation is important Such aims are best achieved by having telescopes that are dedicated solely to polarimetry The results published by Kemp s group at the University of Oregon and by the Wisconsin group (see Nordsieck, Babler, Bjorkman, et al, 1992) owe their success to this Unfortunately, this means that available apertures will inevitably be fairly small, limiting such polarimetric studies to the brighter stars.

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