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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 elescope 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 is 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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the single-scattering plus attenuation prediction For these reasons, the combined effects of multiple scattering, plus absorptive opacity, provides much larger polarization discontinuities at the Balmer jump than previous predictions For geometrically thick equatorial disc-like geometries, a position angle ip of 90 can occur shortward of the Balmer jump as the large hydrogen opacity absorbs the multiply scattered photons in the disc, the polarization dominated by singly scattered photons from the polar regions producing negative values of Q Using a Monte Carlo radiative transfer code in respect of spectropolarimetric data, Wood, Bjorkman & Bjorkman (1997) investigated possible geometries for Tau It turned out that the observations could be mimicked by either a geometrically thin disc, with a half-opening angle of 2 5, or a thick disc with a half-opening angle of 56 Key to determining which option should be preferred is the prediction for the thin disc model to produce a polarization ip at 12 m, so that it is orthogonal relative to what is recorded in the visible spectrum As for interpretations and modelling of p ( ) and the intrinsic polarizations associated with the emission lines themselves, McLean (1979) discussed the issues with physical insight The paper demonstrates that all axisymmetric, quasi-optically thin Be star envelopes have approximately the same form of p ( ) in the continuum and that the behaviour is controlled by the average properties of the envelope The size of the oscillation of the position angle across the emission lines, as well as depending on the optical depths of the envelope, is shown to be proportional to cos i A numerical model for the behaviour of Cas was presented by Poeckert & Marlborough (1978a) by assuming a density distribution in a rotating, expanding envelope, with the hydrogen level populations determined appropriately at points through the envelope The Balmer line intensities and polarimetric pro les were then determined by integrating the equation of radiative transfer along the lines of sight, and so including stellar disc occultation effects in the process The exercise was successful in predicting the observed behaviour across the H line An investigation of the physical factors that control the behaviour of p ( ) and ( ) across emission line pro les has been made by Wood, Brown & Fox (1993) based on Thomson scattering in an optically thin circumstellar cloud which is subject to bulk motions in the form of a rotating and/or expanding disc The value of p is asymmetric about the line centre and stronger in the red wing unless there is no disc expansion Changes in across the line occur through the symmetry breaking effects of stellar occultation of the scattering material, and the combination of rotation and expansion of the disc A symmetric p pro le indicates envelope rotation, while pro les which show stronger p in the red wing indicate expansion of a scattering region The ratio of p in the red and blue wings should lead to information on the ratios of expansion to rotation velocities In a later paper, Wood & Brown (1994a) developed the model by considering the star to act as a monochromatic source for scattering by a rotating and expanding isc, the assumption being reasonably realistic, the line broadening being dominated by the scattering rather than in its origins By assuming certain parametric forms for the disc velocity and density distributions, analytic expressions were obtained for the wavelength dependence of the scattered pro les in terms of the veloc-.

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