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one pair of images will carry a direction of vibration orthogonal to that of the other pair Measurement of the polarizations allows the directions of vibration to be referred to the line joining the images which in turn can be related to equatorial coordinates via the catalogued coordinates of the pair of stars Most new polarimetric studies do not undertake fundamental observational procedures as outlined above, but determine the instrumental axis by reference to. 8102 Standard Stars 81021 Polarized Standards For all new observational polarimetric studies, it is important to have standard stars available for concurrent measurement These should comprise stars with a constant, high level of polarization polarized standards with values of p and position angle, known to high levels of accuracy, to provide a reference axis for the instrument on the telescope, and to allow calibration of its modulation ef ciency Another set of stars known to be stable with polarization so small as not to be detectable unpolarized standards should also be available to allow investigation of any instrumental polarization (see Section 55) For the polarized standards, it may also be important to know their wavelength-dependent behaviour A problem associated with the provision of standards for position angle was exposed by Gehrels & Silvester (1970) who discovered that many stars exhibit spectral dispersion in this parameter, possibly as a result of complications in the interstellar clouds along the line of sight Many observationalists refer to tables within Serkowski (1974b), which provide a selection of standard stars; his Polarized Standards are re-listed in Table 81 and the Unpolarized Standards are given in Table 82, with his supplementary list in Table 83 A self-inherent problem concerns the stability of measurements of stars with relatively high values of polarization, and it is likely that variability of some Polarized Standards is inherent to some degree In order for large interstellar polarization to accrue, a considerable line of sight dust column is required The accompanying interstellar absorption imposes that for stars to have a reasonable apparent brightness to allow easy measurement, they tend to be intrinsically bright early-type supergiants Several nearby stars of this type, with little or no interstellar polarization, are known to exhibit variable polarization (e g see Hayes, 1984, 1986) If the polarigenic sources involve a combination of intrinsic stellar atmospheric effects and the interstellar medium, small levels of variability may be recorded, if the star is itself variable With respect to the values of position angle, Dolan & Tapia (1986) conducted a special study on stability and found that 9 of 11 selected stars from Serkowski s Table of Standard Stars with Large Interstellar Polarization exhibited signi cant spectral dispersion of position angle, primarily caused by the vector combinations of intrinsic and interstellar effects Their summary concludes that / is generally not linear but complex, and that no stars can be taken as satisfactory standards at the 0 1 level of accuracy Hsu & Breger (1982) have discussed some of the problems associated with the establishment of standard stars and suggest that 55 Cyg (HD 198478), 9 Gem (HD 43384) and HD 183143, sometime taken as polarized standards, all display variability Vir halmy (1986) also provides evidence that 55 Cyg, a well-known supergiant spectrum variable, is polarimetrically vari-. 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