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Surface Polarimetry of the Milky Way

Published online by Cambridge University Press:  14 August 2015

Ramon D. Wolstencroft
Ramon D. Wolstencroft*
Affiliation:
Institute for Astronomy, University of Hawaii, H.I., U.S.A.

Abstract

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Two methods of determining the state of polarization of the integrated light from the Milky Way are discussed. In the symmetry method it is assumed that the polarized foreground zodiacal light possesses north/south symmetry relative to the ecliptic: an average polarized intensity of at least 10 S10(R) is derived for the Milky Way at l ≃ 90° and 270°, which is consistent with the result of Sparrow and Ney (1972) who obtained 18 S10 (R) at l = 35° and 210°. In the method of two epochs the above assumption is not needed but instead time variations of the zodiacal light are assumed to be insignificant: the results obtained by this method (in S10 (V) units), although compatible with the values found by the symmetry method, do however show that time variations may have influenced this result. Although the evidence for a definite polarization of the Milky Way is persuasive it cannot yet be considered conclusive.

Type
Part III Reflection Nebulae and Diffuse Galactic Light
Information
Symposium - International Astronomical Union , Volume 52: Interstellar Dust and Related Topics , 1973 , pp. 99 - 108
Copyright
Copyright © Reidel 1973 

References

Schmidt, T. and Leinert, C.: 1966, Z. Astrophys. 64, 110.Google Scholar
Sparrow, J. G. and Ney, E. P., 1972, Astrophys. J. 174, 705.Google Scholar
Wolstencroft, R. D. and Brandt, J. C.: 1967, in Weinberg, J. L. (ed.), The Zodiacal Light and the Interplanetary Medium , NASA Sp-150, Washington, D.C., p. 57.Google Scholar
Wolstencroft, R. D. and van Breda, I. G.: 1967, Astrophys. J. 147, 255.Google Scholar