Hostname: page-component-cd9895bd7-mkpzs Total loading time: 0 Render date: 2024-12-12T11:46:55.161Z Has data issue: false hasContentIssue false
  • English
  • Français

System Requirements for Polarization Capability

Published online by Cambridge University Press:  12 April 2016

J. Tinbergen
J. Tinbergen*
Affiliation:
Sterrewacht Leiden, Kapteyn Sterrenwacht Werkgroep, Roden

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The purpose of this paper is to point out that

1) proper treatment of polarization by a telescope is not only important for polarimetry, but also for other observations requiring high signal-to-noise ratio, and

2) this does put a constraint on telescope design, which, however, is not unduly restrictive.

Polarimetry is the observational technique which can detect anisotropics in point sources, their environment, or the medium between them and us. Modern optical polarimetry can be linear or circular, and is making progress towards spectropolarimetry and imaging polarimetry using panoramic detectors (e.g. McLean, 1984). Given sufficient photons, the precision obtained is as high as 1 part in 50 000 (see Odell, 1981 for a project requiring this precision), but more often a precision between 1 part in 1 000 to 10 000 is sufficient. (Spectro)polarimetry has been applied to planets, the Sun and other stars, stellar systems and galaxy nuclei; for a few modern investigations, see Baur, 1981; Jones et al, 1981; Schmidt and Miller, 1980. Experience in radio-astronomy has shown that when facilities for polarimetry are offered, many applications emerge from the astronomical community, yielding data that cannot be obtained by other techniques. It is essential that at least some of the large optical telescopes are capable of ob-serving polarization cleanly.

Type
IV. Instrumentation - Components
Information
International Astronomical Union Colloquium , Volume 79: Very Large Telescopes, their Instrumentation and Programs , 1984 , pp. 569 - 573
Copyright
Copyright © ESO 1984

References

Andersen, J., Clausen, J.V., Giménez, A. and Nordström, B., 1983, Astron. Astrophys. 128, 17.Google Scholar
Baur, T.G., 1981, Optical Engineering 20, 2.CrossRefGoogle Scholar
Bausch and Lomb Inc., 1970, Diffraction Grating Handbook.Google Scholar
Borra, E.F., 1976, Publ. Astron. Soc. Pacific 88, 548.CrossRefGoogle Scholar
Breckinridge, J.B., 1971, Applied Optics 10, 286.CrossRefGoogle Scholar
Clarke, D. and Grainger, J.F., 1971, Polarized Light and Optical Measurement (Pergamon Press).Google Scholar
Jones, D.H.P., Smith, F.G. and Wallace, P.T., 1981, Mon. Not. R.A.S. 196, 45.Google Scholar
Kemp, J.C., 1969, Jour. Opt. Soc. Am. 59, 950.CrossRefGoogle Scholar
McLean, I.S., 1984, Proc. S.P.I.E. 445, 547.Google Scholar
Meinel, A.B. and Meinel, M.P., 1982, sec. VI.3 in: Barr, L. (ed.); “N.N.T.T. Tech. Dev. Progr. Rept. no 3” (Kitt Peak Nat. Obs.).Google Scholar
Miller, J.S., Robinson, L.B. and Schmidt, G.D., 1980, Publ. Astron. Soc. Pacific 92, 702.CrossRefGoogle Scholar
Odell, A.P., 1981, Astrophys. Jour.Letters 246, L 77.Google Scholar
Piirola, V., 1973, Astron. Astrophys. 27, 383.Google Scholar
Schmidt, G.D. and Miller, J.S., 1980, Ap. J. 240, 759.CrossRefGoogle Scholar
Serkowski, K., 1974, p. 135 in: Gehreis, T. (ed.); “Planets, Stars and Nebulae studied with photopolarimetry” (Univ. of Arizona Press).Google Scholar
Tinbergen, J., 1974, p. 175 in: Gehreis, T. (ed.); “Planets, Stars and Nebulae studied with photopolarimetry” (Univ. of Arizona Press).Google Scholar
Velt, CF. and Tinbergen, J., 1981, Astron. Astrophys. 103, 422.Google Scholar