Hostname: page-component-cd9895bd7-mkpzs Total loading time: 0 Render date: 2024-12-23T20:13:13.423Z Has data issue: false hasContentIssue false
  • English
  • Français

Speckle Interferometry and Image Reconstruction

Published online by Cambridge University Press:  02 August 2016

Gerd P. Weigelt
Gerd P. Weigelt*
Affiliation:
Physikalisches Institut, Universität Erlangen-Nürnberg, 8520 Erlangen, E.-Rommel-Str. 1, West Germany

Abstract

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 angular resolution of conventional astrophotography is limited to about 1 sec of arc due to image degradation by the atmosphere and telescope aberrations. Higher resolution can be achieved by Labeyrie's speckle interferometry, which yields the autocorrelation of astronomical objects with diffraction-limited resolution, e.g. 0.02 sec of arc with 5m telescope aperture.

We have investigated modifications of speckle interferometry, which yield diffraction-limited images. We investigated (1) “speckle holography” for image reconstruction of objects near an unresolvable point source (reference star), (2) “speckle masking” for image reconstruction of binary stars (without a reference star), and (3) “phase flipping” for image reconstruction of centro-symmetric objects. Together these three image reconstruction methods represent a set of speckle evaluation procedures, which can yield high resolution images of most astronomical objects that are bright enough for speckle interferometry. Speckle holography was already applied to astronomical objects. We reconstructed real images of the binary star Zeta Cancri A-B and the triple star ADS 3358 A-B-C ( 0.07 sec of arc resolution with 1.8m telescope aperture).

Type
The Scientific Programme
Information
International Astronomical Union Colloquium , Volume 50: High Angular Resolution Stellar Interferometry , January 1979 , pp. 33-1 - 33-12
Copyright
Copyright © 1979

References

1) Labeyrie, A., Astron.Astrophys. 6 (1970) 85 Google Scholar
2) Gezari, D.Y., Labeyrie, A., Stachnik, R.V., Astrophys.J. 173 (1972) L1 Google Scholar
3) Liu, C.Y-C., Lohmann, A.W., Opt.Comm. 8 (1973) 372 CrossRefGoogle Scholar
4) Bates, R.H.T., Gough, P. T., Napier, P.J., Astron.Astrophys. 22(1973) 319 Google Scholar
5) Gough, P. T., Bates, R.H.T., Opt.Acta 21 (1974) 243 Google Scholar
6) Weigelt, G.P., Optik 43 (1975) 111 Google Scholar
7) Knox, K.T. and Thomson, B.J., Astrophys.J.(Letters) 193 (1974) L45 Google Scholar
8) Lynds, C.R., Worden, S.P. and Harvey, J.W., Astrophys.J. 207 (1976) 174 Google Scholar
9) Ehn, D.C. and Nisenson, P., J.Opt.Soc.Am. 65 (1975) 1196 Google Scholar
10) Weigelt, G.P., Opt.Comm. 21 (1977) 55 Google Scholar
11) Lohmann, A.W. and Weigelt, G.P., in Optical Telescopes of the Future. Conf.Proc. (page 479) Dec.77.Geneva:ESOc/oCERNGoogle Scholar
12) Weigelt, G.P.,“Speckle Holography Measurements of the Stars Zeta Cancri and ADS 3358”, Appl.Opt., Sept. or Oct. 78Google Scholar
13) Lohmann, A.W. and Weigelt, G.P., “Astronomical Speckle Interferometry; Measurements of Isoplanicity and Temporal Correlation”, submitted to OPTIKGoogle Scholar
14) Weigelt, G.P., “Speckle Interferometry Measurements of 12 Binary Stars”, submitted to Astron.Astrophys.Google Scholar
15)for more details see Ref. 12Google Scholar