Hostname: page-component-745bb68f8f-grxwn Total loading time: 0 Render date: 2025-01-30T17:22:07.209Z Has data issue: false hasContentIssue false
  • English
  • Français

Speckle Interferometry, Speckle Masking, Speckle Spectroscopy and Speckle Frame Selection*

Published online by Cambridge University Press:  12 April 2016

Gerd Weigelt
Gerd Weigelt*
Affiliation:
Physikalisches Institut, Rommel-Str. 1, 8520 Erlangen, Fed. Rep. of 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.

High-resolution speckle imaging is one of the most fascinating possibilities of a Very Large Telescope (VLT). Various speckle methods can yield a resolution of about 0.01" with a 8-m to 10-m VLT. As exiting as the resolution is the limiting magnitude of the speckle methods. The limiting magnitude is extremely seeingdependent. The following limiting magnitudes are possible with speckle interferometry, speckle masking and speckle spectroscopy:

4" seeing: limiting magnitude 15

2" seeing: limiting magnitude 17.5

1" seeing: limiting magnitude 20 (!)

Type
III. Atmospheric Seeing, Interferometry, Speckle, MMTs and Arrays
Information
International Astronomical Union Colloquium , Volume 79: Very Large Telescopes, their Instrumentation and Programs , 1984 , pp. 337 - 345
Copyright
Copyright © ESO 1984

Footnotes

*

Based on data collected at the European Southern Observatory, La Silla, Chile

References

Baier, G., Keller, E., Weigelt, G., 1983: Proc. of the Second European Signal Processing Conf., Sep. 12–16, Univ. Erlangen-Nürnberg, FRG Google Scholar
Dainty, J.C., 1975: in Laser Speckle and Related Phenomena, Topics in Appl. Physics, Vol. 9, ed. Dainty, J.C., Springer Google Scholar
Hetterich, N., Weigelt, G.,1983: Astron. Astrophys. 125, 246 Google Scholar
Labeyrie, A., 1970: Astron. Astrophys. 6, 85 Google Scholar
Lohmann, A.W., Weigelt, G., 1979: in Proc. ESA/ESO Workshop on Astronomical Uses of the Space Telescope, Macchetto, F., Pacini, F., and Tarenghi, M., Eds. (ESO, Geneva, 1979) p. 353 Google Scholar
Lohmann, A., Weigelt, G., Wirnitzer, B., 1983: Appl. Opt. 22, 4028 CrossRefGoogle Scholar
Roddier, F., 1975: Signal-to-Noise Ratio in Speckle Interferometry, in Imaging in Astronomy, AAS/SAO/OSA/SPIE Topical Meeting, Boston Google Scholar
Stork, W., Weigelt, G., 1984: Speckle Spectroscopy, in Conf. Proc. International Commission of Optics (ICO-13), Sapporo, Aug. 1984 Google Scholar
Weigelt, G., 1977: Opt. Commun. 21, 55 CrossRefGoogle Scholar
Weigelt, G., 1981: in Proc. of the ESO Conf. on Scientific Importance of High Angular Resolution and IR and Optical Wavelengths, Edited by Ulrich, M.H. and Kjär, K., Garching, March 1981, p. 95 Google Scholar
Weigelt, G., Wirnitzer, B., 1983: Optics Lett. 8, 389 CrossRefGoogle Scholar
Weigelt, G., 1984: High-resolution Astronomical Imaging with Space Telescopes, in Conf. Proc. International Commission of Optics (ICQ-13), Sapporo, Aug. 1984 Google Scholar
Wirnitzer, B., 1984: Bispectral analysis at low light levels and speckle masking, submitted to Optica Acta; and Annual Report 1983 Google Scholar