Abstract

Astronomical seeing measurements are usually made at a single wavelength and extrapolated to other wavelengths of interest using scaling laws that assume a specific energy spectrum for the atmospheric turbulence. We describe a variation of the Differential Image Motion Monitor system that provides a measure of the seeing and evaluation of the scaling law by simultaneously measuring the image motion at three different wavelengths.

© 2002 Optical Society of America

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References

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    [CrossRef]
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    [CrossRef] [PubMed]
  3. M. Sarazin and F. Roddier, �??The ESO differential image motion monitor,�?? Astron. Astrophys. 227, 294-300 (1990).
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  5. J. W. Hardy, Adaptive Optics for Astronomical Telescopes (Oxford University Press, New York, 1998).
  6. R. P. Linfield, M. M. Colavita and B. F. Lane, �??Atmospheric Turbulence Measurements With the Palomar Testbed Interferometer,�?? Astrophys. J. 554, 505-513 (2001).
    [CrossRef]
  7. J. Bally, D. Theil, Y. Billawala, D. Potter, R. F. Loewenstein , F. Mrozek and J. P. Lloyd, �??A Hartmann Differential Image Motion Monitor (H-DIMM) for Atmospheric Turbulence Characterization,�?? Astron. Soc. Publ. Aus. 13, 22-27 (1996).

Appl. Opt. (1)

Astron. Astrophys. (1)

M. Sarazin and F. Roddier, �??The ESO differential image motion monitor,�?? Astron. Astrophys. 227, 294-300 (1990).

Astron. Soc. Publ. Aus. (1)

J. Bally, D. Theil, Y. Billawala, D. Potter, R. F. Loewenstein , F. Mrozek and J. P. Lloyd, �??A Hartmann Differential Image Motion Monitor (H-DIMM) for Atmospheric Turbulence Characterization,�?? Astron. Soc. Publ. Aus. 13, 22-27 (1996).

Astrophys. J. (1)

R. P. Linfield, M. M. Colavita and B. F. Lane, �??Atmospheric Turbulence Measurements With the Palomar Testbed Interferometer,�?? Astrophys. J. 554, 505-513 (2001).
[CrossRef]

J. Opt. Soc. Am. (1)

Other (2)

V. I. Tatarski, Wave Propagation in a Turbulent Medium (McGraw-Hill, New York, 1961).

J. W. Hardy, Adaptive Optics for Astronomical Telescopes (Oxford University Press, New York, 1998).

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Figures (3)

Fig. 1.
Fig. 1.

An optical ray trace for a monochromatic, collimated beam of light passing through the MDIMM system. The light from the telescope is first collimated and then enters the MDIMM system from the left in the diagram. Light from the outer portion of the collimated beam is then passed through a filter and lens and then focused onto the imager.

Fig. 2.
Fig. 2.

A simplified illustration of the MDIMM optics holder showing the relative positions of the lenses and filters.

Fig. 3.
Fig. 3.

A plot showing the results of simulations of the deflection of the light for an individual focused subaperture due to the angle of arrival of a wavefront. The small variations in the plot are due to collimation errors over the 3 wavelengths from using a single lens. This plot shows that the displacement of the spot for a given tilt angle is wavelength independent.

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