A system of active optics that includes a wavefront sensor and a deformable mirror has been demonstrated to be an effective means of partly correcting wavefront aberrations introduced by fixed optics (lenses and mirrors) in telescopes. It is envisioned that after further development, active optics would be used to reduce wavefront aberrations of about one wave or less in telescopes having aperture diameters of the order of meters or tens of meters. Although this remaining amount of aberration would be considered excessive in scientific applications in which diffraction-limited performance is required, it would be acceptable for free space optical-communication applications at wavelengths of the order of 1 μm.
To prevent misunderstanding, it is important to state the following:
- The technological discipline of active optics, in which the primary or secondary mirror of a telescope is directly and dynamically tilted, distorted, and/or otherwise varied to reduce wavefront aberrations, has existed for decades. The term “active optics” does not necessarily mean the same thing as does “adaptive optics,” even though active optics and adaptive optics are related.
- The term "adaptive optics" is often used to refer to wavefront correction at speeds characterized by frequencies ranging up to between hundreds of hertz and several kilohertz — high enough to enable mitigation of adverse effects of fluctuations in atmospheric refraction upon propagation of light beams. The term “active optics” usually appears in reference to wavefront correction at significantly lower speeds, characterized by times ranging from about 1 second to as long as minutes.
Hence, the novelty of the present development lies, not in the basic concept of active or adaptive optics, but in the envisioned application of active optics in conjunction with a deformable mirror to achieve acceptably small wavefront errors in free-space optical communication systems that include multimeter- diameter telescope mirrors that are relatively inexpensive because their surface figures are characterized by errors as large as about 10 waves. Figure 1 schematically depicts the apparatus used in an experiment to demonstrate such an application on a reduced scale involving a 30-cm-diameter aperture. The apparatus included a source of illumination at a wavelength of 1,064 nm; an object to be imaged (an illuminated dollar bill); two 30-cm amateur astronomical telescopes facing each other to emulate far-field imaging; a 19-element thermally actuated deformable mirror at the pupil plane of the receiving telescope; a Hartmann wavefront sensor; an image detector at the receiving-telescope focal plane; associated lenses, filters, beam splitters; and a flat mirror. The output of the wavefront sensor was processed, by a rescomputer, to control signals for the thermal actuators on the deformable mirror. The lenses were chosen and arranged to reduce the diameter of the light beam to the widths of the deformable mirror and the wavefront sensor. The deformable mirror was placed at the pupil plane of the receiving telescope.
The various optics introduced aberrations characterized by, among other parameters, 1.4 wavelengths of root mean square (RMS) wavefront error. Then the closed loop control system consisting of the wavefront sensor, computer, and deformable-mirror actuators was turned on, thereby reducing the aberrations (see Figure 2) to 0.05 wavelength RMS wavefront error. In addition, the Strehl ratio (the ratio between the peak intensity in the point spread function of an optical system and that of an equivalent diffraction-limited system) was increased from 0.08 percent to 89 percent.
This work was done by Hamid Hemmati and Yijian Chen of Caltech for NASA’s Jet Propulsion Laboratory. For more information, download the Technical Support Package (free white paper) at www.techbriefs.com/tsp under the Physical Sciences category. NPO-43173