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Deformable Mirror (deformable + mirror)

Distribution by Scientific Domains

Medical Sciences	60%

Selected Abstracts

Limits of spherical blur determined with an adaptive optics mirror

OPHTHALMIC AND PHYSIOLOGICAL OPTICS, Issue 3 2009
David A. Atchison
Abstract We extended an earlier study (Vision Research, 45, 1967,1974, 2005) in which we investigated limits at which induced blur of letter targets becomes noticeable, troublesome and objectionable. Here we used a deformable adaptive optics mirror to vary spherical defocus for conditions of a white background with correction of astigmatism; a white background with reduction of all aberrations other than defocus; and a monochromatic background with reduction of all aberrations other than defocus. We used seven cyclopleged subjects, lines of three high-contrast letters as targets, 3,6 mm artificial pupils, and 0.1,0.6 logMAR letter sizes. Subjects used a method of adjustment to control the defocus component of the mirror to set the ,just noticeable', ,just troublesome' and ,just objectionable' defocus levels. For the white-no adaptive optics condition combined with 0.1 logMAR letter size, mean ,noticeable' blur limits were ±0.30, ±0.24 and ±0.23 D at 3, 4 and 6 mm pupils, respectively. White-adaptive optics and monochromatic-adaptive optics conditions reduced blur limits by 8% and 20%, respectively. Increasing pupil size from 3,6 mm decreased blur limits by 29%, and increasing letter size increased blur limits by 79%. Ratios of troublesome to noticeable, and of objectionable to noticeable, blur limits were 1.9 and 2.7 times, respectively. The study shows that the deformable mirror can be used to vary defocus in vision experiments. Overall, the results of noticeable, troublesome and objectionable blur agreed well with those of the previous study. Attempting to reduce higher-order aberrations or chromatic aberrations, reduced blur limits to only a small extent. [source]

Scientific instrumentation for the 1.6 m New Solar Telescope in Big Bear

ASTRONOMISCHE NACHRICHTEN, Issue 6 2010
W. Cao
Abstract The NST (New Solar Telescope), a 1.6 m clear aperture, off-axis telescope, is in its commissioning phase at Big Bear Solar Observatory (BBSO). It will be the most capable, largest aperture solar telescope in the US until the 4 m ATST (Advanced Technology Solar Telescope) comes on-line late in the next decade. The NST will be outfitted with state-of-the-art scientific instruments at the Nasmyth focus on the telescope floor and in the Coudé Lab beneath the telescope. At the Nasmyth focus, several filtergraphs already in routine operation have offered high spatial resolution photometry in TiO 706 nm, H, 656 nm, G-band 430 nm and the near infrared (NIR), with the aid of a correlation tracker and image reconstruction system. Also, a Cryogenic Infrared Spectrograph (CYRA) is being developed to supply high signal-to-noise-ratio spectrometry and polarimetry spanning 1.0 to 5.0 ,m. The Coudé Lab instrumentation will include Adaptive Optics (AO), InfraRed Imaging Magnetograph (IRIM), Visible Imaging Magnetograph (VIM), and Fast Imaging Solar Spectrograph (FISS). A 308 sub-aperture (349-actuator deformable mirror) AO system will enable nearly diffraction limited observations over the NST's principal operating wavelengths from 0.4 ,m through 1.7 ,m. IRIM and VIM are Fabry-Pérot based narrow-band tunable filters, which provide high resolution two-dimensional spectroscopic and polarimetric imaging in the NIR and visible respectively. FISS is a collaboration between BBSO and Seoul National University focussing on chromosphere dynamics. This paper reports the up-to-date progress on these instruments including an overview of each instrument and details of the current state of design, integration, calibration and setup/testing on the NST (© 2010 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim) [source]

Principle of adaptive optics

ACTA OPHTHALMOLOGICA, Issue 2009
PG SÖDERBERG
Purpose To provide an overview of adaptive optics imaging of the retina. Methods In ophthalmoscopical imaging, the two dimensional spatial radiance variation of the back scattered light from the retinal surface is measured. Perfect imaging would require that light backscattered from one point on the retina examined is refocused to one point on the detector. Due to diffraction, light scattering and aberrations, some of the light, injected into the eye examined and some of the light back scatted from the retina examined, are deviated. This leads to loss of contrast. Aberrations induced are, for each individual, specific to the optics of the eye examined. In AOSLO, in addition to confocal illumination and light detection, aberrations induced by the optics of the eye examined are individually measured by wave front sensing and corrected for. Results In the AOSLO, a wave front sensor is introduced between the light source and the eye examined. The information from the wave front sensor is fed back to a deformable mirror, also placed in between the light source and the eye examined. The deformable mirror corrects the wave front aberrations induced by the optics of the eye examined. This allows the injected light to form a point on the retinal surface and simultaneously, the backscattered light from the retina of the eye examined to be focused to a point on a detector. An x-y scanner in front of the eye allows sequential illumination and capturing of aberration minimized back scattered light from an x-y matrix of the retinal surface of the eye examined. The relative radiances measured in the x-y matrix represent the image. Conclusion Adaptive optics in ophthalmoscopy improves contrast in the image of the retina examined by correcting for aberrations induced by the optics of the eye examined. [source]

European Solar Telescope: Progress status

ASTRONOMISCHE NACHRICHTEN, Issue 6 2010
M. Collados
Abstract In this paper, the present status of the development of the design of the European Solar Telescope is described. The telescope is devised to have the best possible angular resolution and polarimetric performance, maximizing the throughput of the whole system. To that aim, adaptive optics and multi-conjugate adaptive optics are integrated in the optical path. The system will have the possibility to correct for the diurnal variation of the distance to the turbulence layers, by using several deformable mirrors, conjugated at different heights. The present optical design of the telescope distributes the optical elements along the optical path in such a way that the instrumental polarization induced by the telescope is minimized and independent of the solar elevation and azimuth. This property represents a large advantage for polarimetric measurements. The ensemble of instruments that are planned is also presented (© 2010 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim) [source]

3236: Corneal grafting assisted by wavelength-optimised ultrashort pulser lasers

ACTA OPHTHALMOLOGICA, Issue 2010
TAL MARCIANO
Purpose We realized an innovative device for ocular surgery by ultrafast pulse laser optimised for corneal grafting. Methods We constructed a demonstrator device that reproduces surgical conditions of corneal transplant. It is thus possible to realize with the help of an easy handling automatised interface all the kinds of already existing corneal transplants. Also, in order to maximize the spatial quality of the beam, a wavefront correction system using a deformable mirror module has been added. The Demonstrator contains an erbium fiber laser emitting at 1,6 microns. This laser delivers a beam of a few Joule with pulse duration of 700 femtoseconds and a repetition rate of 100-200 KHz. It includes deformable mirrors permitting horizontal displacements and a wavefront sensor. It also contains the administration system of the laser beam. Results The experiments carried out with a surgical tunable source confirmed the initial assumptions: the penetration depth is limited to wavelengths close to 1 microns. When increasing the wavelength, the drop of the scattering compensates the absorption and therefore the penetration depth is slowly varying when increasing the wavelength. The laser does not penetrate near the maximum of the water absorption band located at 1,45 microns. However, the use of a wavelength of 1,6 micros enables an important increasing of penetration depth (factor 3) while conserving the same energy of current technologies. Conclusion The use of a laser source with a wavelength corresponding to the window of transparency of the cornea (1,65 microns) permits to increase both the penetration depth of an ultrafast laser source and the cut quality. [source]