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1 What are the conditions needed for the image to be larger than the object 2 Review the methods used for data collection Identify sources of error and what might be done to improve accuracy



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1 Use Numbers Calculate 1/do and 1/di and enter the values in the calculation table 2 Use Numbers Calculate the sum of 1/do and 1/di and enter the values in the calculation table Calculate the reciprocal of this number and enter it in the calculation table as fcalc 3 Error Analysis Compare the experimental focal length, fcalc , with f, the accepted focal length, by finding the percent error percent error = What advantage would there be in using a telescope with a concave mirror

observe from Earth because they twinkle Our moving, unevenlyheated atmosphere refracts their light in a chaotic manner It s like trying to look at a small object through the bottom of an empty, clear, glass jar while rotating the jar

Adaptive mirror Light from telescope Distorted wave front Beam splitter Control system Corrected wave front

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The capacitor (also available from the same sources) should be 150-pF to 250pF maximum capacitance high-voltage variable So-called transmitting variables are usually ok if the plate spacing is at least 1 8 in Tuning of the longwire is simplicity itself If the tuner does not have a built-in VSWR meter, then install one in the line between the transmitter output and the tuner input Adjust both L1 and C1 (they are a bit interactive so do it several times) for the lowest VSWR If you use the alligator clip method, turn off the darn transmitter before adjusting the clip position RF burns are nasty!

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An adaptive optical system (AOS) continuously compensates for the distortion of the atmosphere, removing the twinkle from star Wave-front images to allow astronomers to sensor view and photograph steady High-resolution images of the most distant objects camera in the visible universe AOS compensates for distortion An AOS directs the magnified when viewing Titan, Saturn s largest moon image of the stars from the telescope onto a flexible adaptive mirror made of thin glass This mirror is stretched across 20 30 movable pistons that can poke or pull the surface of the mirror into many complicated shapes Each piston is driven by a fast, computer-controlled Conventional Hubble Space Keck telescope motor When the mirror surface is telescope Telescope with AOS shaped into just the right pattern at just the right time, it will compenThe computer looks at this error and calcusate for the convective movement of the atmoslates how the adaptive mirror should be phere between the telescope and the star, and wrinkled to bring each of the lenslet images reflect a clear image to the observer or camera back into place The star image reflected to the observer then will be correct, and a clear image Wave-Front Sensor To detect the atmosof all other objects (like galaxies and planets) in pheric distortion at each instant of time, a the vicinity also will be seen clearly The adaptive wave-front sensor looks at a single star through mirror is re-shaped about 1000 times per second the telescope This device has an array of tiny lenses (lenslets) in several rows Each lenslet forms an image of the star on a sensitive screen behind it The position of each image can be Going Further read by the computer If each image is not directly behind its lenslet, 1 Research What is done if there is not then the computer knows that the star s light a suitable star for the wave-front sensor waves are being distorted by the atmosphere to analyze in a region of space under A star is a distant point source of light, so it observation should produce plane waves Distorted images 2 Apply Research how adaptive optics of a star are non-planar light waves, and these will be used in the future to correct uneven waves cause the images of the star vision behind some of the lenslets to be displaced 476.

specular reflection (p 459) diffuse reflection (p 459) plane mirror (p 461) object (p 461) image (p 461) virtual image (p 461)

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According to the law of reflection, the angle that an incident ray makes with the normal equals the angle that the reflected ray makes with the normal

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