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The formula for resolution is
R = D/lamda
where D = diameter
lamda= wavelength.
Wavelength is essentially constant for light (ie 400- 700nm) and is a very small number conpared to the diameter of the scope. For radio frequencies the wavelength is much longer (21cm is a common frequency used) and even for a dish 20m in diameter it is a significant amount. This is why radio dishes need to be so large and why arrays of dishes are used to simulate a telescope that is many km in diameter to overcome this problem.
The AAO isn't a great example as they are not known for terribly high resolution. That is why other places in the world are favoured like high in the Andes or at Dome C in antarctica.
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