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The descent stages were a little over 4 meters wide (the landing legs spread out were 9 meters across, but are narrow, so the bulk of the stage would be easier to see). As an example, a person standing next to you is easy to see and easily identifiable.
But from a mile away that human is far more difficult to see, and from ten miles away is just a dot (if that).
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Over the course of three more years, we did it five more times.
There are 3600 arcseconds to a degree, and to give you an idea of how small a measure this is, the Moon is about 0.5 degrees = 1800 arcseconds across. Hubble’s mirror is 2.4 meters = 240 centimeters across.
Second, there’s a statistical rule that says that you actually need an object to be twice that theoretical size to be properly resolved (I won’t go into boring details, but you can look up the Nyquist Sampling Theorem if you’re looking for an excuse to slack off at work).
So really, Hubble’s working resolution limit is about 0.1 arcseconds.
Plugging that into the formula, we see that Hubble’s resolution is 11.6 / 240 = 0.05 arcseconds. The first is that there’s a wavelength dependence too; for a given telescope size, the shorter the wavelength the more resolution you get (a telescope will resolve blue objects better than red ones, since blue has a shorter wavelength).
That’s an incredibly small size; a human would have to be nearly 8000 kilometers (4900 miles) away to be 0.05 arcseconds in size! But this is pretty minor compared to mirror size, and we can ignore it here (plus it’s already compensated for in the constant 11.6 that we used above).