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The Hubble Space Telescope (HST) is a marvel of astronomical engineering, launched into low Earth orbit in 1990. It allows us to peer deep into the cosmos, capturing stunning images and shedding light on countless astronomical phenomena. One of the Hubble’s most crucial features is its large aperture, measuring 2.4 meters across. This size is key, as it allows Hubble to focus visible light, ranging from 380 nm to 750 nm. With such an aperture, the telescope can achieve a diffraction-limited resolution, which depends on both the wavelength of light it observes and the size of its aperture. The larger the aperture, the finer the details it can resolve. Specifically for the Hubble, this impressive capability allows it to see small features as tiny as 110 meters across on the moon's surface, even when observing from hundreds of thousands of kilometers away.

Angular resolution is a measure of a telescope's ability to distinguish between two closely spaced objects. It is defined by the smallest angle between two points that a telescope can effectively distinguish as separate. The angular resolution is determined using the formula \( \theta = 1.22 \frac{\lambda}{D} \), where \( \theta \) is the angular resolution in radians, \( \lambda \) is the wavelength, and \( D \) is the telescope's aperture diameter. A smaller angular resolution value implies a sharper, more detailed image, as the telescope can resolve finer details. For Hubble, this equates to being able to discern features as small as fractions of a meter when at close distances, such as observing objects in Earth's orbit. For distant celestial bodies like the moon, this still enables high precision, resolving features down to 110 meters.

Telescopic resolution refers to the ability of a telescope to distinguish fine details and separate objects that are close together. While it might seem similar to angular resolution, telescopic resolution specifically considers the practical application of these calculations in observational astronomy. Factors such as weather conditions, atmosphere, and the quality of the telescope's optics can all affect telescopic resolution. The Hubble Space Telescope, with its significant aperture and operation above Earth's atmosphere, circumvents many of these challenges. This allows it to achieve a resolution limited mainly by diffraction, meaning it can observe significantly smaller features compared to many ground-based telescopes, whose resolutions are often degraded by atmospheric interference.

Radio telescopes operate at much longer wavelengths than their optical counterparts, which presents unique challenges and opportunities. The Arecibo radio telescope, before its closure, was one of the most noteworthy, boasting a massive 305-meter diameter. It focused on radio wavelengths around 75 cm. Due to its large diameter, Arecibo had a decent angular resolution for its wavelength, though not as fine as those achieved by optical telescopes for visible light. This is a fundamental characteristic of radio astronomy; the longer the wavelength, the larger the telescope needed to achieve high resolution. Consequently, Arecibo could only resolve features around 1150 meters on the lunar surface, much larger than the capabilities of an optical telescope like Hubble. The construction of radio telescopes often involves creating massive dishes or arrays, underscoring their important role in capturing cosmic radio waves from deep within the universe.