Spread Out Formula Resolution For Free

In order to increase the resolution, d = ?/(2NA), the specimen must be viewed using either a shorter wavelength (?) of light or through an imaging medium with a relatively high refractive index or with optical components which have a high NA (or, indeed, a combination of all of these factors).

In practice, the resolvance is stated in the form R=? /?? for applications like the observation of the sodium doublet. We know the wavelength difference to be ?? = . 59 nm, so the resolvance can help us to anticipate whether a particular diffraction grating could resolve that difference.

Resolving Power = D/d = a / 1.22 ? D = is distance of the objects from objective of the telescope. a - is critical width of the rectangular slit for just resolution of two slits or objects.

This occurs for two point objects separated by the angle ?=1.22?D ? = 1.22 ? D , where ? is the wavelength of light (or other electromagnetic radiation) and D is the diameter of the aperture, lens, mirror, etc. This equation also gives the angular spreading of a source of light having a diameter D.

The factor of 1.22 applies to circular apertures like the pupil of your eye or the apertures in telescopes and cameras. When light passes through an aperture with diameter D, then diffraction limits the resolution to ? = 1.22?/D. If the angular separation of two sources is less than ?, they cannot be resolved.

Assuming for small angles AFOV= (0.5?/D)?180/? degrees where ? is the wavelength of radio frequency. Second is the resolving power of the radio telescope which is as given, ?=1.22?/A where A is the aperture of the radio telescope.

Telescopic observation. The angular resolving power (or resolution) of a telescope is the smallest angle between close objects that can be seen clearly to be separate. Resolution is limited by the wave nature of light.