Sky-Watcher EQ2 MOUNT - Manual (Page 20)

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When you are looking at astronomical objects, you are looking through a column of air that reaches to the edge of
space and that column seldom stays still. Similarly, when viewing over land you are often looking through heat waves
radiating from the ground, house, buildings, etc. Your telescope may be able to give very high magnification but what
you end up magnifying is all the turbulence between the telescope and the subject. A good rule of thumb is that the
usable magnification of a telescope is about 2X per mm of aperture under good conditions.
Calculating the field of view
The size of the view that you see through your telescope is called the true (or actual) field of view and it is determined
by the design of the eyepiece. Every eyepiece has a value, called the apparent field of view, which is supplied by the
manufacturer. Field of view is usually measured in degrees and/or arc-minutes (there are 60 arc-minutes in a degree).
The true field of view produced by your telescope is calculated by dividing the eyepiece's apparent field of view by
the magnification that you previously calculated for the combination. Using the figures in the previous magnification
example, if your 10mm eyepiece has an apparent field of view of 52 degrees, then the true field of view is 0.65
degrees or 39 arc-minutes.
True Field of View =
Apparent Field of View
Magnification
= 0.65°
52°
80X
=
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hoosing the Appropriate Eyepiece
magnification =
=
= 80X
Focal length of the telescope
Focal length of the eyepiece
800mm
10mm
Calculating the magnification (power)
The magnification produced by a telescope is determined by the focal length of the eyepiece that is used with it. To
determine a magnification for your telescope, divide its focal length by the focal length of the eyepieces you are
going to use. For example, a 10mm focal length eyepiece will give 80X magnification with an 800mm focal length
telescope.
To put this in perspective, the moon is about 0.5° or 30 arc-minutes in diameter, so this combination would be fine for
viewing the whole moon with a little room to spare. Remember, too much magnification and too small a field of view
can make it very hard to find things. It is usually best to start at a lower magnification with its wider field and then
increase the magnification when you have found what you are looking for. First find the moon then look at the
shadows in the craters!
C
alculating the exit pupil
The Exit Pupil is the diameter (in mm) of the narrowest point of the cone of light leaving your telescope. Knowing this
value for a telescope-eyepiece combination tells you whether your eye is receiving all of the light that your primary
lens or mirror is providing. The average person has a fully dilated pupil diameter of about 7mm. This value varies a bit
from person to person, is less until your eyes become fully dark adapted and decreases as you get older. To determine
an exit pupil, you divide the diameter of the primary of your telescope (in mm) by the magnification.
Exit Pupil =
Diameter of Primary mirror in mm
Magnification
For example, a 200mm f/5 telescope with a 40mm eyepiece produces a magnification of 25x and an exit pupil of
8mm. This combination can probably be used by a young person but would not be of much value to a senior citizen.
The same telescope used with a 32mm eyepiece gives a magnification of about 31x and an exit pupil of 6.4mm which
should be fine for most dark adapted eyes. In contrast, a 200mm f/10 telescope with the 40mm eyepiece gives a
magnification of 50x and an exit pupil of 4mm, which is fine for everyone.