setting circle and slightly loosen the two bolts located under the knob. Now turn the
circle unit until it reads 89.2°, the Declination of Polaris. Then tighten down the two
bolts and replace the knurled knob.
Should you wish to use the manual setting circles, the R.A. setting circle (Fig. 38) must
be calibrated manually on the Right Ascension of a star every time the telescope is set
up. (The R.A. setting circle has two sets of numbers, the inner set is for Southern
hemisphere use, while the other is for Northern hemisphere use.) Locate a star with
which you’re familiar. Look up the R.A. for the star in a star chart or other aid. With the
star centered in the telescope’s eyepiece, move the R.A. setting circle, using one of
knobs (Fig. 41, C), so that the R.A. of the star lines up with the tick mark on the base
of the telescope (Fig. 41, B).
Precise Polar Alignment
It should be emphasized that while doing casual observing, precise alignment of the
telescope’s polar axis to the celestial pole is not necessary. Don’t allow a time-
consuming effort at lining up with the pole to interfere with your basic enjoyment of the
telescope. For long-exposure photography, however, the ground rules are quite
different, and precise polar alignment is not only advisable, but almost essential.
Even though the
LX200-ACF telescopes offers a very precise and sophisticated drive
system, the fewer tracking corrections required during the course of a long-exposure
photograph, the better. (“Long-exposure” means any photograph of a celestial object
that last for 10 minutes or longer). In particular, the number of Declination corrections
required is a direct function of the precision of polar alignment.
Precise polar alignment requires the use of a crosshair eyepiece. The Meade
Illuminated Reticle Eyepiece (see
OPTIONAL ACCESSORIES, page 44) is well-suited in
this application, but it is also preferable to increase the effective magnification through
the use of a 2X or 3X Barlow lens as well. Follow this procedure (particularly if the pole
star is not visible), sometimes better known as the “Drift” method:
1. Obtain a rough polar alignment as described earlier. Place the illuminated
reticle eyepiece (or eyepiece/Barlow combination) into the eyepiece holder of
the telescope.
2. Point the telescope, with the motor drive running, at a moderately bright star near
where the meridian (the North-South line passing through your local zenith)
and the celestial equator intersect. For best results, the star should be located
within ±30 minutes in R.A. of the meridian and within ±5° of the celestial equator
(see
CELESTIAL COORDINATES, page 53). Pointing the telescope at a star that
is straight up, with the Declination set to 0°, will point the telescope in the
right direction.
3. Note the extent of the star’s drift in Declination (disregard drift in Right Ascension):
a. If the star drifts South (or down), the telescope’s polar axis is pointing too far
East.
b. If the star drifts North (or up), the telescope’s polar axis is pointing too far
West.
4. Move the wedge in azimuth (horizontally) to effect the appropriate change in polar
alignment. Reposition the telescope’s East-West polar axis orientation until there
is no further North-South drift by the star. Track the star for a period of time to be
certain that its Declination drift has ceased.
5. Next, point the telescope at another moderately bright star near the Eastern
horizon, but still near the celestial equator. For best results, the star should be
about 20° or 30° above the Eastern horizon and within ± 5° of the celestial
equator.
6. Again note the extent of the star’s drift in Declination:
a. If the star drifts South, (or down) the telescope’s polar axis is pointing too low.
b. If the star drifts North, (or up) the telescope’s polar axis is pointing too high.
7. Use the altitude adjust control on the wedge to make appropriate changes in
altitude, based on your observations above. Again, track the star for a period of
time to be certain that Declination drift has ceased.
The above procedure results in very accurate polar alignment, and minimizes the need
for tracking corrections during astrophotography.
Fig. 42:
LX200-ACF
mounted on an
equatorial wedge.
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