Meade Lx70 Counterweight Instruction Manual LX70_Manual_Grey

2015-05-15

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Instruction Manual
LX70 Series
German Equatorial
Telescopes

WARNING!
Never use a Meade® LX70™ Telescope to look at the Sun!
Looking at or near the Sun will cause instant and irreversible damage to
your eye. Eye damage is often painless, so there is no warning to the observer that damage
has occurred until it is too late. Do not point the telescope at or near the Sun. Children should
always have adult supervision while observing.

® The name “Meade” and the Meade logo are trademarks registered with the U.S. Patent and Trademark Office
and in principal countries throughout the world.
Protected by U.S. Patent: US 6,392,799 and other Patents Pending
© 2014 Meade Instruments Corp.

Table of Contents
LX70 Key Features. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .4
Getting Started . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .7
Unpacking and Assembly. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 7
Balancing the Telescope . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .10
Aligning the Viewfinder. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .11
Choosing an Eyepiece . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .12
Using the Bubble Level. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .12
Observing by Moving the Telescope Manually. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 12
Observe the Moon . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 13
Tracking Objects. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .13
Locating the Celestial Pole. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 14
General Maintenance . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 15
Inspecting the Optics . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .15
Collimating the Newtonian Reflector . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .16
Optional Accessories . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .18
Appendix A: Celestial Coordinates. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .19
Appendix B: Setting Circles . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .20
Appendix C: Latitude Chart . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .21
Appendix D: Basic Astronomy . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .22
Meade Customer Service. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .24
Meade Warranty. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .24

LX70 Mount Key Features
24
18
17
20

23
21

22
5

Mount Close-up

13
24
16

DEC Axis

3
2

RA Axis
RA & DEC Axes

1
LX70 Telescope
1
2
3
4
5
6
7
8
9
10
11
12

Tripod Leg Lock Knob
Tripod Spreader Lock Knob
Tripod Spreader
Mount Locking Knob and Shaft
Azimuth Adjustment Knob
Latitude Adjustment Knob
North Tripod Leg
Latitude Scale
Counterweight Shaft
Counterweight Shaft Safety Nut
Counterweight
Counterweight Locking Knob

13
14
15
16
17
18
19
20
21
22
23
24

Figure 1: LX70 Key Features
4

Counterweight Shaft Locking Nut
DEC Setting Circle
RA Setting Circle (not shown)
RA Setting Circle Locking Knob
RA Clutch Locking Knob (see inset)
DEC Clutch Locking Knob
DEC Slow Motion Control Knob
RA Slow Motion Control Knob
Polar Scope Front Cap
Polar Scope Rear Cap
R.A. Motor Cover(R.A. motor not included)
OTA Dovetail Lock Knobs(see inset)

LX70 OTA Key Features
25

31
36
32

39
25
26
27
28
29
30
31
32
33

Front Dust Cover (not shown)
Dovetail Rail
Cradle Ring & Cradle Ring Lock Knobs
1/4-20 Accessory Mounting Screw with Lock
Focuser and Focuser Wheel
Focuser Lock Knob
Eyepiece
Eyepiece Holder Thumbscrews
Viewfinder

34
35
36
37
38
39
40
41

Viewfinder Dust Caps
Viewfinder Adjustment Screws
Viewfinder Bracket with Lock Knob
Optical Tube Assembly (OTA)
Objective Lens Cell
Dewshield
Diagonal Mirror
Diagonal Mirror Thumbscrews

Figure 2: LX70 Refractor Optical Tube

42
44

48
43
42

47
35

44
29

Front View

Rear View

47
48

25
25
26
27
28
29
30
31
32
33
34

Front Dust Cover (not shown)
Dovetail Rail
Cradle Ring & Cradle Ring Lock Knobs
1/4-20 Accessory Mounting Screw with Lock
Focuser & Focuser Wheel
Focuser Lock Knob
Eyepiece
Eyepiece Holder Thumbscrews
Viewfinder
Viewfinder Dust Caps

37
35

Viewfinder Adjustment Screws
Viewfinder Bracket with Lock Knob
Optical Tube Assembly (OTA)
Primary Mirror (see inset)
Primary Mirror Collimation Adjustment Knobs
Primary Mirror Collimation Lock Knobs
Spider Vane (see inset)
Spider Vane Tension Knobs
Secondary Mirror (see inset)
Secondary Mirror Collimation Screws (see inset)

36
37
42
43
44
45
46
47
48

Figure 3: LX70 Reflector Optical Tube
5

LX70 OTA Key Features
34

37
31
25
36
29

25
26
29
31
32
33
34

Front Dust Cover (not shown)
Dovetail Rail
Focuser Knob (not shown)
Eyepiece
Eyepiece Holder Thumbscrews
Viewfinder
Viewfinder Dust Caps

Viewfinder Adjustment Screws
Viewfinder Bracket with Lock Knob
Optical Tube Assembly (OTA)
Diagonal Mirror
Diagonal Mirror Thumbscrews
Extension Tube

35
36
37
40
41
49

Figure 4: LX70 Maksutov Optical Tube

Getting Started

shaft with the flat side facing up. Loosely thread
on the Tripod Spreader Lock Knob and washer

The Meade LX70 series models are versatile, high-resolution telescopes. They offer unmatched mechanical and optical performance
that reveal nature in an ever-expanding level of
detail. Observe the feather structure of an eagle
from 50 yards or study the rings of the planet
Saturn from a distance of 800 million miles. Focus beyond the Solar System and observe majestic nebulae, ancient star clusters, and remote
galaxies.

Figure 6: Tripod spreader

Meade LX70 series telescopes are instruments
fully capable of growing with your interest and
can meet the requirements of the most demanding advanced observer. Before using your telescope, read the entire instructions carefully. Your
telescope should be assembled during daylight
hours and setup in an area that allows you to
unpack all the included parts.

Figure 5: Installing the
mount locking knob and shaft

to prevent the tripod spreader from falling off the
shaft.

4. Attach mount to tripod: Place the LX70
mount onto the tripod head with the protrusion
on top of the tripod’s head positioned between
the fine azimuth adjustment knobs (Fig 1, #5 ).
Unpacking and Assembly
If necessary, back off the azimuth adjustment
knobs wide enough for the protrusion to fit be1. Remove the components from the boxes: tween them.
Remove and identify the telescope’s equipment.
Refer to FIG. 1 - 4 for images of the parts and Next, tighten the Mount Locking Knob (Fig. 1,
the overall assembly of your telescope.
#4) so the mount secures to the tripod head.
Tighten this knob to a firm feel. Then rotate the
When removing the tripod from the box, hold the Tripod Spreader (Fig. 1, #3) so the wings of the
assembly parallel (horizontal) to the ground or spreader align with each tripod leg. Tighten the
the inner tripod leg extensions may slide out if Tripod Spreader Lock Knob(Fig. 1, #2) until firm.
they are not locked in place. Tighten the tripod When you wish to collapse the tripod, loosen
leg lock knobs (Fig. 1. #1) to secure the legs in the Tripod Spreader Lock Knob and rotate the
place.
wings so they are between the tripod legs. You
do not need to remove the Tripod Spreader un2. Adjust the tripod legs: Spread the tripod less desired.
legs as far apart as they will open. Now adjust
the individual tripod legs by loosening the tripod
leg lock knobs and extending the inner legs until the tripod head is approximately level to the
ground. Relock the leg lock knob until firm.
3. Attach the spreader bar to the tripod:
Thread the small end of the Mount Locking
Knob and Shaft (Fig. 1, #4) along with the washer all the way into the bottom of the tripod head.
When complete, the shaft will be held captive
and allowed to be raised above the threads.

Figure 8: Tightening the spreader
lock knob
Figure 7: Attaching mount
to tripod

Next, remove the Tripod Spreader Lock Knob
(Fig. 1, #2) and washer. Place the center hole of
the Tripod Spreader (Fig. 1, #3) onto the chrome
7

5. Attach the counterweight shaft: Locate
the counterweight shaft (Fig. 1, #9) and thread
down the Locking Nut (Fig. 1, #13) until it stops.
Next, thread the counterweight shaft into the
threaded hole on the front side of the mount,

When the pointer points at your latitude, tighten
both screws until they make contact with the
mount. At your observing site, set up the telescope assembly so that the tripod leg below the
counterweight shaft, labeled “N”, (FIG. 1, #7)
approximately faces True North (or True South
in the Southern Hemisphere). For more informations see page 14 LOCATING THE CELESTIAL POLE.

8. Attach the slow motion control cables:
The LX70 comes equipped with flexible slow
motion control cables for both the RA & Dec
axes. Each cable is securely fastened on each
Figure 10: Set the latitude
axis by a small Phillips head screw. Locate the
Figure 9: Attach the counterRA worm shaft mounting location and notice
weight shaft
that it has a flat portion on one side(see Fig 13).
Slide one of the cables onto the shaft so the
below the declination setting circle (Fig. 1, #14). Phillips head locking screw is aligned with the
Tighten to a firm feel. Adjust the Locking Nut flat portion on the shaft. Using the included Philupward toward the mount until it stops. Tighten lips screw driver, secure the slow motion control
to a firm feel.
cable onto the shaft until firm. Repeat this pro6. Install the latitude adjusting screws: Lo- cess for the declination cable(see Fig 14).
cate the two threaded latitude knobs (Fig. 1, #6)
in the box. Thread the longer latitude adjustment knob into the rear of the mount and the
shorter latitude adjustment knob into the front of
the mount as shown.
7. Set the latitude: Setting the latitude is easier
if it is set before you attach the optical tube and
counterweights. Locate the latitude dial (Fig. 1,
#8); note that there is a triangular pointer above
the dial located on the mount. The pointer is not
fixed; it moves as the mount moves.

Figure 14: Attach the DEC
slow motion control cable
Figure 13: Attach the RA
slow motion control cable

Determine the latitude of your observing location. See APPENDIX C: LATITUDE CHART
for a list of latitudes, or check the internet. Move
the latitude screws in order to move the mount
until the pointer points to your latitude. The 9. Attach the counterweight(s): Look through
two latitude screws work in a “push - pull” op- the hole in the counterweight (Fig. 1, #11) and
eration—as you tighten one, loosen the other. note the pin blocking the hole. Loosen the coun-

Pointer

Figure 11: Latitude pointer
Figure 12: North tripod leg

Figure 15: Remove the
safety nut

Figure 16: Install the counterweight

terweight lock knob so the pin is not obstructing the hole. Unscrew the safety cap (Fig. 1,
#10) from the shaft. Holding the counterweight
firmly in one hand, slip the counterweight to approximately the midpoint of the counterweight
shaft. Tighten the counterweight lock knob(Fig.
1, #12) to a firm feel. Replace the safety cap.
Note: If the counterweight ever slips, the safety
cap prevents the counterweight from sliding entirely off the shaft. Always leave the safety cap
in place when the counterweight is on the shaft.

will need to balance the telescope before use.
See the section BALANCING THE TELESCOPE.
11. Assemble the viewfinder: Locate the viewfinder bracket. Carefully remove the rubber Oring from the bracket and position the O-ring
into the groove located approximately half-way
down the viewfinder tube(see Fig 18 & 19). Unscrew the black alignment screws on the bracket and slide the viewfinder optical tube until the
O-ring seats into the bracket. One alignment
screw on the bracket is spring loaded to allow
easier alignment of the viewfinder. Pull out on
the spring loaded alignment screw to retract it,
allowing the viewfinder tube to fit properly into
the bracket. When the O-ring is properly seated
in the bracket, tighten the two alignment screws
to secure the viewfinder in place.

10. Attach the optical tube: Before attaching
the optical tube, lock both the RA and DEC axes
(Fig. 1, #17 & 18) so the mount does not move
during installation. Verify the cradle ring lock
knobs (Fig. 2 or 3, #27) are tight and securely
fastened to the OTA. The cradle rings should be
roughly centered on the OTA during installation.
While firmly holding the optical tube with both
hands, slide the cradle assembly onto the cradle mounting slot at the top of the mount(see
Fig 17).

Figure 20: Attaching the viewfinder bracket

12. Attach viewfinder bracket: Slide the viewfinder bracket into its receiver on the OTA (Fig.
Figure 17: Tightening the dovetail lock knobs
2 - 4, #36). To secure the viewfinder to the telescope, tighten the viewfinder bracket lock knob
Tighten both OTA dovetail lock knobs (Fig. 1, to a firm feel.
#24) onto the dovetail rail (Fig. 2 - 4, #26) to a
firm feel. The cradle rings and OTA will now be 13. Insert the eyepiece:
securely fastened to the mount.
Newtonian Reflector Models only (Fig 3):
After attaching all accessories to the OTA, you Lift to remove the dust cap from the eyepiece
holder on the focuser assembly (Fig 3, #30). Set
the dust cap aside in a safe place and replace it

Figure 19: Installing the viewfinder
o-ring

Figure 21: Insert the 26mm eyepiece

Figure 18: Viewfinder parts

when you have finished observing. Back off the 4, #31) into the diagonal mirror. Tighten the eyeeyepiece thumbscrews (Fig 3, #32) and insert piece holder thumbscrews(Fig. 4, #32) to a firm
the supplied eyepiece( Fig 3. #31) into the eye- feel to secure the eyepiece.
piece holder. Tighten the holder thumbscrews
to a firm feel to secure the eyepiece.
Balancing the Telescope
Note: Some models require an extension tube In order for the telescope to be stable on the
(if included) be used to reach focus.
tripod and for it to move smoothly, it must be
balanced. To balance the telescope, unlock
Achromatic Refractor only (Fig 2): Lift to re- the Right Ascension or R.A. lock (Fig 1, #17).
move the dust cap from the eyepiece holder on When this axis is unlocked, the telescope pivots
the focuser assembly(Fig 2, # 30). Set the dust on the R.A. axis(see Fig. 1 inset). Later in the
cap aside in a safe place and replace it when procedure, you will also unlock the Declination
you have finished observing. Back off the eye- or Dec. lock (Fig. 1, #18).When unlocked, the
piece thumbscrews (Fig. 2, #41) and slide the telescope pivots on the Dec. axis (see Fig 1 indiagonal(Fig. 2, #40) into the holder tightening set). Most of the motion of the telescope takes
the thumbscrews to a firm feel only. Insert the place by moving about these two axes, sepasupplied 26mm eyepiece(Fig. 2, #31) into the rately or simultaneously. Try to become familiar
diagonal. Tighten the eyepiece holder thumb- with these locks and observe how the telescope
screws (Fig. 2, #32) to a firm feel to secure the moves on each axis. To obtain a fine balance of
eyepiece.
the telescope, follow the following method:
Adjust counterweights
until balanced

↔

Figure 22: Attach the diagonal
Figure 23: Insert the
eyepiece

Maksutov Models only (Fig 4): Lift to remove
the dust cap from the extension tube (Fig 4, #
49). Set the dust cap aside in a safe place and
replace it when you have finished observing.
Back off the diagonal mirror thumbscrews (Fig.
4, #41) and slide the diagonal(Fig. 4, #40) into
the holder and tighten the thumbscrews to a
firm feel only. Insert the supplied eyepiece(Fig.

Figure 26: Balancing the RA axis

↔

Adjust OTA or dovetail rail
until balanced

Figure 24: Attach the diagonal
Figure 25: Insert the
eyepiece
Figure 27: Balancing the DEC axis.

1. Firmly hold the counterweight shaft secure so
it cannot swing freely. Loosen the R.A. lock(Fig.
1, #17). The optical tube now moves freely about
the R.A. axis. Rotate the telescope so that the
counterweight shaft (Fig. 1, #9) is parallel (horizontal) to the ground(see Fig. #26).

the wide-field viewfinder, then look into the eyepiece of the main telescope for a detailed view.
To align the viewfinder, perform steps 1 through
7 during the daytime; perform step 8 at night.
Focus Lock ring

2. Unlock the counterweight lock knob and slide
the counterweight along the counterweight shaft
until the telescope remains in one position without tending to drift down in either direction about
the RA axis. Then re-tighten the counterweight
lock knob, locking the counterweight securely in
position.

Alignment
screws

Front Lens Cell
Figure 28: Viewfinder adjustments

Now, hold the optical tube so that it cannot
swing freely. Lock the R.A. lock and while holding the OTA in place, unlock the Dec. lock (Fig.
1, #18). The OTA is now able to move freely
about the Dec. axis. Lightly loosen the cradle
ring lock knobs (Fig. 2 - 4, #27) so that the main
tube slides easily back and forth in the cradle
rings. Do not loosen the cradle ring lock knobs
too much or the OTA can slip out of the cradle
rings.
Move the main tube in the cradle rings until the
telescope remains in one position without tending to drift down in either direction. Re-lock the
Dec. lock (Fig. 2 - 4, #27).

1. Remove the dust covers from the optical tube
and the viewfinder.
2. If you have not already done so, insert the
low-power 26mm eyepiece into the eyepiece
holder or diagonal of the main telescope.
3. Look through the viewfinder eyepiece at an
object at least 200 yards away.
4. If the distant object is not in focus, turn the focus lock ring on the front of the viewfinder counterclockwise to loosen the viewfinder front lens
cell(see Fig. 28). Twist the front cell until focus is
achieved and retighten the focus lock ring.

The telescope is now properly balanced on both
axes. Next, the viewfinder must be aligned.
5. Unlock the R.A. and Dec locks so the telescope turns freely on both axes. Then point the
Aligning the Viewfinder
main telescope at a tall, well defined and stationary land object (e.g., the top of a telephone
NEVER point the telescope directly at or near pole) at least 200 yards distant and center the
the Sun at any time! Observing the Sun, even object in the telescope’s eyepiece.
for the smallest fraction of a second, will result
in instant and irreversible eye damage, as well 6. Focus the image by turning the OTA focus
as physical damage to the telescope itself.
knobs (Fig. 2 - 4, #29). Retighten the R.A. and
Dec. locks.
The wide field of view of the telescope’s
viewfinder(Fig. 2 - 4, #33) provides an easier 7. Look through the viewfinder and loosen or
way to initially sight objects than the main tele- tighten, as appropriate, one or both of the viewscope’s eyepiece, which has a much narrower finder alignment thumbscrews (Fig. 2 - 4, #35)
field of view. If you have not already attached until the viewfinder’s crosshairs are precisely
the viewfinder to the telescope tube assembly, centered on the object you previously centered
see the section UNPACKING AND ASSEMBLY. in the main telescope’s eyepiece. You are now
ready to make your first observations with your
In order for the viewfinder to be useful, it must be telescope!
aligned to the main telescope, so both the viewfinder and telescope’s optical tube point at the 8. Check this alignment on a celestial object,
same position in the sky. This alignment makes such as a bright star or the Moon, and make
it easier to find objects: First locate an object in any necessary refinements, using the method
11

outlined above. With this alignment performed,
objects first located in the wide-field viewfinder
will also appear in the telescope’s eyepiece.

ditions cannot reasonably support. Keep in mind
that a smaller, but bright and well-resolved image is far superior to one that is larger, but dim
and poorly resolved.

Choosing an Eyepiece

Powers above 400X should be employed only
under the steadiest atmospheric conditions.
Most observers will eventually want three or
four additional eyepieces to achieve the full
range of reasonable magnifications possible
with the LX70 telescopes. See OPTIONAL ACCESSORIES.

A telescope’s eyepiece magnifies the image
formed by the telescope’s main optics. Each
eyepiece has a focal length, expressed in millimeters, or “mm.” The smaller the focal length,
the higher the magnification. For example,
an eyepiece with a focal length of 9mm has a
higher magnification than an eyepiece with a
focal length of 26mm. Your telescope comes
supplied with a 26mm eyepiece which gives a
wide, comfortable field of view with high image
resolution.

Using the Bubble Level
For best telescope performance, the equatorial
mount should be properly leveled. A level tripod allows better weight distribution and easier
alignment on the night sky. The LX70 mount includes a small bubble level near its base. Adjust
the height of each tripod leg until the bubble appears in the center of the circle.

Low power eyepieces offer a wide field of view,
bright, high-contrast images, and eye relief
during long observing sessions. To find an object with a telescope, always start with a lower
power eyepiece such as the 26mm. When the
object is located and centered in the eyepiece,
you may wish to switch to a higher power eyepiece to enlarge the image as much as practical
for prevailing seeing conditions. For information
about optional eyepieces for the LX70 Series
models, see OPTIONAL ACCESSORIES.

Note: Adjusting the tripod on a fully assembled
mount can be dangerous. Get the assistance of
a friend if attempting to adjust the tripod height
while fully assembled.

Observing by Moving the
Telescope Manually

The power, or magnification of a telescope is
determined by the focal length of the telescope
and the focal length of the eyepiece being
used. To calculate eyepiece power, divide the
telescope’s focal length by the eyepiece’s focal
length.

After the telescope is assembled and balanced
as described previously, you are ready to begin
manual observations. View easy-to-find terrestrial objects such as street signs or traffic lights
For example, a 26mm eyepiece is supplied with to become accustomed to the functions and opthe LX70 series. The focal length of the 8” re- erations of the telescope. For the best results
flector model is 1000mm.
during observations, follow the suggestions below:
Telescope Focal Length ÷ Eyepiece Focal Length = Magnification (Power)
Telescope Focal Length = 1000mm
Eyepiece Focal Length = 26mm
1000 ÷ 26 = 38.46

When you wish to locate an object to observe,
first loosen the telescope’s R.A. lock and Dec.
lock. The telescope can now turn freely on its
axes. Unlock each axis separately and practice
moving your telescope. Then practice with two
The eyepiece power, or magnification is there- unlocked axes at the same time. It is very imfore 38X (approximately).
portant to practice this step to understand how
your telescope moves, as the movement of an
Can you ever have too much power? If the type equatorial mount is not intuitive.
of power you’re referring to is eyepiece magnification, yes, you can! The most common mis- Use the aligned viewfinder (see ALIGNING
take of the beginning observer is to “overpower” THE VIEWFINDER, pg 11) to sight-in on the
a telescope by using high magnifications which object you wish to observe. When the object is
the telescope’s aperture and atmospheric con- centered in the viewfinder’s crosshairs, re-tight12

en the R.A. and Dec. locks.

Tracking Objects

Once centered, an object can be focused by
turning one of the knobs of the focusing mechanism. Notice that when observing astronomical
objects, the field of view begins to slowly drift
across the eyepiece field. This motion is caused
by the rotation of the Earth on its axis. Objects
appear to move through the field more rapidly at
higher powers. See TRACKING OBJECTS for
detailed information on how you can counteract
the drift in the field of view.

As the Earth rotates beneath the night sky, the
stars appear to move from East to West. The
speed at which the stars move is called the sidereal rate. You can track objects at this rate
by using the RA and DEC slow motion control
cables(Fig. 1, #19 and #20) on each axis. To
properly track night sky objects, it is best to perform a procedure called a polar alignment.
In the northern hemisphere the polar alignment requires pointing the mounts RA axis at
the north star Polaris as accurately as possible.
In the southern hemisphere the polar alignment
requires pointing at the southern celestial pole.
For using the telescope visually, high precision is not needed for the polar alignment. Only
when using the telescope for astrophotography
will higher precision for the polar alignment be
necessary.

Observe the Moon
Point your telescope at the Moon (note that the
Moon is not visible every night). The Moon contains many interesting features, including craters, mountain ranges, and fault lines. The best
time to view the Moon is during its crescent or
half phase. Sunlight strikes the Moon at an angle during these periods and adds a depth to the
view (see Fig 46). No shadows are seen during
a full Moon, making the overly bright surface to
appear flat and rather uninteresting. Consider
the use of a neutral density Moon filter when
observing the Moon. See OPTIONAL ACCESSORIES. Not only does it cut down the Moon’s
bright glare, but it also enhances contrast, providing a more dramatic image.

To point at Polaris, start by aiming the north leg
of the tripod north. Adjust the latitude(Fig. 1, #6)
and azimuth(Fig. 1, #5) mount adjustments so
that you can see Polaris through the polar axis
view port(Fig. 1, #22).
An optional polar axis scope is available if a
higher precision alignment is desired. See OPTIONAL ACCESSORIES. Polaris will be positioned at an altitude equal to your observing
sites latitude. If you know your local latitude
simply adjust the front and back latitude adjustment bolts until the indicator points to your local
latitude on the scale(Fig. 1, #8). To find your local latitude you can consult a road map , look it
up on the Internet, or see Appendix C: LATITUDE CHART.

Locating the Celestial Pole
In the northern Hemisphere, find the North Star
Polaris by facing North. To get basic bearings
at an observing location, take note of where the
Sun rises (East) and sets (West) each day. After
the site is dark, face North by pointing your left
shoulder toward where the Sun set. To precisely point at the pole, find the North Star (Polaris)
by using the Big Dipper as a guide (See figure
below).
In the southern Hemisphere, you align the
mount to the southern celestial pole. To do this
it is necessary to reference star patterns since
the southern celestial pole has no nearby bright
stars. The closest bright star to the south celestial pole is Sigma Octanis, which is about one
degree away. Using Sigma Octanis and other
bright stars will help you locate the pole.
Toward
True North

Toward
True North
Side
View

Figure 30: RA Polar Axis
toward True North (Polaris)

Top View

Figure 31: RA Polar Axis
toward True North (Polaris)
Pointer

Little Dipper

Figure 29: Latitude Scale with pointer

Polaris
(North Star)

Big Dipper

Cassiopeia

Figure 32 : Finding Polaris (North Star) For Northern
Hemisphere observers

Maintenance

Inspecting the Optics

General Maintenance

A Note about the Flashlight Test: If a flashlight or
other high-intensity light source is pointed down
the main telescope tube, the view (depending
upon the observer’s line of sight and the angle
of the light) may reveal what appears to be
scratches, dark or bright spots, or just generally
uneven coatings, giving the appearance of poor
quality optics. These items are only seen when
a high intensity light is transmitted through lenses or reflected off the mirrors, and can be seen
on any high quality optical system, including giant research telescopes. The optical quality of
a telescope cannot be judged by the “flashlight
test;” the true test of optical quality can only be
conducted through careful star testing.

LX70-Series telescopes are precision optical
instruments designed to yield a lifetime of rewarding views. Given the care and respect due
any precision instrument, your LX70 will rarely,
if ever, require factory servicing. Maintenance
guidelines include:
a. Avoid cleaning the telescope’s optics: A little
dust on the mirrors or the front surface of the
telescope’s lens causes virtually no degradation of image quality and should not be considered reason to clean the lens.
b. When absolutely necessary, dust on the mirrors or front lens should be removed with gentle
strokes of a camel hair brush or blown off with
an ear syringe (available at any pharmacy).
DO NOT use a commercial photographic lens
cleaner.
c. Organic materials (e.g., fingerprints) on the
front lens may be removed with a solution of
3 parts distilled water to 1 part isopropyl alcohol. You may also add 1 drop of biodegradable dishwashing soap per pint of solution. Use
soft, white facial tissues and make short, gentle
strokes. Change tissues often. Caution: Do not
use scented or lotion tissues or damage could
result to the optics.

Figure 33: Correct (1) and incorrect (2) collimation as viewed
during a star test

d. If the LX70 is used outdoors on a humid
night, water condensation on the telescope surfaces will probably result. While such condensation does not normally cause any damage to
the telescope, it is recommended that the entire
telescope be wiped down with a dry cloth before
the telescope is packed away. Do not, however,
wipe any of the optical surfaces. Rather, simply
allow the telescope to sit for some time in the
warm indoor air, so that the wet optical surfaces
can dry unattended.

ly unthreaded to the point where the secondary
mirror-holder (Fig. 35, #3) can rotate about its
axis parallel to the main tube. Grasp the secondary mirror-holder (avoid touching the mirror surface!) with your hand and rotate it until,
looking through the drawtube, you can see the
primary mirror centered as well as possible in
the reflection of the secondary mirror. With the
rotation of the secondary mirror-holder at this
best-possible position, thread in the three secondary collimation screws (Fig. 35, #2) to lock
the rotational position. Then, if necessary, make
adjustments to these three collimation screws
to refine the tilt-angle of the secondary mirror,
until the entire primary mirror can be seen centered within the secondary mirror’s reflection.
With the secondary mirror thus aligned the image through the drawtube appears as in Fig. 40.

Alignment (Collimation) of
the Newtonian Reflector OTA
The optical systems of Newtonian Reflector
telescopes include the following parts: primary
mirror (Fig. 34, #1); secondary mirror (Fig. 34,
#2); secondary mirror-holder (Fig. 34, #3); secondary mirror-vanes (Fig. 34, #4) and (Fig. 35,
#1); primary mirror-tilt screws (Fig. 34, #5). The
telescope’s image is brought to a focus at (Fig.
34, #6).
1. Confirm alignment - To confirm optical
alignment look down the focuser drawtube (Fig.
37, #1) with the eyepiece removed. The edge of
the focuser drawtube frames reflections of the
primary mirror (Fig. 37, #2), the secondary mirror (Fig. 37, #3), the four (“spider”) vanes (Fig.
37, #4) holding the secondary mirror, and the
observer’s eye (Fig. 37, #5). With the optics
properly aligned, all of these reflections appear
concentric (centered), as shown in Fig. 37. Any
deviation from concentricity of any of these telescope parts with the eye requires adjustments
to the secondary mirror-holder (Fig. 35) and/or
the primary mirror cell (Fig. 36), as described
below.

4. Primary mirror adjustments: If the secondary mirror (Fig. 40, #1) and the reflection of the
primary mirror (Fig. 40, #2) appear centered
within the drawtube (Fig. 40, #3), but the reflection of your eye and the reflection of the secondary mirror (Fig. 40, #4) appear off-center,
then the primary mirror tilt requires adjusting,
using the Phillips head screws of the primary
mirror cell (Fig. 36, #3). These primary mirror-tilt
screws are located behind the primary mirror,
at the lower end of the main tube. See Fig. 36.
Before adjusting the primary mirror-tilt screws,
first unscrew by several turns the three long
primary mirror lock screws (Fig. 36, #2) which
are also located on the rear surface of the primary mirror cell and which alternate around the
cell’s circumference with the three long and thin
thumbscrews. These lock screws do not have
springs beneath them. Then by trial and error
turn the primary mirror tilt thumbscrews (Fig. 36,
#3) until you develop a feel for which way to turn
each screw to center the reflection of your eye
in the drawtube. (An assistant is helpful in this
operation.) With your eye centered as shown in
Fig. 37, turn the three long and thin mirror lock
screws (Fig. 36, #2) to re-lock the tilt-angle of
the primary mirror.

2. Secondary mirror-vane adjustments: If the
secondary mirror (1, Fig. 38) is left or right of
center within the drawtube (Fig. 38, #2), slightly
loosen the 3 collimation screws on the top of
the secondary mirror holder (Fig. 35, #2). Next,
tighten or loosen as necessary, the central
Phillips screw to center the secondary mirror
position in the focuser draw tube. When correctly positioned, lightly tighten the 3 collimation screws (Fig. 35, #2) until they touch the top
of the secondary mirror. The secondary mirror
should now be centered in the focuser drawtube
left or right. If the secondary mirror (Fig. 38, #1)
is above- or below-center within the drawtube,
thread inward one of the adjustment/lock knobs
(Fig. 35, #1) while unthreading another of these
knobs. Only make adjustments to two knobs at
a time until the secondary mirror appears as in 5. The telescope’s optical system is now aligned,
Fig. 39.
or collimated. This collimation should be rechecked from time to time, with small adjust3. Secondary mirror-holder adjustments: If ments (per steps 1, 2, and/or 3, above) effected
the secondary mirror (Fig. 39, #1) is centered as required to keep the optics well-aligned.
in the focuser drawtube (Fig. 39, #2), but the
primary mirror is only partially visible in the reflection (Fig. 39, #3), the three secondary mirror
collimation screws (Fig. 35, #2) should be slight16

Figure 34

Newtonian Reflector (section view)

2
1

3
2

Figure 35

Figure 36

1
2
2

Figure 37

Figure 38

2
4
2
3

Figure 39

Figure 40

OPTIONAL ACCESSORIES
A wide assortment of professional Meade accessories is available for the LX70 Series telescope
models. The premium quality of these accessories
is well-suited to the quality of the instrument itself.
Consult the Meade Website (www.meade.com) for
complete details on these and other accessories.

#905 Variable Polarizer (1.25”): The #905 system includes 2 Polarizer filters mounted in a specially-machined cell, for glare-reduction in observing the Moon. Rotate the thumbscrew at the side
of the unit to achieve light transmission between
5% and 25% of its original value. The #905 inserts
into the diagonal of the telescope, followed by an
eyepiece.

#670010 LX70 Polar Scope: The Meade LX70
Polar scope is designed to assist the user in performing a polar alignment on the night sky. The
polar scope includes a reticule pattern which is
used in the alignment process, making the LX70
polar scope even more user friendly. As a result,
the LX70 mount can be aligned with a higher precision and allows the user to more quickly enjoy the
night sky. See the Meade website for more details.

Series 4000 Photo-Visual Color Filters: Color filters significantly enhance visual and photographic
image contrast of the Moon and planets. Each filter threads into the barrel of any Meade 1.25” eyepiece, and into the barrels of virtually all other eyepiece brands as well. Meade filters are available in
12 colors for lunar and planetary applications, and
in Neutral Density as a lunar glare-reduction filter.

#670011 LX70 Motor Drive Kit: The LX70 motor drive kit attaches to both telescope axes. The
motor drive kit allows tracking of celestial objects
at the speed of the earth’s rotation. The included
hand controller is used to adjust the mount when
using the mount for astrophotography. Use of the
LX70 motor drive kit requires the LX70 mount to
be properly polar aligned on the night sky. See the
Meade website for more details.

Series 4000 Nebular Filters: A modern boon to
the city-dwelling deep-space observer, the interference nebular filter effectively cancels out the
effects of most urban light pollution, while leaving
the light of deep-space nebular emissions virtually
un-attenuated. Meade Series 4000 Nebular Filters
utilize the very latest in coating technology, and
are available with threaded cells for eyepieces or
for attachment to the rear cells of Meade ACF telescopes.

Laser Collimator: Meade’s Laser collimator helps
make collimation of Newtonian telescopes quick
and easy. Collimation is a method to align your
telescope’s optics. Your telescope is aligned at the
factory, but shipping and handling can sometimes
mis-align collimation. Misaligned collimation can
mean dimmer and blurrier images in your telescope eyepiece. Make collimation quick and easy
with a Meade laser collimator.
Series 4000 8 - 24mm Zoom Eyepiece: The internal zoom optics of this eyepiece move on smooth,
precisely machined surfaces which maintain optical collimation at all zoom settings. A scale graduated in 1mm units indicates the zoom focal length
in operation. An excellent addition to any eyepiece
set.

#91101 Meade LED Flashlight: The LED flashlight features a very bright beam from 16 LED’s
and is push button selectable from white for normal illumination to red to preserve night vision.
Heavy duty metal construction, with threaded battery compartment. (3 “AAA” batteries required.)
Meade Series 4000 Eyepiece and Filter Set:
Complete set of the most popular accessories.
Includes six popular Meade Series 4000 Super Plossl Eyepieces in focal lengths of 6.4mm,
9.7mm, 12.4mm, 15mm, 32mm and 40mm. All
eyepieces feature a standard 1.25” barrel size,
with a 52° apparent field of view and are of a 4-element design with premium optical glass. This this
kit also contains a Meade Series 4000 Color Filter Set #1 including high quality “dyed in glass”
#12 Yellow, #23 Light Red, #58 Green and # 80A
Blue filters which are very useful for bringing out
various details on the planets. There is also a Series 4000 ND96 Moon Filter to reduce glare and
increase clarity when observing the Moon.

#140 2x Barlow Lens: A 3-element design, doubles each eyepiece power while maintaining uncompromised image resolution, color correction,
and contrast. Insert the #140 into the telescope’s
eyepiece holder first, followed by the diagonal
(as applicable) and eyepiece. The #126 2x Bar- To find out more about these and other accessories
low Lens, a compact 2-element alternative to the available for your telescope, check out the Meade
#140, may also be employed with any LX70 Se- website or contact your local Meade dealer.
ries telescope.
18

APPENDIX A:
Celestial Coordinates
A celestial coordinate system was created that
maps an imaginary sphere surrounding the
Earth upon which all stars appear to be placed.
This mapping system is similar to the system of
latitude and longitude on Earth surface maps.
In mapping the surface of the Earth, lines of longitude are drawn between the North and South
Poles and lines of latitude are drawn in an EastWest direction, parallel to the Earth’s equator.
Similarly, imaginary lines have been drawn to
form a latitude and longitude grid for the celestial sphere. These lines are known as Right Ascension and
Declination.

Right Ascension (R.A.): This celestial version
of longitude is measured in units of hours (hr),
minutes (min), and seconds (sec) on a 24-hour
“clock” (similar to how Earth’s time zones are
determined by longitude lines). The “zero” line
was arbitrarily chosen to pass through the constellation Pegasus — a sort of cosmic Greenwich meridian. R.A. coordinates range from 0hr
0min 0sec to 23hr 59min 59sec. There are 24
primary lines of R.A., located at 15-degree intervals along the celestial equator. Objects located
further and further East of the zero R.A. grid line
(0hr 0min 0sec) carry higher R.A. coordinates.

Practice moving the telescope from one easy-tofind object to another. In this way, the precision
required for accurate object location becomes
evident.

North
Celestial
Pole
(Vicinity
of Polaris)

+90 Dec.
Star

1
17
18
19

13 12

ation
clin
De

The celestial map also contains two poles and
an equator just like a map of the Earth. The
poles of this coordinate system are defined as
those two points where the Earth’s north and
south poles (i.e., the Earth’s axis), if extended to
infinity, would cross the celestial sphere. Thus,
the North Celestial Pole (1, Fig. 41) is that point
in the sky where an extension of the North Pole
intersects the celestial sphere. The North Star,
Polaris is located very near the North Celestial
Pole. The celestial equator (2, Fig. 41) is a projection of the Earth’s equator onto the celestial sphere. Just as an object’s position on the
Earth’s surface can be located by its latitude and
longitude, celestial objects may also be located
using Right Ascension and Declination. For example, you could locate Los Angeles, California,
by its latitude (+34°) and longitude (118°). Similarly, you could locate the Ring Nebula (M57)
by its Right Ascension (18hr) and its Declination
(+33°).

Declination (Dec.): This celestial version of latitude is measured in degrees, arc-minutes, and
arc-seconds (e.g., 15° 27’ 33”). Dec. locations
north of the celestial equator are indicated with
a plus (+) sign (e.g., the Dec. of the North celestial pole is +90°). Dec. locations south of the
celestial equator are indicated with a minus (–)
sign (e.g., the Dec. of the South celestial pole is
–90°). Any point on the celestial equator (such
as the constellations of Orion, Virgo, and Aquarius) is said to have a Declination of zero, shown
as 0° 0’ 0.”APPENDIX B: Setting Circles
Setting circles permit the location of faint celestial objects not easily found by direct visual
observation. With the telescope pointed at the
North Celestial Pole, the Dec. circle (see Fig.
43) should read 90° (understood to mean +90°).
Each division of the Dec. circle represents a 1°
increment. The R.A. circle (see Fig. 42) runs
from 0hr to (but not including) 24hr, and reads in
increments of 10 minutes. Using setting circles
requires a developed technique. When using
the circles for the first time, try hopping from one
bright star (the calibration star) to another bright
star of known coordinates.

Earth’s
Rotation

20 21

Right Ascension

8
4

7
6
5

Celestial
Equator
0 Dec.

2
South
Celestial
Pole

-90 Dec.

Figure 41: Celestial Sphere

APPENDIX B:
Setting Circles

the objects DEC coordinate is aligned with the 0
registration mark. If the procedure has been followed carefully, the bright star should now be in
the center of the telescope eyepiece and setting
circles showing the bright star coordinates.

To use the setting circles to locate an object not
easily found by direct visual observation:
Insert a low-power eyepiece, such as a 26mm,
into the focuser assembly. Pick out a bright star
with which you are familiar (or is easily located)
that is in the area of the sky in which your target
object is located. Look up the R.A. coordinate of
the bright star, and also of the object you wish
to locate, in a star atlas or on the internet. Point
the telescope at the bright star. Then loosen the
R.A. setting circle lock knob (see Fig. 42) and
turn the R.A. setting circle to read the correct
R.A. coordinate of the bright star; lock the R.A.
setting circle lock knob to secure the setting
circle in place (If you are in the northern hemisphere, use the top numbers on the RA setting
circle. If you are in the southern hemisphere use
the bottom numbers.). Next, adjust the DEC setting circle by moving the setting circle ring until

To locate another object, unlock the RA and
DEC locks and move the telescope so the RA
and DEC setting circle coordinates match the
target object. Then lock each axis and use the
slow motion controls to track the object.
If when using the setting circles to locate objects, you do not immediately see the object
you are seeking, try searching the adjacent sky
area. Start with the 26mm eyepiece when locating object since it has a wider field of view than
the 9mm. Because of its much wider field, the
viewfinder may be of significant assistance in
locating and centering objects, after the setting
circles have been used to locate the approximate position of the object.

RA Setting Circle
Lock Knob
DEC Setting Circle
RA Setting Circle

Figure 42: RA setting circle and lock knob

Figure 43: DEC setting circle

APPENDIX C:
Latitude Chart
Latitude Chart for Major Cities of the World
To aid in the polar alignment procedure, latitudes of major cities around the world are listed below. To determine the latitude of an observing site not listed on the chart, locate the city closest
to your site or locate your site on the internet. Then follow the procedure below:
Northern hemisphere observers (N): If the site is over 70 miles (110 km) north of the listed
city, add one degree for every 70 miles. If the site is over 70 miles South of the listed city, subtract one degree per 70 miles.
Southern Hemisphere observers (S): If the site is over 70 miles (110 km) north of the listed
city, subtract one degree for every 70 miles. If the site is over 70 miles South of the listed city,
add one degree per 70 miles.
NORTH AMERICA
City
Albuquerque
Anchorage
Atlanta
Boston
Calgary
Chicago
Cleveland
Dallas
Denver
Detroit
Honolulu
Jackson
Kansas City
Kenosha
Las Vegas
Little Rock
Los Angeles
Mexico City
Miami
Minneapolis
Nashville
New Orleans
New York
Oklahoma City
Ottawa
Philadelphia
Phoenix
Portland
Salt Lake City
San Antonio
San Diego
San Francisco
Seattle
Washington
EUROPE
City
Amsterdam
Athens
Bern
Copenhagen
Dublin
Frankfurt
Glasgow
Helsinki
Lisbon
London
Madrid

State/Prov./Country
New Mexico
Alaska
Georgia
Massachusetts
Alberta
Illinois
Ohio
Texas
Colorado
Michigan
Hawaii
Mississippi
Missouri
Wisconsin
Nevada
Arkansas
California
Mexico
Florida
Minnesota
Tennessee
Louisiana
New York
Oklahoma
Ontario
Pennsylvania
Arizona
Oregon
Utah
Texas
California
California
Washington
District of Columbia

Latitude
35° N
61° N
34° N
42° N
51° N
42° N
41° N
33° N
40° N
42° N
21° N
32° N
39° N
45° N
36° N
35° N
34° N
19° N
26° N
45° N
36° N
30° N
41° N
35° N
45° N
40° N
33° N
46° N
41° N
29° N
33° N
38° N
47° N
39° N

Country
Netherlands
Greece
Switzerland
Denmark
Ireland
Germany
Scotland
Finland
Portugal
England
Spain

Latitude
52° N
38° N
47° N
56° N
53° N
50° N
56° N
60° N
39° N
51° N
40° N

EUROPE (continued)
City
Country
Oslo
Norway
Paris
France
Rome
Italy
Stockholm
Sweden
Vienna
Austria
Warsaw
Poland
SOUTH AMERICA
City
Country
Bogotá
Colombia
São Paulo
Brazil
Buenos Aires
Argentina
Montevideo
Uruguay
Santiago
Chile
Caracas
Venezuela
ASIA
City
Country
Beijing
China
Hong Kong
China
Seoul
South Korea
Taipei
Taiwan
Tokyo
Japan
Sapporo
Japan
Bombay
India
Calcutta
India
Hanoi
Vietnam
Jedda
Saudi Arabia
AFRICA
City
Country
Cairo
Egypt
Cape Town
South Africa
Rabat
Morocco
Tunis
Tunisia
Windhoek
Namibia
AUSTRALIA AND OCEANIA
City
State/Country
Adelaide
South Australia
Brisbane
Queensland
Canberra
New South Wales
Alice Springs
Northern Territory
Hobart
Tasmania
Perth
Western Australia
Sydney
New South Wales
Melbourne
Victoria
Auckland
New Zealand

Figure 44: Latitude for major cities
21

Latitude
60° N
49° N
42° N
59° N
48° N
52° N
Latitude
4° N
23° S
35° S
35° S
34° S
10° N
Latitude
40° N
23° N
37° N
25° N
36° N
43° N
19° N
22° N
21° N
21° N
Latitude
30° N
34° S
34° N
37° N
23° S
Latitude
35° S
27° S
35° S
24° S
43° S
32° S
34° S
38° S
37° S

served during its crescent or half phase when
Sunlight strikes the Moon’s surface at an angle.
It casts shadows and adds a sense of depth
to the view. No shadows are seen during a full
Moon, causing the overly bright Moon to appear flat and rather uninteresting through the
telescope. Be sure to use a neutral Moon filter
when observing the Moon. Not only does it protect your eyes from the bright glare of the Moon,
but it also helps enhance contrast, providing a
more dramatic image. Using your telescope,
brilliant detail can be observed on the Moon,
including hundreds of lunar craters and Maria,
described below.

APPENDIX D:
Basic Astronomy
In the early 17th century Italian Scientist Galileo, using a telescope smaller than your LX70,
turned it skyward instead of looking at the distant trees and mountains. What he saw, and
what he realized about what he saw, has forever changed the way mankind thinks about
the universe. Imagine what it must have been
like being the first human to see moons revolve
around the planet Jupiter or to see the changing
phases of Venus! Because of his observations,
Galileo correctly realized Earth’s movement and
position around the Sun, and in doing so, gave
birth to modern astronomy. Yet Galileo’s telescope was so crude, he could not clearly make
out the rings of Saturn. Galileo’s discoveries
laid the foundation for understanding the motion
and nature of the planets, stars, and galaxies.
Building on his foundation, Henrietta Leavitt determined how to measure the distance to stars,
Edwin Hubble gave us a glimpse into the possible origin of the universe, Albert Einstein unraveled the crucial relationship of time and light,
and 21st-century astronomers are currently
discovering planets around stars outside our
solar system. Almost daily, using sophisticated
successors to Galileo’s telescope, such as the
Hubble Space Telescope and the Chandra XRay Telescope, more and more mysteries of the
universe are being probed and understood.

Craters are round meteor impact sites covering most of the Moon’s surface. With no atmosphere on the Moon, no weather conditions exist, so the only erosive force is meteor strikes.
Under these conditions, lunar craters can last
for millions of years.
Maria (plural for mare) are smooth, dark areas
scattered across the lunar surface. These dark
areas are large ancient impact basins that were
filled with lava from the interior of the Moon by
the depth and force of a meteor or comet impact. Twelve Apollo astronauts left their boot
prints on the Moon in the late 1960’s and early
1970’s. However, no telescope on Earth is able
to see these footprints or any other artifacts.
In fact, the smallest lunar features that may be
seen with the largest telescope on Earth are
about one-half mile across.
Planets change positions in the sky as they orbit around the Sun. To locate the planets on a
given day or month, consult a monthly astronomy magazine, such as Sky and Telescope or
Astronomy. Listed below are the best planets
for viewing through the LX70 telescope.

We are living in the golden age of astronomy.
Unlike other sciences, astronomy welcomes
contributions from amateurs. Much of the
knowledge we have on subjects such as comets, meteor showers, double and variable stars,
the Moon, and our solar system comes from
observations made by amateur astronomers.
So as you look through your Meade telescope,
keep in mind Galileo. To him, a telescope was
not merely a machine made of glass and metal,
but something far more—a window of incredible discovery. Each glimpse offers a potential
secret waiting to be revealed.

Venus is about nine-tenths the diameter of
Earth. As Venus orbits the Sun, observers can
see it go through phases (crescent, half, and
full) much like those of the Moon. The disk of
Venus appears white as Sunlight is reflected off
the thick cloud cover that completely obscures
any surface detail.

Objects in Space Listed below are some of the Mars is about half the diameter of Earth, and apmany astronomical objects that can be seen pears through the telescope as a tiny reddishwith your telescope:
orange disk. It may be possible to see a hint
of white at one of the planet’s Polar ice caps.
The Moon is, on average, a distance of 239,000 Approximately every two years, when Mars is
miles (380,000km) from Earth and is best ob- closest to Earth in its orbit, additional detail and
22

coloring on the planet’s surface may be visible.
Jupiter is the largest planet in our solar system
and is eleven times the diameter of Earth. The
planet appears as a disk with dark lines stretching across the surface. These lines are cloud
bands in the atmosphere. Four of Jupiter’s
moons (Io, Europa, Ganymede, and Calisto) can
be seen as “star-like” points of light when using
even the lowest magnification. These moons
orbit Jupiter so that the number of moons visible on any given night changes as they circle
around the giant planet.

start with an easy grouping of stars, such as the
Big Dipper in Ursa Major. Then, use a star chart
to explore across the sky.

Galaxies are large assemblies of stars, nebulae, and star clusters that are bound by gravity.
The most common shape is spiral (such as our
own Milky Way), but galaxies can also be elliptical, or even irregular blobs. The Andromeda
Galaxy (M31) is the closest spiral-type galaxy to
our own. This galaxy appears fuzzy and cigarshaped. It is 2.2 million light years away in the
constellation Andromeda, located between the
Saturn is nine times the diameter of Earth and large “W” of Cassiopeia and the great square of
appears as a small, round disk with rings ex- Pegasus.
tending out from either side. In 1610, Galileo,
the first person to observe Saturn through a
telescope, did not understand that what he was
seeing were rings. Instead, he believed that
Saturn had “ears.” Saturn’s rings are composed
of billions of ice particles ranging in size from a
speck of dust to the size of a house. The major division in Saturn’s rings, called the Cassini
Division, is occasionally visible through medium
sized telescopes. Titan, the largest of Saturn’s
moons can also be seen as a bright, star-like
object near the planet.
Deep-Sky Objects: Star charts can be used to
locate constellations, individual stars and deepsky objects. Examples of various deep-sky objects are given below:

Figure 45: Saturn

Stars are large gaseous objects that are self-illuminated by nuclear fusion in their core. Because
of their vast distances from our solar system, all
stars appear as pinpoints of light, irrespective of
the size of the telescope used.
Nebulae are vast interstellar clouds of gas and
dust where stars are formed. Most impressive
of these is the Great Nebula in Orion (M42), a
diffuse nebula that appears as a faint wispy gray
cloud. M42 is 1600 light years from Earth.
Open Clusters are loose groupings of young
stars, all recently formed from the same diffuse
nebula. The Pleiades is an open cluster 410
light years away. Through the LX70 telescope
numerous stars are visible.

Figure 47: Jupiter
Figure 46: Craters on the
Moon

Constellations are large, imaginary patterns of
stars believed by ancient civilizations to be the
celestial equivalent of objects, animals, people,
or gods. These patterns are too large to be seen
through a telescope. To learn the constellations,
23

Meade Customer Service
If you have a question concerning your LX70-Series telescope, contact the Meade Instruments
Customer Service Department at:
Telephone: (800) 626-3233.
Customer Service hours are 7:00 AM to 5:00 PM, Pacific Time, Monday through Friday. In the unlikely event that your LX70-Series telescope requires factory servicing or repairs, write or call the
Meade Customer Service Department first, before returning the telescope to the factory, giving full
particulars as to the nature of the problem, as well as your name, address, and daytime telephone
number. The great majority of servicing issues can be resolved by telephone, avoiding return of
the telescope to the factory. If factory service is required, you will be assigned a Return Goods
Authorization (RGA) number prior to return.

Meade Limited Warranty
Every Meade telescope, spotting scope, and telescope accessory is warranted by Meade Instruments Corp. (“Meade”) to be free of defects in materials and workmanship for a period of ONE
YEAR from the date of original purchase in the U.S.A. and Canada. Meade will repair or replace
a product, or part thereof, found by Meade to be defective, provided the defective part is returned
to Meade, freight-prepaid, with proof of purchase. This warranty applies to the original purchaser
only and is non-transferable. Meade products purchased outside North America are not included
in this warranty, but are covered under separate warranties issued by Meade international distributors.
RGA Number Required: Prior to the return of any product or part, a Return Goods Authorization
(RGA) number must be obtained from Meade by writing, or calling (949) 451-1450. Each returned
part or product must include a written statement detailing the nature of the claimed defect, as well
as the owner’s name, address, and phone number.
This warranty is not valid in cases where the product has been abused or mishandled, where unauthorized repairs have been attempted or performed, or where depreciation of the product is due
to normal wear-and-tear. Meade specifically disclaims special, indirect, or consequential damages
or lost profit which may result from a breach of this warranty. Any implied warranties which cannot
be disclaimed are hereby limited to a term of one year from the date of original retail purchase.
This warranty gives you specific rights. You may have other rights which vary from state to state.
Meade reserves the right to change product specifications or to discontinue products without notice.

OBSERVATION LOG

© 2014 Meade Instruments Corp. reserves the right to change product specifications or to discontinue products without
notice.
12/2014 LX70 SERIES
14-9287-00 Rev 0
28

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