Omegon N114/900 EQ-1 User manual

Instructions Manual
Omegon® N114/900 EQ-1
English version 9.2016 Rev A Art. Nr 11266

The Omegon® N 114/900 EQ-1
Congratulations on the purchase
of the new Omegon® N 114/900
EQ-1. This telescope will give you
hours of fun, with its all optical
mirror lens and light gathering
capability; it is the ideal
companion to start in the world
of amateur astronomy. With this
telescope, you will be able to see
the craters on the Moon, star
clusters, some nebulae, the
Jupite’sr disc features and its
Galilean moons and the rings of
Saturn.
Included parts. Besides the
complete telescope, we have
also included the following
accessories: Eyepiece K25mm,
Eyepiece K10mm, Barlow lens
2x, Finderscope;
1. Knowing your telescope.
1- Focuser; 8- Tripod leg;
2- Finderscope; 9- Altitude side fix knob (partially shown);
3- Tube ring; 10- R.A. adjustment handle;
4- Optical tube; 11- Accessory tray;
5- Collimation thumbscrew for primary mirror; 12- Counterweigth stop/foot saver;
6- Declination adjustment handle; 13- Counterweight;
7- Altitude/Latitude adjustment; 14- Counterweight shaft;
2. Getting Started. It is very simple to get started. Here is how the telescope works. The telescope
should point to the object being observed. The mirror at the bottom of the telescope’s tube gathers
the object’s light and reflects it to the secondary mirror that brings it to the eyepiece. Close to the
telescope’s aperture, there is the focuser. The focuser tube moves up and down to get a precise
focused image. At the focuser, one can use the supplied accessories. Different accessories
combinations give different results, such as different image magnifications or correct image. But all
this will be explained in detail in the next pages. 3. Assembly. Start by setting up the tripod as
shown in figure 2. Use the supplied bolts and nuts. Next, place the accessory tray (part #11 –fig. 1)
and fix it using the wing nuts and small screws –fig. 3. After this, the tripod should be stable. Place
the equatorial mount head on top of the tripods base, as shown in figure 4. Use the supplied hand-
bolt to fix it. Thread the counter-weight shaft and slide the counter-weight (figure 5). Use the
counter-weight’s thumbscrew to avoid it from slipping. Place the control-handles as shown in figure
6. Now fix the tube’s ring (figure 7) and place the tube. The mount’s altitude axis can be adjusted as
shown in figure 8. Use the side hand-knob to tighten or release the altitude’s axis (fig. 9). Release the
R.A. locking thumbscrew so that the R.A. axis is loose. Slide the counter-weight’s position to balance
the axis (figure 10). Proceed likewise with the Dec. Axis; slide the tube (figure 11).
Figure 1. Parts description.

Figure 2. Tripod assembly.
Figure 3. Tray placement.
Figure 4. Place equatorial head on top of tripod.
Figure 5. Thread the counter-weight shaft. Insert counterweight.
Figure 6. Fix Dec. and R.A. handles.
Figure 7. Fix the tube’s ring.

4. How to use the equatorial
mount. The equatorial mount is a
powerful tool for astronomical
observation. The main purpose of
an equatorial mount is to accurately
point a telescope to a certain
object. There are two axis in the
equatorial mount. A R.A. axis and a
Dec. axis. The telescope’s tube sits
on the Dec axis.
Equatorial mount parts description
1- Declination Handle 2- Declination Fixing Knob 3- R.A. Axis
4- Latitude/altitude adjustment 5- Counterweight 6- Counterweight shaft
7- R.A. Handle 8- R.A. Fixing Knob 9- Dec. Axis
Figure 8. Adjust Dec. axis.
Figure 9. Tighten the side hand-knob.
Figure 10. Balance the R.A. axis with counterweight.
Figure 11. Balance the Dec. axis.
Figure 12. Detailed mount parts.
Figure 13. Adjusting latitude/altitude.

There are two axis in the eq. mount. One is the R.A. (Right Ascension) axis as shown in fig. 14. This
means the telescope can rotate around this axis. The R.A. should point north to Polaris. Tracking (see
what this is below) is made using the R.A. axis. To lock the rotation the locking R.A. knob should be
used (fig. 15). The second axis is the Dec (Declination) axis –fig. 16. To lock this axis use the Dec
locking knob as shown in figure 17.
4.1. What is tracking?
Star’s positions rotate, slowly but surely, in the night sky. This is caused by the Earth’s rotation. Every
24 hours the Earth make a complete turn. So does the night sky. This means that, when observing
through a telescope, the stars will move away from the field of view after a few seconds. This is even
more evident when using high power eyepieces. They go away quite easily from the field of view.
Use the Dec and R.A. handles to precise point the telescope. Make sure the axis are securely locked.
To keep a star in the centre of the field of view tracking is required. Tracking can be done manually
or by a motor. Manual tracking can be done using the tow Dec and R.A. handles. They allow small
Figure 14. R.A. Axis.
Figure 15. Locking the R.A. axis.
Figure 17. Locking the Dec. Axis.
Figure 16. Dec. Axis.

corrections to be made in each axis. However this is not the recommend procedure to track an
object. The mount should be placed in station i.e. aligned in such a way that only the R.A. is required
to turn to track a start. 4.2. How to set the mount in station. Point the telescope’s R.A. axis to
north –fig. 18. Release the altitude break - fig. 19- so that the R.A. inclination can be adjusted.
Rotate the latitude adjustment so that the inclination of the mount is the same as the latitude of
observers. For an observer in Munich the latitude is 48 degrees. The inclination angle (Ɵ) should be
approximately 48 degrees. Make sure to re-tighten the altitude break. Now that the mount is
pointing north and has the observer’s location latitude your mount is set on station. This mean that
the mount should not be moved during observation. The two R.A. and Dec. axis can be used to
position and point the telescope to any part of the sky.
The altitude/latitude adjustment should NOT be used when
observing. Continuous use can cause wear or even break the knob.
Figure 18. Mount points north.
Figure 19. Release altitude break and adjust inclination.
Figure 20. Adjust inclination to latitude.
Figure 21. Check your latitude.

5. Aligning the Finderscope
Figure A. A distant object is centered at the telescope’s field
of view. In this example we have a house with a chimney.
The chimney is the reference point to place at the center of
the field of view. We first look through the telescope with
the lowest magnification possible (H20mm should be
preferrable). So we have the widest field of view.
STEP 1
Figure B. Looking through the finderscope we see the same
building but in this case the chimney is not centered. We
adjust the finderscope using the three thumbscrews so that
the finderscope moves slightly. This is enough to correct the
objects position in the finderscope. Trial and error is required
to get a satisfactory result. Make sure to tighten the 3 screws
after finishing so that the finderscope tube does not move.
STEP 2
Figure C. After playing with the three findercope
thumbscrews and some trial and error we get the
finderscope recticle close to the center (in this case the
chimney). The Finderscope is now ready to use!
STEP 3
6. Alignment of the optics and collimation.
Telescopes require periodical checking for the alignment of the optics. The optics should be
aligned (or collimated) so that the telescope can achieve a good performance and deliver a

sharp image. This is especially important for reflector telescopes (that use mirrors). First
let’s start by checking collimation.
Look for a bright star in the evening sky and centre it in the eyepiece field of view. Some
power is required to check alignment, make sure the star is focused. Now use the focuser
knobs and rotate so that the star comes out of focus (defocused). You will be able to see a
defocused star. It will appear as a series of rings. These are called diffraction rings and they
will be important to determine how good (or how bad is the alignment –figure 23). If the
optics are well aligned you will be able to see a defocused star similar to a series of
concentric rings (1 in figure 23), a poorly aligned telescopes will show a series of eccentric
rings (2 in figure 23).
The telescope is equipped with a set of collimation screws for both the secondary mirror
(figure 25) and for the primary mirror (figure 26). They can be used to adjust the tilt of both
mirrors and to achieve alignment. This information is for your reference.
6. Collimate the optics.
Remove the eyepiece from the telescope’s
focuser. If look directly to the secondary mirror
will see a reflection of your eye. The light is
being reflected from the secondary mirror to
the primary and back.
Figure 22 shows the different stages of
collimation.
1- Telescope optics completely out of
collimation. Adjustment is necessary both in
the secondary as in the primary mirror.
2- Secondary mirror is aligned but primary
mirror needs adjustments.
3- Telescope´s optics are aligned and star test
should show concentric rings. The telescope
will perform at its best.
6.1. So how to get to good alignment?
6.1.1. Let’s start with the secondary mirror.
Peeking at the focuser without the eyepiece
and looking at the secondary mirror one can
see the reflected eye. One can also see the
telescope secondary spider vanes (4 vanes
cross shaped) and the primary mirror’s holding
pads (figure 24).
Figure 22. Different stages of collimation.

The secondary mirror can be adjusted by using the 3
screws (figure 25). Releasing it can make the secondary
mirror support to rotate. So make sure you only adjust a
screw at a time to avoid it. The secondary mirror should
always show up as a circle and not an ellipse. Please make
sure this is the case.
As soon as you get the primary mirror and the primary
mirror pads centred (figure 22 –2) you are good to go to
the next step.
6.1.2. The primary mirror needs to be adjusted. Adjusting
the primary mirror will move the secondary mirror
reflection to the centre. Use the 6 screws on the back of
the telescope. Notice that 3 screws are used to adjust the
tilt of the primary mirror while the three others are used
to hold the tilt position. Adjust the primary mirror so that
you get all reflections centred (figure 22 –3). Your
telescope is now collimated. Check the diffraction rings
(figure 23) and repeat it necessary.
ATTENTION! Never look at the Sun through a telescope. Concentrated
Sun light may cause serious eye injury. Children should use only with
adult supervision!
Figure 24. Vanes and primary pads.
Figure 25. Secondary mirror adjustment screws.
Figure 26. Primary mirror adjustment screws.
Figure 23. Diffraction Rings: 1. good
alignment and 2. Poorly aligned

7. What can been seen with this telescope?
Below you will find some examples of what you can expect to see when using this telescope.
7.1. The Moon is one of the most spectular objects
to be seen through a telescope. Even a small
telescope will reveal high detail of the Moon’s
surface. You will be able to see the craters on the
Moon’s surface and other features like the Marea.
The moon is a very bright object. It is better to
observe it when the Moon is not full. Try the
crescent Moon and look for features along the
terminator (between illuminated and dark surfaces).
7.2. Jupiter is the biggest planet of our solar system.
It is also one of the favorite targets for beginners.
Galileo was able to discover that the four tiny dots
that turn around the planet were in fact part of
Jupiters system of moons. With this telescope you
will not only be able to see Jupiter’s planet disc with
its two major discernible bands, but also its biggest
moons, Io, Europa, Ganymedes and Callisto.
7.3. The “lord of the rings” of the night skies, Saturn
is by far the most popular target for small
telescopes. Saturn’s rings are discernible even at
60x magnification. In a very good night you will be
able to see the Cassini’s division (the darker band
on the Saturn’s rings).

8. Using the accessories, a bit of math
to understand how all it works.
Using the accessories is easy and fun. To
change magnification simply swap
eyepieces. To get more magnification
simply use the barlow lens. But how does
all of this work?
8.1. Power (magnification)
Your telescope has a focal length of
900mm. This is approximately the distance
between the telescope lens and its focal
point (very similar to the distance between
the focus point of a loupe and the loupe
lens). This is a very important feature, that
allows to determine several interesting
facts such as magnification.
The magnification is determined by the
telescope’s focal length and the used
eyepiece. You probably noticed that the
two supplied eyepieces are K25mm and
K10mm. This means that the K25mm is a
25mm focal length eyepiece while the
K10mm is a 10mm focal length eyepiece.
To determine the magnification just divide
the telescope’s focal length by the
eyepiece’s focal length. Let’s give an
example for our telescope and the supplied
eyepieces:
Telescope’s focal length is 900mm.
K25mm eyepiece’s focal length is 25mm.
900𝑚𝑚
25𝑚𝑚 =36 𝑝𝑜𝑤𝑒𝑟
This means that the K25mm eyepiece
provides a 36x power (magnification). This
seems low, but when you try it, you will
see a bright image with some (very good)
details.
8.2. Barlow Lens
The barlow lens is a very interesting device.
It is a negative lens, that multiplies the
telescope’s focal length. So a 2x Barlow
multiplies the original focal length by 2x, in
this case 900𝑚𝑚 𝑥 2 = 1800𝑚𝑚.
A 3x Barlow lens multiplies by 3x.
Your telescope is supplied with a 2x Barlow
lens. When used with the H20mm eyepiece
you get 2x the power obtained before
36 𝑝𝑜𝑤𝑒𝑟 𝑋 2𝑥 𝐵𝑎𝑟𝑙𝑜𝑤 = 72 𝑝𝑜𝑤𝑒𝑟
8.3. Erecting lens (not included)
The erecting lens gets you an upright image
view with the telescope. It also adds some
power like the barlow lens. The Erecting
Lens provides an extra 1.5x power.
Some possible accessory combinations
Terrestrial
View
Moon
Deep Sky
Jupiter and
Saturn
Barlow Lens 2x
Yes
K25mm Eyepiece
Yes
K10mm Eyepiece
Yes
Yes
Power
Does not apply
90x
36x
180x