Helios 9877 User manual

Astronomical
Telescope
User Guide
OPTICAL VISION LIMITED
www.opticalvision.co.uk
®
WARNING!!
Never point the telescope directly at or near the Sun at any time.
Observing the Sun, even for a fraction of a second, will result in
instant and ir reversible eye damage. Please ensure minors ar e
supervised by an adult conversant with this real danger when
using telescopes or binoculars.

Of all the many and varied telescopes
available for use by amateur
astronomers and nature watchers, all
can be categorised into three types: the
refractor, the reflector & the catadioptric.
Each have their relative strengths and weak-
nesses, but they all have a common function:
to gather and focus light from distant objects
to produce a bright image that may be magni-
fied. In this respect it is the aperture (i.e. the
diameter of the main mirror or lens) of the
telescope that performs a critical function.
With larger apertures, more light is gathered
so fainter objects may be perceived and the
resolving power (i.e. the ability to see fine
detail) is increased.
When comparing telescopes of similar type
but of differing apertures, an instrument that
has a main lens or mirror twice the size of
another gathers four times as much light, not
twice. We are comparing the collecting areas
of the larger and smaller telescopes, which is
proportional to the squares of the apertures.
So, for example, a 120mm telescope gathers
2.25 times (225%) as much light as an instru-
ment of 80mm aperture (120/80 = 1.5, 1.5
squared = 2.25).
When it comes to seeing fine detail in an
image, we are simply comparing apertures:
a 120mm telescope will enable you to
perceive lunar craters, for example, half the
size of those visible in a 60mm instrument.
No amount of magnification applied to the
smaller telescope will show you that which
will be visible in the larger instrument, though
both images may appear equally sharp. The
larger telescope merely forms its images out
of smaller 'dots'.
However, the resolving power (as it is cor-
rectly termed) of even the smallest telescope
is awesome: a 60mm telescope is capable of
resolving detail as small as a £1 coin at a dis-
tance of 2.35 km - nearly 1.5 miles!
< The refractor:
This is the type of
instrument that the lay-
man thinks of when
conjuring up a mental
picture of a telescope.
At the end of the tube
furthest away from the
observer there is an
objectivelens (orrather
two glass elements
sandwiched together
for reasons to be ex-
plained in a moment)
that gathers light from
the objectunderscrutiny,
to form an image at the
other end which is
viewed by means of an
eyepiece.
The objective lens can-
not be made of a single
piece of glass since
such an element is
incapable of bringing
light of differing wave-
lengths to a common
focus, introducing a
prismatic effect that
causes bright objects
to be surrounded by
false rainbow colours.
This undesirable quality
of refractors is virtually
eliminated by making
the objective out of two
glass elements with
optical characteristics
that effectively 'cancel
out' the false colour.
2
Types of Telescope...

Consequently, an objective lens is a piece of
optical equipment that is difficult to manufac-
ture and explains why refractors are the most
expensive form of telescope, aperture for
aperture. However, a refractor can deliver
exquisite images that are very well corrected
and extremly high in contrast, suitable for
observing fine lunar and planetary detail, or
for separating difficult double stars.
^ The catadioptric:
The goal of the telescope designer is to pro-
duce an optical system that delivers an image
as free from any aberrations (defects) as
possible in a package that is compact and
manageable. This has led to designs incorpo-
rating both reflecting and refracting elements
to produce an instrument that combines the
best attributes of both systems.
Thus, we now see many commercial tele-
scopes similar to the Maksutov-Cassegrain
system illustrated above that packs a long
focal length into a physically short tube, while
preserving the high-contrast imagery associ-
ated with refractors of the same aperture.
Catadioptric variations of the Newtonian tele-
scope are currently very much in vogue,
offering compact tube assemblies with conve-
nient viewing positions. Since these systems
often have optical windows sealing the end of
the tube (which would otherwise be open in a
conventional Newtonian), the internal optical
components are far better protected from the
elements and dust.
Remember that no particular design of tele-
scope is intrinsically better than another
– each is well suited to a wide variety of
observational subjects. The important consid-
eration is that the optics should be accurately
manufactured and be precisely collimated
(aligned).
3
Refractors are well suit-
ed for people on the
move since it is
extremely difficult for
the optical components
to come out of align-
ment. Also, the lenses
will not need to be
recoated in a lifetime's
use and maintenance is
minimal.
< The reflector: This
is the cheapest form of
telescope, aperture for
aperture, that money
can buy. In the form
most encountered, the
Newtonian (after Isaac
Newton's design in
1668) uses a concave
mirror at the base of the
tube to gather
and focus the
light from the
object under
scrutiny. The
light is intercepted
before coming to a
focus near the mouth of
the tube by a small, flat
mirror inclined at 45° to
the optical axis which
relays the image out of
a hole in the side of the tube to a waiting
eyepiece that magnifies the image in the nor-
mal fashion. Since the light is not refracted in
any way, and a mirror reflects light of all
colours equally, there is no false colour from
a reflecting telescope.

Of all the many and varied telescopes
available for use by the amateur
astronomers, the mountings that sup-
port them fall into two types - the alt-azimuth
and the equatorial. The 'Using your telescope'
section of this booklet that follows will tell you
more about these terms and the actual use of
your instrument, so we will concentrate on
the actual initial assembly and adjustments of
your telescope here.
The initial assembly of your telescope is best
undertaken in daylight with plenty of room to
lay outthe components and to familiarise with
the accompanying images to see how the
assembled instrument should look.
The three legs should be attachedto the tripod
head one by one by the three bolts and wing
nuts provided. They should not be overtight-
ened, but just made finger tight. Pay particular
attention to the orientation of each leg prior to
assembly such that the tripod tray bracket is
facing inward. The tripod may now be placed
on the ground with the legs splayed enough
for the accessory tray to be attached. Adjust
the height of each leg so that the tripod head
is initially kept low for maximum rigidity,
taking note that the thumb screws holding the
legs in place are securely tightened prior to
the next stage.
Next, attach the alt-azimuth/equatorial mount
(depending on your particular model: see the
ALT-AZ or EQ label with the accompanying
photographs) to the tripod head, followed by
the accessory tray between the tripod legs if
you haven't already done so.
If your telescope mount is fitted with flexible
slow motion controls (e.g. AZ-3, EQ-1, EQ2
and EQ3-2) these may now be attached to the
two small chrome shafts on the mounting via
the thumb screws on the ends of the cables,
taking care to locate the screw in the
machined 'notch' on each shaft.
4
Telescopes & Mounts...
ALT-AZ
EQ-5
ALT-AZ

Balancing the Telescope: To eliminate
stresses on the EQ equatorial mounts and to
ensure smooth, judder-free motion of the
telescope the instrument needs to be
balanced about both the declination and polar
(right ascension) axis. This is especially im-
portant if you propose to use a motor drive
for astrophotography at a future date.
(i) Locate the right ascension clamp and
loosen it whilst holding the telescope tube.
Turn the telescope about this axis until the
counterweight bar isapproximately horizontal.
GENTLY release your grip on the tube and
note if the counterweight has a tendency to
fall or rise: if it RISES, unlock the counter-
weight locking screw and slide it away from
the telescope; if it FALLS , slowly slide the
counterweight towards the telescope side of
the mount. Repeat this process until the
counterweight bar remains in one place with-
out support and clamp the counterweight
screw firmly - the telescope is now balanced
about the polar (right ascension) axis.
(ii) With the counterweight bar horizontal,
ensure that the right ascension clamp is
locked and unlock the declination clamp and
turn the telescope tube so that it is also hori-
zontal. As before, GENTLY release your grip
on the tube and note is there is a tendency for
one end to rise in the air.If so, slowly loosen
the clamps holding the tube and slowly slide
the tube towards the end that rises. Lock the
tube clamp rings once more and see if the
telescope remains horizontal when so posi-
tioned. Repeatthis process untilthe telescope
remains wherever you place it.
The telescope is now balanced about both the
declination and polar (right ascension) axes,
In due course you will add various acces-
sories to the telescope that will slightly alter
the balance position particularly if it is a cam-
era for astrophotography) in which case you
will have to go through processes (i) and (ii)
again, but for now you may care to mark the
balance points on the counterweight bar and
the telescope tube with small pieces of tape
for fast assembly in future.
5
AZ-3
EQ-2
EQ3-2
EQ-1

Attaching the finderscope:
An essential prerequisite for the easy location
of objects on both land and in the sky is the
correct location and alignment of the finder-
scope that attaches to the tube of the tele-
scope. It is, in fact, a smaller version of the
main telescope that is designed to have a low
magnification and a wide field of view so that
the desired target may be easily located. The
eyepiece of the finder scope is equipped with
cross-hairs much like a gun sight marking the
centre of the field of view.
Aligning the finderscope:
(i) Setup the telescope on its mount outdoors
in the day time and ensure that it is balanced
as previously described. You may wish to
extend the tripod legs and securely lock them
again once you have the telescope at a com-
fortable working height. Enlisting the help of
a friend will aid this process. Select the lowest
magnification eyepiece in the set (this is the
one with the largest number engraved on the
cap: usually 20mm or 25mm) and place it in
the focuser drawtube as previously described.
(ii) Select a distant prominent object such as
the tip of an electricity pylon or the tip of a
church spire, though any distant, well-defined
object will do: the further away the better. In
the case of an equatorial mount loosen the
declination and right ascension clamps, or the
altitude and azimuth locks on the alt-az
mount. Sight along the tube and position it
such that the telescope is pointing towards
the distant landmark.
(iii) This first attempt will call for a little trial
and error since the telescope will not be cor-
rectly focused, so as soon as one sees some-
thing blurred through the eyepiece lock the
declination/right ascension clamps (equatorial
mount )or the altitude and azimuth clamps
(Alt-az mount). Use the slow motion controls
as necessary to centre the object in the field
of view.
(iv) Turn the focuser knobs back or forth until
the image becomes crisp and sharp. Do not
be concerned that the image appears upside
down (reflecting telescope) or reversed in a
left to right plane (refractor with zenith prism)
- this is perfectly natural for an astronomical
telescope since there is no 'up' or 'down' in
the sky and you will soon get used to it. With
the image correctly focused you may wish to
use the slow motion controls to perfect the
alignment on the distant target.
(v) Now we can proceed to the Finder. You
will note that the image it offers is upside
down for the same reasons as that of the
main telescope. Depending on the design of
the telescope that you possess, the Finder will
be attached to the main telescope by a brack-
et that will have either three or six radially
spacedadjustingscrews:ifyours isofthelatter
type, adjust the front three screws to permit
the tube of the Finder to be held centrally in
the bracket. Once this has been achieved,
check that the target is still central to the field
of view of the main telescope then slowly
adjust the rear three screws of the finder
bracket until the same object is positioned in
the centre of the cross-wires in the finder's
eyepiece. Again it may help to have a friend to
help you with this procedure. Once achieved,
ensure that the lock nuts of the Finder adjust-
ing screws are secure. Now you can loosen
the locks on the polar (/azimuth) and declina-
tion (/altitude) axes and practice locating
objects during the day.
Telescope basics:
Calculating the telescope's magnification
The magnifying power of any given telescope
and eyepiece is given by a simple formula that
requires a knowledge of the instrument's
focal length and that of the eyepiece. As we
have seen, the focal length of an eyepiece is
usually engraved on its cap: 10mm or 25mm,
for example.
6

The focal length of the telescope is usually
given on a label near the eyepiece focuser and
is the distance from the main lens or mirror
to the point at which it forms an image of a
distant object. The magnification of any given
telescope/eyepiece combination is given thus:
Magnification = focal length of telescope
focal length of eyepiece
For example, a telescope with a focal length of
1000mm used in conjunction with a 7.5mm
eyepiece would yield a magnification of 133x
(1000÷7.5 and rounded to the nearest whole
number), whereas the same instrument used
with a 20mm eyepiece would deliver 50x. It
follows that the larger the focal length of the
eyepiece, the lower the magnification it will
deliver with any given telescope.
Why do we need to use eyepieces of differing
magnification? Apart from making the image
of the subject larger or smaller, magnification
has a bearing on the area of sky (termed the
field of view) that is visible: Higher magnifica-
tions have smaller fields of view, which can
make finding objects that much more difficult
(especially if your Finder is not correctly
aligned) - another reason for spending some
time in daylight perfecting the process as out-
lined above.
The field of view in degrees may also be
obtained by another simple formula which is
valid for most types of eyepieces commonly
found in amateur hands, thus:
Field of view (degrees) = 42
magnification
Again, for example, a telescope with a focal
length of 1000mm using a 15mm eyepiece
will deliver a magnification of 67x which,
using the formula above, will give a field of
view of 0.63 degrees.To give you some idea
of scale, the Full Moon is almost exactly 0.5
degrees in diameter, so our telescope/eyepiece
example would enable us to display the whole
of the Moon's disc within the eyepiece's field
of view.
Howmany eyepiecesshouldyou have? Three
is ideal - one low, one medium and one high
magnification - though two will suffice at a
pinch. A low magnification of 30-50x is
advisable for observing star clusters, galaxies
and nebulae since they are often spread over
a wide area of sky. Medium magnifications of
80-100x are convenient for studying the
craters and valleys of the Moon's surface,
seeing the rings of Saturn or Jupiter and its
four principal moons. Higher powers of 150-
200x will permit you to scrutinise mountain
peaks and fine lunar detail, the surface features
of Mars or to separate close double stars.
You can buy other eyepieces to increase the
versatility of your telescope, or you may care
to purchase something known as a Barlow
lens that is inserted into the focusing tube
before the eyepiece which doubles the magni-
fication - a good way of getting double the
performance out of each eyepiece!
As you get more proficient at observing you
will come to appreciate that merely adding
more magnification is useless unless the
atmospheric conditions are steady enough to
permit their use. On many nights the air may
appear steady to the naked eye, but in the
telescope the image of a bright planet such as
Jupiter or Saturn will appear to shimmer, or
the edge of the Moon may appear to ripple;
these are the nights of so-called 'poor seeing'.
Even on a night of steady air a good general
rule to employ is that you will be approaching
the practical limits of your instrument on
most nights when the magnification exceeds
twice the aperture of your telescope in
millimetres: this means that the maximum
working power of an 80mm aperture instru-
ment will be in the region of 160x, or 300x for
a 150mm telescope.
7

Depending on the type of telescope
mount that you possess, there are two
ways in which you can move the instru-
ment in order to locate and track objects in
the sky. I stress ‘track’ here since, unlike
viewing stationary terrestrial objects, the rota-
tion of the Earth on it’s axis once in 24 hours
from west to east causes the sky to make one
revolution about the celestial poles in the
same period (incidentally, if you have not yet
familiarised yourself with the ‘Get to know the
sky’ section of this booklet, now might be a
good time to familiarise yourself with some of
the concepts contained within it).
The Alt-azimuth mount: this is the the sim-
plest type of telescope mounting to under-
stand and, in some senses, to use. There are
variations that I’ll discuss in a moment, but all
share the common characteristic that there
are two axes about which the telescope can
be moved which are perpendicular to one
another (see Fig.1, page 10). The first axis
permits the telescope tube to be moved from
horizontal to vertical and is known as the ‘alti-
tude’ axis. the second allows the instrument
to be moved in an arc parallel to the horizon
through a complete 360° circuit of the com-
pass; this is the ‘azimuth’ axis. So, a mount-
ing permitting motion about both such axes is
called an ‘alt-azimuth’.
In its most basic form (as provided with the
Astrolux, Lunar-Cadet 1, Mercury-607 &
Mercury-707) there is usually a ‘slow-motion’
control in the form of a threaded rod that is
operated by a thumbwheel permitting precise
control of the telescope’s tube in altitude. On
more sophisticated mounts (such as provided
with the Capricorn 70-2 and the Evostar 90-3)
there is provision for slow motion controls in
both altitude and azimuth — this makes for
much finer control when tracking celestial
objects at high power.
Alt-azimuth conventions: As has been dis-
cussed elsewhere, looking up at the night sky
gives the impression that the observer is at
the centre of a vast hemisphere — the so-
called ‘Celestial Sphere’. The stars, Moon and
planets all appear to lie on the inside surface
of this hemisphere an infinite distance from
the observer. This is, of course, an illusion
since the Moon and stars are in reality at
greatly differing distances away from us.
However, the Celestial Sphere concept has its
advantages in that it makes it easy to define
coordinates for objects in the sky and to pre-
dict where a given star or planet will be at any
given time.
Looking at Fig. 1 once more, note that the
portion of the Celestial Sphere shown in the
diagram has been divided up by lines and arcs
in much the same way as the surface of the
Earth has been divided up into latitude and
longitude. By careful observation you will
note that the star Polaris which resides in the
constellation of Ursa Minor (the Little Bear)
always appears stationary above the northern
horizon at an angle very close to that of the
observer’s latitude. This is because Polaris is
very close to the northern celestial pole and
all the other stars appear to circle around it in
a counter-clockwise direction once every 24
hours. Lying close to due north means that
Polaris will always have an Azimuth bearing
close to zero, or 0°. For an observer in the
British Isles its Altitude bearing will lie
between 50˚ and 55°.
8
Using your telescop e...

The further that one moves across the sky
from Polaris, the apparent motion of the stars
becomes more evident and their Altitudes and
Azimuths will be continually changing. Taking
the star labelled ‘AA’ in Fig. 1, at the instant of
the observation its Altitude was 60° and its
Azimuth bearing was also 60°. It can be seen
that Azimuths are measured in degrees from
due north (0°) through east (90°), south
(180°), west (270°) and back to north (360˚
or 0°). Altitudes are measured in degrees over
a maximum range of 90 — objects exactly on
the horizon are at 0° and those overhead are
at 90° (it is possible to have Altitudes of neg-
ative sign, but this means that the object is
below the horizon and therefore invisible).
The continual changing of Altitude and
Azimuth as a celestial body rises in the east,
traverses the sky and sets to the west makes
tracking an object at high magnifications quite
a challenge, but it is surprising how soon one
becomes proficient at doing so. However,
should the observer wish to attempt any form
of time exposure with the telescope to photo-
graph a faint galaxy, for example, then a dif-
ferent type of instrument mounting known as
an Equatorial is required.
The Equatorial mount: the equatorial mount
consists of two axes that lie perpendicular to
one another (as per the Alt-azimuth system),
but one is tilted such that it is aligned parallel
tothe Earth’s axis,whichmeans for observers
in the northern hemisphere one axis will
always point close to Polaris in the northern
sky — not surprisingly, this is termed the
Polar Axis. As depicted in Fig. 2 on page 11,
the Equatorial is the mounting of choice if any
form of astrophotography is envisaged. It
also makes the process of prolonged tracking
so much easier since the telescope can be
motorised about the Polar Axis such as to
automatically follow the Moon, planets and
stars in their diurnal paths across the sky.The
so-called declination axis can remain locked
once the desired object has been located.
Unlike the Alt-azimuth system, the coordi-
nates of objects remain (relatively) fixed and a
slightly different convention has to be used.
Equatorial conventions: the coordinate sys-
tem is based on projections of the Earth’s
gridwork of latitude and longitude projected
onto the Celestial Sphere. Consequently, a
star such as Polaris that lies very close to the
northern celestial pole would be always over-
head for an observer on the North Pole,
whereas a star such as that labelled ‘BA’
which lies 90° away from Polaris will be over-
head at some point for an observer on the
Earth’s equator. This is known as the star’s
Declination and varies from +90° near Polaris
to -90° at the opposite celestial pole. The
other coordinate is termed Right Ascension
and is measured in hours from 0 to 24. Thus,
star BA has a Right Ascension of 2h and a
declination of 0°.
All telescopes in the Helios range designed for
prolonged and serious use are mounted in the
Equatorial fashion, which as has been
described makes for far more convenient
viewing. Motorised tracking is available for
most models which makes for prolonged
exposures for astrophotography or lengthy
observations of the Moon and planets at high
magnifications.
9

10

The Earth's eastward rotation causes
stars to apparently rotate around a point
in the sky which is a projection of the
Earth's axis, called the celestial pole. A star's
path through the sky from an earthbound
observer'sviewpoint is therefore an arc of this
rotation; it rises in the east towards its highest
altitude (on the local meridian - directly south)
and then sets in the west. It does not travel in
a line parallel to the horizon. (Except at the
north pole, from where the celestial pole is at
the zenith!)
Telescopes are generaly provided with one of
two basic designs of mountings. The so called
alt-az allows a telescope to move in altitude
(up/down) and azimuth (left/right). This does
not allow easy tracking of a star's curved path
through the skysince an alt-az has to move in a
seriesof vertical and horizontal steps, which for
the purpose of steady observation, are cumber-
some.
In the Equatorial, the alt-az mounting is in effect
tipped at an angle, provision being made for the
azimuthaxis to be alignedtotheEarth's rotational
axis(towardsthecelestialpole). This allows atele-
scope to follow a star by simply countering the
Earth's rotation in one motion, rather than the
combination of two movements which would be
necessary with an alt-az. A motive force, either
manual or motorised, applied to what we must
nowcall the'polar'axis,isall that isnecessaryto
track astar through the sky.
In order for this action to follow a star without
deviation thepolaraxisoftheequatorialmounting
must bevery accurately aligned on the celestial
pole. The better this is done, the less requirement
there will be for minor adjustments during
observation.
Polar axis alignment
(approximate setting)
Try to carry out polar axis alignment on a level
surface,wherethelocationofthetripod(or pillar)
feet can be permanently recorded to allow the
telescope to be placed in exactly the same
position for subsequent observations. If a
choice of observing location is limited, try to
position the telescope for the best view of the
southern sky as possible.
Adjust the angle on the latitude scale of the
polar axis, shown in figure 1, until this
equates to your latitude (previously deter-
mined from an OS map).
For the sake of ease and safety, it is recom-
mend that the telescope and its counter-
weights be removed from the mounting for
this exercise.
The polar axis itself should then be aligned
north-south, with its upper end facing true
north. (Not magnetic north!) An approximate
heading can be obtained by sighting along the
polar axis so that it points towards Polaris.
With such approximate alignment, the tele-
scope should be able to track objects with
only occasional corrections on the declination
axis.
11
The equatorial mounting...
Setting up and using an
equatorial mount

12
Polar axis alignment
(precise setting)
The following process will allow tracking
without the need for occasional corrections,
and is essential if photography using a
motorised drive is envisioned. If the approx-
imate alignment described above has been
carried out correctly, only very minor adjust-
ments in azimuth (north-south line) and polar
axis elevation are now required. These need
to be carried out via observation of a star
through the telescope.
Polar axis elevation
(altitude) alignment
Choose a bright star in the east and locate in
the eyepiece field. Establish the current axial
motion of the telescope by gently moving the
telescope tube back and forth, (rotating east-
westonthepolaraxisonlyasshowninfigure2a)
so that the star is impelled to move from one
side of the eyepiece field to the other. It will
help if you arrange this line of motion to
bisect the eyepiece field (as in figure 2b).
This procedure can be made easier if a reticle
is placed at the eyepiece focus and aligned to
indicate this motion, rather than having to
remember it in the mind's eye.
The reticle can be a rolled piece of cardboard,
joined by sticky tape, of such a diameter that
it snugly fits into the inner barrel of the eye-
piece. A hair or thread is fastened across one
end of this cardboard tube, approximately
bisecting it (figure 3a). A cross hair reticle
may already be supplied with your instrument
(figure 3b).
Holding the eyepiece up to the light, it should
be possible to insert the reticle until the fila-
ment comes into focus. (Note. The insertion
of a reticle is only possible with certain
eyepiece designs.) The filament, or one of the
cross hairs, can then be aligned (by turning the
eyepiece) to establish the direction of axial
movement as required (as in figure 4).
Declination
Circle
North Celestial Pole
(near Polaris)
Latitude
Polar axis
Polar axis
stars motion
hair or thread
reticle
line
(aligned to
axial motion)
Right
Ascension
Circle
Rotation for
east-west
axial motion
Movement
for altitude
adjustment
Movement for
east-west adjustment
Figure 1
Figure 2 Figure 4
Figure 3
ab

13
Once this line of axial movement has been
established, set the star at the edge of the
field and allow it to drift across via its own
motion. If the star drifts upwards from this
line (figure 5a), then the north end of the
polar axis needs to be raised. If the star drifts
below this line (figure 5b), the north end of
the polar axis needs to be lowered.
This altitude adjustment is shownin figure 1a.
Polar axis (azimuth) alignment
Now observe a star in the south and repeat
the preceding observation exercise. This
time, an upward drift (figure 5a) indicates
that the north end of the polar axis should be
shifted west; if the star drops (figure 5b), the
shift should be east. This azimuth adjustment
is shown in figure 1b.
It may be necessary to alternate a few times
between these two alignment exercises. Once
these adjustments have been completed suc-
cessfully, a star allowed to drift across the field
should run parallel to the line established by
manual axial movement, to point c in figure 5.
(Asshown with the reticles in figure 4.)
It cannot be emphasised enough that the
additional adjustments made should be slight
and as the correct alignment is approached
the tell tale deviations will become harder to
detect.
Having aligned the telescope mount with the
Earth's polar axis it now becomes possible to
use the sky's co-ordinate system to find objects
not visible to the eye orfinderscope.
The setting circles
The sky is plotted in a similar way to the
Earth's longitude and latitude system, except
that the celestial equivalents are called Right
Ascension(R.A.) and Declinationrespectively.
Right Ascension is divided into 24 'hours',
each subdivided into minutes and seconds.
Declination is measured in degrees, com-
mencing with +90° at the north celestial pole
(towards which the telescope's polar axis
points, for northern observers) decreasing to
0° at the celestial equator.
Below the celestial equator, declinations are
designated as minus, rising from 0° to -90° at
the south celestial pole.
Calibrating the declination circle.
In order to use the equatorial mount's
declination scale effectively, the declination
circle needs to be fixed so that pointer indi-
cates +90° when the telescope is aimed at
the celestial pole.
Use the telescope at its highest power to
observe a star whose declination is known.
(All good star atlases should have this
information available. In lieu of such a
source, a list of bright stars easily found in
a star map appears in the appendix.)
Keeping the star in the centre of the eyepiece
field, loosen the locking mechanism of the
declination circle. Turn the declination circle
until the star's correct declination is indexed
by the pointer and lock the circle. There
should be no need to repeat this exercise - so
long as polar axis alignment is maintained.
axial motion line
Figure 5
a
c
b

14
Using the setting circles
(The following applies to telescopes using a
single index on the R.A. circle)
The easiest way to use setting circles is to off-
set from a known position. Set the telescope
on an object whose position is known (i.e. a
bright star in a recognisable constellation -
such as listed in the appendix). Unclamp and
turn the R.A. circle so that the its pointer
indexes the observed object's positional hour
and minute. E.g. In figure 6 , the R.A. circle
has been set to indicate that the initial object
has a listed position of 5 hours 40 minutes.
(The declination circle should read the
object's declination correctly if the polar axis
alignment has been maintained.) It is now
only necessary to move the telescope in both
axes until the R.A. and Declination pointers
index the new object's position.
E.g. In figure 7, the telescope has been
moved to a new object having an R.A. of 7
hours 30 minutes. If the 'target' is not visible,
delicate 'sweeping' with a low power eyepiece
should bring it into view.
Appendix
Most good star atlases will list the R.A. and Dec. co-ordinates of the principle stars and interesting objects
within each constellation. Below is a list of easily found stars, at least one of which should be visible at
any one time for use as starting points.
Constellation Star Right Ascension Declination
Spring
Bootes Arcturus (αBoötis) 14h 13.4m +19˚ 27'
Virgo Spica (αVirginis) 13h 22.6m - 10˚ 54'
Leo Regulus (αLeonis) 10h 05.7m +12˚ 13'
Summer
Aquila Altair (αAquilae) 19h 48.3m +8˚ 44'
Cygnus Deneb (αCygni) 20h 39.7m +45˚ 06'
Lyra Vega (αLyrae) 18h 35.2m +38˚ 44'
Autumn
Perseus Algenib (αPersei) 3h 20.7m +49˚ 41'
Cassiopea Schedir (αCassiopeiae) 0h 37.7m +56˚ 16'
Pegasus Markab (αPegasi) 23h 02.3m +14˚ 56'
Winter
CanisMajor Sirius (αCanis Majoris) 6h 42.9m -16˚ 39'
Orion Betelguese (αOrionis) 5h 52.5m +7˚ 24'
Auriga Capella (αAurigae) 5h 13.0m +45˚ 57'
Taurus Aldebaren (αTauri) 4h 33.0m +16˚ 25'
Figure 6
Figure 7

15
W
ith the telescope assembled, balanced
andpolar-aligned asdescribedpreviously,
you are ready to begin observations.
Decide on an easy to find object such as the
Moon, if visible, or a bright star to become
accustomed to the functions and operations of
thetelescope. Forthebestresultsduringobserva-
tions,followthesuggestionsgiven as follows:-
●To centre an object in the main telescope,
loosen the telescope's R.A. and DEC locks.
The telescope can now turn freely on its axes.
Use the aligned viewfinder's crosshairs and
re-tighten the R.A. and DEC. locks.
●If you have purchased an assortment of
eyepieces, always start an observation with a
low power eyepiece (e.g. a 20mm or 25mm
eyepiece). Get the objectwellcenteredinthefield
of view and sharply focused. Then try the next
step up in magnification. If the image starts to
becomefuzzyas youincreasemagnification,then
back down to a lower power as the atmospheric
steadinessisnot sufficienttosupporthighpowers
atthe timeyouareobserving.Keepinmind thata
bright, clearly resolved but smaller image will
show far more detail than a dimmer, poorly
resolved larger image. Eyepieces of 20mm and
25mm focal length provide a wide field of view,
ideal for general astronomical observing of star
fields,clustersofstars,nebulaeandgalaxies.They
areprobablythebesteyepiecestouse intheinitial
findingandcentringofany object.
●Once centered, the object can be focused
by turning one of the knobs of the focusing
mechanism.You willnotice thattheastronomical
object in the field of view will begin to slowly
move across the eyepiece field. This motion is
caused by the rotation of the Earth on its axis,
although the planets and stars are for practical
purposes fixed in their positions in the sky. The
platform on which the telescope is sitting (the
Earth) rotates once every 24 hours under these
objects.To keep astronomical objectsin the field
of view of the polar aligned telescope, simply
turnthe R.A. slow motion control. These objects
willappeartomovethroughthefieldmorerapidlyat
higherpowers.
Note: The Declination slow motion control is
only used for centring purposes, not for
tracking.
●Avoid touching the eyepiece while looking
through the telescope. Vibrations resulting
from such contact will cause the image to
move.
●You should allow a few minutes for your
eyes to become dark adapted before attempting
any serious astronomical observations. Use a
red filtered flashlight to protect your night
vision when reading star maps or inspecting
the components of the telescope.
●Avoid setting up the telescope inside a
room and observing through an open window
(orworsestill,aclosedwindow).Imagesviewed
in such a manner may appeared blurred or dis-
torted due to a temperature difference between
theinside and the outside air.
Tips on observing with your
telescope...

16
Since the dawn of mankind there have
been independent thinkers who have
sought to understand the nature of the
Universe and our relationship to it. It is per-
haps the city or suburban observer who feels
the call of the cosmos most intensely when he
or she experiences the majesty of the night
sky from a truly rural location for the very first
time. Assuming that you have been overawed
by a similar experience, how do you go about
becoming an astronomer? Perhaps the first
step should be a trip to your local library to
find out where and when your local astro-
nomical society meets. There are over a hun-
dred such groups in the United Kingdom
alone, so there is bound to be a town near you
that has one.
Getting started: When we leave the cosy con-
fines of the living room and enter the realm of
the night we lose many of our everyday
frames of reference when we look up at the
broad expanse of the sky. Familiar visual
clues to judge size and distance are useless
against the starry background where every-
thing is so exceedingly remote as to be an
infinite distance away. In fact, it is convenient
to imagine the stars as being fixed upon the
inside surface of a vast hemisphere, or dome,
of infinite radius centred on your location -
this concept is known as the celestial sphere,
and it must be said that from a pitch-black
location the heavens do, indeed, appear to be
anenormous domeaboveour heads andrest-
ing on the horizon.
Over the years astronomers have convenient-
ly divided up the celestial sphere into grids
much like that of the lines of latitude and lon-
gitude that crisscross a terrestrial globe, such
that all objects in the sky can be given a pre-
cise coordinate for later reference. When you
become more proficient in your observing
you will refer to detailed "road maps" of the
stars that will use these very coordinate sys-
tems, but for now you need not worry about
them. Star charts are of little use to the novice
since many are confusingly covered with
lines, labels which frequently fail to give any
indication as to how large a constellation (or
star group) will appear to the naked eye.
Joining the dots... : If you were good at see-
ing the pictures in those dotty puzzles that we
used to draw around as a child, then you will
have a distinct advantage when it comes to
recognising and remembering constellation
patterns! It is as well to note that the constel-
lation outlines are entirely arbitrary – the
familiar figures of Hercules, Leo and Orion are
but three of the eighty-eight groups known to
astronomers that are largely the result of the
classicists' fertile imaginations. Note, too,
that the stars of any given constellation are
not necessarily associated with one another:
they are in reality at greatly differing distances
from us.
Finding that first constellation: A casual look
at the moonless night sky, particularly from a
rural location, will reveal so many thousands
of stars that the absolute beginner will feel
utterly lost and bewildered. However, the way
to start is to locate a particularly prominent
star pattern and use it as a starting point. For
the winter observer there is no better celestial
marker than the constellation of Orion, which
straddles the celestial equator and is therefore
visible from anywhere on the surface of the
Earth.
Getting a sense of scale: Using a star chart
from a monthly magazine that depicts the sky
to the east in December you will get an
impression of how large Orion appears in
relation to the other constellations that border
it, but just how big will it seem to the unaided
eye? To get a sense of scale it is very conve-
nient to use the outstretched hand at arms
length as a convenient guide. You will discov-
er that the distance from the tip of your little
finger tothatof your thumb will be just sufficient
Get to know the sky...

17
to cover the seven principal stars that delin-
eate the figure of Orion.
If we wish to be a little bolder we can relate
the span of our outstretched hand to actual
angular measure. It so happens that the span
of our hand corresponds to just over 20
degrees (the symbol for degree is°), while the
length of our thumb is about 7°. This latter
figure conveniently matches the field of view
of a low power pair of binoculars of the 7x50
or 8x30 variety (incidentally, all binoculars are
labelled XX x YY, where XX is the magnifica-
tion and YY is the diameter of the from lenses
in millimetres).
The length of a thumb at arms length – 7°–
it's not a great deal, is it? If you have a pair of
binoculars then perhaps now you can appre-
ciate just how small an area of sky is revealed
to you at any one time, and why it can be a
problem finding objects. Contrast this with
the field of view of a typical astronomical tele-
scope which is in the region of half a degree,
or the apparent width of the Full Moon. It may
surprise many of you to discover that the
angular size of the Moon is so small (it can be
covered by the equivalent of your little finger
nail at arms length) – the proverbial man in
the street would probably say that the Moon
is as big as tennis ball or a small plate. If you
don't believe me, try it!
Back to the constellations and naked eye
viewing. Once we are confident that we have
located, say, Orion (hint: the three so-called
'belt stars' at the centre of the pattern are the
real giveaway), then we can use the figure as
a stepping stone to the adjacent constella-
tions. For example, just over a handspan
above the belt of Orion brings you to the
prominentorangestar Aldebaran (pronounced
'Al-deh-bah-ran', which means "follower" in
Arabic)in the constellation ofTaurus,theBull.
With Orion's belt low to the south-east, we
can move one and a halfhand spansto the left
parallel to the horizon to encounter the bright
star Procyon (pronounced 'Pro-sigh-on') in
theconstellationofCanis Minor, theLesserDog.
A further hand span to the upper left brings
you to the celestial twins of Gemini, Castor
and Pollux.
Another very familiar pattern visible through-
out the year is the constellation of Ursa Major,
or the Great Bear. Also known as the 'Plough'
or the 'Big Dipper', the seven stars that com-
prise this easily identified pattern lie low to
the northern horizon in winter months. Like
Orion, the main part of this constellation sub-
tends about the width of an outstretched hand
at arms length. In this fashion you can use the
prominent seasonal star groups as a kind of
framework, then you can fill in the fainter con-
stellations as your knowledge grows – and
rest assured it will.
Broadening your horizons: Assuming that
you feel confidentin identifying the starsvisible
in any particular season, preferably with the
help of members of your local astronomical
society and the star charts of a magazine,
then you may have already been introduced to
the pleasures of binocular or telescopic
astronomy. Having 'served yourapprentiship',
so to speak, you will be in a better position to
appreciate thetrue potentialofanygivenoptical
instrument. As was mentioned earlier, the art
of observing is a skill to be acquired with con-
stant practice, and in some individuals this
faculty has been developed to an extraordi-
nary degree such that they can perceive a
celestial interloper such as a nova or comet at
a glance.
Streetlights and light pollution: If you are
fortunate to live in a rural area that is not
plagued by streetlighting, then your view of
theheavenswillnotbeimpaired.However, for
the observer living in city or suburban areas
the subtle phenomena of the skies are largely
lost – this is why the clear, dark skies of coun-
try areas are such a revelation to many town
dwellers: there is so much to see when the
veil of light pollution has been lifted! So how
can we alleviate the problem? Other than lob-
bying your Local Authority or private compa-
nies responsible, it is possible to invest in

18
special filters that can almost magically
remove the orange cast to the sky created by
sodium streetlights revealing a dark, star-
studded sky beyond. These filters are not
cheap – you can spend £100 quite easily for
two for a pair of binoculars – but to the tele-
scope user they are almost mandatory for any
serious work concerned with hunting for
galaxies and faint nebulae.
For the lunar and planetary observer, howev-
er, it is a very different story. The Moon is
never impaired by the streetlight's glow
(though the delicacy of earthshine on a very
young crescent moon to the west shortly after
sunset may be lost) and the bright planets
such as Venus, Mars, Jupiter and Saturn may
all be comfortably observed even from the
heart of a city. One word of warning, though –
if you have to set your telescope up on tarmac
or concrete, especially after a warm day, the
ground can reradiate absorbed heat after dark
that causes a shimmering effect in the tele-
scope, rather like looking through running
water.
This rippling effect is caused by air currents
circulating in and around the telescope that
distorts the image. Always position a tele-
scope outside for half an hour or so (security
willing, of course) prior to commencing
observing so that optics and conditions can
settle down such that you will get the best
views. Once you have a powerful telescope
you will notice that the air is very unsettled
on some nights, even after standing the tele-
scope out for its cooling-off period. The fault
then lies in the upper atmosphere and you will
have to leave detailed planetary viewing to
another night!
Photography: Sooner of later you will feel the
desire to capture some of the beauty of the
night sky on film to show to friends and rela-
tives. You may be surprised to learn that an
expensive camera and sophisticated drive
system to follow the stars in the diurnal
courses is not necessary in order to get very
attractive pictures of the constellations: all
that you need is a 35mm camera with a manual
(or 'B' setting) setting, a standard 50mm lens,
a fast colour (or B/W, it's up to you) film, tri-
pod and cable release.
The film you will need can be print or trans-
parency (slide), but you need to buy one with
a speed of about ISO 400 (ASA). With a
50mm lens set to its widest aperture of f/1.4
or f/2 and focused at infinity we can capture
stars fainter than those we can see with the
naked eye over an area of sky that encom-
passes two spans of the outstretched hand at
arms length, or about 40 degrees.
Since the camera is more sensitive than the
eye to faint light, we have to very careful to set
our camera and tripod well away from any
direct street or security lighting - standing in
the shade of a fence or wall will usually do the
trick. It is also a good idea to tell members or
your household that you are going out to do
someastrophotography,sothatthebathroom
lightdoesnot come on unexpectedly, flooding
your back garden with light and ruining your
carefully obtained exposure!
One accessory that you will find immensely
useful is a small flashlight fitted with a dim
red bulb or a red filter over the lamp. The pre-
cious dark adaption that you gain through
being in pitch blackness for a period of 15
minutes or more is less affected by red light
than any other, so it is excellent for making
notes or ensuring that you camera has been
correctly set without ruining your night
vision.
Taking the exposures: With your subject suit-
ably framed within the viewfinder (all but the
brighter stars will be difficult to see with the
screen of some SLR cameras) make sure that
the lens of the camera is wide open, the dis-
tance scale set to infinity and the cable release
is firmly screwed in. With the palm of your
hand held covering the lens (but NOT touch-
ing the camera), open the shutter with the
cable release and lock it. Now briskly move
your hand to one side to start the exposure
without jogging the camera - this technique is

19
a simple way to avoid camera shake which
ruins many a time exposure.
So how long should you leave the lens uncov-
ered? Under dark skies with ISO 400 film and
a 50mm f/2.8 lens you can expose for up to
about 20 seconds before the motion of the
stars becomes evident as small trails on the
film. However, if the sky is exceptionally dark
and the camera is pointed toward the north,
especially in the vicinity of the Pole Star,
Polaris, then you may take exposures up to
two minutes or more since the diurnal motion
of the stars are much less pronounced there.
To finish the exposure, place your palm in
front of the lens (again without jogging the
camera) and unlock the cable release.
If you are feeling artistic then it always pays to
have some foreground subject to 'frame' the
stars. A gnarled old Oak tree devoid of leaves
with its 'fingers' stretching to the sky would
make a good silhouette for an atmospheric
picture! A word about processing: with the
advent of the high street 1 hour processing
booth you can get very quick results with
print films that use the C41 process. But do
make sure that the technician knows that your
subject matter is astronomical since it is very
frustrating to return to pick up your hard-
earned snaps only to be told that the roll was
unexposed - they're just not used to seeing
tiny white dots! Just tell them to print all
frames regardless. If you can intersperse the
pictures with everyday terrestrial scenes then
so much the better, since this makes it easier
for them to note the edge of a frame - nothing
is more infuriating than an otherwise perfect
night sky scene negative that has been care-
lessly cut in half.
With practice you will be able to photograph
scenes of great beauty, especially if you have
used colour film to capture the myriad
colours of the stars. You may notice, too, that
you have photographed things that you didn't
notice at the time, like the streak of a meteor
as it burned up in our atmosphere in a flash
of incandescence or the longer trail of an
artificial satellite as passed through the
camera's field of view. Rarer sights such as
moonbows and aurorae may also be captured
by the attentive astrophotographer armed
with no more than their tripod mounted camera.
CLEANING
As with any quality optical instrument, lens or mirror surfaces should be
cleaned as infrequently as possible. Front surface aluminised mirrors, in
particular,shouldonlybecleanedwhenabsolutelynecessary.Inallcasesavoid
touching any mirror surface. A little dust on the surface of a mirror or lens
causes negligible loss of performance and should not be considered reason
to clean the surface. When lens or mirror cleaning does become necessary,
use a soft camel-hair brush or compressed air to gently remove the dust.
If a telescope's dust cover is replaced after each observing session, cleaning
of the optics will seldom be required.

20