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10 Micron Technical and Warranty Support

Please Note

All technical support in respect of 10 Micron Products is provided via the 10 Micron User Support Forum via this link

For warranty repairs please contact the following

1) GM1000 HPS - IanKingImaging
2) GM2000/3000/4000 HPS Baader Planetarium tel
Tel 0049 - 8145-8089-0
or via this link

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10 Micron - An Introduction

HPS Technology

Often, it happens that a potential customer asks: Why should I buy a 10micron HPS mount?
The short answer is: Because it works better, integrates a whole set of features that others
haven’t and will not in the foreseeable future, has absolute encoders on both axes for the best
accuracy, all of this is useful whatever others may say, and it will change forever your way of
thinking about astronomical observation.

If you aren’t satisfied with the short answer, please read on.

What does HPS mean?

HPS means “High Precision and Speed” and is the name for the new series of astronomical
mounts by 10micron. The HPS mounts feature two high-precision absolute encoders mounted
directly on each axis to ensure unprecedented pointing and tracking accuracy, and high
performance servo motors and drivers for high speed pointing. This radical performance
improvement over previous technology enables a radical change in the workflow of observers and
astroimagers.

In the vast majority of applications, including long exposure deep-sky imaging, the need for autoguiding is eliminated. The pointing accuracy allows you to be confident that, once the mount is properly setup, objects will be centered in the smallest field of view, even with a mobile
setup on a remote meadow in the mountains. Furthermore, the internal electronics allows the
mount to do almost everything without the need for an external PC.

The encoder system

The absolute encoders provide high-accuracy, subarcsecond feedback to the motion of the
mount. The absolute encoders render the axes “live” and free to react also to any external forces like wind and vibrations or accidental contact.

Furthermore, this feedback is provided regardless of any zeroing or homing procedure.
This means that the electronics will always know the position of the mount. You may move
around the mount with the clutches unlocked and the electronics powered off, lock the clutches in any position and switch on the mount: the electronics will know where the telescope is looking.
You may effectively use the mount as a Dobsonian telescope with manual pointing, retaining the
full, sub- arcsecond accuracy of the encoders.
This means ease of use when operating in the field, since the setup procedure is much faster.
With regard to the right ascension axis, virtually all the mechanical error from the reduction gearing is eliminated. Not only the so-called “Periodic Error”, which comprises the periodic irregularities due to imperfection in the manufacturing and assembling of the worm, but also the non-periodic errors due to imperfections in the wormwheel, bearings, belts and so on.

With regard to the declination axis, it may seem that the encoder system is less important, since
there is no sidereal tracking motion. The reality is that the declination axis is critical to sidereal tracking. If you want to compensate for refraction, telescope and mount flexure and so on, you will have to move the declination axis at very small speeds. Furthermore, while the right ascension axis works always at the same speed (plus or minus small corrections), the declination axis works always at near-zero speeds, with the occasional inversion of the direction of motion. This means that mechanical backlash, belt flexure and friction forces show in the declination axis, and you can’t
count on any “Periodic Error Correction” to compensate for them.
Tricks for minimizing the effect of these forces in traditional mounts require having very small preload on the worm, with the risk of
uncontrolled motion when the telescope is subjected to even small external forces, because of the disengaging of the worm from the worm wheel; painstakingly calibrating software backlash compensation procedures; manually adjusting the meshing of gears. Or, maybe, introducing forcefully small alignment errors, to force autoguide corrections always in the same direction. So,having an encoder mounted directly on-axis is at least as important in declination as in right ascension.

Tracking objects and mount modelling

The task of tracking astronomical objects can be decomposed into several sub-tasks that we will
discuss in the next paragraphs.

Modelling the orientation of the mount with respect to Earth.

Modelling the orientation of the telescope with respect to the mount.

Modelling the errors of the mechanical system with respect to an “ideal” one.

Modelling the influence of the atmosphere on the path of light rays.

Modelling the orientation of Earth.

Modelling the motion of astronomical objects themselves.
In order to obtain the sub-arcsecond tracking accuracy of HPS mounts, all of this must be taken into consideration. Furthermore, many “subtle” effects begin to show, and they need special attention.

Modelling the orientation of the mount with respect to Earth
An ideal equatorial mount has its right ascension axis pointed directly at the celestial poles. If there are errors with this, the mount will exhibit various pointing and tracking errors, in both axes, varying across the sky. So, with a typical mount that tracks objects by setting a constant velocity on its right
ascension axis, it is of utmost importance to approach this ideal situation. There are many
methods for achieving this, from the universal (but slow) Bigourdan method, to iterative methods exploiting the capabilities of computerized mounts, to the traditional polar scope (which is, anyway, more difficult to align and use correctly than you may think). Many computerized mounts allow you to point to one, two or three stars, with less and less assumptions on the correctness of the initial
alignment, and compute the polar misalignment. This information is then used, at least, for pointing at objects. The HPS mounts can do the same, with the additional usage of this piece of information
for correcting the tracking of objects. This means that tracking objects will always be correct,
even if the mount is not aligned to the celestial pole. Of course, you may want to ensure a
reasonably correct alignment to avoiding field rotation on long sequences of imaging. Various
functions are provided by the 10micron firmware: even the number of turns you must apply to the
adjustment handles for the azimuth and altitude is given. So we eliminated the polar scope, to the advantage of mechanical stiffness of the mount, since the initial alignment can be done with the mount misaligned even by many degrees from the pole, and approximately centering two
bright stars in the eyepiece (using even manual movements, like in a Dobsonian), then centering a third star with the adjustment handles is much quicker than aligning the typical polar finder with date and time, compensating for longitude, and knee yourself to center the right star pattern for your hemisphere in its too-small field of view.
All of the above requires a reasonably accurate knowledge of time and your location on Earth. If
you plan to reuse the alignment later (for example if you are in an observatory), you will have to keep the mount’s clock accurately synchronized and use very precise coordinates for your site. For this reason, beyond the usual data entries from the keypad or with an external PC, 10micron mounts support also reading all these data from an optional GPS module.

Modelling the orientation of the telescope with respect to the mount.
Of course, your telescope’s optical axis will not be perfectly perpendicular to the declination axis,and it will not be perfectly aligned with the zero angle of the absolute encoder. When you add the third star to the alignment procedure, these errors are automatically computed and corrected from
now on.

Modelling the errors of the mechanical system with respect to an “ideal” one.

We know that no mechanics is ideal. Even with high-accuracy encoders mounted directly on the
axes, we still have the issue of mechanical flexure. In the great majority of mounts the mechanical errors are not dealt with at a software level. Of course, mechanical errors can minimized through careful designing and manufacturing. But, for example, if you allow for an error of one arcsecond during the exposure of an image, a little calculation will show that this error can be introduced by a
deformation of a leg of the typical tripod of just 5 thousandths of a millimeter! A deformation like this can be easily caused just by moving around the barycenter of a non-perfectly balanced telescope.

So, the best thing we can do is to build a model that accounts for the mechanical flexure of the
mount and telescope. We will have to point to various locations in the sky, and compare them
against the encoder readout (i.e., the absolute angle set on the mount’s axes). With enough points, flexure can be modeled well enough to allow for high-precision pointing. As far as we know, no mount on the market allows this without the use of an external computer. With 10micron mounts, the procedure can be as simple as adding stars to the ones you already used for the initial alignment. Of course, this can be automated in a very efficient way by using external tools that point to a predefined set of locations in the sky, take a picture, measure the exact coordinates by a process called “plate solving” and feed the coordinates back to the mount. You can use up to 100
alignment stars/points for this task, and everything can be done in a surprisingly little amount of time, thanks to the high pointing speed.
Of course, all of this works if mechanical errors are repeatable. This means that, while mechanical flexure can be usually modeled with excellent accuracy, this doesn’t apply to mechanical play or backlash. The on-axis encoders ensure that no backlash in the mount will ever get in your way while creating a pointing model, tracking or pointing objects, while you have the task of eliminating flopping mirrors, loose focuser tubes and so on.

Modelling the influence of the atmosphere on the path of light rays.

Earth’s atmosphere bends the rays of light from astronomical objects, depending on air density.
This is called “atmospheric refraction”. With traditional mounts, often it is advised to point the right ascension axis to the refracted celestial pole, and set a special tracking speed (the so-called “king” speed) that compensates for the apparent speed difference due to refraction (in right ascension only).
10micron mounts allow for setting of the barometric pressure and atmospheric temperature, and even changing it during an observation session, in order to continuously correct their pointing and tracking to account for atmospheric changes. This can be done manually, with the keypad, or from an external PC

Modelling the orientation of Earth.

As everybody knows, Earth rotates with respect to astronomical objects. By far, its main motion is the daily rotation. So, for being called an “equatorial mount”, often it is enough to provide a constant-rate rotation around the right ascension axis. This rate, usually, is given by a quartz clock, and so it should be reasonably accurate. What many don’t know is that typical quartz oscillators used in electronics (and also in your typical PC) are not temperature compensated.

Why not autoguiding? It seems simpler…

Autoguiding is simpler… for the mount manufacturer. For the user, autoguiding means additional trouble. In case you use an external guider scope, it means that you can’t compensate all flexures between the two instruments, and you have additional, heavy equipment. In case you use a dedicated guider camera, it means additional cabling, software installation and setup. In any case, it means additional trouble searching for suitable guide stars, looking f
software parameters, calibration. HPS mounts can be aligned to bright stars during twilight, then
every second of darkness can be used for imaging. Furthermore, autoguiding is not always
possible. The typical situation is imaging a fa
autoguiding, HPS mounts provide a standard ST4 port, as well as all the usual settings and
controls by remote software.

Pointing objects

The HPS mounts feature a very rich database of objects, comprising not only the classical Messier and NGC/IC catalogues, but many catalogues of stars, including variables and doubles, and of deep-sky objects. Also, a catalogue of moon features is available and useful thanks to the high pointing accuracy.
The high speed of the mount is necessary, beyond speeding up the alignment procedures, for fast
satellites catching (especially after a meridian crossing). Furthermore, it helps to reduce loss of time in research application, increasing the amount of data that can be obtained in the often short observing nights.

Instrument setup

The HPS mounts feature a rich system of accessories for mounting various instruments. Even multiple instruments can be mounted on a single mount, in order to have the right imaging
equipment always ready. Since the pointing and tracking model depends on the specific nstrument
(the flexure is different), the mount allows for different models, one for each instrument, that can be saved in the internal memory and reloaded when required.
Another useful feature, especially for heavier mounts, is the electronic balance function. With this function you may measure the unbalancing of the instrumentation and adjust accordingly. The
high speed is very useful also to speed up this procedure.

Remote operation and connectivity.

The HPS mounts provide a great deal of connecting options. While you may choose the traditional RS-232 connection to control the electronics from an external PC, today you may prefer to dedicate it to controlling directly a computerized dome. The firmware will provide all the relevant computations even for mounts mounted off-center and instruments mounted with offset. The GPS port doubles as an additional RS-232 port, if you don’t use the GPS. But the best way of connecting the mount to your PC is using the LAN connection, via TCP/IP, or the Wireless connection. The mount can connect to an existing WLAN, or it can be used as an hotspot to which your PC, tablet or smartphone can connect.

The LAN connection offer superior high-voltage tolerance with respect to the typical RS-232
connection; this is even better with the WLAN which is… wireless. In case of remote observatories, which are subject to lightning, this may make the difference between a healthy electronics and a fried one!

The mount supports up to ten simultaneous TCP/IP connections, so you can use different software, and also different devices, at the same time. 10micron provides an ASCOM driver for Windows, but if you want to implement your own control system, we provide the command set that can be used both on the RS-232, LAN and WLAN connections. The command set is largely
LX200 compatible, but includes many more functions and operating modes. In remote operation, you will appreciate also the additional security provided by the absolute encoders: in no case you will lose your alignment, even in case of slipping clutches.
The HPS mounts are able to operate up to 30° beyond the meridian, in both directions (this
means, with the counterweight bar up, and the telescope down). This allows at least an arc of 60° for tracking every object, corresponding to at least four hours of tracking for objects crossing the meridian (provided that the object doesn’t set or encounter another limit). This amount is configurable from 0° to 30° to obtain the maximum flexibility. The mount will warn you when it is reaching tracking limits; at the limit, tracking will stop. You will have to point the object again to force a meridian flip.

10 Micron GM1000 HPS High Precision Mounting

The GM1000HPS mount is built for the demanding observer using photographic
instruments up to a weight of 25kg – 55 lbs (counterweights not included).
Movements are driven by two AC servo motors, with timing belt reduction having zerobacklash.
Both axes feature a classic worm – wormwheel pairing. The wormwheels are made of bronze (B14), with a diameter of 125mm and 250 teeth, while the worms are built of alloy steel with a diameter of 20mm. The axes themselves are made of 30mm diameter alloy steel, for the maximum rigidity.
The double dovetail mounting plate guarantees the maximum compatibility with many telescope manufacturers.

The electronics are housed in an independent control box, easily removable. The connections of motors, encoders and hand pad feature secutiry lock screws. The mount can be controlled using the included hand pad, without connecting an external PC. The keypad is built in order to maintain the maximum readability in all lighting conditions. Both the display and the ergonomic keys, allowing for the use of gloves, feature a red backlight. A heater keeps the display warm for usage below freezing temperatures.
The mount can be controlled using the most
common software packages by connecting it to a
PC with the RS-232 serial port or the Ethernet
connection, via the proprietary 10micron ASCOM
driver or the Meade compatible command protocol. Furthermore, a dedicated software (also
included with the mount) can be used to create a
"virtual hand pad" replicating exactly the functions
of the physical hand pad. The RS-232 port can also be used to control an external dome. This
flexibility makes the GM1000HPS an ideal mount
for observatories and remotized observing sites.
The object database contains many star catalogs
and deep-sky objects up to the 16th magnitude.
Solar system objects can be tracked so that their motion is compensated with respect to the stars. You may load orbital elements of comets,
asteroids and artificial satellites into the mount, so that these objects can be tracked directly using the hand pad (without any external PC).
The connections of the control box.
Pointing is made accurate through the
usage of a model containing up to 100 stars,
which allows for the correction of the classical polar alignment and conic errors,and also of the most important flexure terms of the optical tube. In this way it is possible to obtain pointing accuracies of the order of 20 arcseconds RMS. The same model can be used in order to obtain the maximum tracking accuracy, compensating also for the atmospheric refraction (depending on the local atmospheric pressure and
temperature).

A series of auxiliary functions is provided to help the user for quick aligning the mount to
the celestial pole.
You may save and recover the alignment data of different observing sessions. This function
is very useful if you have many instruments in different setups, each one requiring different
flexure corrections.
Tracking through the meridian, a typical problem with german mounts, is solved allowing
for tracking for up to 30° past the meridian (configurable), in both directions. In this way
any object can be tracked for at least four hours.
The tracking accuracy makes autoguiding not necessary for many uses. The absolute
encoders on both axes allows to obtain a typical tracking error below 1 arcsecond. It is
possible to autoguide anyway, using the ST4-compatible port or through the
serial/Ethernet connection, with a guide rate configurable from 0.1x to 1x. The guide rate
can be automatically corrected for the declination of the target, so that there is no need of
recalibrating the autoguide when observing at different declinations.
Designed for field use, the GM1000HPS is easily transportable. The main body of the mount, without the counterweight shaft, has a weight of only 19.5 kg – 43 lbs.

Other functions of the mount are designed in order to obtain the maximum flexibility in
the most usage conditions.
The mount can be switched on and off using the dedicated connector on the control box
panel.
You can use the electronic balance functions in order to balance your instrument without
unlocking the clutches.
The mount can be parked in different user-defined positions.
An external dome can be controlled directly using the RS-232 serial port, avoiding the
need of using a dedicated external PC. Once configured with your instrument parameters,
the firmware is able to make all the calculations required for positioning the dome slit in front of your optical tube, for almost all instrument configurations.

Technical Specs:

TECHNICAL DATA SHEET
Type German Equatorial Mount
Weight (mount) 19.5 kg – 43 lbs without accessories
Instrument payload capacity ~ 25 kg – 55 lbs
Latitude range 0° – 82° (90° optional)
Azimuth fine adjustment range +/− 7.5°
Counterweight shaft 30 mm diameter, stainless steel, weight 1.7 kg – 3.7 lbs
Axes 30 mm diameter, alloy steel
Bearings Pre-loaded tapered roller bearings
Roller thrust bearings
Worm wheels 250 teeth, 125 mm diameter, B14 bronze
Worms diameter 20mm, alloy steel, grinded and lapped
Transmission system Backlash-free system with timing belt and automatic
backlash recovery
Motors 2 axes AC servo brushless
Power supply 24 V DC
Power consumption
~ 0,5 A while tracking
~ 3 A at maximum speed
~ 4 A peak
Go-to speed Adjustable from 2°/s to 15°/s
Pointing accuracy < 20” with internal multiple-stars software mapping
Average tracking accuracy
< +/− 1" typical for 15 minutes (< 0.7" RMS)
with multiple-stars software mapping and compensation
of flexure and polar alignment errors
Security stop +/− 30° past meridian in r.a. (software)
+/− 45° past meridian in r.a. (mechanical)
Communication ports RS–232 port; GPS port; autoguide ST-4 protocol port;
Ethernet port
Database
Stars: by name, Bayer designation, Flamsteed designation,
Bright Star Catalogue, SAO, HIP, HD, PPM, ADS, GCVS.
Deep-sky: M, NGC, IC, PGC ,UGC limited up to mV = 16.
Solar system: Sun, Moon, planets, asteroids, comets,
artificial satellites. Equatorial and altazimuth coordinates.
User defined objects, fast slewing positions.
Firmware features
User defined mount parking position, 2-stars and 3-stars
alignment function, up to 100 alignment stars for
modeling, correction of polar alignment and orthogonality
errors, estimate of average pointing error, storage of
multiple pointing models, sidereal, solar and lunar tracking
speed adjustable on both axes, declination-based
autoguide speed correction, adjustable horizon height
limit, pointing and tracking past meridian,, assisted
balance adjustment, manual or GPS based time and
coordinates setting, dome control via RS-232, configurable
atmospheric refraction, network settings, comets and
asteroids filter, multi-language interface. Remote Assist via
Internet connection.
PC control
Remote control via RS-232 or Ethernet; proprietary
ASCOM driver or Meade compatible protocol; update of
firmware and orbital elements of comets, asteroids and
artificial satellites via RS-232 or Ethernet; virtual control
panel via RS-232 or Ethernet. Optional Wi-Fi.

£1,715.00

10 Micron Upgrade-Package "Economy" for GM 1000 HPS

consisting of the following accessories:

1452072/1452073 Counterweight set of 3kg and 6kg, stainless steel

2451010 Black Baader Aluminium T-Pod 110mm

1451062 Hardcase-Set from TTX01® (2 pcs),

1451070 Power-Supply outdoor type 230V / 24V- 4A - 90W

1455010 PERSEUS Software Package

£2,495.00

10 Micron Upgrade-Package "Professional" for GM 1000 HPS

consisting of the following accessories:

• 1452072/1452073 Counterweight set of 3kg and 6kg, stainless steel

• ARIES Aluminium Tripod (complete with upholstered Cordura transport-bag)

1451062 Hardcase-Set from TTX01® (2 pcs),

• 1451070 Power-Supply outdoor type 230V / 24V- 4A - 90W

1455010 PERSEUS Software Package

10 Micron GM 2000 HPS Mounting

The GM2000HPS mount, now in the new M2 version, is built for the demanding observer
using photographic instruments up to a weight of 60kg – 130 lbs (counterweights not
included).
Movements are driven by two AC servo motors, with timing belt reduction having zerobacklash.
Both axes feature a classic worm – wormwheel pairing. The wormwheels are made of bronze (B14), with a diameter of 172mm and 215 teeth, while the worms are made of alloy steel with a diameter of 24mm. The axes themselves are made of 50mm diameter alloy steel, for the maximum rigidity.

The electronics are housed in an independent control box, easily removable. The connections of the mount and keypad feature secutiry lock screws.
The mount can be controlled using the included
keypad, without connecting an external PC. The
keypad is built in order to maintain the maximum
readability in all lighting conditions. Both the display and the ergonomic keys, allowing for the use of gloves, feature a red backlight. An heater keeps the display warm for usage below freezing temperatures.
The mount can be controlled using the most common software packages by connecting it to a PC with the RS-232 serial port or the Ethernet connection, via the 10micron ASCOM driver or the Meade compatible command protocol. Furthermore, a dedicated software (also included with the mount) can be used to create a "virtual keypad" replicating exactly the functions of the physical keypad. The RS-232 port can also be used to control an external dome. This flexibility makes the GM2000HPS an ideal mount for observatories and remotized observing sites.
The object database contains many star catalogs and deep-sky objects up to the 16th magnitude. Solar system objects can be tracked so that their motion is compensated with respect to the stars. You may load orbital elements of comets, asteroids and artificial satellites into the mount, so that these objects can be tracked directly using the keypad (without any external PC).
Pointing is made accurate through the usage of a model containing up to 100 stars, which
allows for the correction of the classical polar alignment and conic errors, and also of the most important flexure terms of the optical tube. In this way it is possible to obtain pointing accuracies of the order of 20 arcseconds
RMS. The same model can be used in order to
obtain the maximum tracking accuracy,
compensating also for the atmospheric refraction
(depending on the local atmospheric pressure and
temperature). A series of auxiliary functions is
provided to help the user for quick aligning the
mount to the celestial pole. You may also save and recover the alignment data of different observing sessions. This function is very useful if you have many instruments in different setups, each one requiring different flexure corrections.
Tracking through the meridian, a typical problem
with german mounts, is solved allowing for tracking for up to 30° past the meridian
(configurable), in both directions. In this way any object can be tracked for at least four
hours.

The tracking accuracy makes autoguiding
not necessary for many uses. The absolute encoders on both axes allows to obtain a
typical tracking error below 1 arcsecond. It
is possible to autoguide anyway, using the ST4-compatible port or through the serial/Ethernet connection, with a guide rate configurable from 0.1x to 1x. The guide rate can be automatically corrected for the declination of the target, so that there is no need of recalibrating the autoguide when different declinations.
Among the other functions, you will find the
electronically-assisted balance and the ability of parking the mount in different user-defined positions.
Designed for field use, the ultraportable version is easily divided into two parts. All
electrical connections are made automatically when assembling the mount. The biggest
piece has a weight of only 15 kg – 33 lbs, and in combination with the Centaurus II (21 kg –
46 lbs) you obtain a winning combination for the mobile observer.

Technical Specs:

TECHNICAL DATA SHEET
Type German Equatorial Mount
Weight (mount) 30 kg – 66 lbs without accessories
Weight, Ultraportable version (mount) 15 kg – 33 lbs + 15 kg – 33 lbs without accessories
Instrument payload capacity 60 kg – 132 lbs
Latitude range 20° – 70°
Azimuth fine adjustment range +/− 10°
Counterweight shaft 40 mm diameter, stainless steel, weight 4 kg – 9 lbs
Axes 50 mm diameter, alloy steel
Bearings Pre-loaded tapered roller bearing
Worm wheels 215 teeth, 172 mm diameter, B14 bronze
Worms diameter 24mm, tempered alloy steel, grinded and lapped
Transmission system Backlash-free system with timing belt and automatic
backlash recovery
Motors 2 axes AC servo brushless
Power supply 24 V DC
Power consumption
~ 0,7 A while tracking
~ 3 A at maximum speed
~ 5 A peak
Go-to speed Adjustable from 2°/s to 20°/s
Pointing accuracy < 20” with internal multiple-stars software mapping
Average tracking accuracy
< +/− 1" typical for 15 minutes (< 0.7" RMS)
with internal multiple-stars software mapping and
compensation of flexure and polar alignment errors
Security stop +/− 30° past meridian in r.a. (software)
+/− 45° past meridian in r.a. (mechanical)
Communication ports RS–232 port; GPS port; autoguide ST-4 protocol port;
Ethernet port
Database
Stars: by name, Bayer designation, Flamsteed designation,
Bright Star Catalogue, SAO, HIP, HD, PPM, ADS, GCVS.
Deep-sky: M, NGC, IC, PGC ,UGC limited up to mV = 16.
Solar system: Sun, Moon, planets, asteroids, comets,
artificial satellites. Equatorial and altazimuth coordinates.
User defined objects, fast slewing positions.
Firmware features
User defined mount parking position, 2-stars and 3-stars
alignment function, up to 100 alignment stars for
modeling, correction of polar alignment and orthogonality
errors, estimate of average pointing error, storage of
multiple pointing models, sidereal, solar and lunar tracking
speed adjustable on both axes, declination-based
autoguide speed correction, adjustable horizon height
limit, pointing and tracking past meridian,, assisted
balance adjustment, manual or GPS based time and
coordinates setting, dome control via RS-232, configurable
atmospheric refraction, network settings, comets and
asteroids filter, multi-language interface. Remote Assist via
Internet connection.
PC control
Remote control via RS-232 or Ethernet; proprietary
ASCOM driver or Meade compatible protocol; update of
firmware and orbital elements of comets, asteroids and
artificial satellites via RS-232 or Ethernet; virtual control
panel via RS-232 or Ethernet. Optional Wi-Fi.

£4,050.00

10 Micron Upgrade-Package "Professional" for GM 2000 (QCI/HPS) „Monolith“

consisting of the following accessories:

1452075/1452080 Counterweight set of 6kg and 12kg - stainless steel

1452085 Losmandy-compatible dovetail plate

1452057 Centaurus II Tripod, complete with upholstered Cordura transport-bag

1452062 Head- and Counterweight-Flight-Case, set for MONOLITH - QCI (2 pc)

1455010 PERSEUS Software Package

1452070 Power-Supply outdoor type 230V / 27V- 6A 150W

10 Micron GM3000 HPS

Evolving perfection.
The GM3000HPS mount is built for observatories with an instrumentation up to a weight of 100 kg – 220 lbs (excluding counterweights). It is ideal for remotized observation sites, and its loading capacity allows for mounting instruments like 200 mm diameter refractors,300 mm diameter Newton reflectors, 450 mm diameter Cassegrains and so on.

Movements are driven by two AC servo motors, with timing belt reduction having zerobacklash.
Both axes feature a classic worm – wormwheel pairing. The wormwheels are made of bronze (B14), with a diameter of 244 mm and 315 teeth in right ascension, and a diameter of 192 mm and 250 teeth in declination. The worms are made of alloy tempered steel with a diameter of 32 mm and 24 mm respectively. The axes themselves are made of alloy steel, with a diameter of 80 mm (right ascension) and 60 mm (declination), for the maximum rigidity.

The electronics is housed in an independent control box, easily removable. The
connections of the mount and keypad secutiry lock screws. Only one cable runs from the
control box to the mount. The axes feature an hole allowing for the passage of instrumentation cables. This effectively solves the problem of entangling cables and damaging instruments, especially for remote observatories.

The mount is powered with low voltage, requiring
a maximum power of about 100W. This makes
possible using the mount even in locations with
limited power available.
The GM3000HPS can be controlled completely
using the included keypad, without requiring any
external PC. The keypad is built in order to maintain the maximum readability in all lighting conditions. Both the display and the ergonomic keys, allowing for the use of gloves, feature a red backlight. An heater keeps the display warm for usage below freezing temperatures.
The mount can be controlled using the most common software packages by connecting it
to a PC with the RS-232 serial port or the Ethernet connection, via the 10micron ASCOM
driver or the Meade compatible command protocol. Furthermore, a dedicated software (also included with the mount) can be used to create a "virtual keypad" replicating exactly the functions of the physical keypad. The RS-232 port can also be used to control an external dome. This flexibility makes the GM3000HPS an ideal mount for observatories and remotized observing sites.
The object database contains many star catalogs and deep-sky objects up to the 16th magnitude. Solar system objects can be tracked so that their motion is compensated with respect to the stars. You may load orbital elements of comets, asteroids and artificial satellites into the mount, so that these objects can be tracked directly.

Pointing is made accurate through the usage
of a model containing up to 100 stars, which
allows for the correction of the classical polar
alignment and conic errors, and also of the
most important flexure terms of the optical
tube. In this way it is possible to obtain
pointing accuracies of the order of 15
arcseconds RMS. The same model can be used
in order to obtain the maximum tracking
accuracy, compensating also for the
atmospheric refraction (depending on the
local atmospheric pressure and temperature).
A series of auxiliary functions is provided to
help the user for quick aligning the mount to
the celestial pole. You may also save and
recover the alignment data of different
observing sessions. This function is very useful
if you have many instruments in different
setups, each one requiring different flexure
corrections.
Tracking through the meridian, a typical
problem with german mounts, is solved
allowing for tracking for up to 30° past the
meridian (configurable), in both directions. In
this way any object can be tracked for at least
four hours.
The tracking accuracy makes autoguiding not necessary for many uses. The absolute
encoders on both axes allows to obtain a typical tracking error below 1 arcsecond. It is
possible to autoguide anyway, using the ST4-compatible port or through the
serial/Ethernet connection, with a guide rate configurable from 0.1x to 1x. The guide rate
can be automatically corrected for the declination of the target, so that there is no need ofrecalibrating the autoguide when observing at different declinations.
The mount has also dedicated function for easy use in the observatory. A dedicated
connector on the control box panel is used for remotized switching on and off. The instrument can be electronically balanced, without disengaging the worm from the wormwheel. The mount can be parked in different user-defined positions.
The serial RS-232 port can be used to control directly an external dome, avoiding the need
of using a dedicated external PC. Once onfigured with your instrument parameters, the firmware is able to make all the calculations required for positioning the dome slit in front of your optical tube, for almost all instrument configurations.

Technical Specs:

TECHNICAL DATA SHEET
Type German Equatorial Mount
Weight (mount) 65 kg – 143 lbs without accessories
Instrument payload capacity 100 kg – 220 lbs
Latitude range 20° – 70°
Azimuth fine adjustment range +/− 10°
Counterweight shaft 50 mm diameter, stainless steel, weight 8 kg – 18 lbs
Axes r.a. 80 mm diameter, alloy steel
dec. 50 mm diameter, alloy steel
Bearings Pre-loaded tapered roller bearings
Worm wheels r.a. 315 teeth, 244 mm diameter, B14 bronze
dec. 250 teeth, 192 mm diameter, B14 bronze
Worm gears Diameter 32 mm (r.a.) and 24 mm (dec.), tempered alloy
steel, grinded and lapped
Transmission system Backlash-free system with timing belt and automatic
backlash recovery
Motors 2 axes AC servo brushless
Power supply 24 V DC
Power consumption
~ 1 A at sidereal speed
~ 3 A at maximum speed
~ 5 A peak
Go-to speed Adjustable from 2°/s to 12°/s (9°/s in r.a.)
Pointing accuracy < 20” with internal multiple-stars software mapping
Average tracking accuracy
< +/− 1" typical for 15 minutes (< 0.7" RMS)
with internal multiple-stars software mapping and
compensation of flexure and polar alignment errors
Security stop
+/− 30° past meridian in r.a. (software)
+/− 35° past meridian in r.a. (mechanical)
+/− 170° interval in dec. (software)
+/− 172,5° interval in dec. (mechanical)
Communication ports RS–232 port; GPS port; autoguide ST-4 protocol port;
Ethernet port
Database
Stars: by name, Bayer designation, Flamsteed designation,
Bright Star Catalogue, SAO, HIP, HD, PPM, ADS, GCVS.
Deep-sky: M, NGC, IC, PGC ,UGC limited up to mV = 16.
Solar system: Sun, Moon, planets, asteroids, comets,
artificial satellites. Equatorial and altazimuth coordinates.
User defined objects, fast slewing positions.
Firmware features
User defined mount parking position, 2-stars and 3-stars
alignment function, up to 100 alignment stars for
modeling, correction of polar alignment and orthogonality
errors, estimate of average pointing error, storage of
multiple pointing models, sidereal, solar and lunar tracking
speed adjustable on both axes, declination-based
autoguide speed correction, adjustable horizon height
limit, pointing and tracking past meridian, assisted balance
adjustment, manual or GPS based time and coordinates
setting, dome control via RS-232, configurable
atmospheric refraction, network settings, comets and
asteroids filter, multi-language interface. Remote Assist via
Internet connection.
PC control
Remote control via RS-232 or Ethernet; proprietary
ASCOM driver or Meade compatible protocol; update of
firmware and orbital elements of comets, asteroids and
artificial satellites via RS-232 or Ethernet; virtual control
panel via RS-232 or Ethernet. Optional Wi-Fi.

10 Micron GM4000 HPS

Evolving perfection.

The GM4000HPS mount, now in the new M2 version, is built for observatories with an instrumentation up to a weight of 150 kg – 330 lbs (excluding counterweights). It is ideal
for remotized observation sites, and its loading capacity allows for mounting instruments
like 300 mm diameter refractors, 400 mm diameter Newton reflectors, 600 mm diameter
Cassegrains and so on.
Movements are driven by two AC servo motors, with timing belt reduction having zerobacklash.
Both axes feature a classic worm – wormwheel pairing. The wormwheels are made of bronze (B14), with a diameter of 330 mm and 430 teeth in right ascension, and a diameter of 244 mm and 315 teeth in declination. The worms are made of alloy tempered steel with a diameter of 32 mm. The axes themselves are made of alloy steel, with a diameter of 85 mm (right ascension) and 80 mm (declination), for the maximum rigidity.

The electronics is housed in an easily detachable housing (control box), mounted above
the right ascension axis, in order to obtain the best accessibility of all connections. The
connections of the mount and keypad secutiry lock screws. Only one cable runs from the
control box to the mount.
The axes feature a 60 mm diameter hole allowing for the passage of instrumentation
cables. This effectively solves the problem of entangling cables and damaging instruments,
especially for remote observatories.

The mount is powered with low voltage, requiring a maximum power of about 100W. This makes possible using the mount even in locations with limited power available. The GM4000HPS can be controlled completely using the included hand pad, without requiring any external PC.
The keypad is built in order to maintain the
maximum readability in all lighting conditions.
Both the display and the ergonomic keys,
allowing for the use of gloves, feature a red
backlight. An heater keeps the display warm for usage below freezing temperatures.
The mount can be controlled using the most
common software packages by connecting it
to a PC with the RS-232 serial port or the
Ethernet connection, via the 10micron ASCOM
driver or the Meade compatible command protocol. Furthermore, a dedicated software (also included with the mount) can be used to create a "virtual keypad" replicating exactly the functions of the physical keypad. The RS-232 port can also be used to control an external dome. This flexibility makes the GM4000HPS an ideal mount for observatories and remotized observing sites.
The object database contains many star catalogs and deep-sky objects up to the 16th magnitude. Solar system objects can be tracked so that their motion is compensated with respect to the stars. You may load orbital elements of comets, asteroids and artificial satellites into the mount, so that these objects can be tracked directly.

Pointing is made accurate through the usage of a model containing up to 100 stars, which allows for the correction of the classical polar alignment and conic errors, and also of the most important flexure terms of the optical tube. In this way it is possible to obtain pointing accuracies of the order of 15 arcseconds RMS. The same model can be used in order to obtain the maximum tracking accuracy, compensating also for the atmospheric refraction (depending on the local atmospheric pressure and temperature). A series of auxiliary functions is provided to help the user for quick aligning the mount to the celestial pole. You may also save and recover the alignment data of different observing sessions.
This function is very useful if you have many instruments in different setups, each one
requiring different flexure corrections.
Tracking through the meridian, a typical problem with german mounts, is solved allowing
for tracking for up to 30° past the meridian (configurable), in both directions. In this way
any object can be tracked for at least four hours.
The tracking accuracy makes autoguiding not necessary for many uses. The absolute
encoders on both axes allows to obtain a typical tracking error below 1 arcsecond. It is possible to autoguide anyway, using the ST4-compatible port or through the serial/Ethernet connection, with a guide rate configurable from 0.1x to 1x. The guide rate can be automatically corrected for the declination of the target, so that there is no need of recalibrating the autoguide when observing at different declinations.

The mount has also dedicated function for easy use in the observatory. A dedicated connector
on the control box panel is used for remotized switching on and off.
The instrument can be electronically balanced, without disengaging the worm from the wormwheel. The mount can be parked in different user-defined positions. The serial RS-232 port can be used to control directly an external dome, avoiding the need of using a dedicated external PC. Once configured with your instrument
parameters, the firmware is able to make all the calculations required for positioning the dome slit in front of your optical tube, for almost all instrument configurations.

Technical Specs:

TECHNICAL DATA SHEET
Type German Equatorial Mount
Weight (mount) 125 kg – 276 lbs without accessories
Instrument payload capacity 150 kg – 330 lbs
Latitude range 20° – 70°
Azimuth fine adjustment range +/− 10°
Counterweight shaft 60 mm diameter, stainless steel, weight 13 kg – 29 lbs
Axes r. a. 85 mm diameter, alloy steel
dec. 80 mm diameter, alloy steel
Bearings Pre-loaded tapered roller bearings
Worm wheels a.r. 430 teeth, 330 mm diameter, B14 bronze
dec. 315 teeth, 244 mm diameter, B14 bronze
Worm gears diameter 32mm, tempered alloy steel, grinded and lapped
Transmission system Backlash-free system with timing belt and automatic
backlash recovery
Motors 2 axes AC servo brushless
Power supply 24 V DC
Power consumption
~ 1,5 A at sidereal speed
~ 5 A at maximum speed
~ 6 A peak
Go-to speed Adjustable from 2°/s to 8°/s (6°/s in a.r.)
Pointing accuracy < 20” with internal multiple-stars software mapping
Average tracking accuracy
< +/− 1" typical for 15 minutes (< 0.7" RMS)
with internal multiple-stars software mapping and
compensation of flexure and polar alignment errors
Security stop
+/− 30° past meridian in r.a. (software)
+/− 35° past meridian in r.a. (mechanical)
+/− 170° interval in dec. (software)
+/− 172,5° interval in dec. (mechanical)
Communication ports RS–232 port; GPS port; autoguide ST-4 protocol port;
Ethernet port.
Database
Stars: by name, Bayer designation, Flamsteed designation,
Bright Star Catalogue, SAO, HIP, HD, PPM, ADS, GCVS.
Deep-sky: M, NGC, IC, PGC ,UGC limited up to mV = 16.
Solar system: Sun, Moon, planets, asteroids, comets,
artificial satellites. Equatorial and altazimuth coordinates.
User defined objects, fast slewing positions.
Firmware features
User defined mount parking position, 2-stars and 3-stars
alignment function, up to 100 alignment stars for
modeling, correction of polar alignment and orthogonality
errors, estimate of average pointing error, storage of
multiple pointing models, sidereal, solar and lunar tracking
speed adjustable on both axes, declination-based
autoguide speed correction, adjustable horizon height
limit, pointing and tracking past meridian,, assisted
balance adjustment, manual or GPS based time and
coordinates setting, dome control via RS-232, configurable
atmospheric refraction, network settings, comets and
asteroids filter, multi-language interface. Remote Assist via
Internet connection.
PC control
Remote control via RS-232 or Ethernet; proprietary
ASCOM driver or Meade compatible protocol; update of
firmware and orbital elements of comets, asteroids and
artificial satellites via RS-232 or Ethernet; virtual control
panel via RS-232 or Ethernet. Optional Wi-Fi.