Astronomy Specialist


SKU: 10M5000DD



Encoders: Absolute on both axes

300 kg

Testar Australia is a technical assistant dealer for 10 Micron. Our staff has been trained at the 10 Micron factory to provide assistance, repairs and maintenance on their products.

Top features

  • Direct drive high torque motors specifically designed for astronomy application
  • On-axis high resolution absolute encoders
  • High quality large diameter ball bearings
  • Very stiff and compact fork to minimise vibrations
  • Integrated electronics and on-board computer with internal sky model capability
  • Integrated interface with focuser/derotator control
  • Minimum base height for use with small domes and improved stability
  • Nasmyth focus (option): 100 mm Nasmyth hole diameter
  • Very fast pointing speed up to 30°/sec. – suitable for satellite tracking
  • Very accurate tracking for long exposure unguided imaging
  • One of 10 Micron last projects is the AZ DDS (Direct Drive System), a new generation of professional robotic mounts, in altazimuthal fork configuration with software integrated derotator/focuser.

Thanks to our long experience in robotic astronomical mounts, we are proud to offer this altazimuthal fork mount developed for professional and research applications such as astronomical and satellite fields, which need a really demanding grade of quality and affordability; our AZ mounts integrate all of the last technologies and technical acquirements in mechanical, electrical, electronics, software and design fields: all single features and components have been accurately studied in order to reach the highest level of efficiency that has always characterised 10 Micron products; also, we have integrated some special features in order to ensure the safety of both the instrument and the operator.

Left: The AZ5000 DDS with a Planewave CDK 24" installed. Right: GO1 Rotator/Focuser.

The AZ5000 DDS is typically designed to accommodate a 24″ -26″ diameter optics, which represents the optimal optical size, and we can also supply a complete telescope configuration. The mount is normally available for Cassegrain focus type telescopes only (standard version) and we can supply the correct flanges to accommodate it to your optics.

A Nasmyth focus configuration is available as option.

Ask our team for any customized configuration.

What does HPS mean?
HPS means “High Precision and Speed” and is the name for the new series of astronomical mounts by 10 Micron. 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 astro-imagers. In the vast majority of applications, including long exposure deep-sky imaging, the need for auto-guiding 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. Further, 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 regards 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 minimising the effect of these forces in traditional mounts require having very small pre-load 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 wormwheel; painstakingly calibrating software backlash compensation procedures; manually adjusting the meshing of gears. Or, maybe, introducing forcefully small alignment errors, to force auto-guide 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. Furthermore, they aren’t extremely accurate anyway. At a fairly typical temperature of -5°C, which is not rare for astronomical observation, a typical quartz can have an error of tens of parts per million (ppm). Errors of 20 or 30 ppm are commonly observed, which would cause errors in right ascension accumulating at about 2.5 seconds per day, which means more than one arcsecond per hour. The loss of pointing precision in a 12-hour winter night would be of about 20 arcseconds, and much more if the mount is shut down and powered on days later. This can be corrected by keeping the mount always synchronized to an external time source, like a standard PC with its clock synchronized to the NIST time servers, or with the optional GPS module we already talked about. As of now, all of our motor drivers feature a battery-backed clock with temperature compensation, which is able to keep time with an accuracy of 3.5 ppm from –40°C to +40°C.
A much slower, but nevertheless fundamental, movement is the precession of equinoxes. If you don’t model the precession, you are forced to use standard coordinates (for example, when doing alignment). Some may think that if you make an alignment with J2000.0 coordinates, then you should be able to point objects using J2000.0 coordinates: nothing could be farther from reality! Precession changes the direction of the Earth’s rotation axis, i.e. the celestial pole, so this mean that the alignment would work… for a few minutes, then pointing accuracy would be destroyed. Some systems do not account for precession in their databases. By default, 10Micron mounts work in JNOW when communicating with the outside, i.e. the coordinates you read and set in the keypad are referred to the true equinox of the date of observation. But everything is accounted for in the firmware. Yes, even nutation and light aberration.
Another factor which can limit the accuracy of the mount over long periods is the change in Earth’s rotation rate. What we call the “UTC time” is only an approximation to the angle of rotation of Earth. The angle of rotation of Earth is measured by UT1, if we neglect the pole wandering and seasonal variations, (that anyway amount to less than one arcsecond). UTC is based on atomic clocks, and sometimes a so-called “leap second” is inserted into it to maintain it within 0.9 seconds of UT1. So, when you approximate UT1 with UTC, you may introduce a difference of up to 14 arcseconds into your pointing accuracy. This difference changes very slowly, so that the degradation of pointing models (simply due to terrain creeping and other “very slow” things) is always faster than this change, and you will not notice any problem in practice. But when the leap second is inserted, you have a sudden jump in coordinates. So we are going to implement a full accounting of UTC, UT1 and leap seconds since firmware revision 2.13.1.

Modelling the motion of astronomical objects themselves
Quite a number of astronomical objects exhibit a visible movement. Planets, asteroids, comets, and also artificial satellites of the Earth. The firmware of 10Micron mounts can compute the motion of all these objects directly from their orbital parameters (except for planets, you will have to upload orbital parameters into the mount: you can do it before leaving for your preferred observation site). Artificial satellites are tracked via a special functions which we invite you to explore. Solar system objects are tracked automatically on both axes by leaving the “Follow object” setting on. Please note that the Moon has an appreciable motion in declination that many mounts omit to account for, even if the “moon tracking speed” is selected.

Why not auto-guiding? It seems simpler…
Auto-guiding is simpler… for the mount manufacturer. For the user, auto-guiding 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 for customized guiding software parameters, calibration. HPS mounts can be aligned to bright stars during twilight, then every second of darkness can be used for imaging. Furthermore, auto-guiding is not always possible. The typical situation is imaging a faint, fast-moving comet. Anyway, if you still want / need auto-guiding, 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, doubles and deep-sky objects. Also, a catalogue of moon features is available and useful due 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 instrument (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 directly controlling 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.

Mount type

Alt-azimuth direct drive mount with on-axis high resolution absolute encoders


300 kg (mount without telescope and accessories)

Telescope payload capacity

Up to 250 kg, 650 mm (26”) diameter

Axes bearing

High quality large diameter, special bearings


Professional grade direct drive motors; no worm gears or transmission systems, zero backlash


High resolution absolute encoders

Power supply

48 V

Power consumption

5 A peak

Goto speed

Goto speed 40°/s

Pointing accuracy <10" rms with internal 25 stars software mapping, max 100 stars.
Modeling software (Model Maker) available for auotmatic alignment operation
Average tracking accuracy

1" typical for 15 minutes / 0.6" RMS with internal 25-stars model (REAL sky observations).
<0.01" encoder readout error.

Nasmyth hole diameters

Primary Nasmyth focus: 100 mm diameter; secondary Nasmyth focus 68 mm diameter (special request)

Nasmyth focus payload capacity 30 kg

Safety features

Mechanical stops in both axis
Anti-wrap logic
On board and remotable Emergency stop button with safety relay
Aural warning system
Unbalance/collision protection system

Security stops

Mechanical stops
Az: +/- 300° (~2 turns)
Alt: 100° (-5° / +95°)

Security brakes

Electromechanical brake for unbalanced security in altitude

Dimensions (only mount with standard fork) 1350 x 550 x 1350 mm

Focuser/DeRotator standard

GO1 by 10Micron (optional)


10Micron specific, software integrated control

Payload capacity

25 kg

Temperature compensation Internal temperature probe

Communication ports

RS–232 port; GPS port; auto-guide ST-4 protocol port; Ethernet port

Integrated 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.

Integrated control electronic features

User defined mount parking position.
Mount modeling with up to 100 stars / points.
Storage of multiple pointing models.
Configurable tracking speed.
Adjustable movement limits.
Assisted balance adjustment.
Integrated leap second support.
Direct dome control via RS-232.
Configurable atmospheric refraction compensation.

Keypad control Rugged keypad with metal housing, backlit micro switches, dimmable graphic display.
All the functionality of the mount is available through the keypad without requiring an external PC.

PC control

Remote control via RS-232, Ethernet network.
Update of firmware and orbital elements for satellite tracking and minor planet objects.
Virtual keypad control panel replicating the functionality of the physical keypad.
Mount manager software including advanced user interface.
Usage of any client software supporting the ASCOM standard through proprietary ASCOM driver, or through the LX200 compatible protocol.
NEW professional WEB interface coming soon….

  • Fork Mount
  • Power supply
  • The derotator/focuser is optional
      10 MICRON AZ5000 DDS.

      10 MICRON AZ5000 DDS

      $999,999.00 AUD

      Optical design

      Image circle

      Focal ratio


      Focal length

      Optical thickness



      Colour or Mono

      Pixel size

      Sensor dimensions


      Sensor diagonal

      Quantum efficiency

      Read noise

      Fullwell capacity

      Bit depth


      Camera backfocus

      Filter size

      Filter size

      Bandpass (FWHM)

      Bandpass (FWHM)

      Glass thickness

      Mount type


      Payload capacity

      250 kg, 650mm diameter

      Latitude range

      Dovetail saddle

      Slew speed

      40°/s max


      Encoders: Absolute on both axes

      Periodic error correction

      Not needed

      Counterweight shaft

      Azimuth adjustment range

      Internal diameter

      Illuminated diameter

      Compatible telescope external diameter


      300 kg




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