WHY are the QHY600 monochrome CMOS cameras more expensive than models from other manufacturers that also use the Sony IMX 455 BSI CMOS sensor?
The image sensor - the heart of EVERY astronomical CMOS camera
Image sensors are THE basis of ALL imaging in astronomical photography. The performance of the camera - i.e. the read out raw image after exposure - is based on the quality of the CMOS or CCD sensor and its performance.
Image sensors of many manufacturers are produced in different qualities: In very high quantities the "consumer-grade" sensors and in much lower quantities - and therefore much more expensive - the "industry-grade" sensors, which have to pass more extensive and tougher quality controls before delivery. The monochrome "Industrial-grade" IMX 455 sensor is certified by Sony for 24/7 continuous operation![br]
QHYCCD is one of the few manufacturers of amateur-priced cameras that uses the Sony IMX BSI sensor in "industry-grade" quality in all mono version of QHY600 series use IMX455 industry grade sensor (Grade-K) – except the QHY600-L. WHY?
The QHY600 is a 60 megapixel full frame CMOS camera, which can be supplied with either a monochrome or a color sensor.
The QHY600 PH, QHY600 PRO and QHY600 PH-L(ite) models are immediately available for pre-order.[br]
FRAMOS - a world leader in industrial, scientific and medical imaging technologies and custom camera development - comments on the choice of "consumer-grade" and "industry-grade" sensors and recommends the following to customers): (www.framos.com/en/products/sensors/consumer-sensors/)
Similar to area scan sensors, images produced by consumer grade sensors, provide a fast, high-resolution capture of the entire field of view. The main difference between them and industry grade ones is that consumer sensors have a shorter life span, a shorter MTBF (Mean Time Between Failures) and, as a result, may cost much less than an equivalent industry sensor.
If you have a product that needs to be guaranteed for a long time, have a consistent image between each vision product, or if you need it to last for several years versus just one year you will want to consider an industry sensor instead. If you are purchasing hundreds of thousands of sensors per year and you have satisfied the other requirements, then consumer sensors may be the right choice for your application".
Another important difference between "consumer" and "industry" sensors is the so-called "package" - the housing in which the sensor is embedded. In the case of consumer sensors, this package is often made of plastic, while in the case of industrial sensors ceramic is often used as the base material, which is much more temperature stable and guarantees a high degree of flatness of the sensor array with deep cooling.
The Sony IMX 455 "industry grade" sensor is part of a so-called LGA package. LGA stands for "Land Grid Array" and the base material must be materials that minimize thermo-mechanical stresses as much as possible. This enables a wide temperature working range and the sensor can be used even under extreme environmental conditions.
The industry grade sensor is designed for longer life under normal use and can therefore withstand repeated cooling/heating cycles with less thermal stress, resulting in a longer life for a cooled camera. AND industrial sensors have a significantly lower number of pixel defects.
! The price difference between the "consumer" and "industry" version of the Sony IMX 455 is more than 500 US Dollar in purchasing !
Other advantages and features that ONLY the QHY600 models offer comparing to other camera models with the Sony IMX 455 sensor.
The different readout modes of the QHY 600 PHOTO / 600 PRO and the QHY600 PH-L
The "Readout Mode" selection is a new function developed for the QHY600 and other newer QHYCCD cameras. With the QHY 600 Photo there are (currently, more to follow) 4 different readout modes available, which change the way the image sensor is read out. This is giving the user freedom and control over the performance of the sensor.
The following table shows the differences in the data between mode 0 and mode 1 at different gain (source QHYCCD)
Readout noise
Image Dynamic
Full-Well
Read Mode 0/Gain = 0
7.8 e-
13.4 stops
85003 ke-
Read Mode 0/Gain = 27
2.7 e-
13.26 stops
27045 ke-
Read Mode 1/Gain = 0
3.68 e-
13.75 stops
50639 ke-
Read Mode 1/Gain = 56
1.68 e-
13.65 stops
21657 ke-
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What does this data mean in practice for the user? In readout mode 0 the readout noise of the QHY600 PH is drastically reduced between a gain setting of 25 and 26. It is therefore recommended to set the gain as a starting point to 26. At this gain the full well capacity is 27ke- and the readout noise is only 2.7e-. For longer exposure times, where the readout noise is not so critical, reducing the gain will result in a higher full well capacity. Recommended e.g. for images of objects with a large contrast range (dynamic range), such as the Andromeda nebula or the Orion nebula.
From the optimization point of view, readout mode 1 with gain = 56 will be the most commonly used mode. It offers the lowest readout noise while providing considerable full well capacity. And this practically without loss of dynamic range. Recommended for taking pictures of fainter objects at shorter exposure times.
Readout mode 2 (Extended Full Well Mode, EDR) increases the full well capacity enormously. In this "Ultra-High" Full Well Mode the QHY600 reaches an unbinned Full Well capacity of more than 80.000 ke-. In 2x2 binning mode, full well is greater than 320,000 ke- and in 3x3 binng, full well capacity is greater than 720,000 ke-. High full well values guarantee a wide dynamic range between bright and faint details of the object under observation.
The EDR technology is not new, but is used exclusively by QHY cameras with the Sony IMX 455 sensor. Usually it is used to scale the image to 16 bit data depth in sensors with 12 or 14 bit AD conversion. Now the QHY 600 and the QHY 268C are already cameras with true 16 bit AD conversion. The Extended Dynamic Range readout mode 02 increases the full well capacity from over 51,000 ke- to just over 80,000 ke- with the pixels measuring only 3.76mü - and thus the image dynamics of the raw image also increase. The EDR mode also allows a wider range of gain values to be used without saturating the pixels. This way, extremely "deep" luminescence and RGB raw images can be captured, resulting in full detail and extreme dynamic differences in the raw image - without tricks and "pull-ups" in the final image processing.
New readout mode # 03:
QHYCCD extends from August 2020 the readout modes of the QHY 600 models by the # 03 Extend Fullwell 2CMSIT mode (yellow curve). The advantage of mode # 03 is that it has the same fullwell value and the same system gain as mode #02 Extend Fullwell, but that the readout noise is reduced about 1.3 times. (see graphic, Figure #03).
This readout mode requires an upgrade of the control software to version SDK 2020.6.26 or later. If your software does not show mode # 03, please download the QHY AllInOne installation package to upgrade the SDK (Software Development Kit) in the software. The mode is available for all models of QHY 600 series.
The exact dependencies between readout noise, gain, full well and image dynamics are shown in the graphs of the 3 readout modes.
FPGA stands for Field Programmable Gate Array
The QHY 600 and the QHY 268C camera integrate a FPGA semiconductor chip in the camera electronics. Among other things, the camera firmware is stored in these chips. The firmware itself takes up only 10% of the resources, so that 90% of the hardware logic resources are available to the user for many customer-specific functions. In addition to the customer-specific functions, an online upgrade of future firmware updates via the USB 3.0 port is possible at any time. For example, to implement further, upcoming readout modes.
The internal image memory
The QHY 600 has an internal DDR 3 image memory with a capacity of 1 or 2 Gbyte. Thus the available memory is 4 to 8x larger than in the cameras with IMX 455 sensor of the co-suppliers. What does this mean for the photographer?
The extremely large number of individual pixels of the latest generation of CMOS sensors leads to an increased memory requirement, both for temporary intermediate storage and permanent storage on the computer. For example, the QHY600 Photo Sony IMX 455 sensor generates about 120 MB of data per frame. The transfer of such large amounts of data necessarily requires that the camera itself has a sufficiently large internal buffer memory.
A frame rate of 2.5 frames per second at full resolution generates a data volume of 300 MB in just one second. If the memory has a capacity of only 256 MB, it overflows within 1 second and this can mean a loss of data. With a memory capacity of 1 GB it is possible to bridge about 3 seconds in extreme cases, e.g. if the CPU of the computer is busy with other functions.
Although the cost of the 1 GB image memory is significantly higher than of a 256 MB memory, it makes sense to make the large storage capacity available in the QHY 600 Photo so that the sensor can be read out immediately. BECAUSE: A CMOS BSI image with Rolling Shutter technology is exposed until it is 100% read out - otherwise this leads to irregularities in the image.
The QHY Noise Suppression Technology
Normally, the thermal noise of CMOS and CCD image sensors changes in a reproducible way depending on exposure time and sensor temperature. However, there is another type of thermal noise that some Back Side Illuminated CMOS sensors have, which overlays the characteristics of the reproducible, typical noise with a random noise pattern that is independent of exposure time and sensor temperature (Random Noise).
Each image thus has its own noise characteristic, making a dark image print to reduce thermal noise less effective. The electronics of the QHY600 versions and the QHY 268 C use an innovative technology to suppress random thermal noise, which significantly reduces its influence, as the image examples clearly show. This technology delivers significantly smoother and noise-free backgrounds of the raw image.
Random horizontal noise optimization
The Sony IMX455 sensor offers a number of different readout modes that allow the user to control the image output. In high gain mode, the sensor delivers extremely low readout noise at very high gain. To further improve this mode, QHYCCD has developed an optimization that allows the sensor to deliver a noise-free image beyond factory specifications even at extremely high gain.
Because this effect is usually only visible in mode # 01 (high gain mode), the "Random Noise" optimization is effective in all readout modes and improves the performance of the QHY600 camera in every imaging mode. The hardware and software for optimization is integrated in all QHY models delivered from the beginning of 2020.
The monochrome and the olour version of QHY 600 PRO are optionally available with water cooling. This cools the sensor temperature about 10 degrees lower than the models with standard air cooling. A delta T of 45 degrees to the ambient temperature is achieved. This is an important option if the camera is to be used in regions where night temperatures are well above 20 degrees Celsius in some seasons. The water cooling must be ordered when placing an order, it cannot be retrofitted. We describe further advantages of a water cooling system here.
Highly precise time allocation for exposure time
The QHY 600 PRO models have an interface to connect the QHY GPS Box. The GPS Box provides extremely precise time information about the beginning and end of the exposure time worldwide. The time allocation plays a major role in astronomical observations of objects that change their brightness during the observation time. For example, in the photometry of minor planets or variable stars, in the observation of star occultations and exo planetary transits.
In the many years since the foundation of QHYCCD, engineers and developers have gained experience with CMOS sensors in numerous camera models, thus optimizing hardware and software. You buy this "know-how" with every QHY CMOS or CCD camera.
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Further information and links to QHY600:
Test of the linearity of the QHY 600 Photo:
In general CMOS sensors - compared to CCD sensors - do not work linear at higher full well values, which means that they are not well suited for photometric (brightness measurement) investigations.
New Technology Found in QHY600 and QHY268 Cameras:
1. USB Re-Connection with 12V ON/OFF
The QHY600 / 268 camera's USB interface to the computer will connect or disconnect by turning on and off the camera's 12V power, without the need to plug and unplug the USB cable. This technology enhances the controllability of the camera when used in a remote station. You only need to remotely control the 12V power supply of the camera, or the power of the camera AC adapter, to achieve remote USB connecting and reconnecting of the camera.
2. Extended Full Well Capacity and Multiple Read Modes
With a pixel size of 3.76 µm, these sensors already have an impressive full well capacity of 51ke-. Nevertheless, QHYCCD has implemented a unique approach to achieve a full well capacity higher than 51ke- through innovative user controllable read mode settings. In extended full well readout mode, the QHY600 can achieve a much greater full well, more than 80ke- and the QHY268C can achieve approximately 75ke-. Greater full well capacity provides greater dynamic range and large variations in magnitude of brightness are less likely to saturate. The QHY600 / 268C have each have three user controllable readout modes with different characteristics.
Usually thermal noise in imaging sensors changes with time and temperature in a very reproduceable manner. However, there is another type of thermal noise peculiar to some backilluminated CMOS sensors that has the characteristic of typical fixed pattern noise but the value is not related to the exposure time. Instead, each frame appears to have its own characteristics making dark frame subtraction less effective on the total thermal noise in an image. The QHY600 models / QHY 268 C/M uses an innovative suppression technology that can significantly reduce the level of such random noise.
The two professional models of the QHY 600 are prepared for 2 x 10 Gigabit fiber optic interfaces, which can be optionally enabled at extra cost. In addition, a Fiber PCIE Graber Card is required. With Gigabit interfaces, QHY has introduced the next generation of high-speed data transmission technology. This is a revolutionary leap beyond USB 3.0 transmission technology and solves several important shortcomings of USB 3.0 transmission: limited speed, limited distance and reliability.
QHYCCD Fiber PCIE Graber Card. Support PCIEX8, Four 10G Fiber Input
Limited Speed Although USB 3.0 is quite fast it still cannot fully meet the maximum speed requirements of the latest generation of CMOS image sensors used in the QHY600 PRO models. For example, the IMX455 chip used in the QHY600 can produce four 16-bit, 60 Megapixel frames per second. In this case, the amount of data transferred per second is 120 * 4 = 480MB and the real-world maximum transmission speed via USB3.0 can is generally not much more than 300 MB/s. Via the USB 3.0 interface, image transfer is limited to 2.5 frames per second. In contrast, a transfer speed of up to 2000 Mb/s can be achieved via the 2 x 10 Gbp/s fiber optic interfaces.
Limited Distance
USB 3.0 transmission is generally stable over a limited distance of about 2-3 meters. An active extension cable is usually required for more than 3 meters but even with an active extension the cable may only reach about 15 meters. However, transmission over optical fiber can easily be done at distances up to 300 meters (remote operation !).
Stable transmission without electromagnetic interference
As we know, the propagation of light is not affected by electromagnetic radiation, so transmission through optical cables has very high reliability. There is no conductive medium between the camera and the computer, so it is not affected by various sources of static or leakage effects.
Note: Free switching and upgrading to the fiber optic interfaces is also possible at a later date for the earlier models QHY 600 - Early Bird (EB) and the QHY 600 - PRO - L.
The extremely large number of individual pixels of the latest generation of CMOS sensors leads to increased memory requirements, both for temporary intermediate storage and permanent storage on the computer. For example, the QHY600 Sony IMX 455 sensor produces about 120MB of data per frame. Transferring such a large file sizes necessarily requires the camera to have sufficient memory. The QHY600 models / QHY 268 C/M has adopted a large-capacity memory of up to 1GB (QHY600 PH-L/ QHY 268) and 2GB (QHY600 PRO). This large image buffer meets the needs of high-speed image acquisition and transmission of the new generation of CMOS sensors, making capture of multiple frames smoother and less stuttered, further reducing the pressure on the computer CPU!
The QHY600 mdoels and QHY268 C/M has a million-gate, 20nm process programmable Field Programmable Gate Array chip. The camera firmware itself only occupies 10% of the resources, so 90% of the hardware logic resources can provide users with many custom functions. In the QHY600 PRO model and QHY268 C/M these functions include high-performance GPS trigger imaging, hardware time stamp, high-precision external trigger, continuous mode with latent image elimination, two readouts to reduce readout noise and multi-camera high-precision synchronous shooting and so on to meet a variety of complex application needs.
QHYCCD accepts orders for QHY600 PRO cameras customized for water-cooling. The water cooling must be firmly ordered with an order, a later retrofit is NOT possible. Compared with air cooling, water cooling has the following important advantages:
No vibration. Air-cooling requires the use of a fan inside the camera that may induce small vibrations. Even the highest quality fan cannot avoid some effect on the FWHM (full width at half maximum) of stellar images on certain telescopes. Long focal length optical systems are more sensitive to this effect. However, water cooling achieves temperature reduction through the slow flow of water. There is no moving mechanical component to cause vibration of the camera, eliminating any negative effect on the image.
No hot air turbulence. For optical systems like RASA and Hyperstar where the camera is placed at the secondary position, air turbulence is not generated. When an air-cooled camera is installed infront of the optics, the hot air generated by the air-cooled system passes through the optical path and can generate seeing effects. Water cooling does not produce hot air discharge. The heat is carried away by the liquid so there is no such effect.
Greater Cooling Delta T. With water cooling, the maximum cooling temperature is about 10 degrees Celsius lower than the maximum temperature achieved with air only. This has a particularly positive effect for long exposures and when used under tropical night temperatures.
All three QHY models (PRO, PHOTO and LITE) are also available as short back focus (BFL) versions. Here, the backfocus is only 7mm, instead of the usual 17.5mm, behind the camera body. They are specially designed for the adaptation of Canon and Nikon lenses. An off-axis guider and filter wheels can be integrated. More information at QHYCCD about the BFL version can be found here.
In order to meet the limited back-focus requirements of certain optical configurations of filter wheel and lens or for instruments such as spectrometers, etc., the QHY600 models are also available in a short back-focus version. Here the distance between telescope mount and sensor plane is only 7mm. This custom version requires advance booking. This version also provides a solution for chip tilt adjustment, in order to be able to correct a possible tilting of the sensor plane against the telescope optical path. However, because the glass window of the short back-focus version is closer to the CMOS chip, the risk of condensation is greater than the standard version with 17,5mm even though the sealed window glass heating plate is also integrated. QHYCCD provides a corresponding solution to this situation. Nevertheless, it is recommended that users without such special requirements choose the standard version.
William "Bill" Paolini has been actively involved in optics and amateur astronomy for more than 50 years, and is author of the popular book: : Choosing and Using Astronomical Eyepieces
A detailed test report: Field Test of the Baader MaxBright® II Binoviewerhas now been published by William Paolini in the most popular astro forums. We are very happy about his extremely positive conclusion and would like to highlight two quotations:
Their compact size, moderate weight, solid build quality, precise mechanical function, well thought out ergonimocs, plethora of available accessories, and excellent optical performance has actually made me a fan of binoviewing again!
The performance, ease of operation,and flexibility of the MaxBright II Binoviewer provided for me seemlessly executed and thoroughly rewarding observing experiences, whether using 1.25" eyepieces that produced sweeping low magnification wide field vistas, to those exepieces that produced the highest magnifications possible for detailed lunar and planetary observations. Very highly recommended.
Do you already have experience with the MaxBright® II? Do you have questions about the product? We would be pleased to receive further reviews or comments on this article.
I see spikes on bright objects - is my prism defective?
[product sku="2456120"]
Concerning Amici prisms, there are two factors which can limit the use for astronomy. The first one is the optical quality, i.e. how good is the alignment of the optical surfaces. Most Amicis are made for terrestrial use, where our atmosphere limits the useable magnification to ca. 60x or 70x, anyway. So, it's fine if they don't show a double image up to ca. 100x, as such high magnifications can't be used.
[product sku="2456130"]
Those prisms which are designed for astronomical use are designed for those magnifications which we can use for the night sky – ca. 300x or even more. This high precision makes our Astro-Amici star diagonals so expensive.
But all Amici-prisms – no matter how good they are – suffer from one design feature: There is a line going through the center of the image, where both sides of the prism surfaces com together. This may cause reflections or spikes. To some extent, this will always happen when a bright object like a star is viewed in front of a dark background like the night sky. This should be obvious only with very bright stars or planets, while dimmer stars are no problem. In this case, simply move the telescope a little bit so that the image of the bright light source isn't centered on the prism edge any longer.
To be honest, there is one way to reduce these reflections: by destroying the prism edge. Even a sharp, perfect prism edge with a width of only 1/100 mm will produce reflections. But if you polish it round, there will be no spikes! Unfortunately, in the final image in the eyepiece, there will be a streak with a width of ca. 1 mm where contrast will suffer and details will no longer be visible, because they drown in the multitude of image errors introduced by this wide "bar" cutting the image in two halfes. We decided not to sacrifice the over-all contrast by giving the prism a blunt edge – even if that means that bright objects must be placed a little bit away from the center to avoid spikes.
Using the Baader FlipMirror II Star Diagonal (BFM II) at the Telescope
The [product sku="2458055"] is not only an accessory for professional users, but much more: It is a helpful tool for every amateur astronomer – especially for astrophotography.
First of all, the BFM II is designed to completely replace your standard star diagonal, so that you can keep observing as usual, just like with every good star diagonal. But the BFM II gives you much more options. You can create – from the beginnig, or step-by-step – your own system for photography and keep it always ready-for-use at your telescope. This will save you a lot of time and nerves. In the next months, we want to show some of the many options of this new product here.
In this article we will cover the adjustment options.[br]
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Adjustment options of the FlipMirror II star diagonal
The Baader FlipMirror II offers a variety of adjustment options. Usually you don't need to worry about them – the BFM-II is ready for use "out of the box" if you have the right connecting parts. But if at some point you want to use short, torsion-proof screw connections, you may be dissatisfied with the delivery condition: The beginnings of each thread are different, so a camera will most likely be aligned at an angle to the FlipMirror II. This does not only look strange, but can also cause the hot shoe of a DSLR to interfere with the housing of the FlipMirror II. And most of the time, you'll want to align the camera in such a way that the rows of pixels are oriented along the axes of the mount. Then the cardinal points are not skewed in the image when the shot is displayed with "north up" for better orientation, and the data of a spectrograph can be captured with highest resolution.
Most users will probably use the BFM-II with a 2" nosepiece, so that it can be easily rotated around the optical axis of the telescope together with the camera. Especially on fixed telescopes or when the backfocus is narrow, a screw connection with telescope or eyepiece extension is recommended. For the Baader Diamond SteelTrack® there are various short adapters with connecting threads available, which can replace the original ring clamp. This allows the alignment to be easily reproduced when cameras or instruments are changed to continue an observation on another night. With a plug/clamp connection, this usually only works in good approximation.
The connection threads are adjustable via the four grub screws. Thus accessories like here the DADOS spectrograph can be aligned flush with the housing, or the whole attachment can be rotated if it is firmly screwed to the telescope
The angle of rotation around the optical axis is always adjusted by the same method, no matter if you want to adjust the telescope side or the camera side connection. With the included 1.5 mm Allen wrench you can loosen the two S52/M48 insert rings, which are used to connect the BFM-II to the telescope or the camera. To do so, simply loosen the four countersunk grub screws holding the respective ring, turn it to the desired position, and tighten the screws again. You may "dig" into the material – after all, the ring should not give way when you unscrew accessories.
BFM II - View from above. The connection thread can be aligned using the screws.
Similar to an extender, the upper eyepiece port can be moved a little bit in every direction to place a star which is seen in the middle of the camera sensor also exactly in the middle of the crosshairs. In this way you can easily compensate for a slight decentration of a crosshair or eyepiece. Such a decentration can occur, for example, if the tolerances between the eyepiece diameter and the eyepiece clamping are too large, or if the eyepiece is not always clamped in the same position.
Simply center a star on the sensor of the camera mounted on the rear (straight) port and then move the entire top connector until the star is centered here as well. Then fix the four adjustment screws - done.[br]
The two pins on which the mirror rests.
The tilt angle of the mirror can also be adjusted if necessary. The spring mechanism presses the mirror onto the two conical brass pins. Using the tools provided, the two pins can be adjusted to move the image along the optical axis if necessary.
Normally these screws do not need to be adjusted, but if they do, make sure that the mirror rests on both sides.
The adjustment screws for the lower port of the BFM II
Last but not least, the bottom (AUX-) port e.g. for an Autoguider can also be adjusted a little bit, in order to position the prism perfectly or to be able to adjust everything else as usual via the off-axis-guide. This is done with the three screws that attach the off-axis-guider to the FlipMirror II housing.
No Compulsion, but Possibilities
Don't get intimated by the adjustment possibilities of the FlipMirror II – it is pre-adjusted and many options are either intuitive or only interesting when it is firmly screwed to the telescope and camera. At the latest when you plan such a professional setup with the shortest possible overall length, you will appreciate the possibilities that simpler models with fixed eyepiece clamps cannot offer.
On Rowe-Ackermann Schmidt-Astrographs RASA 11" or RASA 36cm systems it can happen that the respective RASA UFC adapter ([product sku="2459126"] or [product sku="2459135"]) slips laterally to the Schmidt plate, when the telescope moves from east to west. Since the RASA systems do not have a lateral centering collar, the adapter can slip a few tenths of a millimeter. This problem can only be solved by friction.
Therefore it is very important to strongly tighten the union nut first.
In addition, since April 2020 we have slightly roughened the flange surfaces of the adapters to increase friction at this point and prevent slipping.
For all adapters delivered previously, we therefore recommend doing this procedure afterwards. For this purpose we recommend a normal sandpaper with approx. 180 grit.[br]
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We also recommend cross sanding as in the video below to prevent slippage in both the X- and Y-axis.
[br]
1. QHY Planetary and Guiding cameras with uncooled CMOS sensors
The QHYCCD planetary (Lucky Imaging) and guiding cameras are designed in a 1¼ inch eyepiece design. They fit into any 1¼ inch eyepiece mount, are small, lightweight and flexible in use. They allow a very high frame rate via the fast USB 3.0 interface and are highly sensitive at the same time. For use as a guiding camera, you may need a separate Off Axis Guider.
The new QHY-5-III cameras, such as [product sku="1931035"], [product sku="1931031"], [product sku="qhy5III678"], [product sku"1931038"] are the 2nd generation of planetary and guiding cameras. Compared to the first generation 5 III series, the new models have been significantly improved in terms of interfaces and hardware configuration. Among other things:
Larger internal image memory DDR 512MB
Improved front and end design
Compatibility with CS and C-mount lenses
USB 3.2 Type-C interface
Universal ST-4 guiding port
Control LED for status indication
New Sony sensors with extra high sensitivity
The 2nd generation QHY-5-III series planetary and guiding cameras are all equipped with 512 MB DDR3 internal image memory. This increases the safety of losing individual images at high frame rates.
This is a great advantage for solar, lunar and planetary photography, where large amounts of data often have to be transferred to the PC/laptop in a very short time. Some of the DeepSky cameras still on the market today, for example, only have a 256 MB image memory. In comparison, the 512 MB DDR3 memory of the new QHY Series 5-III 2nd generation cameras is a considerable improvement.
For a beginner, it can be confusing to choose the right camera to start with. We therefore advise you to proceed step by step, starting with the equipment that allows to track (guiding) a telescope mount in such a way that your first attempts will also show pinpoint star images.
QHYCCD deep sky cameras feature state-of-the-art CMOS and CCD sensors designed to provide exceptional sensitivity in low light conditions. These sensors are ideal for capturing the faint details of celestial objects, revealing intricate structures and subtle color variations previously accessible only to professional observatories. With their remarkable signal-to-noise ratio, QHYCCD cameras ensure that even the faintest deep-sky objects can be captured.
The Deep-Sky cameras includes all of the cooled cameras with BSI (Back Side Illuminated) and FSI (Front Sike Illuminated) CMOS sensors in optical format sizes smaller than 1 inch (small size cameras) and from 1 inch to Full Frame - 35mm Format (medium size cameras). These same sensors are also used in the uncooled QHY5III Series cameras. However, the camera models include efficient TE cooling as well as other more advanced features not found on the uncooled models.
4164*2796 (11,7 MP) bei 4,63 µm / 14 bit Datentiefe (Mode 0), 46,8 MP bei 2315 µm / 12 bit Datentiefe (Mode 1)
6280*4210 (26 MP)
9600*6422 (61 MP)
Pixel size
2,4 µm
3,76 µm
5,86 µm
4,8 µm
3,8 µm
4,63 / 2.315 µm
3,76 µm
3,76 µm
Frame Rate@ Full Resolution
15 fps
18 fps
138 fps
10 fps
22,5 fps
16,5 fps
6,8 fps
2,5 fps
ADC-Bit depth
12 bit
14 bit
12 bit
14 bit
12 bit
12/14 bit
16 bit
16 bit
Full-Well Capacity
15,5 ke-
58 ke-
32 ke-
46 ke-
20 ke-
65 ke-
51 ke- / >75 ke
51 ke- / >80 ke
Pixel-Fov (@ 1000mm)
0,5"
0,78"
1,21"
0,99"
0,78"
0,96/0,48"
0,78"
0,78"
Special camera: [product sku="1931294" style="imgright"]
– especially for ambitious amateur astrophotographers –
monochrome BSI CMOS camera with 102 MegaPixel and highest quantum efficiency with extremely low readout noise.
Not long ago, the KAF 16803 G-Sense chip was the workhorse of all serious astrographers. With the IMX461 CMOS chip, QHY offers an affordable cameras.[br]
QHYCCD bietet eine breite Palette an Deep-Sky-Kameras, die mit verschiedenen Teleskopen und Einrichtungen kompatibel sind. Egal, ob Sie einen Refraktor, Reflektor oder einen speziellen Astrographen verwenden, für jedes Teleskop gibt es eine passende QHYCCD-Kamera, die sich nahtlos in Ihre Ausrüstung einfügt.
QHYCCD scientific cameras offer the latest technology in scientific imaging at reasonable prices. Scientific CMOS image sensors offer extremely low noise, fast frame rates, wide dynamic range, high quantum efficiency, high resolution and a large field of view simultaneously in one image. In this sense, while QHYCCD cameras for astronomy clearly meet the definition of scientific cameras, QHYCCD differentiates its scientific camera models with additional features not found in similar models for astrophotography.
QHYCCD scientific cameras are characterized not only by extremely low noise, high quantum efficiency, and other scientific CMOS features, but by
Large area, high resolution sensors, SWIR sensors, polarized light sensors,
GPS-enabled timing,
external triggers,
field programmable gate arrays,
2x10 GB fiber optic computer interface and water cooling options.
The following scientific models are suitable for microscopy, spectroscopy, multispectral imaging, inspection, bioluminescence imaging, life science applications, and many other laboratory applications.
Ideal for astronomical and biological science research
Very high quantum efficiency, square (Gpixel)
Low & High-Gain readout like QHY4040
Available also as UV sensitive version
Ideal camera for astronomical and biological imaging as well as spectroscopy
Universal high resolution full frame camera with professional connectivity (GPS & fiber optic connections)
also available as photographic version for high-end users (QHY 600 PH)
With GPS PPS Synced High Precision Hardware Stamp
cooled camera with the smallest sensor
Ideal for multi-site, high precision timing of exoplanet light curve measurements and is the for cooperative multi-site imaging of asteroid occultations.
Universal high resolution full frame camera with professional connectivity (GPS & fiber optic connections)
also available as photographic version (QHY 268 PH)
InGaAs sensor for detection of a very wide spectrum from 0.4 - 1.7 μm
(QHY991: 25% sensor size compared to QHY990)
covers the visual and near infrared wavelength range
Ideal for Material testing, production monitoring, astronomy
World’s highest resolution cooled scientific CMOS Camera uses a 151 Megapixel Sony IMX411 Back-Illuminated Sensor
largest Sony-CMOS-Sensor in production (required image circle: >67mm)
Second highest resolution and second largest Sony CMOS sensor in production with 102 megapixels (required image circle: >52mm)
General recommendation for ultra-high-end users in observatories
Gpixel square sensor, HDR mode
with Gsense 4040 FSI or BSI CMOS Sensor
Ideal for astronomical, biological, X-ray imaging
Largest detector offered by us (Gpixel)
square, extremely high saturation limit (required image circle: > 87mm))
BSI / FSI Cooled Scientific Camera (varoius versions available) with GSENSE6060 CMOS Sensor
Model
QHY1920
Coming Soon
QHY9701
Coming Soon
QHY1253P
Coming Soon
Special Feature
APS sensor with FullHD output
12μm pixel size and high frame rate
Ideal for low signal video recording
Small sensitive detector from UV to NIR spectrum with large pixels.
Wide spectral sensitivity (200-1000nm)
High dynamic range and HDR readout like QHY 2020/4040/6060
Sensor area 143% larger than QHY550
Polarization filters under the microlenses allow measurement of the degree of polarization
4. QHY CCD Cameras of "A" Series
[product sku="1931100"]
QHYCCD All-in-one cooled CCD camera series has build in filter wheel and the OAG interface. It includes the sensor from 1inch,4/3inch, APS-H format and 36.8*36.8 big format sensors.
We offer the following camera model from QHYCCD:
QHY 90A All-in-One cooled 8.3 megapixel CCD camera with built-in seven-position filter wheel that will hold 36mm round unmounted filters and Butterfly Shutter. Uses the popular KAF-8300 4/3-inch monochrome CCD Sensor.[br]
QHYCCD Light Speed Vision Co. Ltd QHYCCD Light Speed Vision (Beijing) Co., Ltd., founded by Qiu Hongyun, Ph.D., designs and manufactures world-leading astronomical cameras, ranging from entry-level to professional, CMOS and CCD, front-illuminated and back-illuminated, specially crafted for amateur and professional astronomers worldwide.
The QHY product line includes over 40 different models and configurations including scientific cameras. Most of the company’s products are exported to the United States and Europe.
The rich QHY product line is renowned for excellent performance and reliable quality. The sensor arrays used in QHY cameras range from 400,000 pixels to more than 50 megapixels. Sensor format sizes range from 1/4 inch to medium format photography size (61mm diagonal), all with complete independent intellectual property rights.
The QHY line of products include
thermoelectrically cooled cameras,
high- resolution scientific grade cameras,
astronomical imaging cameras,
digital X-ray machine DR cameras, UV photography, infrared photography and medical applications
and solar, industrial and laboratory
The extraordinarily low noise and high sensitivity of QHY CMOS cameras has made them the camera of choice for planetary imaging where stacking and processing numerous frames tremendously improves the image. Moreover, the same low noise cameras facilitate taking and combining shorter exposures of deep space objects to achieve similar results as a single long exposure. This makes it much easier to control guiding corrections and focus in each individual sub-frame and to discard a bad frame when necessary without losing an entire night's work.
As many amateur astronomers can testify, in the case of QHYCCD, affordable does not mean lower quality. QHY cameras have been used by amateurs for nearly 15 years with satisfaction and success. The first
observatory established in China by and for amateurs is Xingming Observatory. Set up and managed by amateur Gao Xing, the observatory is housed at the Nanshan Station of Xinjiang Astronomical Observatory affiliated to the Chinese Academy of Sciences. There are about 280 observable nights per year, with median atmospheric seeing around 1.4". Established in 2007, the observatory offers online access to several telescopes and cameras and is currently conducting several scientific surveys including the NSP (nova search plan), CSP (the comet search plan) and SASP (supernovae and asteroids search plan) and various specialized sub-projects. Observations are carried out almost every clear night. In 2010, a half-meter telescope equipped with a QHY9 camera began running the SASP (Supernova and Asteroid Search Plan). This has since been upgraded with a QHY16 camera. Within a few years, the program has found dozens of supernovae and nearly a hundred asteroids.
Whether you are a professional astronomer or an amateur, whether you are doing research or taking aesthetic images, whether you have a blank check from a well endowed foundation or are on a retiree's budget, QHYCCD has a solution that will help you.
QHY 600 M/C Cooled BSI Camera: The new QHY600 is about to change all of this
QHY600 is a 60mega pixel full frame monochrome color CMOS camera. View details
Unlike some companies that primarily offer one type of camera, either CCD or CMOS, QHYCCD has expertise in development of both types, large and small. The newQHY600 camera ist complete.
QHY600
With the advantage of low readout noise and high-speed readout, CMOS technology has revolutionized astronomical imaging. A monochrome, back-illuminated, high-sensitivity, astronomical imaging camera is the ideal choice for astro-imagers.
However, for years we have only seen the 4/3-inch, front-illuminated, monochrome cameras (QHY163M) with QE of about 60%, and one-inch, back-illuminated, monochrome cameras (QHY183M) with higher QE. Although these sensors are quite good and very suitable for beginners, they are still smaller than the full frame (35mm format) sensors desired for more serious deep sky astrophotography. Also, both of these sensors have 12-bit A/D. To achieve 1e- of read noise you must increase the gain and lose some dynamic range in the process, or you use low gain and lose some precision in sampling and greyscale levels.
The new QHY600 is about to change all of this. The QHY600 uses the latest SONY back-illuminated sensor, the IMX455, a full frame (35mm format) sensor with 3.76um pixels and native 16-bit A/D. This sensor is available in both monochrome and color versions. The QHY600 ends the days of non-16bit CMOS cameras and it ends the days non-full frame (and larger) monochrome CMOS cameras.
The most versatile tools: Baader Star Diagonals (T-2 and 2")
A Baader star diagonal (both prisms and mirrors) can show you impressive images for a lifetime and offers more connection and configuration options than standard star diagonals.
Baader Planetarium's star diagonals not only offer the highest mechanical and optical quality, but also have the additional advantage of being part of a large, modular system. They enable very short adaptations as well as threads for direct connections to a telescope or a Baader focuser, as well as adaptation to a wide range of threads for torsion-free use with heavy or long accessories, such as binoviewers.
Decades of customer feedback led Baader Planetarium to create a seemingly overwhelming amount of adapters. But each adapter has its purpose. This is the reason why you can always find the optical length of each part in the product description, so that you can find the best solution for your needs.
To get the most out of them, we recommend that you spend a few minutes reading this brochure.
On the following pages you will find
a guide on how to choose coating and star diagonal type
an overview of the different models,
connection options to the telescope,
an overview of the eyepiece/camera side connection options
and a tabular comparison of the different models.
Please note: since January 2020 included with all 2" BBHS star diagonals: [product sku="2408156"] with Baader proprietory Safety Kerfs for additional grip and security from inadvertent slipping.
[product sku="2458055"]
If you are looking for an even more flexible solution, take a look at the [product sku="2458055"] – its user manual shows how you can connect e.g. camera, eyepiece, autoguider or even a spectrograph at the same time!
[product sku="2957165"], Baader BDS Diamond Steeltrack® and Nikon DSLR-camera attached to a Baader Apo 95/560 Travel Companion on a 10Micron GM 1000 HPS Mount
One Controller for several motor units with SteelGo II Software
With a [product sku="2957165"], you can automatically control your focuser with a computer as well as use the keys of the hand control for precise, vibration-free focusing.
The Steeldrive II consists of a motor unit, which is connected with a timing belt to the focuser's slow-motion-control to work without backlash, and of a control unit with the electronics, which also doubles as hand control. This modular design means that you can equip each of your telescopes with its own motor unit and only need one controller, which you connect to the telescope you are currently using. Only if you operate several telescopes at the same time, then you need several controllers.
SteelDrive II Motor unit and Controller now available separtately
The latest version of the SteelGo II Software for controlling the SteelDrive II motor focuser offers the possibility to comfortably store the data of any number of telescopes (each with its own motor) with its own bookmarks, temperature compensation coefficients and much more and to control them with only one single controller. [br]
[product sku="2957260"]
[product sku="2957265"]
The settings are automatically updated when connecting to the [product sku="2957260"].
This allows you to equip several telescopes with one motor each when using several telescopes. However, only one controller is necessary, which is used alternately. This reduces the purchase costs for several telescopes considerably.[br]
The download archive contains theSteelGo II 32- and 64-bit versions, the latest firmware version as well as the SteelDrive II Firmware UpdateTool to update the firmware. Please update your Controller to version 1.1 - please note the hints in the ReadMe file
The image sensor - the heart of EVERY astronomical CMOS camera
In the many years since the foundation of QHYCCD, engineers and developers have gained experience with CMOS sensors in numerous camera models, thus optimizing hardware and software. You buy this "know-how" with every QHY CMOS or CCD camera.
For a beginner, it can be confusing to choose the right camera to start with. We therefore advise you to proceed step by step, starting with the equipment that allows to track (guiding) a telescope mount in such a way that your first attempts will also show pinpoint star images.
