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Bintel Glebe
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Bintel 84 Wentworth park road, Glebe, 2073, NSW
Phone:(02) 9518 7255
Hours:
Monday9:30 am–5:30 pm
Tuesday9:30 am–5:30 pm
Wednesday9:30 am–5:30 pm
Thursday9:30 am–5:30 pm
Friday9:30 am–5:30 pm
Saturday9:30 am–4 pm
SundayClosed
Deep sky Cameras
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$2,799.00
There's lots of advantages of using a CCD chip for deep-sky imaging compared to CMOS cameras.
Please note this camera uses a "Grade 1" CCD chip.
Specifications
- Built-in autoguider output – compatible with most mounts.
- Built-in triple USB hub ports for accessory control – directly drive filter wheels, GOTO ‘scopes etc.
- Single USB cable control for all features – get rid of that dangerous cable tangle!
- Two stage cooler with dry Argon filled CCD chamber.
- Very low power consumption. Less than 1.5 amps at 12v DC.
- Compact and lightweight – only 75mm in diameter x 70mm long – less than 500 grams load on the telescope.
- CCD type: Sony ICX674ALQ (colour) EXview CCD with ultra low dark current and vertical anti-blooming.
- CCD Full resolution pixel data: Pixel size: 4.54uM x 4.54uM, Image format: 1940 x 1460 pixels
- CCD Image area: 8.81mm (Horizontal) x 6.63mm (Vertical).
- CCD quality: Grade 1 or better – No bad columns, no dead pixels, no more than 50 ‘hot’ pixels (saturated in <10 seconds).
- Spectral Response: QE max at 580nM (~77%), 50% roll-off at 360nM and 770nM.
- Readout Noise: Typically only 3.5 electrons RMS
- Full-well capacity: Greater than 17,000 e- (unbinned)
- Anti-blooming: Overload margin greater than 800x.
- Dark current: Less than 0.003 electrons/second @ – 10C CCD temperature.
- Data format: 16 bits.
- System gain: 0.3 electrons per ADU
- Computer Interface: Built-in USB 2.0 compatible interface.
- Image download time: Typically 2 seconds at full resolution.
- Power requirements: 240VAC @ 12VA, or 12VDC @ 900mA max.
- Cooling system: Regulated set-point cooling supply with thermoelectric cooler to give a minimum CCD temperature of approximately -40C below ambient.
- Size: 75 x 70mm black anodised aluminium barrel with 42mm ‘T2’ thread at the CCD window end & input/output plugs at rear. CCD alignment screws are provided for setting the chip parallel to the focal plane.
- Weight: approx. 450g.
PRODUCT MANUAL Trius-PRO-674C-handbook
PRODUCT DATASHEET 2022-SX-TRIUS-PRO-Blue-Camera-Specification
$2,799.00
There's lots of advantages of using a CCD chip for deep-sky imaging compared to CMOS cameras. If you'd like to know more, read BINTEL's tech article here.
Please note this camera uses a "Grade 1" CCD chip.
Specifications
- CCD type: Sony ICX674ALG (mono) EXview CCD with ultra low dark current and vertical anti-blooming.
- CCD Full resolution pixel data: Pixel size: 4.54uM x 4.54uM, Image format: 1940 x 1460 pixels
- CCD Image area: 8.81mm (Horizontal) x 6.63mm (Vertical).
- CCD quality: Grade 1 or better – No bad columns, no dead pixels, no more than 50 ‘hot’ pixels (saturated in <10 seconds).
- Spectral Response: QE max at 580nM (~77%), 50% roll-off at 360nM and 770nM.
- Readout Noise: Typically only 3.5 electrons RMS
- Full-well capacity: Greater than 17,000 e- (unbinned)
- Anti-blooming: Overload margin greater than 800x.
- Dark current: Less than 0.003 electrons/second @ – 10C CCD temperature.
- Data format: 16 bits.
- System gain: 0.3 electrons per ADU
- Computer Interface: Built-in USB 2.0 compatible interface.
- Image download time: Typically 2 seconds at full resolution.
- Power requirements: 115VAC / 240VAC @ 12VA, or 12VDC @ 900mA max.
- Cooling system: Regulated set-point cooling supply with thermoelectric cooler to give a minimum CCD temperature of approximately -40C below ambient.
- Size: 75 x 70mm black anodised aluminium barrel with 42mm ‘T2’ thread at the CCD window end & input/output plugs at rear. CCD alignment screws are provided for setting the chip parallel to the focal plane.
- Weight: approx. 450g.
PRODUCT MANUAL Trius-PRO-674-handbook
PRODUCT DATASHEET 2022-SX-TRIUS-PRO-Blue-Camera-Specification
$4,899.00
Overview
- Very large, high resolution ‘SuperHAD’ CCD chip, with 6,000,000 x 7.8uM square pixels in a 23.4 x 15.6mm array. Size equivalent to APS film.
- Single-shot colour, using a Bayer matrix of R, G and B on-chip filters. No filter wheel required.
- Triple USB hub for accessories, built-in.
- High performance two stage cooler for better than -35 C chip temperature reduction.
- Dry Argon chamber fill for improved cooling performance.
- Exceptionally low dark signal – No dark frames necessary for most deep sky objects.
- Exceptionally effective anti-blooming with minimal effect on linearity and no lost active area.
- High sensitivity, equivalent to 60% QE at peak of green filters.
- Back focal length 17mm +/-1mm.
- NEW! Built-in super high speed USB 2.0 interface (USB 1.1 compatible) for approx. 3.5 second downloads.
- Built-in autoguider output.
- Single USB cable control for all features – get rid of that dangerous cable tangle!
- Only ONE computer needed to control all of the devices and functions.
- Very low power consumption. Less than 1.5 amps at 12v DC.
- Compact and lightweight – only 75mm in diameter x 100mm long – less than 500 grams load on the ‘scope.
Specifications:
- CCD type: Sony ICX453AQ SuperHAD CCD with ultra low dark current, Bayer RGB matrix and vertical anti-blooming.
- CCD Full resolution Pixel data: Pixel size: 7.8uM x 7.8uM, Image format: 3024 x 2016 pixels
- CCD Image area: 23.4mm (Horizontal) x 15.6mm (Vertical).
- CCD quality: Grade 1 or better – No bad columns, no dead pixels, no more than 50 ‘hot’ pixels (saturated in <10 seconds).
- Spectral Response: QE max at 540nM (~60%), 50% roll-off at 400nM and 650nM.
- Readout Noise: Less than 12 electrons RMS – typically ONLY 7 electrons!
- Full-well capacity: Greater than 25,000 e- (unbinned)
- Anti-blooming: Overload margin greater than 800x.
- Dark current: Dark frame saturation time greater than 100 hours. Less than 0.02 electrons/second @ + 10C ambient.
- Data format: 16 bits.
- System gain: 0.4 electrons per ADU
- Computer Interface: Built-in USB 2.0 compatible interface. Also works with USB 1.1.
- Image download time: Typically 3.5 seconds full resolution using USB 2.0, approximately 8 seconds with USB 1.1.
- Power requirements: 115VAC / 240VAC @ 12VA, or 12VDC @ 1.5 A max.
- Cooling system: Regulated constant current cooling supply with two stage thermoelectric cooler to give a CCD temperature of approximately -35C below ambient.
- Size: 75 x 70mm black anodised aluminium barrel with 42mm ‘T2’ thread at the CCD window end & input/output plugs at rear. CCD alignment screws are provided for setting the chip parallel to the focal plane.
- Weight: approx. 400g
NEW Smart Deep-sky imaging camera from ZWO with Guiding, Imaging and Smart Control of mounts and accessories.
Main Camera Sensor
The main camera sensor is the popular Sony IMX571 featuring an APS-C format and 26MP total pixels. The size is 23.5mm in width x 15.7mm in height, and the diagonal is 28.3mm. The 3.76um x 3.76um small pixel size accommodates an impressive full depth of 50ke. With the new hardware technology, it is even extended to 73ke
Guide Camera Sensor
The SC2210 sensor taken from the ASI220MM Mini camera features very high sensitivity. The QE peak value reaches 92% at 500nm. The read noise is as low as 0.6e. As the new generation of guide sensor, it has achieved great results in guiding, proved by hundreds of astrophotographers.
Enjoy the Beauty of the Night Sky Anywhere. In the city, suburbs or under dark Aussie skies
Take the hassles out of your your Astrophotography Journey
The ASI2600MC Air combines guiding, imaging, and smart control into one compact, lightweight device. Say goodbye to complex setups and enjoy a seamless, hassle-free astrophotography experience.
Easily Connect Multiple Devices
4x USB2.0, 3x DC12V 10A, 1x USB Type-C
USB 2.0 ports for your focuser, filter wheel, and mount; DC 12V 10A input/output ports for reliable power; and USB Type-C port for fast file transfers—you can focus on capturing stunning images without worrying about connectivity issues.
Shoot with Confidence: Ample Storage and Stability
With a massive 256GB eMMC storage, the ASI2600MC Air allows you to capture multiple targets with ease. Rigorously tested with over 300 benchmarks, it ensures system stability. Plus, the USB 2.0 ports support up to 1TB external storage, giving you plenty of room for all your astrophotography needs.
Dive into the Rich Details of the Celestial Targets
In expanded mode, the full well capacity of this camera reaches 73Ke, which is 1.46 times of that of the IMX571 sensor (51ke), making long-exposure shots less prone to overexposure. The large full well capacity and high dynamic range make capturing both light and dark areas with stunning clarity and detail possible. Witness the miracle details and colours of targets like never before!
Dual-Band Wi-Fi for a stable, solid connection
Experience unparalleled connectivity with our enhanced external dual-band antenna, supporting both 2.4G and 5G frequencies and offering stable and smooth usage within 20 metres.
Cross-Platform Device Control
Apart from from the ASIAIR App, ASI2600MC Air can also wirelessly connect to ZWO’s proprietary PC control software, ASIStudio, and also other 3rd-party PC software. 3rd-party software can be controlled through ASCOM extended protocol Alpaca (requires ASCOM Platform version V6.6 or higher).
Bluetooth Connection Supported
Nice and Neat Wiring with ZWO AM3/AM5 mounts
Get Fully Control of Your Entire Rig at Your Fingertips
With the ASIAIR smart app, you can easily control guiding, imaging, your mount, and electronic focuser—all from your phone. It supports multiple imaging modes, making it easy for even beginners to quickly learn and capture professional-quality images.
Instant Post-Processing and Sharing
Live stack is supported during your imaging session. You may also make adjustments to brightness, contrast and others on the final image. Instantly share your masterpieces on social media platforms and astronomy communities, making your work stand out.
Go Further With ZWO’s Self-Developed System
Powered by ZWO’s patented technologies, our system ensures stable astrophotography performance. Continuous App OTA updates keep your device up-to-date with the latest features, enhancing your user experience and expanding your capabilities.
QE value
Main Sensor
Guide Sensor
Dark Current
Power Consumption
IR-Cut coating for OSC camera
Frame Rate
Camera Specifications
The best solution to achieve 55mm back focus length
Mechanical Diagram
What is in the box?
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. The QHY600M-L 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 QHY600M-PH SBFL ends the days of non-16bit CMOS cameras and it ends the days non-full frame (and larger) monochrome CMOS cameras.
The QHY600M-L has extremely low dark current (0.002e/p/s@-20C) using SONY’s Exmor BSI CMOS technology. QHY600M-PH SBFL is also a zero amplifer glow camera. The QHY600M-PH SBFL has only one electron of read noise at high gain and full resolution and 4FPS readout speed. One electron of read noise means the camera can achieve a SNR>3 at only 4 to 6 photons. This is perfect performance when conditions are photon limited, i.e., short exposures, narrow band imaging, etc., making this large area sensor ideal for sky surveys, time domain astronomy, fluorescence imaging, DNA sequencing and microscopy.
Models
QHY600 Series have mutiple models which covers both photographic and scientific using. Below list different types of QHY600 PH (photographic) series:
QHY600PH : Standard version for amateur astrographers;
2GB DDR3 image buffer
In order to provide smooth uninterrupted data transfer of the entire 60MP sensor at high speed, the QHY600 has 2GB DDR3 image buffer. The pixel count of the latest generation of CMOS sensors is very high resulting in greater memory requirements for temporary and permanent storage. For example, the QHY600 sensor produces about 120MB of data per frame. The data band-width is also increased from the original 16-bits to the current 32-bits. Transferring such a large file sizes necessarily requires the camera to have sufficient memory. The QHY600 has adopted a large-capacity memory of up to 2GB. Data throughput is doubled. This large image buffer meets the needs of high-speed image acquisition and transmission of the new generation of CMOS, making shooting of multiple frames smoother and less stuttered, further reducing the pressure on the computer CPU.
Another advantage is that when using some computers that do not have fast processors or have poor support for USB 3.0, the computer can’t transfer high-speed data well, and the data is often lost. The DDR can buffer a lot of image data and send it to the computer. Even if the USB 3.0 transmission frequently gets suspended, it will ensure that data is not lost. There are options in SharpCap to turn DDR buffering on or off. The current version of the ASCOM driver works in DDR mode.
Native 16 bit A/D: The new Sony sensor has native 16-bit A/D on-chip. The output is real 16-bits with 65536 levels. Compared to 12-bit and 14-bit A/D, a 16-bit A/D yields higher sample resolution and the system gain will be less than 1e-/ADU with no sample error noise and very low read noise.
BSI: One benefit of the back-illuminated CMOS structure is improved full well capacity. This is particularly helpful for sensors with small pixels. In a typical front-illuminated sensor, photons from the target entering the photosensitive layer of the sensor must first pass through the metal wiring that is embedded just above the photosensitive layer. The wiring structure reflects some of the photons and reduces the efficiency of the sensor. In the back- illuminated sensor the light is allowed to enter the photosensitive surface from the reverse side. In this case the sensor’s embedded wiring structure is below the photosensitive layer. As a result, more incoming photons strike the photosensitive layer and more electrons are generated and captured in the pixel well. This ratio of photon to electron production is called quantum efficiency. The higher the quantum efficiency the more efficient the sensor is at converting photons to electrons and hence the more sensitive the sensor is to capturing an image of something dim.
Zero Amplify Glow: This is also a zero amplifer glow camera.
TRUE RAW Data: In the DSLR implementation there is a RAW image output, but typically it is not completely RAW. Some evidence of noise reduction and hot pixel removal is still visible on close inspection. This can have a negative effect on the image for astronomy such as the “star eater” effect. However, QHY Cameras offer TRUE RAW IMAGE OUTPUT and produces an image comprised of the original signal only, thereby maintaining the maximum flexibility for post-acquisition astronomical image processing programs and other scientific imaging applications.
Anti-Dew Technology: Based on almost 20-year cooled camera design experience, The QHY cooled camera has implemented the fully dew control solutions. The optic window has built-in dew heater and the chamber is protected from internal humidity condensation. An electric heating board for the chamber window can prevent the formation of dew and the sensor itself is kept dry with our silicon gel tube socket design for control of humidity within the sensor chamber.
Cooling: In addition to dual stage TE cooling, QHYCCD implements proprietary technology in hardware to control the dark current noise.
Multiple Readout Modes are special for QHY 16-bit Cameras (QHY600/268/461/411). Different readout modes have different driver timing, etc., and result in different performance. See details at “Multiple Readout Modes and Curves” Part.
You may find some types of thermal noise can change with time in some back-illuminated CMOS cameras. This thermal noises has the characteristic of the fixed position of typical thermal noise, but the value is not related to the exposure time. Instead, each frame appears to have its own characteristics. The QHY600/268/461/411 use an innovative suppression technology that can significantly reduce the apparent level of such noise.
UVLO（Under Voltage Locking) is to protect the electronic device from damage caused by abnormally low voltages.
Our daily life experience tells us that the actual operational voltage of an electrical device must not significantly exceed the rated voltage, otherwise it will be damaged. For such precision equipment as cameras, long-term work at too low input voltage can also be detrimental to the working life of the camera, and may even make some devices, such as power manager, burn up due to long-term overload. In the all-in-one driver and SDK after 2021.10.23 stable version, the camera will give a warning when the input voltage of the camera is below 11V.
It is common behavior for a CMOS sensor to contain some horizontal banding. Normally, random horizontal banding can be removed with multiple frame stacking so it does not affect the final image. However, periodic horizontal banding is not removed with stacking so it may appear in the final image. By adjust the USB traffic in Single Frame mode or Live Frame mode, you can adjust the frequency of the CMOS sensor driver and it can optimize the horizontal banding appeared on the image. This optimized is very effective to remove the periodic banding in some conditions.
A typical Periodic Horizontal Noise under certain USB_TRAFFIC values.
The camera is designed to use the +12V to reboot the camera without disconnecting and reconnecting the USB interface. This means that you can reboot the camera simply by shutting down the +12V and then powering it back on. This feature is very handy for remote controlling the camera in an observatory. You can use a remotely controlled power supply to reboot the camera. There is no need to consider how to reconnect the USB in the case of remote control.
Specifications
| Model |
QHY600PH (Photographic Version)
QHY600PH SBFL (Short Back Focal Length Version) QHY600PH L (Lite Version) |
| CMOS Sensor | SONY IMX455 |
| Mono/Color | Both Available (while Mono only with QHY600PH-L) |
| FSI/BSI | BSI |
| Pixel Size | 3.76um x 3.76um |
| Effective Pixel Area | 9576*6388
（9600*6422 with overscan and optically black area) |
| Effective Pixels | 61.17 Megapixels (effective area. |
| Sensor Size | Full Frame 36mm x 24mm |
| A/D Sample Depth
|
16-bit (0-65535 levels) at 1X1 binning
18-bit at 2X2, 19-bit at 3X3, 20-bit at 4X4 software binning *QHY600 uses the software digital binning for 2*2binning. With digital sum, 2*2binning will be four 16-bit summed then it is 18-bit. |
| Full Well Capacity (1×1, 2×2, 3×3) | Standard Mode >51ke- / >204ke- / >408ke- Super Full Well Mode >80ke- / >320ke- / >720ke- |
| Full Frame Rate | USB3.0 Port Image Transfer Speed
Full Frame Size: 4.0FPS (8-bit output) Full Frame Size: 2.5FPS (16-bit output) 7.2FPS at 9600×3194, 22.5FPS at 9600×1080, 28FPS at 9600×768, 47FPS at 9600×480, 160FPS at 9600×100, Fiber Port Image Transfer Speed (QHY600Pro only) Full Frame Size: 4.0FPS (16-bit output) |
| Readout Noise | 1.0e- to 3.7e- (Standard Mode) |
| Dark Current | 0.0022e-/p/s @ -20C 0.0046e-/p/s @ -10C |
| Exposure Time Range | 40us – 3600sec |
| Unity Gain* | 25 (Extended Full Well Mode) *
*With the improvement of the CMOS technology, the 16bit CMOS camera has been released, like QHY600/268/411/461. For these cameras, even in lowest gain it has beyond the requirement of unit gain (less than 1e/ADU due to sufficient samples) So you can directly set gain 0 as start. Please note QHY600/268C/411/461 has extend full well mode. In this mode you still need to find out the unit gain position. |
| Amp Control | Zero Amplifer Glow |
| Firmware/FPGA remote Upgrade | Supported. Via Camera USB Port |
| Shutter Type | Electric Rolling Shutter |
| Computer Interface | USB3.0 |
| Built-in Image Buffer | DDR3 memory
PH & PH SBFL ver.: 2GBytes |
| Hardware Frame Sequence Number | Supported |
| Cooling System | Dual Stage TEC cooler: – Long exposures (> 1 second) typically -35C below ambient – Short exposure (< 1second) high FPS, typically -30C below ambient（Test temperature +20°） |
| Optic Window Type | AR+AR High Quality Multi-Layer Anti-Reflection Coating |
| Anti-Dew Heater | Yes |
| Telescope Interface | M54/0.75 |
| Back Focal Length | QHY600PH&QHYPH-L: 17.5mm+6mm (±0.2)
QHY600SBFL: 14.5mm* *The BFL Consumed equals 12.5mm when connecting QHYCFW. About the defination of “BFL Comsumed” and our adapter system please view: https://www.qhyccd.com/adapters/ |
| Weigth | PH Version: 850g Lite Version: 790g |
| Power | 40W/100% 20W/50% 13.8W/0% |
Camera Curves
The curve shows absolute QE
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. The QHY600M-L 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 QHY600M-PH ends the days of non-16bit CMOS cameras and it ends the days non-full frame (and larger) monochrome CMOS cameras.
The QHY600M-L has extremely low dark current (0.002e/p/s@-20C) using SONY’s Exmor BSI CMOS technology. QHY600M-PH is also a zero amplifer glow camera. The QHY600M-PH has only one electron of read noise at high gain and full resolution and 4FPS readout speed. One electron of read noise means the camera can achieve a SNR>3 at only 4 to 6 photons. This is perfect performance when conditions are photon limited, i.e., short exposures, narrow band imaging, etc., making this large area sensor ideal for sky surveys, time domain astronomy, fluorescence imaging, DNA sequencing and microscopy.
Models
QHY600 Series have mutiple models which covers both photographic and scientific using. Below list different types of QHY600 PH (photographic) series:
QHY600PH : Standard version for amateur astrographers;
2GB DDR3 image buffer
In order to provide smooth uninterrupted data transfer of the entire 60MP sensor at high speed, the QHY600 has 2GB DDR3 image buffer. The pixel count of the latest generation of CMOS sensors is very high resulting in greater memory requirements for temporary and permanent storage. For example, the QHY600 sensor produces about 120MB of data per frame. The data band-width is also increased from the original 16-bits to the current 32-bits. Transferring such a large file sizes necessarily requires the camera to have sufficient memory. The QHY600 has adopted a large-capacity memory of up to 2GB. Data throughput is doubled. This large image buffer meets the needs of high-speed image acquisition and transmission of the new generation of CMOS, making shooting of multiple frames smoother and less stuttered, further reducing the pressure on the computer CPU.
Another advantage is that when using some computers that do not have fast processors or have poor support for USB 3.0, the computer can’t transfer high-speed data well, and the data is often lost. The DDR can buffer a lot of image data and send it to the computer. Even if the USB 3.0 transmission frequently gets suspended, it will ensure that data is not lost. There are options in SharpCap to turn DDR buffering on or off. The current version of the ASCOM driver works in DDR mode.
Native 16 bit A/D: The new Sony sensor has native 16-bit A/D on-chip. The output is real 16-bits with 65536 levels. Compared to 12-bit and 14-bit A/D, a 16-bit A/D yields higher sample resolution and the system gain will be less than 1e-/ADU with no sample error noise and very low read noise.
BSI: One benefit of the back-illuminated CMOS structure is improved full well capacity. This is particularly helpful for sensors with small pixels. In a typical front-illuminated sensor, photons from the target entering the photosensitive layer of the sensor must first pass through the metal wiring that is embedded just above the photosensitive layer. The wiring structure reflects some of the photons and reduces the efficiency of the sensor. In the back- illuminated sensor the light is allowed to enter the photosensitive surface from the reverse side. In this case the sensor’s embedded wiring structure is below the photosensitive layer. As a result, more incoming photons strike the photosensitive layer and more electrons are generated and captured in the pixel well. This ratio of photon to electron production is called quantum efficiency. The higher the quantum efficiency the more efficient the sensor is at converting photons to electrons and hence the more sensitive the sensor is to capturing an image of something dim.
Zero Amplify Glow: This is also a zero amplifer glow camera.
TRUE RAW Data: In the DSLR implementation there is a RAW image output, but typically it is not completely RAW. Some evidence of noise reduction and hot pixel removal is still visible on close inspection. This can have a negative effect on the image for astronomy such as the “star eater” effect. However, QHY Cameras offer TRUE RAW IMAGE OUTPUT and produces an image comprised of the original signal only, thereby maintaining the maximum flexibility for post-acquisition astronomical image processing programs and other scientific imaging applications.
Anti-Dew Technology: Based on almost 20-year cooled camera design experience, The QHY cooled camera has implemented the fully dew control solutions. The optic window has built-in dew heater and the chamber is protected from internal humidity condensation. An electric heating board for the chamber window can prevent the formation of dew and the sensor itself is kept dry with our silicon gel tube socket design for control of humidity within the sensor chamber.
Cooling: In addition to dual stage TE cooling, QHYCCD implements proprietary technology in hardware to control the dark current noise.
Multiple Readout Modes are special for QHY 16-bit Cameras (QHY600/268/461/411). Different readout modes have different driver timing, etc., and result in different performance. See details at “Multiple Readout Modes and Curves” Part.
You may find some types of thermal noise can change with time in some back-illuminated CMOS cameras. This thermal noises has the characteristic of the fixed position of typical thermal noise, but the value is not related to the exposure time. Instead, each frame appears to have its own characteristics. The QHY600/268/461/411 use an innovative suppression technology that can significantly reduce the apparent level of such noise.
UVLO（Under Voltage Locking) is to protect the electronic device from damage caused by abnormally low voltages.
Our daily life experience tells us that the actual operational voltage of an electrical device must not significantly exceed the rated voltage, otherwise it will be damaged. For such precision equipment as cameras, long-term work at too low input voltage can also be detrimental to the working life of the camera, and may even make some devices, such as power manager, burn up due to long-term overload. In the all-in-one driver and SDK after 2021.10.23 stable version, the camera will give a warning when the input voltage of the camera is below 11V.
It is common behavior for a CMOS sensor to contain some horizontal banding. Normally, random horizontal banding can be removed with multiple frame stacking so it does not affect the final image. However, periodic horizontal banding is not removed with stacking so it may appear in the final image. By adjust the USB traffic in Single Frame mode or Live Frame mode, you can adjust the frequency of the CMOS sensor driver and it can optimize the horizontal banding appeared on the image. This optimized is very effective to remove the periodic banding in some conditions.
A typical Periodic Horizontal Noise under certain USB_TRAFFIC values.
The camera is designed to use the +12V to reboot the camera without disconnecting and reconnecting the USB interface. This means that you can reboot the camera simply by shutting down the +12V and then powering it back on. This feature is very handy for remote controlling the camera in an observatory. You can use a remotely controlled power supply to reboot the camera. There is no need to consider how to reconnect the USB in the case of remote control.
Specifications
| Model |
QHY600PH (Photographic Version)
QHY600PH SBFL (Short Back Focal Length Version) QHY600PH L (Lite Version) |
| CMOS Sensor | SONY IMX455 |
| Mono/Color | Both Available (while Mono only with QHY600PH-L) |
| FSI/BSI | BSI |
| Pixel Size | 3.76um x 3.76um |
| Effective Pixel Area | 9576*6388
（9600*6422 with overscan and optically black area) |
| Effective Pixels | 61.17 Megapixels (effective area. |
| Sensor Size | Full Frame 36mm x 24mm |
| A/D Sample Depth
|
16-bit (0-65535 levels) at 1X1 binning
18-bit at 2X2, 19-bit at 3X3, 20-bit at 4X4 software binning *QHY600 uses the software digital binning for 2*2binning. With digital sum, 2*2binning will be four 16-bit summed then it is 18-bit. |
| Full Well Capacity (1×1, 2×2, 3×3) | Standard Mode >51ke- / >204ke- / >408ke- Super Full Well Mode >80ke- / >320ke- / >720ke- |
| Full Frame Rate | USB3.0 Port Image Transfer Speed
Full Frame Size: 4.0FPS (8-bit output) Full Frame Size: 2.5FPS (16-bit output) 7.2FPS at 9600×3194, 22.5FPS at 9600×1080, 28FPS at 9600×768, 47FPS at 9600×480, 160FPS at 9600×100, Fiber Port Image Transfer Speed (QHY600Pro only) Full Frame Size: 4.0FPS (16-bit output) |
| Readout Noise | 1.0e- to 3.7e- (Standard Mode) |
| Dark Current | 0.0022e-/p/s @ -20C 0.0046e-/p/s @ -10C |
| Exposure Time Range | 40us – 3600sec |
| Unity Gain* | 25 (Extended Full Well Mode) *
*With the improvement of the CMOS technology, the 16bit CMOS camera has been released, like QHY600/268/411/461. For these cameras, even in lowest gain it has beyond the requirement of unit gain (less than 1e/ADU due to sufficient samples) So you can directly set gain 0 as start. Please note QHY600/268C/411/461 has extend full well mode. In this mode you still need to find out the unit gain position. |
| Amp Control | Zero Amplifer Glow |
| Firmware/FPGA remote Upgrade | Supported. Via Camera USB Port |
| Shutter Type | Electric Rolling Shutter |
| Computer Interface | USB3.0 |
| Built-in Image Buffer | DDR3 memory
PH & PH SBFL ver.: 2GBytes |
| Hardware Frame Sequence Number | Supported |
| Cooling System | Dual Stage TEC cooler: – Long exposures (> 1 second) typically -35C below ambient – Short exposure (< 1second) high FPS, typically -30C below ambient（Test temperature +20°） |
| Optic Window Type | AR+AR High Quality Multi-Layer Anti-Reflection Coating |
| Anti-Dew Heater | Yes |
| Telescope Interface | M54/0.75 |
| Back Focal Length | QHY600PH&QHYPH-L: 17.5mm+6mm (±0.2)
QHY600SBFL: 14.5mm* *The BFL Consumed equals 12.5mm when connecting QHYCFW. About the defination of “BFL Comsumed” and our adapter system please view: https://www.qhyccd.com/adapters/ |
| Weigth | PH Version: 850g Lite Version: 790g |
| Power | 40W/100% 20W/50% 13.8W/0% |
Camera Curves
The curve shows absolute QE
$6,610.00
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. The QHY600M-L 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 QHY600M-L has extremely low dark current (0.002e/p/s@-20C) using SONY’s Exmor BSI CMOS technology. QHY600M-L is also a zero amplifer glow camera. The QHY600M-L has only one electron of read noise at high gain and full resolution and 4FPS readout speed. One electron of read noise means the camera can achieve a SNR>3 at only 4 to 6 photons. This is perfect performance when conditions are photon limited, i.e., short exposures, narrow band imaging, etc., making this large area sensor ideal for sky surveys, time domain astronomy, fluorescence imaging, DNA sequencing and microscopy.
Models
QHY600 Series have mutiple models which covers both photographic and scientific using. Below list different types of QHY600 PH (photographic) series:
QHY600PH : Standard version for amateur astrographers;
2GB DDR3 image buffer
In order to provide smooth uninterrupted data transfer of the entire 60MP sensor at high speed, the QHY600 has 2GB DDR3 image buffer. The pixel count of the latest generation of CMOS sensors is very high resulting in greater memory requirements for temporary and permanent storage. For example, the QHY600 sensor produces about 120MB of data per frame. The data band-width is also increased from the original 16-bits to the current 32-bits. Transferring such a large file sizes necessarily requires the camera to have sufficient memory. The QHY600 has adopted a large-capacity memory of up to 2GB. Data throughput is doubled. This large image buffer meets the needs of high-speed image acquisition and transmission of the new generation of CMOS, making shooting of multiple frames smoother and less stuttered, further reducing the pressure on the computer CPU.
Another advantage is that when using some computers that do not have fast processors or have poor support for USB 3.0, the computer can’t transfer high-speed data well, and the data is often lost. The DDR can buffer a lot of image data and send it to the computer. Even if the USB 3.0 transmission frequently gets suspended, it will ensure that data is not lost. There are options in SharpCap to turn DDR buffering on or off. The current version of the ASCOM driver works in DDR mode.
Native 16 bit A/D: The new Sony sensor has native 16-bit A/D on-chip. The output is real 16-bits with 65536 levels. Compared to 12-bit and 14-bit A/D, a 16-bit A/D yields higher sample resolution and the system gain will be less than 1e-/ADU with no sample error noise and very low read noise.
BSI: One benefit of the back-illuminated CMOS structure is improved full well capacity. This is particularly helpful for sensors with small pixels. In a typical front-illuminated sensor, photons from the target entering the photosensitive layer of the sensor must first pass through the metal wiring that is embedded just above the photosensitive layer. The wiring structure reflects some of the photons and reduces the efficiency of the sensor. In the back- illuminated sensor the light is allowed to enter the photosensitive surface from the reverse side. In this case the sensor’s embedded wiring structure is below the photosensitive layer. As a result, more incoming photons strike the photosensitive layer and more electrons are generated and captured in the pixel well. This ratio of photon to electron production is called quantum efficiency. The higher the quantum efficiency the more efficient the sensor is at converting photons to electrons and hence the more sensitive the sensor is to capturing an image of something dim.
Zero Amplify Glow: This is also a zero amplifer glow camera.
TRUE RAW Data: In the DSLR implementation there is a RAW image output, but typically it is not completely RAW. Some evidence of noise reduction and hot pixel removal is still visible on close inspection. This can have a negative effect on the image for astronomy such as the “star eater” effect. However, QHY Cameras offer TRUE RAW IMAGE OUTPUT and produces an image comprised of the original signal only, thereby maintaining the maximum flexibility for post-acquisition astronomical image processing programs and other scientific imaging applications.
Anti-Dew Technology: Based on almost 20-year cooled camera design experience, The QHY cooled camera has implemented the fully dew control solutions. The optic window has built-in dew heater and the chamber is protected from internal humidity condensation. An electric heating board for the chamber window can prevent the formation of dew and the sensor itself is kept dry with our silicon gel tube socket design for control of humidity within the sensor chamber.
Cooling: In addition to dual stage TE cooling, QHYCCD implements proprietary technology in hardware to control the dark current noise.
Multiple Readout Modes are special for QHY 16-bit Cameras (QHY600/268/461/411). Different readout modes have different driver timing, etc., and result in different performance. See details at “Multiple Readout Modes and Curves” Part.
You may find some types of thermal noise can change with time in some back-illuminated CMOS cameras. This thermal noises has the characteristic of the fixed position of typical thermal noise, but the value is not related to the exposure time. Instead, each frame appears to have its own characteristics. The QHY600/268/461/411 use an innovative suppression technology that can significantly reduce the apparent level of such noise.
UVLO（Under Voltage Locking) is to protect the electronic device from damage caused by abnormally low voltages.
Our daily life experience tells us that the actual operational voltage of an electrical device must not significantly exceed the rated voltage, otherwise it will be damaged. For such precision equipment as cameras, long-term work at too low input voltage can also be detrimental to the working life of the camera, and may even make some devices, such as power manager, burn up due to long-term overload. In the all-in-one driver and SDK after 2021.10.23 stable version, the camera will give a warning when the input voltage of the camera is below 11V.
It is common behavior for a CMOS sensor to contain some horizontal banding. Normally, random horizontal banding can be removed with multiple frame stacking so it does not affect the final image. However, periodic horizontal banding is not removed with stacking so it may appear in the final image. By adjust the USB traffic in Single Frame mode or Live Frame mode, you can adjust the frequency of the CMOS sensor driver and it can optimize the horizontal banding appeared on the image. This optimized is very effective to remove the periodic banding in some conditions.
A typical Periodic Horizontal Noise under certain USB_TRAFFIC values.
The camera is designed to use the +12V to reboot the camera without disconnecting and reconnecting the USB interface. This means that you can reboot the camera simply by shutting down the +12V and then powering it back on. This feature is very handy for remote controlling the camera in an observatory. You can use a remotely controlled power supply to reboot the camera. There is no need to consider how to reconnect the USB in the case of remote control.
Specifications
| Model |
QHY600PH (Photographic Version)
QHY600PH SBFL (Short Back Focal Length Version) QHY600PH L (Lite Version) |
| CMOS Sensor | SONY IMX455 |
| Mono/Color | Both Available (while Mono only with QHY600PH-L) |
| FSI/BSI | BSI |
| Pixel Size | 3.76um x 3.76um |
| Effective Pixel Area | 9576*6388
（9600*6422 with overscan and optically black area) |
| Effective Pixels | 61.17 Megapixels (effective area. |
| Sensor Size | Full Frame 36mm x 24mm |
| A/D Sample Depth
|
16-bit (0-65535 levels) at 1X1 binning
18-bit at 2X2, 19-bit at 3X3, 20-bit at 4X4 software binning *QHY600 uses the software digital binning for 2*2binning. With digital sum, 2*2binning will be four 16-bit summed then it is 18-bit. |
| Full Well Capacity (1×1, 2×2, 3×3) | Standard Mode >51ke- / >204ke- / >408ke- Super Full Well Mode >80ke- / >320ke- / >720ke- |
| Full Frame Rate | USB3.0 Port Image Transfer Speed
Full Frame Size: 4.0FPS (8-bit output) Full Frame Size: 2.5FPS (16-bit output) 7.2FPS at 9600×3194, 22.5FPS at 9600×1080, 28FPS at 9600×768, 47FPS at 9600×480, 160FPS at 9600×100, Fiber Port Image Transfer Speed (QHY600Pro only) Full Frame Size: 4.0FPS (16-bit output) |
| Readout Noise | 1.0e- to 3.7e- (Standard Mode) |
| Dark Current | 0.0022e-/p/s @ -20C 0.0046e-/p/s @ -10C |
| Exposure Time Range | 40us – 3600sec |
| Unity Gain* | 25 (Extended Full Well Mode) *
*With the improvement of the CMOS technology, the 16bit CMOS camera has been released, like QHY600/268/411/461. For these cameras, even in lowest gain it has beyond the requirement of unit gain (less than 1e/ADU due to sufficient samples) So you can directly set gain 0 as start. Please note QHY600/268C/411/461 has extend full well mode. In this mode you still need to find out the unit gain position. |
| Amp Control | Zero Amplifer Glow |
| Firmware/FPGA remote Upgrade | Supported. Via Camera USB Port |
| Shutter Type | Electric Rolling Shutter |
| Computer Interface | USB3.0 |
| Built-in Image Buffer | DDR3 memory
PH & PH SBFL ver.: 2GBytes |
| Hardware Frame Sequence Number | Supported |
| Cooling System | Dual Stage TEC cooler: – Long exposures (> 1 second) typically -35C below ambient – Short exposure (< 1second) high FPS, typically -30C below ambient（Test temperature +20°） |
| Optic Window Type | AR+AR High Quality Multi-Layer Anti-Reflection Coating |
| Anti-Dew Heater | Yes |
| Telescope Interface | M54/0.75 |
| Back Focal Length | QHY600PH&QHYPH-L: 17.5mm+6mm (±0.2)
QHY600SBFL: 14.5mm* *The BFL Consumed equals 12.5mm when connecting QHYCFW. About the defination of “BFL Comsumed” and our adapter system please view: https://www.qhyccd.com/adapters/ |
| Weigth | PH Version: 850g Lite Version: 790g |
| Power | 40W/100% 20W/50% 13.8W/0% |
Camera Curves
The curve shows absolute QE
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. The QHY600M-L 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 QHY600C-PH ends the days of non-16bit CMOS cameras and it ends the days non-full frame (and larger) monochrome CMOS cameras.
The QHY600C-PH has extremely low dark current (0.002e/p/s@-20C) using SONY’s Exmor BSI CMOS technology. QHY600C-PH is also a zero amplifer glow camera. The QHY600C-PH has only one electron of read noise at high gain and full resolution and 4FPS readout speed. One electron of read noise means the camera can achieve a SNR>3 at only 4 to 6 photons. This is perfect performance when conditions are photon limited, i.e., short exposures, narrow band imaging, etc., making this large area sensor ideal for sky surveys, time domain astronomy, fluorescence imaging, DNA sequencing and microscopy.
Models
QHY600 Series have mutiple models which covers both photographic and scientific using. Below list different types of QHY600 PH (photographic) series:
QHY600PH : Standard version for amateur astrographers;
2GB DDR3 image buffer
In order to provide smooth uninterrupted data transfer of the entire 60MP sensor at high speed, the QHY600 has 2GB DDR3 image buffer. The pixel count of the latest generation of CMOS sensors is very high resulting in greater memory requirements for temporary and permanent storage. For example, the QHY600 sensor produces about 120MB of data per frame. The data band-width is also increased from the original 16-bits to the current 32-bits. Transferring such a large file sizes necessarily requires the camera to have sufficient memory. The QHY600 has adopted a large-capacity memory of up to 2GB. Data throughput is doubled. This large image buffer meets the needs of high-speed image acquisition and transmission of the new generation of CMOS, making shooting of multiple frames smoother and less stuttered, further reducing the pressure on the computer CPU.
Another advantage is that when using some computers that do not have fast processors or have poor support for USB 3.0, the computer can’t transfer high-speed data well, and the data is often lost. The DDR can buffer a lot of image data and send it to the computer. Even if the USB 3.0 transmission frequently gets suspended, it will ensure that data is not lost. There are options in SharpCap to turn DDR buffering on or off. The current version of the ASCOM driver works in DDR mode.
Native 16 bit A/D: The new Sony sensor has native 16-bit A/D on-chip. The output is real 16-bits with 65536 levels. Compared to 12-bit and 14-bit A/D, a 16-bit A/D yields higher sample resolution and the system gain will be less than 1e-/ADU with no sample error noise and very low read noise.
BSI: One benefit of the back-illuminated CMOS structure is improved full well capacity. This is particularly helpful for sensors with small pixels. In a typical front-illuminated sensor, photons from the target entering the photosensitive layer of the sensor must first pass through the metal wiring that is embedded just above the photosensitive layer. The wiring structure reflects some of the photons and reduces the efficiency of the sensor. In the back- illuminated sensor the light is allowed to enter the photosensitive surface from the reverse side. In this case the sensor’s embedded wiring structure is below the photosensitive layer. As a result, more incoming photons strike the photosensitive layer and more electrons are generated and captured in the pixel well. This ratio of photon to electron production is called quantum efficiency. The higher the quantum efficiency the more efficient the sensor is at converting photons to electrons and hence the more sensitive the sensor is to capturing an image of something dim.
Zero Amplify Glow: This is also a zero amplifer glow camera.
TRUE RAW Data: In the DSLR implementation there is a RAW image output, but typically it is not completely RAW. Some evidence of noise reduction and hot pixel removal is still visible on close inspection. This can have a negative effect on the image for astronomy such as the “star eater” effect. However, QHY Cameras offer TRUE RAW IMAGE OUTPUT and produces an image comprised of the original signal only, thereby maintaining the maximum flexibility for post-acquisition astronomical image processing programs and other scientific imaging applications.
Anti-Dew Technology: Based on almost 20-year cooled camera design experience, The QHY cooled camera has implemented the fully dew control solutions. The optic window has built-in dew heater and the chamber is protected from internal humidity condensation. An electric heating board for the chamber window can prevent the formation of dew and the sensor itself is kept dry with our silicon gel tube socket design for control of humidity within the sensor chamber.
Cooling: In addition to dual stage TE cooling, QHYCCD implements proprietary technology in hardware to control the dark current noise.
Multiple Readout Modes are special for QHY 16-bit Cameras (QHY600/268/461/411). Different readout modes have different driver timing, etc., and result in different performance. See details at “Multiple Readout Modes and Curves” Part.
You may find some types of thermal noise can change with time in some back-illuminated CMOS cameras. This thermal noises has the characteristic of the fixed position of typical thermal noise, but the value is not related to the exposure time. Instead, each frame appears to have its own characteristics. The QHY600/268/461/411 use an innovative suppression technology that can significantly reduce the apparent level of such noise.
UVLO（Under Voltage Locking) is to protect the electronic device from damage caused by abnormally low voltages.
Our daily life experience tells us that the actual operational voltage of an electrical device must not significantly exceed the rated voltage, otherwise it will be damaged. For such precision equipment as cameras, long-term work at too low input voltage can also be detrimental to the working life of the camera, and may even make some devices, such as power manager, burn up due to long-term overload. In the all-in-one driver and SDK after 2021.10.23 stable version, the camera will give a warning when the input voltage of the camera is below 11V.
It is common behavior for a CMOS sensor to contain some horizontal banding. Normally, random horizontal banding can be removed with multiple frame stacking so it does not affect the final image. However, periodic horizontal banding is not removed with stacking so it may appear in the final image. By adjust the USB traffic in Single Frame mode or Live Frame mode, you can adjust the frequency of the CMOS sensor driver and it can optimize the horizontal banding appeared on the image. This optimized is very effective to remove the periodic banding in some conditions.
A typical Periodic Horizontal Noise under certain USB_TRAFFIC values.
The camera is designed to use the +12V to reboot the camera without disconnecting and reconnecting the USB interface. This means that you can reboot the camera simply by shutting down the +12V and then powering it back on. This feature is very handy for remote controlling the camera in an observatory. You can use a remotely controlled power supply to reboot the camera. There is no need to consider how to reconnect the USB in the case of remote control.
Specifications
| Model |
QHY600PH (Photographic Version)
QHY600PH SBFL (Short Back Focal Length Version) QHY600PH L (Lite Version) |
| CMOS Sensor | SONY IMX455 |
| Mono/Color | Both Available (while Mono only with QHY600PH-L) |
| FSI/BSI | BSI |
| Pixel Size | 3.76um x 3.76um |
| Effective Pixel Area | 9576*6388
（9600*6422 with overscan and optically black area) |
| Effective Pixels | 61.17 Megapixels (effective area. |
| Sensor Size | Full Frame 36mm x 24mm |
| A/D Sample Depth
|
16-bit (0-65535 levels) at 1X1 binning
18-bit at 2X2, 19-bit at 3X3, 20-bit at 4X4 software binning *QHY600 uses the software digital binning for 2*2binning. With digital sum, 2*2binning will be four 16-bit summed then it is 18-bit. |
| Full Well Capacity (1×1, 2×2, 3×3) | Standard Mode >51ke- / >204ke- / >408ke- Super Full Well Mode >80ke- / >320ke- / >720ke- |
| Full Frame Rate | USB3.0 Port Image Transfer Speed
Full Frame Size: 4.0FPS (8-bit output) Full Frame Size: 2.5FPS (16-bit output) 7.2FPS at 9600×3194, 22.5FPS at 9600×1080, 28FPS at 9600×768, 47FPS at 9600×480, 160FPS at 9600×100, Fiber Port Image Transfer Speed (QHY600Pro only) Full Frame Size: 4.0FPS (16-bit output) |
| Readout Noise | 1.0e- to 3.7e- (Standard Mode) |
| Dark Current | 0.0022e-/p/s @ -20C 0.0046e-/p/s @ -10C |
| Exposure Time Range | 40us – 3600sec |
| Unity Gain* | 25 (Extended Full Well Mode) *
*With the improvement of the CMOS technology, the 16bit CMOS camera has been released, like QHY600/268/411/461. For these cameras, even in lowest gain it has beyond the requirement of unit gain (less than 1e/ADU due to sufficient samples) So you can directly set gain 0 as start. Please note QHY600/268C/411/461 has extend full well mode. In this mode you still need to find out the unit gain position. |
| Amp Control | Zero Amplifer Glow |
| Firmware/FPGA remote Upgrade | Supported. Via Camera USB Port |
| Shutter Type | Electric Rolling Shutter |
| Computer Interface | USB3.0 |
| Built-in Image Buffer | DDR3 memory
PH & PH SBFL ver.: 2GBytes |
| Hardware Frame Sequence Number | Supported |
| Cooling System | Dual Stage TEC cooler: – Long exposures (> 1 second) typically -35C below ambient – Short exposure (< 1second) high FPS, typically -30C below ambient（Test temperature +20°） |
| Optic Window Type | AR+AR High Quality Multi-Layer Anti-Reflection Coating |
| Anti-Dew Heater | Yes |
| Telescope Interface | M54/0.75 |
| Back Focal Length | QHY600PH&QHYPH-L: 17.5mm+6mm (±0.2)
QHY600SBFL: 14.5mm* *The BFL Consumed equals 12.5mm when connecting QHYCFW. About the defination of “BFL Comsumed” and our adapter system please view: https://www.qhyccd.com/adapters/ |
| Weigth | PH Version: 850g Lite Version: 790g |
| Power | 40W/100% 20W/50% 13.8W/0% |
Camera Curves
The curve shows absolute QE
BSI
One benefit of the back-illuminated CMOS structure is improved full well capacity. This is particularly helpful for sensors with small pixels like the QHY533 Colour. In a typical front-illuminated sensor, photons from the target entering the photosensitive layer of the sensor must first pass through the metal wiring that is embedded just above the photosensitive layer. The wiring structure reflects some of the photons and reduces the efficiency of the sensor.
In the back- illuminated sensor the light is allowed to enter the photosensitive surface from the reverse side. In this case the sensor’s embedded wiring structure is below the photosensitive layer. As a result, more incoming photons strike the photosensitive layer and more electrons are generated and captured in the pixel well. This ratio of photon to electron production is called quantum efficiency. The higher the quantum efficiency the more efficient the sensor is at converting photons to electrons and hence the more sensitive the sensor is to capturing an image of something dim.
TRUE RAW Data
In the DSLR implementation there is a RAW image output, but typically it is not completely RAW. Some evidence of noise reduction and hot pixel removal is still visible on close inspection. This can have a negative effect on the image for astronomy such as the “star eater” effect. However, QHY Cameras offer TRUE RAW IMAGE OUTPUT and produces an image comprised of the original signal only, thereby maintaining the maximum flexibility for post-acquisition astronomical image processing programs and other scientific imaging applications.
Based on almost 20-year cooled camera design experience, The QHY cooled camera has implemented the fully dew control solutions. The optic window has built-in dew heater and the chamber is protected from internal humidity condensation. An electric heating board for the chamber window can prevent the formation of dew and the sensor itself is kept dry with our silicon gel tube socket design for control of humidity within the sensor chamber.
In addition to dual stage TE cooling, QHYCCD implements proprietary technology in hardware to control the dark current noise.
Amplify Control
Compare last generation’s astrocam for beginners, like QHY183 or QHY 163, QHY533M has much better amplify control.
QHY533M Dark Frame, 300s
QHY183M Dark Frame, 300s
QHY533M Dark frame
600s, with highest gain (170) and strech–only very slight amplify can be detected at the corner.
| Model | QHY533M | QHY533C |
| COMS Sensor | SONY IMX533 M | SONY IMX533 C |
| Mono/Color | Mono | Color |
| FSI/BSI | BSI | |
| Pixel Size | 3.76um x 3.76um | |
| Effective Pixel Area | 3008*3028 (includes the optically black area and overscan area) | |
| Effective Pixels | 9MP | |
| Sensor Size | 1 inch | |
| A/D Sample Depth
|
Native 14-bit A/D | |
| Full Well Capacity (1×1, 2×2, 3×3) | 58ke- | |
| Full Frame Rate | USB3.0 Port: Full Resolution 26.5FPS @8BIT 20FPS @16BIT2160Lines 37FPS @8BIT 28.5FPS@16BIT1080Lines 71.5FPS @8BIT 55FPS @16BIT768Lines 97FPS @8BIT 76FPS @16BIT480Lines 152FPS @8BIT 117FPS @16BIT240Lines 280FPS @8BIT 215FPS@16BIT |
|
| Readout Noise | 1.3 to 3.4e- | |
| Dark Current | -20C，0.0005e- /pixel/sec | |
| Exposure Time Range | 30us-3600sec | |
| Unity Gain | 68 | |
| Shutter Type | Electronic Shutter | |
| Computer Interface | USB3.0 | |
| Built-in Image Buffer | 1Gbyte DDR3 Memory | |
| Cooling System | Two-stage TEC cooler
Less than 1S lower than ambient temperature -30C in continuous mode More than 1S continuous mode or lower than ambient temperature -35C in single frame mode （Test temperature +20°） |
|
| Optic Window Type | AR+AR High Quality Multi-Layer Anti-Reflection Coating | |
| Anti-Dew Heater | Yes | |
| Telescope Interface | – | Support M48 (with adapter) |
| Back Focal Length | Actual Back Focal Consumed: 14 mm (Combined with CFW)
Standard BFL: 17.5mm（±0.5） |
17mm |
| Weight | 845g | 845g |
Multiple Readout Modes
Multiple Readout Modes are special for QHY 16-bit Cameras (QHY600/268/461/411). Different readout modes have different driver timing, etc., and result in different performance. See details at “Multiple Readout Modes and Curves” Part.
Random change thermal noise suppression function
You may find some types of thermal noise can change with time in some back-illuminated CMOS cameras. This thermal noises has the characteristic of the fixed position of typical thermal noise, but the value is not related to the exposure time. Instead, each frame appears to have its own characteristics. The QHY600/268/461/411 use an innovative suppression technology that can significantly reduce the apparent level of such noise.
UVLO Protection
UVLO（Under Voltage Locking) is to protect the electronic device from damage caused by abnormally low voltages.
Our daily life experience tells us that the actual operational voltage of an electrical device must not significantly exceed the rated voltage, otherwise it will be damaged. For such precision equipment as cameras, long-term work at too low input voltage can also be detrimental to the working life of the camera, and may even make some devices, such as power manager, burn up due to long-term overload. In the all-in-one driver and SDK after 2021.10.23 stable version, the camera will give a warning when the input voltage of the camera is below 11V.
Optimizing USB Traffic to Minimize Horizontal Banding
It is common behavior for a CMOS sensor to contain some horizontal banding. Normally, random horizontal banding can be removed with multiple frame stacking so it does not affect the final image. However, periodic horizontal banding is not removed with stacking so it may appear in the final image. By adjust the USB traffic in Single Frame mode or Live Frame mode, you can adjust the frequency of the CMOS sensor driver and it can optimize the horizontal banding appeared on the image. This optimized is very effective to remove the periodic banding in some conditions.
A typical Periodic Horizontal Noise under certain USB_TRAFFIC values.
After Adjusting the USB Traffic to avoid the periodic horizontal noise.
Reboot the camera by power off and on
The camera is designed to use the +12V to reboot the camera without disconnecting and reconnecting the USB interface. This means that you can reboot the camera simply by shutting down the +12V and then powering it back on. This feature is very handy for remote controlling the camera in an observatory. You can use a remotely controlled power supply to reboot the camera. There is no need to consider how to reconnect the USB in the case of remote control.
Specifications
| Model | QHY461PH |
| Image Sensor | SONY IMX461 BSI CMOS Sensor |
| Pixel Size | 3.76um x 3.76um |
| Color / Mono Version | Mono Only |
| Image Resolution | 11760 × 8896 |
| Effective Pixels | 102 Megapixels |
| Effective Image Area | 44mm x 33mm |
| Sensor Surface Glass | AR+AR Multi-Coating Clear Glass |
| Full Well Capacity (1×1, 2×2, 3×3) | 50ke- / 200ke- / 450ke- in Standard Mode 80ke- / 320ke- / 720ke- in Extend Full Well Mode |
| A/D | 16-bit (0-65535 greyscale) for 1X1Binning18bit in 2X2 19BIT in 3X3 20BIT in 4*4 software Binning |
| Sensor Size | TYPICAL 3.4inch |
| Read Noise | 1e to 3.7e (in HGC mode) |
| Dark Current | Approx 0.003e/pixel/sec @ -20C |
| Exposure Time Range | 50us – 3600sec |
| Frame Rate | 2.7FPS @ 8BIT 1.3FPS@16BIT on USB3.0 2.7FPS @ 16BIT 6FPS @ 14BIT on 10Gigabit Fiber |
| Shutter Type | Electric Rolling Shutter |
| Computer Interface | USB3.0 |
| Filter Wheel Interface | 4PIN QHYCCD CFW Port |
| Built-in Image Buffer | 1GByte DDR3 Buffer |
| Cooling System | Dual Stage TEC cooler（-35C below ambient with air cooling). |
| Anti-Dew Heater | Yes |
| Telescope Interface | – |
| Optic Window Type | AR+AR High Quality Multi-Layer Anti-Reflection Coating |
| Back Focal Length | 32.5mm |
Camera Curves
$3,190.00
The QHY268M/C is a new generation of back-illuminated CMOS cameras with true 16-bit A/D and 3.76um pixels. This new Sony sensor is an ideal CMOS sensor exhibiting no amplifer glow. 16-bit A/D gives high resolution sampling of the whole full well range. Digitizing 0-65535 levels yields a smooth image with continuous gradation of greyscale levels. The QHY268M/C is a cooled, back-illuminated, CMOS camera based on the Sony IMX571 sensor with native 16-bit A/D and 3.76um pixels.
1GB DDR3 image buffer
In order to provide smooth uninterrupted data transfer of the entire 26MP sensor at high speed, the QHY268 has 1GB DDR3 image buffer. The pixel count of the latest generation of CMOS sensors is very high resulting in greater memory requirements for temporary and permanent storage. The QHY268 has adopted a large-capacity memory of up to 1GB. Data throughput is doubled. This large image buffer meets the needs of high-speed image acquisition and transmission of the new generation of CMOS, making shooting of multiple frames smoother and less stuttered, further reducing the pressure on the computer CPU.
QHY268M has a unique internal humidity sensor (while QHY268C doesn’t). The Blue curve shown below represents humidity.
Multiple Readout Modes are special for QHY 16-bit Cameras (QHY600/268/461/411). Different readout modes have different driver timing, etc., and result in different performance. See details at “Multiple Readout Modes and Curves” Part.
You may find some types of thermal noise can change with time in some back-illuminated CMOS cameras. This thermal noises has the characteristic of the fixed position of typical thermal noise, but the value is not related to the exposure time. Instead, each frame appears to have its own characteristics. The QHY600/268/461/411 use an innovative suppression technology that can significantly reduce the apparent level of such noise.
UVLO（Under Voltage Locking) is to protect the electronic device from damage caused by abnormally low voltages.
Our daily life experience tells us that the actual operational voltage of an electrical device must not significantly exceed the rated voltage, otherwise it will be damaged. For such precision equipment as cameras, long-term work at too low input voltage can also be detrimental to the working life of the camera, and may even make some devices, such as power manager, burn up due to long-term overload. In the all-in-one driver and SDK after 2021.10.23 stable version, the camera will give a warning when the input voltage of the camera is below 11V.
It is common behavior for a CMOS sensor to contain some horizontal banding. Normally, random horizontal banding can be removed with multiple frame stacking so it does not affect the final image. However, periodic horizontal banding is not removed with stacking so it may appear in the final image. By adjust the USB traffic in Single Frame mode or Live Frame mode, you can adjust the frequency of the CMOS sensor driver and it can optimize the horizontal banding appeared on the image. This optimized is very effective to remove the periodic banding in some conditions.
A typical Periodic Horizontal Noise under certain USB_TRAFFIC values.
Reboot the camera by power off and on
The camera is designed to use the +12V to reboot the camera without disconnecting and reconnecting the USB interface. This means that you can reboot the camera simply by shutting down the +12V and then powering it back on. This feature is very handy for remote controlling the camera in an observatory. You can use a remotely controlled power supply to reboot the camera. There is no need to consider how to reconnect the USB in the case of remote control.
| Model | QHY268M | QHY268C |
| CMOS Sensor | SONY IMX571 M | SONY IMX571 C |
| Mono/Color | Mono | Color |
| FSI/BSI | BSI | |
| Pixel Size | 3.76um x 3.76um | |
| Effective Pixel Area | 6280*4210 (includes the optically black area and overscan area) | |
| Effective Pixels | 26MP | |
| Sensor Size | APS-C | |
| A/D Sample Depth
|
Native 16-bit (0-65535 greyscale) A/D | |
| Full Well Capacity (1×1, 2×2, 3×3) | 51ke- 75ke- or above in extended full well mode |
|
| Full Frame Rate | USB3.0 Port: Full Resolution 6.8FPS @8BIT 6FPS @16BIT 2048lines 13.6FPS @8BIT 11.5FPS@16BIT 1080lines 25.4FPS @8BIT 19.5FPS@16BIT 768lines 35FPS @8BIT 25FPS@16BIT 480lines 50FPS @8BIT 34FPS@16BIT |
|
| Readout Noise | 1.1e- High Gain,
3.5e- Low Gain (5.3e- to 7.4e- in extended full well mode) |
|
| Dark Current | -20C，0.0005e /pixel/sec
-10C，0.001e /pixel/sec |
|
| Exposure Time Range | 30us-3600sec | |
| Recommend Gain* | 30 (PH Mode，or Extended Full Well Mode)
56 (High Gain Mode) *With the improvement of the CMOS technology, For these 16bit CMOS cameras, even in lowest gain it has beyond the requirement of unit gain (less than 1e/ADU due to sufficient samples). Learn more at the “Readout Modes” part of this page. |
|
| Amp Control | Zero Amplifer Glow | |
| Firmware/FPGA remote Upgrade | Fully support via Camera USB port | |
| Shutter Type | Electronic Shutter | |
| Computer Interface | USB3.0 | |
| Built-in Image Buffer | 1GByte DDR3 Memory | |
| Cooling System | Two-stage TEC cooler
Less than 1S lower than ambient temperature -30C in continuous mode More than 1S continuous mode or lower than ambient temperature -35C in single frame mode （Test temperature +20°） |
|
| Optic Window Type | AR+AR High Quality Multi-Layer Anti-Reflection Coating | |
| Anti-Dew Heater | Yes | |
| Humidity Sensor* | Yes | No |
| Telescope Interface | Support M54 or M48 (Combined with adapters ) | Support M54 or M48 (Combined with adapters ) |
| Back Focal Length | QHY268M: 12.5mm* *If companied with the QHY filter wheel, the BFL consumed is counted as 12.5mm. The actual BFL (the intercept from the CMOS chip to the top of the camera) is 14.3mm (±0.3). Since most users will match CFW with monochrome cams, please take 12.5mm as major reference. |
QHY268C: 14.3mm（±0.3）*
*Since 2023, the top part of QHY268C is the same as 268M. |
| Weigth | About 810g | About 810g |
Camera Curves
$1,249.00
At just over 4 inches in diameter and a few inches thick (IMX585), the new miniCAM8 is a compact, high-resolution, high-performance, cooled imaging system capable of exceptional, high-quality deep space images as well as high-quality, high-resolution planetary images.
So often, compactness in astroimaging is achieved at the expense of some other critical feature found in multi-component cooled systems, such as sensor quality or thermoelectric cooling, etc. Such is not the case with the new miniCAM8. Based on Sony’s IMX585 8 MP sensor, the miniCAM8 includes full TE cooling capable of reaching a delta of -45℃ from ambient along with a built-in 8-position filter wheel for complete LRGB and narrowband imaging.
High Near-Infrared Sensitivity
The IMX585 is a Sony Starvis II processor that enables high sensitivity and high dynamic range (HDR). It also improves sensitivity in the near-infrared range by approximately 1.7 times* compared to the IMX485. The new camera miniCAM8 has a maximum quantum efficiency of 60% in the near-infrared band and 92% in the visible wavelength band.
*This data is officially provided by Sony: https://www.sony-semicon.com/cn/news/2021/2021062901.html
BSI
One benefit of the back-illuminated CMOS structure is improved full-well capacity. This is particularly helpful for sensors with small pixels. In a typical front-illuminated sensor, photons from the target entering the photosensitive layer of the sensor must first pass through the metal wiring that is embedded just above the photosensitive layer. The wiring structure reflects some of the photons and reduces the efficiency of the sensor.
In the back-illuminated sensor, the light is allowed to enter the photosensitive surface from the reverse side. In this case, the sensor’s embedded wiring structure is below the photosensitive layer. As a result, more incoming photons strike the photosensitive layer, and more electrons are generated and captured in the pixel well. This ratio of photon to electron production is called quantum efficiency. The higher the quantum efficiency, the more efficient the sensor is at converting photons to electrons, and hence the more sensitive the sensor is to capturing an image of something dim.
Zero Amplify Glow
miniCAM8 is also a zero amplifier glow camera.
Anti-Dew Technology
Based on almost 20-year cooled camera design experience, the QHY cooled camera has implemented the fully dew control solutions. The optic window has a built-in dew heater, and the chamber is protected from internal humidity condensation. An electric heating board for the chamber window can prevent the formation of dew, and the sensor itself is kept dry with our silicon gel tube socket design for control of humidity within the sensor chamber.
Cooling
In addition to dual-stage TE cooling, QHYCCD implements proprietary technology in hardware to control the dark current noise.
Filters
The astronomical filters included with the miniCAM8 deepsky combos are custom-designed to match the specific characteristics of the cameras. The size is 19 mm * 12 mm * 1.1 mm. The LRGB and SHO narrowband filters for the miniCAM8M deepsky combo are customized by XiMei Filters. The LRGB filters have an optical density (OD) value of 3, while the narrowband filters have an OD value of 5.
| Model | miniCAM8 |
| CMOS Sensor | Sony IMX585 |
| Mono/Color | Both Available |
| BSI/FSI | BSI |
| Sensor Size | 1/1.2inch |
| Pixel Size | 2.9μm*2.9μm |
| Total Pixel Area | 3856*2180 |
| Effective Pixels | 8 MP |
| Full Well Capacity | 54ke-
Linearity HDR Mode: 46ke- |
| Readout Noise | 0.76 – 7.8 e-
Linearity HDR Mode: 1.0e- |
| Peak QE | M: 92%
C: R: 82%; G: 87%; B: 75% |
| Dynamic Range | Linearity HDR mode: The dynamic range reaches up to 46,300:1, equivalent to 93 dB or 15.5 stops. |
| A/D | Dual 12-bit (output as 16-bit) |
| Full Frame Rates | Full Resolution: 41.5FPS@8bit，23.5FPS @16bit |
| ROI Frame Rates | Full Resolution 1080Lines, 82FPS@8bit, 47FPS@16bit；640Lines, 177FPS@8bit, 105FPS@16bit |
| Exposure Time Range | 11μs-900sec |
| Shutter Type | Electronic Rolling Shutter |
| Built-in Image Buffer | 512MB DDR3 |
| Computer Interface | USB3.0 |
| Telescope Interface | 1.25 inch |
| Optic Window Type | AR+AR |
| Filter Wheel | Built-in 8-Position Carousel |
| Back Focal Length | 17.5mm |
| Cooling System | Dual Stage TEC cooler:
Long exposures (> 1 second) typically -45℃ below ambient |
| Weight | 480g |
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