QHYCCD QHY461PH (Mono) Astronomy Cooled Camera (QHY461PH)
QHYCCD QHY461PH (Mono) Astronomy Cooled Camera (QHY461PH)
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The QHY461-PH is a photographic version of the larger, scientific QHY461M-PRO. Using the same Sony IMX461 sensor, the QHY461-PH is more compact with just the features needed for astrophotography. The result is all of the features and performance essential to astrophotography at a significantly lower price than the scientific model.
The IMX461 is the first scientific CMOS sensor with a native 16-bit A/D on-chip. In addition, the sensor is back-illuminated, resulting in extraordinarily high quantum efficiency and extremely low dark current. Another benefit of back-illumination is an increased full-well capacity, including an Extended Full Well Mode. Lastly, this camera has zero amplifier glow, even at long exposures.
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.
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.
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.
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.
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（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.
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.
|Sony IMX461 BSI CMOS Sensor
|3.76um * 3.76um
|Color / Mono Version
|11760 x 8896
|Effective Image Area
|44mm x 33mm
|Sensor Surface Glass
|AR+AR Multi-Coating Clear Glass
|Full Well Capacity (1x1, 2x2, 3x3)
|50ke- / 200ke- / 450ke- in Standard Mode
80ke- / 320ke- / 720ke- in Extend Full Well Mode
|16-bit (0-65535 greyscale) for 1X1Binning
18bit in 2X2
19BIT in 3X3
20BIT in 4*4 software Binning
|1e to 3.7e (in HGC mode)
|Approx 0.003e/pixel/sec @ -20C
|Exposure Time Range
|50us - 3600sec
|2.7FPS @ 8BIT 1.3FPS@16BIT on USB3.0
2.7FPS @ 16BIT 6FPS @ 14BIT on 10Gigabit Fiber
|Electric Rolling Shutter
|Filter Wheel Interface
|4PIN QHYCCD CFW Port
|Built-in Image Buffer
|1GByte DDR3 Buffer
|Dual Stage TEC cooler (-35C below ambient with air cooling).
|Optic Window Type
|AR+AR High Quality Multi-Layer Anti-Reflection Coating
|Back Focal Length
Additional Articles, Videos, and Links
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