With the advantage of low readout noise and high-speed readout, CMOS technology has revolutionized astronomical imaging. 

Διαθέσιμο με Προπαραγγελία

Διαθέσιμο με Προπαραγγελία

Στην περίπτωση αυτή περιλαμβάνονται προϊόντα που συνήθως δεν κρατάμε σε στοκ και για κάποιους λόγους - που δεν εξαρτώνται από την εταιρία μας - ΔΕΝ μπορούν να είναι διαθέσιμα σε διάστημα μικρότερο των 14 ημερών.Στην κατηγορία αυτή περιλαμβάνονται και προϊόντα που προδιαφημίζονται από τους κατασκευαστές αλλά δεν άρχισε ακόμη η επίσημη διανομή τους στην ελληνική αγορά. Πιθανόν για τα είδη αυτά να παρέχεται δυνατότητα προπαραγγελίας με ειδική προνομιακή τιμή. Αν γνωρίζουμε ήδη την πιθανή ημερομηνία άφιξης του συγκεκριμένου προϊόντος, στις αποθήκες μας, τότε αυτή θα αναγράφεται ξεχωριστά και επάνω από την ένδειξη «Διαθέσιμο με Προπαραγγελία»

Διαθεσιμότητα: Σε απόθεμα

Camera QHY600C-PH SBFL* (colored)


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 QHY600 Series uses SONY  IMX455, a BSI 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 Series ends the days of non-16bit cooling CMOS cameras and it ends the days non-full frame (and larger) monochrome cooling CMOS cameras.

  • Extremely low dark current (0.002e/p/s@-20C) using SONY’s Exmor BSI CMOS technology.
  • Zero amplifer glow.
  • 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.

In order to provide smooth uninterrupted data transfer of the entire 60MP sensor at high speed, the QHY600 Series (except QHY600M-PH L) have 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. 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. 

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. 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. 

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.

One benefit of the back-illuminated CMOS structure is improved full well capacity. 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.

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.

Zero Amplify Glow:
This is also a zero amplifer glow camera.

Cooling & Anti-dew Control:
In addition to dual stage TE cooling, QHYCCD implements proprietary technology in hardware to control the dark current noise. 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.

Sealing Technology:
Based on almost 20-year cooled camera design experience, The QHY cooled camera has implemented the sealing control solutions. The sensor itself is kept dry with our silicon gel tube socket design for control of humidity within the sensor chamber. By the way, there’s no oil leaking.

Advanced Functions

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.

*SBFL–has a shorter back focal length.


  • CMOS Sensor: SONY IMX455
  • Mono/Color: Both Available (while Mono only with QHY600PH-L)
  • 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
  • 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-
  • Frame Rate:
    • Full Resolution
      4.0FPS (8-bit output) ; 2.5FPS (16-bit output)
    • ROI
      7.2FPS at 9600×3194, 22.5FPS at 9600×1080, 28FPS at 9600×768, 47FPS at 9600×480, 160FPS at 9600×100
  • Readout Noise: 1.0e- to 3.7e-  (Standard Mode)
  • Dark Current: 0.0022e-/p/s @ -20℃    0.0046e-/p/s @ -10℃
  • 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: PH & PH SBFL Ver.: 2GB DDR3  PH L Ver. : 1GB DDR3
  • Hardware Frame Sequence Number: Supported
  • Cooling System:  Dual Stage TEC cooler:
    – Long exposures (> 1 second) typically -35℃ below ambient
    – Short exposure (< 1second) high FPS, typically -30℃ 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&QHY PH-L: 17.5mm+6mm (CAA)
    • QHY600SBFL: 14.5mm*
      *The BFL Consumed equals 12.5mm when connecting QHYCFW. About the defination of “BFL Comsumed” and our adapter system please view:
  • Weigth:
    • PH & PH SBFL Ver.: 850g
    • PH L Ver. : 790g
  • Power:
    • 40W/100%
    • 20W/50%
    • 13.8W/0%

Mechanical Dimensions

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