The QHY5III462 camera uses the Sixth Generation Sony 2.1 megapixel IMX462 STARVIS CMOS sensor. The pixel size is 2.9um making it the same size and resolution as the sensor used in the QHY5III290 camera that has been so successfully used for planetary imaging by some of the best planetary imagers in the world. Like other cameras in the 5III series, the QHY5III462 is USB 3.0 powered and controlled. No additional power is required.

The IMX462 sensor is back-illuminated and incorporates new technology that gives it some significant advantage over other planetary cameras: First, the IMX462 sensor has sHCG (Super High Conversion Gain) for very low read noise at high gain. This is ideal for stacking hundreds or thousands of short planetary images. Second, it is exceptionally sensitive in the NIR.

In this latest generation of sensors, the photodiode portion of the pixel well is physically deeper than in previous Sony BSI sensors, allowing photons of longer wavelength to penetrate deeper into the substrate. This dramatically increases the sensor’s sensitivity to red and near infrared (NIR) light. The RGB filters over the pixels become transparent at NIR wavelengths, so the sensor displays almost equal peak sensitivity to NIR light as it does to light in the visible spectrum.

The peak QE in the NIR around 800nm is as high as the peak QE in the visible wavelengths. For planetary imagers using a methane filter that passes light around 880nm this is welcome news.

BSI

One benefit of the back-illuminated CMOS structure is improved sensitivity. 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.

Extended Near Infrared Sensitivity

Logically, one would think, each generation of Exmor sensor would be built upon and incorporate all of the improvements of the generation immediately preceding. However, this was not the case with the fifth generation Exmor R sensors.

The first back-illuminated sensors used shallower pixel wells (like the third-generation front- illuminated designs) than the physically deeper pixels of the fourth generation. So, while the back- illuminated structure increased the sensitivity in the visible range by 2X, the shallower pixels did not improve the NIR. The answer to this is seen in the latest, sixth generation, Sony Exmor R sensors, like the IMX462. Using physically deeper pixels in conjunction with the back-illuminated structure has dramatically improved the sensor’s sensitivity to both the visible and near infrared wavelengths.

sHCG Mode

Another advantage of the QHY5III462 is the camera’s “Super High Conversion Gain” capability. By using a lower capacitance, a small amount of charge can be converted to a high voltage resulting in higher sensitivity in low-light conditions. The readout noise of the QHY5III462 in high gain mode is as low as 0.5 electrons!

The test exposures below demonstrate the low light improvement over the IMX290 sensor. The QHY5III462C image is on the left and the corresponding QHY5III290C image is on the right. The low light conditions and exposures are identical for each top and bottom pair of images and a UV/IR filter was in place for each camera. So this test demonstrates the QHY5III462C’s increase in sensitivity and SNR over the QHY5III290C under the same conditions in the visual light spectrum alone.

Color and Mono Imaging

The filter matrix in the IMX462 uses organic dye filters. These filters are very efficient at visible wavelengths but become completely transparent in the NIR. For this reason, good RGB color balance requires an external UV/IR filter that blocks NIR wavelengths.

Many color cameras build this UV/IR filter into the camera or optical window for normal color imaging. However, in order to fully exploit the capabilities of the 462C sensor, in the QHY5III462C camera the optical window is AR coated only with no UV or IR blocking. Instead, the QHY5III462C camera includes two 1.25″ screw-in filters, a UV/IR cut filter to isolate the visible wavelengths for normal RGB imaging and an IR850 filter that will cut the visible wavelengths but pass wavelengths above 850nm.

Specifications

Camera Curves

Overview

The QHY5III715C is an ultra-high resolution back-illuminated color camera with extremely low read noise. The sensor has a 1/2.8-inch optical format, similar to the QHY5III462C. However, the QHY5III715C has 4X as many pixels as the QHY5III462C for 4K resolution with 1.45um pixels.

This makes the new QHY5III715C ideal for smaller short focal length refractors. The exceptionally small pixels subtend a FOV of less than 1 arcsecond at focal lengths of 12 inches (300mm) or longer. The QHY5III715C inherits all of the updates and improvements of the QHY5III Series Ver. 2 line of cameras (See below).

Sample Images

"New Moon"

• Telescope: Celestron C8HD
  Camera: QHY5III715C
  2000frames
  6ms exposure per frame
  37% stacked

515MB DDR3 Memory

https://www.youtube.com/watch?v=WYb5d5-5aWw

The QHY5III (Ver. 2) series planetary and guiding cameras are all equipped with a 512MB DDR3 image buffer which can effectively reduce the pressure on computer transmission, a great help for planetary photography which often requires writing a large amount of data in a short period of time.

Some deep-sky astrophotography cameras on the market today only have 256MB, for example.

In comparison, the 512MB DDR3 memory of the new 5III (Ver. 2) series cameras represents a significant upgrade.

Specifications

Extended Near Infrared Sensitivity

In this latest generation of sensors, the photodiode portion of the pixel well is physically deeper than in previous sensors, allowing photons of longer wavelengths to penetrate deeper into the substrate. This dramatically increases the sensor’s sensitivity to red and near-infrared (NIR) light. The sensor displays almost equal peak sensitivity to NIR light as it does to light in the visible spectrum.

Curves

QHY5III200M is a new generation of QHY5III V2 series planetary guide camera, using domestic CMOS, with excellent quality, and near-infrared high sensitivity similar to 5III462C. QHY5III200 is also the first mono CMOS planetary camera with near-infrared enhancement characteristics QHY developed. In addition, the 4um large picture elements make it easier to use for guiding.

The QHY5III (Ver. 2) series planetary and guiding cameras are all equipped with a 512MB DDR3 image buffer which can effectively reduce the pressure on computer transmission, a great help for planetary photography which often requires writing a large amount of data in a short period of time. Some deep-sky astrophotography cameras on the market today only have 256MB, for example.

The new QHY5III (Ver.2) series cameras all use the USB3.2 Gen1 Type-C interface. Compared to the USB3.0 Type-B interface used in the previous generation, the Type-C interface has a longer life and is more flexible.

Tips: It is recommended to use the official standard Type-C data cable of QHYCCD. As the market is flooded with a large number of poor-quality Type-C cables, casual use may lead to the camera malfunctioning. If you use your own spare cable, please make sure it is a high-quality cable.

The custom interfaces of the previous generation of planetary cameras and guiders has been replaced in the QHY5III (Ver.2) cameras with a more universal ST-4 compatible guiding interface. Now, even if the guiding cable is lost or damaged, you will be able to easily get a replacement on the market at a low cost.

The new QHY5III (Ver.2) series of cameras is equipped with a status indicator at the back of the camera. If the camera experiences an abnormal status, the multi-colored indicator light will help to determine the situation with different colors signifying different conditions. During normal operation this indicator light is off, so there is no worry about light contaminating the image.

Specifications

Camera Curves

QHY5III485C uses Sony’s new IMX485, back-illuminated, 8.4 megapixel color CMOS sensor with an array of 3864 x 2180 pixels at 2.9um. With USB 3.0 interface, the full frame rate of 44 FPS at 8-bits or 18.5 FPS at 16-bits. Smaller regions of interest will yield even faster frame rates.

The resolution of QHY5III485C is 16:9, which is equivalent to the mainstream video output ratio. With the native high resolution, 485C can play a special role in recording astronomical video and astronomical science live broadcast.

QHY5III485C is specially equipped with 128MB DDR bulid-in image buffer. In non-video output mode, DDR built-in buffer can effectively relieve the transmission pressure brought by high-resolution large data volume and reduce information loss.

One benefit of the back-illuminated CMOS structure is improved sensitivity. 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.

The QHY5III485C standard package includes a 2.5mm Fisheye lens that converts the planetary camera into a high-resolution, 8.4 Megapixel All Sky camera with 180-degree field of view.

Specifications

QHY5III678c is a new planetary and guiding camera of the 2nd generation of QHY5III series, the upgraded version of QHY5III178M/C, with excellent near-infrared high sensitivity.

USB-c connectivity

The new QHY5III678c series cameras all use the USB3.2 Gen1 Type-C interface. Compared to the USB3.0 Type-B interface used in the previous generation, the Type-C interface has a longer life and is more flexible.

Tips: It is recommended to use the official standard Type-C data cable of QHYCCD. As the market is flooded with a large number of poor-quality Type-C cables, casual use may lead to the camera malfunctioning. If you use your own spare cable, please make sure it is a high-quality cable.

Universal Guiding Interface

The custom interfaces of the previous generation of planetary cameras and guiders has been replaced in the QHY5III (Ver.2) cameras with a more universal ST-4 compatible guiding interface. Now, even if the guiding cable is lost or damaged, you will be able to easily get a replacement on the market at a low cost.

Indicator LED

The new QHY5III (Ver.2) series of cameras is equipped with a status indicator at the back of the camera. If the camera experiences an abnormal status, the multi-colored indicator light will help to determine the situation with different colors signifying different conditions. During normal operation this indicator light is off, so there is no worry about light contaminating the image.

Specifications

Camera Curves

The QHY294 Pro is a 4/3-inch back-illuminated camera, equipped with Sony IMX294 (Color) and IMX 492 (Mono) sensor. The 294 Pro has 11.7 MP at 4.63um, 14-bits A/D. The IMX294 and IMX492 chips have 46.8 million 2.315um pixels, which Sony 2×2 bins on-chip to create the sensor’s advertised 11.7 million 4.63um pixel array. The QHY294 Pro series camera is capable of locking and unlocking the on-chip binning to provide two readout modes. The first mode reads the sensor “locked” mode to produce 11.6mp images with 4.63um pixel size and 14 bits per pixel. The second read mode unlocks the binning to produce 46.8mp images with 2.315um pixel size at 12 bits per pixel.

The QHY294 Pro CMOS sensor has a dual gain mode, HGC (high gain) and LGC (Low gain). The QHY294 Pro will switch the two modes automatically when the gain is set to 1600 you will get the benefits of the ultra low read noise (1e- to 1.6e-) of the HGC mode and a full well capacity of about 14.5ke- at the switch point setting.

The QHY5III462 camera uses the Sixth Generation Sony 2.1 megapixel IMX462 STARVIS CMOS sensor. The pixel size is 2.9um making it the same size and resolution as the sensor used in the QHY5III290 camera that has been so successfully used for planetary imaging by some of the best planetary imagers in the world. Like other cameras in the 5III series, the QHY5III462 is USB 3.0 powered and controlled. No additional power is required.

The IMX462 sensor is back-illuminated and incorporates new technology that gives it some significant advantage over other planetary cameras: First, the IMX462 sensor has sHCG (Super High Conversion Gain) for very low read noise at high gain. This is ideal for stacking hundreds or thousands of short planetary images. Second, it is exceptionally sensitive in the NIR.

In this latest generation of sensors, the photodiode portion of the pixel well is physically deeper than in previous Sony BSI sensors, allowing photons of longer wavelength to penetrate deeper into the substrate. This dramatically increases the sensor’s sensitivity to red and near infrared (NIR) light. The RGB filters over the pixels become transparent at NIR wavelengths, so the sensor displays almost equal peak sensitivity to NIR light as it does to light in the visible spectrum.

The peak QE in the NIR around 800nm is as high as the peak QE in the visible wavelengths. For planetary imagers using a methane filter that passes light around 880nm this is welcome news.

BSI

One benefit of the back-illuminated CMOS structure is improved sensitivity. 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.

Extended Near Infrared Sensitivity

Logically, one would think, each generation of Exmor sensor would be built upon and incorporate all of the improvements of the generation immediately preceding. However, this was not the case with the fifth generation Exmor R sensors.

The first back-illuminated sensors used shallower pixel wells (like the third-generation front- illuminated designs) than the physically deeper pixels of the fourth generation. So, while the back- illuminated structure increased the sensitivity in the visible range by 2X, the shallower pixels did not improve the NIR. The answer to this is seen in the latest, sixth generation, Sony Exmor R sensors, like the IMX462. Using physically deeper pixels in conjunction with the back-illuminated structure has dramatically improved the sensor’s sensitivity to both the visible and near infrared wavelengths.

sHCG Mode

Another advantage of the QHY5III462 is the camera’s “Super High Conversion Gain” capability. By using a lower capacitance, a small amount of charge can be converted to a high voltage resulting in higher sensitivity in low-light conditions. The readout noise of the QHY5III462 in high gain mode is as low as 0.5 electrons!

The test exposures below demonstrate the low light improvement over the IMX290 sensor. The QHY5III462C image is on the left and the corresponding QHY5III290C image is on the right. The low light conditions and exposures are identical for each top and bottom pair of images and a UV/IR filter was in place for each camera. So this test demonstrates the QHY5III462C’s increase in sensitivity and SNR over the QHY5III290C under the same conditions in the visual light spectrum alone.

Color and Mono Imaging

The filter matrix in the IMX462 uses organic dye filters. These filters are very efficient at visible wavelengths but become completely transparent in the NIR. For this reason, good RGB color balance requires an external UV/IR filter that blocks NIR wavelengths.

Many color cameras build this UV/IR filter into the camera or optical window for normal color imaging. However, in order to fully exploit the capabilities of the 462C sensor, in the QHY5III462C camera the optical window is AR coated only with no UV or IR blocking. Instead, the QHY5III462C camera includes two 1.25″ screw-in filters, a UV/IR cut filter to isolate the visible wavelengths for normal RGB imaging and an IR850 filter that will cut the visible wavelengths but pass wavelengths above 850nm.

Specifications

Camera Curves

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 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.

Internal Humidity Sensor

QHY268M has a unique internal humidity sensor (while QHY268C doesn’t). The Blue curve shown below represents humidity.

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.

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 SBFL ends the days of non-16bit CMOS cameras and it ends the days non-full frame (and larger) monochrome CMOS cameras.

The QHY600C-PH SBFL has extremely low dark current (0.002e/p/s@-20C) using SONY’s Exmor BSI CMOS technology. QHY600C-PH SBFL is also a zero amplifer glow camera. The QHY600C-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;

QHY600PH-SBFL (Short back-focal length version) ：specially designed for DSLR lens users or those who has special requirment of short back focal length. This version has a special front part version which has 14mm B.F.L only (The B.F.L consumed equals 12.5mm when connecting QHYCFW. About the defination of “BFL Comsumed” and our adapter system please view: https://www.qhyccd.com/astronomical-camera-adapter-bfl-solution/). QHY600SBFL can easily match Canon/Nikon lens even with filter wheel. On the side of this adapter there is a 4mm hole to connect air pump through plastic pipe in case of the dewing glass when necessary.

QHY600L : a lite, shorter and cheaper version. Compared with QHY600PH, QHY600PH-Lite has the following features compared with previous models: QHY600L only has mono version; The body length becomes shorter, which is about 112mm, and its price is lowered compared with QHY600PH; The Built-in DDR3 Buffer (memory storage) is adjusted to 1GB compared to 2GB of QHY600PH/Pro. Other specifications of QHY600L keep the same with QHY600PH except the body length and weight.

The new CFW3 series filter wheels are available in four sizes to accommodate filters from 1.25-inch to 50 millimeters square.

For filter wheel control a custom QHY 4-pin filter wheel port is included that provides power and control signals for QHY dual control filter wheels like the series 3 filter wheels. Both the series 2 and new series 3 filter wheels can be controlled by either an independent external program using the filter wheel’s USB port or via the QHY 4-pin serial port. When connected to the QHY 4-pin port there is no need for an additional power cable or control program. All of the filter wheel functions are controlled through the camera and its operating Software.

The series 3 filter wheels utilize a new motor with direct drive and will reverse direction to take the shortest path when moving from one filter to another. For Example, in this demonstration the wheel moves from filter position 1 to position 2 to position 3 and then back to 1 again, over to position 7 and back to position 1 without ever making a complete rotation of the carousel. This saves time if you’re doing a lot of filter changes in one imaging session.

LED changes color for each filter position. The tricolor LED assigns one unique color or combination of colors to each filter position so you can tell if it’s moved to the correct position without removing it from the Telescope.

The CFW3 is also thin. This feature and the short back focus of the COLDMOS cameras means you can add one of several camera lens adapters for Canon and Nikon camera lenses for wide field imaging with the filter wheel.

In the center of the back plate is a 12-volt DC power port. This port is threaded for a short extension cable that is supplied with the camera that securely attaches such that it will not accidentally disconnect while you are imaging.

QHY183C is a model designed for astrophotography beginners. It exhibits excellent sensitivity and low noise, with the back illuminated QHY183C having higher sensitivity and somewhat higher resolution. It is well suited to planetary and deep-space imaging particularly when mated with the CFW3 filter wheel. This model has two-stage thermal electric cooling of the sensor to about minus 40 degrees C below ambient for maximum reduction of dark current noise in long exposures.

QHY183 incorporates QHY’s Anti-Amp Glow technology to significantly reduce typical CMOS amplifier glow to a minimum, allowing excellent calibration by subtracting a dark frame.

QHY183 utilizes the Anti-Dew features common to the QHY COLDMOS cameras. Dew is moisture that condenses from the air onto the outside of the chamber window. Frost is water vapor that freezes when it comes into contact with the inside of the chamber window or the surface of the sensor. QHY has nearly 20 years of experience designing cooled cameras and these models benefit from those years of anti-dew and anti-frost design experience. To help prevent dew from forming on the chamber window heating elements are built into the light shield just above the chamber. To avoid frost from forming inside the chamber a desiccant tube is provided that can easily be attached by the user to the outside of the camera when needed to dry the internal atmosphere of the chamber and remove any built-up moisture.

QHY183 models can be used as guiding devices, too. The opto-isolated guiding port is a standard ST-4 configuration using an RJ11 style Jack. A guiding cable is included with each camera.

The 183 with its smaller higher resolution sensor is a good match to short focal length telescopes or for imaging smaller dim objects through a large scope. The larger 163 gives a greater field of view and would be a good choice for imaging larger areas of the sky such as nebula or when coupled to a longer focal length telescope to take greater advantage of the scopes full field.

The QHY183M is a one-inch, 20 Megapixel back-illuminated monochrome CMOS camera with a peak QE of 84%. The pixel size is 2.4um, yielding high-resolution with modest size telescopes. The camera is capable of producing 15FPS@20 Megapixels. It has a two-stage TEC that cools the sensor to -40C to -45C below ambient. The ADC is 12-bit / 16-bit with 1e- read noise! The computer interface is USB 3.0 and exposure times can be set from 50us to 3600sec.

Specifications

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.

QHY5III678 is a new planetary and guiding camera of the 2nd generation of QHY5III series, the upgraded version of QHY5III178M/C, with excellent near-infrared high sensitivity.

USB-c connectivity

The new QHY5III678 series cameras all use the USB3.2 Gen1 Type-C interface. Compared to the USB3.0 Type-B interface used in the previous generation, the Type-C interface has a longer life and is more flexible.

Tips: It is recommended to use the official standard Type-C data cable of QHYCCD. As the market is flooded with a large number of poor-quality Type-C cables, casual use may lead to the camera malfunctioning. If you use your own spare cable, please make sure it is a high-quality cable.

Universal Guiding Interface

The custom interfaces of the previous generation of planetary cameras and guiders has been replaced in the QHY5III (Ver.2) cameras with a more universal ST-4 compatible guiding interface. Now, even if the guiding cable is lost or damaged, you will be able to easily get a replacement on the market at a low cost.

Indicator LED

The new QHY5III (Ver.2) series of cameras is equipped with a status indicator at the back of the camera. If the camera experiences an abnormal status, the multi-colored indicator light will help to determine the situation with different colors signifying different conditions. During normal operation this indicator light is off, so there is no worry about light contaminating the image.

Specifications

Camera Curves

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;

QHY600PH-SBFL (Short back-focal length version) ：specially designed for DSLR lens users or those who has special requirment of short back focal length. This version has a special front part version which has 14mm B.F.L only (The B.F.L consumed equals 12.5mm when connecting QHYCFW. About the defination of “BFL Comsumed” and our adapter system please view: https://www.qhyccd.com/astronomical-camera-adapter-bfl-solution/). QHY600SBFL can easily match Canon/Nikon lens even with filter wheel. On the side of this adapter there is a 4mm hole to connect air pump through plastic pipe in case of the dewing glass when necessary.

QHY600L : a lite, shorter and cheaper version. Compared with QHY600PH, QHY600PH-Lite has the following features compared with previous models: QHY600L only has mono version; The body length becomes shorter, which is about 112mm, and its price is lowered compared with QHY600PH; The Built-in DDR3 Buffer (memory storage) is adjusted to 1GB compared to 2GB of QHY600PH/Pro. Other specifications of QHY600L keep the same with QHY600PH except the body length and weight.

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

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

Camera Curves

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;

QHY600PH-SBFL (Short back-focal length version) ：specially designed for DSLR lens users or those who has special requirment of short back focal length. This version has a special front part version which has 14mm B.F.L only (The B.F.L consumed equals 12.5mm when connecting QHYCFW. About the defination of “BFL Comsumed” and our adapter system please view: https://www.qhyccd.com/astronomical-camera-adapter-bfl-solution/). QHY600SBFL can easily match Canon/Nikon lens even with filter wheel. On the side of this adapter there is a 4mm hole to connect air pump through plastic pipe in case of the dewing glass when necessary.

QHY600L : a lite, shorter and cheaper version. Compared with QHY600PH, QHY600PH-Lite has the following features compared with previous models: QHY600L only has mono version; The body length becomes shorter, which is about 112mm, and its price is lowered compared with QHY600PH; The Built-in DDR3 Buffer (memory storage) is adjusted to 1GB compared to 2GB of QHY600PH/Pro. Other specifications of QHY600L keep the same with QHY600PH except the body length and weight.

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;

QHY600PH-SBFL (Short back-focal length version) ：specially designed for DSLR lens users or those who has special requirment of short back focal length. This version has a special front part version which has 14mm B.F.L only (The B.F.L consumed equals 12.5mm when connecting QHYCFW. About the defination of “BFL Comsumed” and our adapter system please view: https://www.qhyccd.com/astronomical-camera-adapter-bfl-solution/). QHY600SBFL can easily match Canon/Nikon lens even with filter wheel. On the side of this adapter there is a 4mm hole to connect air pump through plastic pipe in case of the dewing glass when necessary.

QHY600L : a lite, shorter and cheaper version. Compared with QHY600PH, QHY600PH-Lite has the following features compared with previous models: QHY600L only has mono version; The body length becomes shorter, which is about 112mm, and its price is lowered compared with QHY600PH; The Built-in DDR3 Buffer (memory storage) is adjusted to 1GB compared to 2GB of QHY600PH/Pro. Other specifications of QHY600L keep the same with QHY600PH except the body length and weight.

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;

QHY600PH-SBFL (Short back-focal length version) ：specially designed for DSLR lens users or those who has special requirment of short back focal length. This version has a special front part version which has 14mm B.F.L only (The B.F.L consumed equals 12.5mm when connecting QHYCFW. About the defination of “BFL Comsumed” and our adapter system please view: https://www.qhyccd.com/astronomical-camera-adapter-bfl-solution/). QHY600SBFL can easily match Canon/Nikon lens even with filter wheel. On the side of this adapter there is a 4mm hole to connect air pump through plastic pipe in case of the dewing glass when necessary.

QHY600L : a lite, shorter and cheaper version. Compared with QHY600PH, QHY600PH-Lite has the following features compared with previous models: QHY600L only has mono version; The body length becomes shorter, which is about 112mm, and its price is lowered compared with QHY600PH; The Built-in DDR3 Buffer (memory storage) is adjusted to 1GB compared to 2GB of QHY600PH/Pro. Other specifications of QHY600L keep the same with QHY600PH except the body length and weight.

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.

Internal Humidity Sensor

QHY268M has a unique internal humidity sensor (while QHY268C doesn’t). The Blue curve shown below represents humidity.

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.

QHY5III174M uses a 1/1.2-inch, 2.3 Megapixel, SONY Exmore IMX174 CMOS sensor with global shutter. Available in both monochrome and color. The large sensor size is a great choice for solar imaging and the large pixel size and high QE makes it excellent for deep-sky imaging as well. Typical of all models in the QHY5III Series, this camera produces a high frame rate with the USB 3.0 interface, 138 frames per second at full resolution, up to 490 FPS at selected ROI.The QHY5-III series cameras are USB3 super-speed cameras and guiders. They can be used in a standard 1.25-inch eyepiece holder. All QHY5III series cameras come in a very small but powerful package!

Specifications QHY5III174M