Specifications for the Atik 414EX Mono

Sony EXview HAD CCD II ICX825 sensor - Super Sensitive

The fact that you're reading this this shows you've made it past the most common trap in choosing a camera for astroimaging - how many megapixels is it?

There are 2 variables in your camera that are far more important to consider when imaging faint deep sky objects. Sensitivity and noise.

The sensitivity tells us how many precious photons will be converted to signal...this is were the new Sony ICX825 shines! But how much more sensitive is it? Compared with Atik's previous 314L+ at 650nm, the 414EX is 60% more sensitive. In fact, the 414EX is even more sensitive than the already spectacular 460EX, making it the perfect camera for the enthusiast with a limited budget. The graph below shows the striking difference between the ICX285 and ICX825:

Low noise and effective cooling

Atik's 414EX has more than just great sensitivity.

Another feature of the 414EXmaking it a winner for astrophotography is it's exceptionally low noise. When capturing a stunning portrait of your favourite deep sky target you will understand how delicately faint it is. This means the data you wish to capture is sparse.

If the electronics of the camera add noise (unwanted signal) to your image the end result will be lacking in detail and contrast. To ensure the contribution from noise is minimised Atik's 414EX has thermoelectric cooling that can easily lower the CCD chip to 30ºC below ambient, and is regulated, so that your image calibration is consistent. This results in a noise level so low that for most applications dark frames are an option rather than a requirement. The upshot is that you can spend more time imaging!

An image of M106 taken with Atik 414EX (courtesy of atik-cameras.com)

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

Main Features:

Anti-dew

ASI6200 Pro comes with the polyimide heater that can avoid any dew problems.
The anti-dew heater which completely fit the protective window will heat it to avoid any dew problems.

Full Frame format

The ASI6200 Pro camera uses a full-frame format. The outstanding 9576x6388 resolution provided by the onboard Sony IMX455 sensor makes this camera a 61.2-megapixel full frame powerhouse! The sensor length and width are 36mm x 24mm respectively, and the diagonal is 43.3mm. This is a camera with a small pixel size of 3.76um that can accommodate a large well depth of 51.4ke.

Native 16bit ADC

ASI6200 Pro camera is our first batch of CMOS astronomy cameras with true 16-bit ADC. It is not a CCD-style 16-bit ADC – it really can achieve a dynamic range output of 14 stops. This significantly improves the image sharpness and contrast, and the contrast gradients are smoother and more natural-looking.

Built for astrophotography

USB3.0 & 512M DDR3 Memory
The ASI6200 Pro camera is equipped with a USB 3.0 transmission interface and a built-in 512MB DDR3 cache to ensure stable and secure data transmission.

QE value

The QE peak value of the ASI6200MC Pro camera is 80%.

Relative response（ASI6200MC Pro）

The QE peak value of the ASI6200MM Pro camera is 91%.

Ultra-low dark current

The unique dark current suppression technology can further reduce dark current noise. At a cooling temperature of 0°C, the dark current noise is only 0.0017e/s/pix. This means a 300s exposure will only cause a dark current noise of 0.51 e/pix, which is completely negligible!

Camera Details

Some images by ZWO users

The best solution of 55mm back focus length

Mechanical Diagram

What's in the box?

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.

Astronomical camera with large full well capacity
ASI585MM

ASI585MC adopts Sony IMX585 CMOS sensor. As one of ZWO's latest planetary cameras, it features a large sensor format of 1/1.2", a high resolution of 3840*2160, and a surprisingly amazing characteristic of ZERO AMP GLOW! The pixel size is 2.9um*2.9um. In 12-bit mode, it produces 46.9 FPS with super low readout noise!

8.29MP Senor

ASI585MM has the same pixel size of the ASI462MC at 2.9um, but its resolution is 4 times that of ASI462MC, which is a total of 8.29 megapixels. The sensor size is 11.13*6.26mm, and the diagonal length is 12.84mm. The 1/1.2" large sensor format makes it very suitable for solar and lunar imaging. It can also be used as an all-sky camera or live camera to observe and monitor cloud cover, rain, meteors and other weather conditions.

STARVIS 2

ASI585MM adopts the Latest SONY IMX585 sensor with STARVIS 2 technology. Featuring zero amp glow, lower dark current noise, and 3 times larger full well capacity, this camera is regarded as an upgrade of ASI485MC. It is also more sensitive to red, green and near infrared (NIR) lights compared to ASI485MC, especially in >850nm wavelength range, its light sensitivity is 1.5 times greater than ASI485MC.

Upgraded Model

The ASI585MM is an upgraded camera to the ASI485. Compared with the ASI485MC, it has the characteristics of a larger full well depth and no amp glow.

Large Full Well Depth

Thanks to the back-illuminated sensor structure and advanced pixel technology, the camera has very low readout noise and a large full well depth. Especially in low light conditions, the camera performs excellent, capturing very clear images of celestial objects.

Camera Curve

Low read noise, high dynamic range

The camera has a built-in HCG mode, which can effectively reduce readout noise at high gain and allow the camera to m aintain the same high dynamic range as it does at low gain. When the gain is 150, the HCG mode is automatically turned on and the dynamic range reaches a level close to 12bit. The readout noise is as low as 0.8e.

Specifications for the Atik 414EX Colour

Sony EXview HAD CCD II ICX825 sensor - Super Sensitive

The fact that you're reading this this shows you've made it past the most common trap in choosing a camera for astroimaging - how many megapixels is it?

There are 2 variables in your camera that are far more important to consider when imaging faint deep sky objects. Sensitivity and noise.

The sensitivity tells us how many precious photons will be converted to signal...this is were the Sony ICX825 shines! But how much more sensitive is it? Compared with Atik's previous 314L+ at 650nm, the 414EX is 60% more sensitive. In fact, the 414EX is even more sensitive than the already spectacular 460EX, making it the perfect camera for the enthusiast with a limited budget. The graph below shows the striking difference between the ICX285 and ICX825:

Low noise and effective cooling

Atik's 414EX has more than just great sensitivity.

Another feature of the 414EXmaking it a winner for astrophotography is it's exceptionally low noise. When capturing a stunning portrait of your favourite deep sky target you will understand how delicately faint it is. This means the data you wish to capture is sparse.

If the electronics of the camera add noise (unwanted signal) to your image the end result will be lacking in detail and contrast. To ensure the contribution from noise is minimised Atik's 414EX has thermoelectric cooling that can easily lower the CCD chip to 30ºC below ambient, and is regulated, so that your image calibration is consistent. This results in a noise level so low that for most applications dark frames are an option rather than a requirement. The upshot is that you can spend more time imaging!

The Atik 460EX offers the latest and greatest of Sony's CCDs, the ICX694. Featuring the latest generation EXview technology, this camera has outstanding Quantum Efficiency, very low noise, and excellent thermal management.

This model is an ideal match for telescopes commonly used by amateurs, up to bigger SCTs or RCs. Its excellent sensitivity makes it one of the best cameras for deep-sky astrophotography, offering a logical upgrade path for smaller CCD camera owners looking for uncompromising performance.

With more than twice the imaging area than the venerable ICX285, it will satisfy the need for larger sky coverage while maintaining excellent low-noise characteristics.

The Atik 460EX fully supports 1.25" filters down to f/2, so you won't need to replace any of your current investments in wheels or filters. This is an added advantage when looking to invest in a CCD camera that may go through multiple telescopes.

The Atik-4 Series cameras are a development of the renowned 3-Series cameras, featuring better cooling and a narrower body. They benefit from setpoint cooling to make taking matching dark frames a snap, and simple 12V power requirement to facilitate field operation. The impressive sensitivity, great cooling, and narrow profile make the Atik Series 4 outstanding CCD cameras to use on modern telescopes, including Hyperstar/Fastar systems.

Specifications

Instruction Manual

Combination CCD imaging kit including:

• TRIUS PRO-694 Blue Edition Camera
• Lodestar PRO Guider
• Midi Filter Wheel with built-in OAG (with 7 x 1.25″ filter wheel carousel)

Camera Details

• Medium format, high resolution ‘Exview’ CCD chip, with 6,050,000 x 4.54uM square pixels in a 15.98mm diagonal array.
• Exceptionally low dark signal – No dark frames necessary for most deep sky objects.
• Excellent QE of 77% peak in yellow light, 65% at Hydrogen alpha (656 nm).
• Three port powered USB hub built-in. Can drive a Lodestar PRO or Ultrastar PRO + SX filter wheel.
• High performance two stage cooling for better than -40C delta T
• Dry Argon CCD chamber fill for improved cooling performance.
• Exceptionally effective anti-blooming with minimal effect on linearity and no lost active area.
• Back focal length 16mm +/-1mm.

• High speed USB 2.0 interface for approx. 2.5 second downloads.
• Built-in triple powered USB hub for guider and filter wheel control.
• Single USB cable control for all features – get rid of that dangerous cable tangle!
• 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.

Specification

• CCD type: ICX694AL 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: 2750 x 2200 pixels
• CCD Image area: 12.49mm (Horizontal) x 9.99mm (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 0.002 electrons/second @ – 10C CCD temperature.
• Data format: 16 bits.
• System gain: 0.27 electrons per ADU
• Computer Interface: Built-in USB 2.0 compatible interface.
• Image download time: Typically 2.5 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.

Loadstar Pro details

The Lodestar PRO is an upgraded version of the very popular Lodestar X2 autoguider with quicker download times and lower read noise electronics. The original Lodestar used the ICX429 Exview chip from Sony and offered excellent sensitivity. However, the Lodestar X2 and the Lodestar PRO utilise Sony’s upgraded version of the CCD, the ICX829, with considerably improved QE and read noise. This new ‘Exview 2’ chip approximately doubles the Lodestar sensitivity and adds nearly a full star magnitude to the minimum guide star brightness. We have also redesigned the boards so that a standard RJ12 guide socket can be used. This will please many users who have found the small ‘ZH’ cable socket to be too delicate.

Specification

• CCD – Sony ICX829AL ExView2 monochrome CCD
• Pixel count – 752(H) x 580(V)
• Pixel size – 8.6 x 8.3uM
• Optical size – 6.47 x 4.81 mm
• Read noise – Typically 5.5 electrons
• Gain – 0.4 e/ADU
• Barrel size – 31.75mm dia. x 85mm long (1.25 inch eyepiece push fit size)
• Barrel thread – 25.4mm x 0.75mm ‘CS’ mount lens thread
• Computer connection – ‘Mini B’ USB socket for USB2.0
• Output connection – Standard RJ12 autoguider socket
• Output type – Opto-isolated 4 lines (N,S,E & W) pull down with common return line
• Download rate – Approx. 10 frames per second in binned 2×2 mode (recommended)

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

The Atik 16200 Monochrome camera has been designed from the ground up around the KAF-16200 sensor. With a diagonal measurement of 35mm (APS-H format) and 6 μm pixels this camera is an incredible mix of high resolution and sensor real estate.

It is a great match for a range of telescopes, and all at a much more accessible price than the likes of KAF-11002 and KAF-16803 based cameras.

The design sees the CCD housed in a sealed, argon-purged chamber, complemented by a powerful dual-stage peltier and heatsink for optimum cooling. This camera has the lowest delta you’ve ever seen from Atik, at -45°C typical, and a whopping -50°C max.

Atik 16200 Monochrome Technical Specifications

• Sensor Type: CCD - KAF-16200
• Horizontal Resolution: 4499 pixels
• Vertical Resolution: 3599 pixels
• Pixel Size: 6 µm x 6 µm
• ADC: 16 bit
• Readout Noise: 9e- typical value
• Gain Factor: 0.6e-/ ADU
• Full Well: ~40,000e-
• Dark Current: >0.25 electrons/second at 0°C
• Interface: USB 2.0 High Speed
• Power: 12v DC 2.5A
• Maximum Exposure Length: Unlimited
• Minimum Exposure Length: 200 ms
• Cooling: Thermoelectric set point with max ΔT=>-50°C (-45°C typ.)
• Weight: approx. 1.3 kg
• Backfocus: ±19.5 mm
• Available as mono or colour, with colour version to follow early 2017

The Atik 383L+ is an 8-megapixel camera using the Truesense KAF-8300 CCD. Much has been written about this CCD to justify its place in astronomers' hearts. It can be succinctly summed up by saying that it's a fabulous CCD, with a huge number of good-sized pixels, and is currently available at an irresistible price.

This sensor has redefined mid-range astro-imaging, making multi-megapixel cooled cameras much more accessible.

Atik prides itself on providing cameras offering the very highest image quality at a reasonable cost. They have built on the success of the highly-regarded Atik 314 platform to support Kodak's KAF-8300. This immediately offers a huge number of advantages, including the very low read-noise circuits and the reliability of using this established design.

Specifications for the Atik 383L+ Mono

Mechanical Drawing

Quality hardware

The key to any high-quality camera is the ability to convert light collected by the sensor into digital information while ensuring that as little noise as possible is added. The digital image needs to truly reflect the light collected. The Atik 383L+ achieves this, by having:

• Very low read-noise, 7 electrons, on par with many Sony sensors, enabling faint details to be detected.
• Great linearity, with a regression correlation coefficient of R = 0.9998 over the range of 1,000 to 64,000, making the camera suitable for sensitive photometric measurements.
• The bias frame histogram from the camera shows the ideal Gaussian shape, indicating that maximum detail can be extracted on processing.

The Atik 383L+ is a dream combination of low-noise electronics and a scientific-grade sensor that we are able to offer at a fantastic price. Whether you are an established imager or are just starting, the Atik 383L+ is a great choice.

Instruction Manual

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

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

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.

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.

New Planetary Camera from ZWO

ZWO ASI664MC is a remarkable new planetary CMOS camera. The 1/1.8" Sony IMX664 sensor features a small pixel size of 2.4µm pixel and a high resolution of 2704 x 1536 (4.15Mp). In high-speed mode the frame rate reaches 95 fps, while the read-out noise remains at a low level, as low as 0.46e!

Starvis 2 Technology

If you're not familiar with SONY STARVIS technology it offers the ZWO ASI664MC outstanding image quality and image performance.

High Transmission Speed

This camera has a USB 3.0 Interface, along with the built-in 256MB DDR# cache, ensuring high-speed, smooth, and stable data transmission.

ZWO ASI664MC vs ZWO ASI662MC

ZWO ASI664MC can be considered as an iteration of the ASI662MC. With the great improvement in sensor size and resolution, it provides a larger FOV and results in high-quality images containing more details.

Zero Amp Glow

ZWO ASI664MC adopts no-glow circuitry to avoid annoying amp glow being produced and ensure the image quality no matter how long the exposure and how high the gain value is.

(NOTE: This feature is implemented directly at the hardware level, it does not require software control.)

Camera Curve

Low readout noise, high dynamic range

The camera has a built-in HCG mode, which can effectively reduce readout noise at high gain and keep the dynamic range at the same level as it does at low gain. At 252 and above the HCG is automatically turned on; the dynamic range is close to 11bit; the readout noise can be lower than 1.0e.

Quantum Efficiency

QE noise and readout are very important parameters to measure the camera's performance. Higher QE and lower readout noise are necessary to improve the image signal-to-noise ratio. according to our estimation, the QE peak value of the ZWO ASI664MC is about 91%

Protective Window

The ASI664MC adopts an AR-coated filter as a protective window (Diameter: 21mm, Thickness: 1,1mm). It improved the camera's performance in UV and NIR wavelengths.

Designed and manufactured in the USA with same extreme reliability as the thousands of FLI OEM cameras. Install in remote observatories around the world with complete confidence in a long, trouble-free life. High sensitivity CMOS camera with 90% quantum efficiency and 15.9 mm diagonal field of view is an ideal replacement for 1" format CCDs.

Designed and manufactured in the USA with same extreme reliability as the thousands of FLI OEM cameras. Install in remote observatories around the world with complete confidence in a long, trouble-free life. High sensitivity with exceptionally low noise and dark current. Great combination of resolution and frame rate.

Designed and manufactured in the USA with same extreme reliability as the thousands of FLI OEM cameras. Install in remote observatories around the world with complete confidence in a long, trouble-free life. Full frame sensor with 90% quantum efficiency and massive 43.1mm diagonal field of view to increase throughput.