Antlia ALP-T Dual Band 5nm Highspeed Filters are optimized to work with high-speed imaging systems by shifting slightly the passband and center wavelength. Using these highspeed filters between optics f/2.2 and f/3.6 shows much stronger and more contrasted in nebulae imaging compared to the standard version, if you seek the best possible performance with any optics faster than f/2.2, the highspeed version is the best choice.

But keep in mind, the blue shift data by the computer simulation indicates narrowband filter shifts its bandwidth to shorter wavelengths with faster optics than f/2, transmission at the emission wavelength may decrease perhaps 15%-20%. Although the Antlia ALP-T highspeed filter has similar transmission rates reduction in the H-a and OIII when the filter is used on fast optics, based on current standard version users’ data, it is evident that the filter still has the high performance of increase in emission nebula contrast and minimized halo.

The highspeed version price is the same as the standard filters and double benefits for the high-speed optics users. Worth mentioning is that Antlia inspected and measured products piece by piece with one of Agilent Cary’s professional spectrophotometer, resolution/slit width is up to 0.2nm, which make us provide highly reliable and consistent products to you.

The Antlia ALP-T dual band 5nm series filter is a dual line-pass filter that was designed to be used primarily with one-shot color (OSC) cameras such as DSLR's and astronomical OSC cameras. It can also be used as a narrowband filter for monochrome cameras to save imaging time. The advanced multi-coatings on our ALP-T ultra dual band filter effectively isolate the red Ha and the blue-green OIII lines light from emission nebulae, with almost total suppression of optical density (OD)4.5 on unwanted wavelengths from light pollution, moonlight, and airglow. The result is that our ALP-T dual band 5nm filter creates a superior signal-to-noise ratio and better contrast in your images.

The filter enables the capture of the two main emission nebulae bands at the same time, whilst suppressing unwanted light pollution. It enables you to capture cleaner data and reduces the post-processing efforts to isolate faint details from the background light pollution.

Application and Performance:

Designed especially for fast astronomy optics, in particular f-ratios f/2.2 to f/3.6

Engineered specifically for use with DSLR, CMOS, and CCD color cameras

Suppression of optical density (OD)4.5 on unwanted wavelengths adds signal-to-noise

Extremely steep bandpass edges minimize internal reflections

Ideal flat-top and moderate bandpass reducing spectrum down shifts

Ion Gun Assisted Deposition coating technology on the double-sided polished substrate making it the most consistent and accurate light pollution suppression filter

Designed to suppress artificial lighting from Bortle scale 1 to Bortle scale 8

Near IR (NIR) is blocked up to 1050nm

Technical Specifications:

Filter Ring:

2'' (M48*0.75)

Ultra-thin filter cell to minimize vignetting by maximize possible clear aperture

Black Anodized Finish

Laser Engraving No Fading

Spectrum Curve:

Not Recommended:

Solar imaging

Night visual observation

Not Permitted:

DO NOT LOOK AT THE SUN WITH THIS FILTER

Serious eye damage will result if you fail to observe the warning

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

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 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.

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 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.

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.

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

Embark on another cosmic adventure and discover the striking artistry of NASA’s mission patches and logos. This beautifully illustrated book offers a visual tour of NASA’s heritage symbolism from the early Mercury missions of the 1960s to the rovers, orbital telescopes and brand-new lunar capsules of the 2020s.

The countdown is underway! NASA’s first Moon landing since 1972 is now on the near horizon and this follow-up to the popular Space: Posters & Paintings is the perfect way to prepare for take-off. Celebrating the achievements of the men and women who dared to venture into the beyond, Space: The Mission Patches uncovers the story of the space administration through the indelible artwork of their historic insignias. Perfect for space aficionados, design enthusiasts and kids old and young, this meeting of art and exploration is the definitive testament to the enduring legacy of NASA’s trailblazing journeys to the unknown.

AUTHOR:
For over 25 years, Bill Schwartz has been involved in the production, distribution, licensing and branding of high-profile entertainment content on a global basis. Along with licensing or acquiring thousands of hours of feature films, television series and documentaries, Bill has created and produced 20 broadcast documentaries, including Terror On The Titanic, Howard Hughes: The Real Aviator and Valkyrie: The Plot To Kill Hitler. Of all of Bill’s productions, his passion project was Journey to Mars, a documentary about NASA’s Viking Pathfinder, the first vehicle to explore the surface of Mars. The story, the trust and the investment required gave a true insight to the drama and courage of the people and technology at NASA.

The IRDK14 from PlaneWave Instruments is a precisely engineered optical system designed for high performance in infrared wavelengths. It is an excellent tool for advanced astronomical research and remote sensing applications, offering superior performance for infrared imaging.

IRDK14’s Key Features

Large Aperture and Optimized Focal Ratio

The IRDK14 features a 356 mm aperture and an f/7.2 focal ratio, enhancing its capacity to gather infrared light effectively. This setup is ideal for detailed infrared observations and long-exposure imaging, providing exceptional light-gathering capabilities.

Specialized Optical Design for Infrared

The Dall-Kirkham optical design of the IRDK14 is optimized for infrared wavelengths. There are no refractive lenses, only reflective fused silica mirrors. The reflective coatings are a protected gold with better than 98% reflectivity from .65 microns (650nm) to 5 microns (5000nm), making it well-suited for infrared astronomy or LIDAR applications. UV-optimized coatings can also be provided, and potential customers are encouraged to contact our technical sales team to discuss UV optimization.

Robust Mechanical Structure

Constructed using carbon fiber, the optical tube of the IRDK14 offers durability and stability with minimal thermal expansion. This design ensures consistent performance under various environmental conditions, making it suitable for intensive scientific applications.

Advanced Thermal Management

The IRDK14 includes cooling fans and a system prepared for Delta-T applications, promoting rapid thermal equilibrium. This feature is critical for minimizing air turbulence within the tube, thus reducing potential image distortion and enhancing overall imaging quality.

Integrated Dew Control

Infrared observations are prone to condensation, but the IRDK14 tackles this with advanced dew prevention technology. Heater pads, controlled via PlaneWave’s software, ensure the optical surfaces stay clear from dew, maintaining consistent and clear imaging performance.

Application-Specific Benefits

Infrared Astronomy

The IRDK14 excels in infrared astronomy, where its significant aperture and infrared-optimized optics allow for precise observation of celestial objects in infrared light. This capability is essential for studying astrophysical phenomena invisible to the naked eye or standard optical wavelengths.

Advanced Research and LIDAR Applications

With its specialized design and infrared optimization, the IRDK14 is a robust platform for advanced scientific research, including LIDAR and other remote sensing applications.

Key Features Overview

The IRDK14 comes with impressive specifications tailored for infrared optimization:

• Gold-coated mirrors optimized for high reflectivity in infrared wavelengths (ultraviolet optimization available)
• 14-inch (356 mm) aperture
• 2563 mm focal length
• f/7.2 focal ratio
• 282mm back focus from mounting surface
• 70mm image circle
• Rock-solid fused silica mirrors with low thermal expansion
• Lightweight and rigid carbon fiber optical tube assembly

Optical Systems

Secondary Mirror

Primary Mirror

The Paramount ME II Large Dovetail is an optional accessory that enables the Paramount ME II’s Versa-Plate to accept optical tube assemblies that use the Planewave Instrument dovetails (including PlaneWave Instruments and Officina Stellare telescopes).

The large dovetail is rated to carry 108 kg.

Total additional weight is 1.5kg

This unit is included in the Multi OTA Mounting Kit

Capturing the most stunning astrophotographs possible is something our team is passionate about. From design to manufacture, our goal with the Corrected Dall-Kirkham (CDK) 20″ telescope was centered around performance and ease of use. The Planewave CDK20 f/7.7 OTA is an incredible breakthrough in telescope technology and produces no off-axis coma and no off-axis astigmatism. Additionally, the CDK20 provides a perfectly flat field so your astrophotographs will have stunning clarity from corner to corner of the image without field curvature degrading the photos. Offering the simplicity of single-mirror collimation, the stray light control of advanced baffles, structural performance created through finite element analysis (FEA), and decades of telescope design experience, the CDK20 is an exceptional diffraction-limited telescope. CDK20 users can experience pinpoint stars edge-to-edge and a 45 x 45 arcminute field of view when using large 16803 size camera sensors. When equipment fades into the background and simply performs, the astrophotography experience becomes even more fun and rewarding!

• The Delta T controller is an optional accessory for dew prevention on CDK14 through CDK24 OTAs and the CDK700 system.
• CDK12.5 to CDK24 and CDK700 telescopes come with primary and secondary mirror dew heating pads (CDK700 adds tertiary mirror heating), which are ready to accept the Delta T controller.
• Controlled via PWI3 software for CDK12.5 through CDK24 OTAs (PWI2 for the CDK700).

With Delta T you can:

• Have Full Control of Primary and Secondary Heater using PlaneWave Interface (PWI3) Software.
• Monitor current temperature of primary mirror, secondary mirror and surrounding ambient temperature.
• Automatically maintains mirror temperature set point as outside temperature changes.
• Displays real time graph of all temperature sensors.

The CDK400 Observatory System from PlaneWave Instruments is designed for the sophisticated astrophotographer and dedicated astronomy researcher. This premium package combines the high-performing CDK17 optical tube with the advanced L-500 direct-drive mount to provide a superior observational platform that excels in a range of applications, from detailed celestial research to high-end astrophotography.

Key Features of the CDK400 Observatory System

CDK17 Optical Tube Assembly

• Aperture and Focal Length: Features a 17-inch aperture and a 2939 mm focal length at an f/6.8 focal ratio, optimizing it for deep-sky imaging with excellent depth and clarity.
• Advanced Optical Design: Utilizes a Corrected Dall-Kirkham optical design, delivering a field free of off-axis coma and astigmatism and achieving a perfectly flat field across a 70 mm image circle, resulting in critically sharp images across the entire viewing area.
• High-Quality Construction: Made with lightweight yet robust carbon fiber, reducing thermal expansion and allowing for rapid thermal equilibration, which helps maintain precise optical alignment under fluctuating temperatures.
• Superior Mirrors and Coatings: Equipped with high-stability fused silica mirrors known for minimal thermal expansion, paired with high-performance coatings that maximize light throughput while minimizing stray light for optimal imaging quality.
• Thermal Management: Features an advanced cooling system with strategically placed fans that promote rapid thermal stabilization, essential for maintaining consistent high-quality imaging and minimizing focus shifts caused by temperature changes.

L-500 Direct Drive Mount

• Direct Drive Motors: Employs state-of-the-art direct-drive motors on each axis, ensuring smooth, fast, and virtually silent movement of the telescope with zero backlash and zero periodic error, perfect for precise tracking and swift repositioning of celestial objects.
• High-Resolution Encoders: Outfitted with high-resolution optical encoders on both axes, providing exacting positioning and movement, crucial for top-tier astrophotography and detailed astronomical studies.
• Azimuth Dovetail Balance System: Incorporates a finely adjustable balance system that improves the stability and performance of the setup in both alt-azimuth and equatorial configurations, essential for prolonged accurate tracking and reducing stress on the mount during extended observations.
• Rapid Target Acquisition: Achieves impressive slew speeds up to 50 degrees per second, allowing for quick and efficient targeting of celestial bodies and satellites, vital for dynamic observations and responsive astrophotography.

Application-Specific Advantages

Astrophotography

The CDK400 stands out as a formidable system for astrophotographers, offering unmatched tracking accuracy and image stability which facilitate capturing spectacular celestial images with detailed resolution and vibrant colors.

Astronomy Research

Researchers will appreciate the CDK400 for its consistent performance and precise data collection capabilities. It serves as a robust platform for sophisticated photometry, spectroscopy, and minor planet tracking, offering a solid foundation for scientific discovery and exploration.

Visual Observations

For enthusiasts of visual astronomy, the CDK400 delivers vibrant and detailed views of the universe. Its significant aperture and high-quality optical components ensure exceptional viewing of planetary, lunar, and deep-sky objects, enriching every observational experience.

Space Situational Awareness (SSA) and Space Domain Awareness (SDA)

With its swift and precise repositioning capabilities, the L-500 mount in the CDK400 system is capable of tracking satellites and space debris. However, it's important to note that while the L-series mounts are highly effective for astrophotography and research applications, they might not meet the optimal performance standards required for dedicated SSA/SDA operations. For those needs, we recommend exploring our T-600 Direct-Drive Gimbal, specifically engineered to exceed the demanding requirements for SSA/SDA applications, ensuring superior tracking and responsiveness in monitoring and cataloging space objects.

Mount System 

Control System

Optical Systems

Mechanical Structure

Motion control

System Performance 

Included items

IRDK17’s Key Features

Large Aperture and Optimized Focal Ratio

The IRDK17 features a considerable 432 mm aperture and an f/6.8 focal ratio, enhancing its ability to capture infrared light effectively. This configuration is ideal for precise infrared observations and long-exposure imaging, offering superior light-gathering capabilities.

Specialized Optical Design for Infrared

The Dall-Kirkham optical design of the IRDK17 is finely tuned for infrared wavelengths. There are no refractive lenses, only reflective components made from fused silica. The reflective coatings are a protected gold with better than 98% reflectivity from .65 microns (650nm) to 5 microns (5000nm), making it optimal for infrared astronomy or LIDAR applications. UV-optimized coatings can also be provided, enhancing the telescope's versatility—please contact our technical sales team to discuss UV optimization.

Robust Mechanical Structure

Constructed using carbon fiber, the optical tube of the IRDK17 ensures durability and stability with minimal thermal expansion. This feature guarantees consistent performance across various conditions and is suitable for intensive scientific and research applications.

Advanced Thermal Management

The IRDK17 has cooling fans and a system ready for Delta-T applications, promoting rapid thermal equilibrium. This system is essential for minimizing air turbulence within the tube, reducing potential image distortion, and improving overall imaging quality.

Integrated Dew Control

Given that infrared observations are prone to condensation, the IRDK17 incorporates advanced dew-prevention technology. Heater pads, controlled via PlaneWave’s software, ensure the optical surfaces remain clear from dew, maintaining consistent and sharp imaging performance.

Application-Specific Benefits

Infrared Astronomy

The IRDK17 excels in infrared astronomy, where its large aperture and infrared-optimized optics allow for detailed observation of celestial objects in infrared light. This capability is vital for uncovering astrophysical phenomena invisible to the naked eye or conventional optical wavelengths.

Advanced Research and LIDAR Applications

With its specialized design and infrared optimization, the IRDK17 is a robust platform for advanced scientific research, including applications in LIDAR, leveraging its specialized optical capabilities.

Optical Systems

Secondary Mirror

Primary Mirror

PlaneWave CDK 12.5 Fused Silica

Capturing the most stunning astrophotographs possible is something our team is passionate about. From design to manufacture, our goal with the Corrected Dall-Kirkham (CDK) 12.5″ telescope was centered around performance and ease of use. The PlaneWave CDK 12.5 Fused Silica is an incredible breakthrough in telescope technology and produces no off-axis coma and no off-axis astigmatism. Additionally, the PlaneWave CDK 12.5 Fused Silica provides a perfectly flat field so your astrophotographs will have stunning clarity from corner to corner of the image without field curvature degrading the photos. Offering the simplicity of single-mirror collimation, the stray light control of advanced baffles, structural performance created through finite element analysis (FEA), and decades of telescope design experience, the CDK12.5 is an exceptional diffraction-limited telescope. CDK12.5 users can experience pinpoint stars edge-to-edge and a 70 x 70 arcminute field of view when using large camera sensors. When equipment fades into the background and simply performs, the astrophotography experience becomes even more fun and rewarding!

The PlaneWave CDK 12.5 Fused Silica is a 12.5 inch (0.32 m) f/8 Corrected Dall-Kirkham Astrograph telescope. The telescope has a closed carbon fiber tube, with 3 cooling fans ejecting air from the back of the telescope. The PlaneWave CDK 12.5 covers a 52 mm field of view without any field curvature, off-axis coma, or astigmatism. The instrument weight is 21kg and comes standard with the large capacity 2.75 inch Hedrick focuser.

Technology

The CDK Optical Design

The CDK telescope is based on a new optical design developed by Dave Rowe. The goal of the design is to make an affordable astrographic telescope with a large enough imaging plane to take advantage of the large format CCD cameras of today. Most telescope images degrade as you move off-axis from either coma, off-axis astigmatism, or field curvature. The CDK design suffers from none of these problems. The CDK is coma free, has no off-axis astigmatism, and has a flat field. The design is a simple and elegant solution to the problems posed above. The CDK consists of three components: an ellipsoidal primary mirror, a spherical secondary mirror and a lens group. All these components are optimized to work in concert in order to create superb pinpoint stars across the entire 52mm image plane.

Optical Performance

Shown are two simulations showing the CDK’s stunning performance. The first is a diffraction simulation and the second is a spot diagram. In both simulations the small squares are 9×9 microns, about the size of a CCD pixel. In the diffraction simulation the star images on axis and off-axis are nearly identical. In the spot diagram 21mm off-axis the spot size is an incredible 6 microns RMS diameter. This means stars across a 52 mm image circle are going to be pinpoints as small as the atmospheric seeing will allow.

Both of the simulations take into consideration a flat field, which is a more accurate representation of how the optics would perform on a flat CCD camera chip. For visual use some amount of field curvature would be allowed since the eye is able to compensate for a curved field. The diffraction simulation was calculated at 585nm. The spot diagram was calculated at 720, 585, and 430nm. Many companies show spot diagrams in only one wavelength, but you cannot see the chromatic performance with only one wavelength.

Comparison: CDK vs. Ritchey Chrétien

The simulations shown compares the optical performance of the CDK design to the Ritchey Chrétien (RC) design. The Ritchey design was popularized as an astroimaging telescope due to its use in many professional

observatories. Although very difficult and expensive to manufacture and align, the Ritchey is successful in eliminating many of the problems that plague many other designs, namely off-axis coma. However the Ritchey does nothing to eliminate the damaging effects of off-axis astigmatism and field curvature.

The CDK design tackles the off-axis coma problem by integrating a pair of correcting lenses into a two mirror design. The beauty is that this design also corrects for astigmatism and field curvature. Because the lenses are relatively close to the focal plane (unlike the Schmidt corrector plate found in various Schmidt Cassegrain designs), and because these lenses work together as a doublet, there is no chromatic aberration. The CDK offers a wide aberration-free, flat field of view that allows the user to take full advantage of the very large imaging chip cameras in the market place today.

Having an aberration free telescope design means nothing if the optics cannot be aligned properly. Many Ritchey owners never get to take full advantage of their instrument’s performance because the Ritchey is very difficult to collimate. Aligning the hyperbolic secondary mirror’s optical axis to the optical axis of the primary mirror is critical in the Ritchey design, and the tolerances are unforgiving. The secondary mirror of the CDK design is spherical. It has no optical axis and so the centering tolerance of the CDK secondary mirror is comparatively huge. With the help of some very simple tools, the CDK user will be able to set the secondary spacing, collimate the optics and begin enjoying the full performance potential the instrument has to offer within a few minutes.

The drastic difference in performance between the CDK and the RC is apparent. The biggest component that degrades the off-axis performance of the RC is the defocus due to field curvature. In many diagrams shown by RC manufacturers, the diagrams look better than this because they are showing a curved field. This is fine for visual use because the eye can compensate for some amount of curvature of field. But CCD arrays are flat and so in order to evaluate the performance a spot diagrams and/or diffraction simulations requires a flat field as shown.

PlaneWave CDK 12.5 Specifications

OPTICAL SYSTEM

SECONDARY MIRROR

PRIMARY MIRROR

LENS GROUP

SHIPPING

INCLUDED ACCESSORIES

Collimation and Spacing Instructions

PlaneWave CDK 14" Fused Silica

The CDK (Corrected Dall-Kirkham) Optical Design is an innovative solution for unsurpassed astroimaging quality at an affordable price. The CDK telescope design provides excellent imaging with large format CCD cameras while remaining superb for visual use. The CDK design far exceeds the off-axis performance of most commercial telescope designs including the Ritchey-Chrétien design.

FUSED SILICA

Fused Silica is a synthetic amorphous silica glass of the highest purity and one of the most transparent glasses made.

The optical and thermal properties of fused silica are superior to other types of glass due to its purity. Its transmission and homogeneity exceed those of crystalline quartz without the problems of temperature instability inherent in the crystalline form.

Fused Silica has a coefficient of thermal six times lower than Borosilicate glass, which means that as fused silica cools down, it preserves its shape to a high degree of accuracy. This translates into consistent optical performance and unchanging focus over temperature changes.

With high melting temperature (~1,600 degrees Celsius), a very low coefficient of thermal expansion and resistance to thermal shock, fused silica is the material of choice for professional observatories as well as various scientific applications.

This no-compromise design is unique in making the optical alignment forgiving and collimation very easy. This guarantees the user the best possible performance from the telescope. The end result at the image plane of the CDK design is no off-axis coma, no off-axis astigmatism, perfectly flat field (no off-axis defocus). The CDK design will give you pinpoint stars from the center to the corner of the field of view.

More about our Optical Design

Features:

PlaneWave CDK 14" Fused Silica Specifications

OPTICAL SYSTEM

SECONDARY MIRROR

PRIMARY MIRROR

LENS GROUP

STANDARD FEATURES

SHIPPING

NOTE: This product has a lengthy lead time. Please contact education@bintel.com.au for further information.

The PlaneWave L500 combines versatility, simplicity and affordability by combining all the technology of our Observatory class telescopes into a compact stand-alone mount. In its Alt/Az configuration it is considerably more compact than its equatorial counterpart, allowing a larger telescope to fit in a smaller enclosure. The mass it takes to make a rigid alt/az mount is substantially less, leading to cost savings. Unlike German Equatorial mounts, there are no meridian flips to deal with, and no large protruding counterweights to create a dangerous hazard in a public observatory. Alt/Az is more intuitive to use and no polar alignment is needed. Besides, it is the way the pros do it!

Planewave L500 Mount Features:

• Direct-drive motors on each axis for smooth, fast, and virtually silent movement of the telescope
• Slew speeds up to 50 degrees per second
• High resolution encoders on each axis for precise positioning
• Zero backlash
• Zero periodic error
• PointXP mount modeling software
• Enclosed electronics
• Through the mount cabling

FEATURES:

MOUNT SYSTEM

CONTROL SYSTEM

MOTION CONTROL

SYSTEM PERFORMANCE

Check the PlaneWave website for Instructions and Schematics.

This spacer ring lets you obtain the correct spacing between a 1.25" Star Analyser 100 and a camera sensor.

50 mm bright. 42 mm light.
ZEISS SFL 50 Binoculars

The ZEISS SFL 50 binoculars offer premium optics in an exceptionally lightweight and compact design, rivalling traditional 42mm models. Combining outstanding optical performance with portability, they are the perfect choice for those seeking optical excellence and convenience.

The SFL 8x50, featuring 8x magnification, offers a wide field of view that is perfect for observing fast-moving birds and scanning expansive natural landscapes.

Compact and as light as 42 mm binoculars

The optical design prioritizes optimal compactness, featuring thinner lens elements, reduced lens diameter and minimized spacing between lenses. The magnesium housing ensures durability while keeping the weight low, allowing for comfortable, long-term use without fatigue.

Lighter and more compact - how?

The SFL range has become a favourite with bird watchers and nature fans since their launch. Now the SFL 50 delivers viewing normally found in larger optics, but in a smaller size body. 

The ZEISS SFL is shorter and more compact than many other other premium binoculars due to:

Thinner lens elements

Smart design reduces the distance between optical components

Schmidt-Pechan prism design reduces the size while maintaining optical performance

Experience nature in all its splendour

The Ultra-High-Definition (UHD) concept features a special coating and an improved optical design that ensures the binoculars deliver the highest level of detail and reproduce colours with natural fidelity. This makes it possible to precisely identify the smallest features in the plumage and reliably distinguish between species. 

High Performance Optics with UHD Concept

• Large entrance & exit pupils combined with 90 % light transmission ensure bright viewing experience especially in low light conditions
• True-to-life colours provide exceptional colour fidelity for accurate identification of wildlife
• Wide Field of View making it easier to track moving subjects
• Close Focusing Distance of just 1.8 m allows detailed observation of nearby targets.

Bright images even in low light

With 90% light transmission, their large entrance pupil of 50 mm and the ZEISS T* multi-layer coating, you can clearly and precisely see details even in low-light situations and at dusk.

Waterproof, fogproof and UV resistant - perfect for Australian conditions

• Natural rubber armouring material, a NRB compound which is Latex-free and PAH compliant
• Water repellent ZEISS LotuTec lens coating ensures that water beads off without residue immediately, and that dirt and fingerprints do not adhere to the surface. 

Perfect Ergonomics

• SmartFocus Concept features a large focus wheel positioned for optimal accessibility, preventing over-stretching of the focusing finger
• Quick & Precise focusing for fast adjustments, even when wearing gloves
• Perfectly balanced in the hands, enabling long and steady observation
• Smooth and robust eyecups enhance comfort and usability

Upsize 

What are the benefits of 50 mm optics compared to 42 mm optics?

45% more light>

50mm binoculars collect 42% more light than a 42mm models for brighter views and better clarity.  They also offer a larger exit pupil for more comfortable viewing and more immersive experience.

ZEISS SFL 8x50 Specifications

Visit BINTEL for a personal demonstration of this premium ZEISS viewing experience

The world of nature and birding is already truly fascinating when observed with the naked eye. But viewing it through a Victory® Harpia transforms into an entirely new experience.

The unusual optical system features a 3× wide-angle zoom, up to 70× magnification and an objective lens diameter of 95 millimetres. The extremely wide fields of view prove their worth in every situation. The Harpia 95 also features precise focusing with convenient automatic transition from rapid to fine adjustment, even at high magnification factors.

Thanks to its unique, 72° wide-angle field of view throughout the entire 3× zoom range, the unrivalled dynamic of the Victory Harpia guarantees superior performance at long or short distances in every unexpected viewing situation. DualSpeed Focus enables fast focusing and easy, precise, fine focus adjustment, even at high magnification factors.

Elaborate lens system

FL glass and other custom glass ensure an absolutely sharp and colour fidelity image even at maximum magnification.

Subjective 72° angle of vision over the entire zoom range for a noticeably greater overview of the terrain

A clear view, whatever the weather

There are always exciting things to be seen in the world of nature – even in wet weather. This is why ZEISS developed LotuTec®. A coating for the lenses of binoculars and spotting scopes that enables a clear and unhindered view in all weather conditions.

DualSpeed focus

Precise focussing with automatic switching between rapid and fine adjustment.

Compact high performance eyepiece

Slim construction for a comfortable viewing experience. Securely lockable bayonet mount.

ZEISS T* Coating

ZEISS T* coating is a guarantee of the brilliant, high-contrast images­­ which you will experience above all in adverse light conditions and in the twilight. Behind it, however, there is no specific formula for building up the layers. Instead, it is a technology that is constantly adjusted to suit new glass materials and requirements, which varies from lens to lens.

Specifications