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Canada's top-tier Telescopes & Accessories

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12 products

  1. $4,276.26 USD
    Back Order / Waiting List

    Atik Cameras: The Atik 16200 is the highest resolution astrophotography camera in the Atik Cameras range. It has the signature Atik blend of form and function, boasting an APS-H size sensor with a 35mm diagonal in a whole new case design. 

    The sensor has a generous 6µm pixel size which makes it suitable for a huge range of telescopes. The large format size of the camera makes it ideal for astrophotographers looking to capture widefield views of the night sky. It’s also an excellent match for longer focal lengths, capturing intricate details on even the smallest and faintest of objects. Whatever your astrophotography style, the large size of the images give you the freedom and flexibility to zoom in and take a closer look at regions of interest with the level of detail you’d expect from your main target.

    The large size of the sensor is a match for 2″ filters, and is perfectly complemented by the 2″ model of the EFW2. It’s also fully compatible with Atik Air, making it easy to add wifi and ethernet connectivity to your set up.

    The CCD is housed in a sealed, argon-purged chamber to create a dry, condensation free environment. We’ve also introduced a dual-stage peltier and powerful new heatsink for optimum cooling performance. At -45°C typical and a huge -50°C maximum, it’s our best delta yet. All this means you can take stunning low noise images, even when the temperature’s high outside.

    Atik’s high-quality, custom electronics power the sensor to give a read noise of just 9e-. There’s also a new blade shutter which provides consistent and reliable performance over the camera’s lifespan.

    All this is housed inside a brand new case design that gives you optimum performance with minimum fuss, making the Atik 16200 the perfect camera for astrophotographers who want large format images, without the large format price tag.

    A note on CCD Grades

    The Atik 16200 comes with a class II sensor fitted as standard. We feel that the premium prices placed on class 1 sensors just aren’t justifiable when using the camera for astrophotography. If you do require a camera with a class 1 sensor, please get in touch with your Atik dealer.

    What's in the box?

    Camera body with 2” adapter
    3-metre USB cable
    1.8-metre battery power connector (car lighter plug)
    CD-ROM with drivers, software and user's manual (PDF)
    Quickstart guide (paper)

    Our highly acclaimed Artemis Capture software is included for camera control and data acquisition, along with a full ASCOM driver and plug-ins to allow use with Astroart and Maxim DL.

    A universal (110-230V) power adapter is optional.

  2. $12,379.85 USD
    Back Order / Waiting List

    Flight Lakes Instrumentation: The KL400's Low Dynamic Range (LDR) mode reads the image once and digitizes it to 12-bits. The user has eight gains to select from in LDR mode. Adjusting the gain affects full well size, dark current growth, and linearity.

    The High Dynamic Range (HDR) mode reads the pixels twice, digitizing with different gains. (Unlike CCDs that only read the charge from each pixel once, CMOS sensors can measure the charge multiple times.) The two images are merged to create a 16 bit image with the linearity of a single image, thus allowing an HDR image to show detail in both low-count and high-count areas of an image. Because of the additional read time, the maximum HDR frame rate is half that of the LDR mode.

    The Kepler camera also features a Low Dark Current (LDC) options for both LDR and HDR. When used, the LDC option minimizes dark current at the expense of reduced full well capacity. For short exposures where dark current growth is not a problem, LDC is not generally used. Standard modes (not LDC) provide the highest full well capacity and widest dynamic range. On the other hand LDC mode is very useful for imaging dim objects that require very long exposures where dark current growth can be significant.

    The following may be useful in making the decision on which mode is most appropriate:

    Choose LDR mode for required frame rate greater than 24 FPS (exposures <42 ms).

    Choose HDR mode for a dynamic range greater than 0 – 4095 counts

    Choose LDC when your exposures are sufficiently long that dark current growth uses a significant percentage of full well capacity. (Also cool sensor to lowest possible operating temp.)

    Do not choose LDC for short exposures.

     
    A Signal to Noise Ratio Comparison: PL16803 CCD vs. KL4040 sCMOS
    The ProLine PL16803 has been the de facto standard for astrophotography since its release in 2006, and the Kepler KL4040 continues the tradition of excellence. Both cameras use a 4k x 4k sensor with 9 micron pixels. The difference is the ProLine uses a traditional CCD while the Kepler uses a Scientific CMOS sensor.

    The table below is a comparison of the ProLine PL16803 and the Kepler KL4040 cameras, using a low flux value of 1 photon/pixel/second.

    KAF-16803 vs GSense4040
    Sensor    KAF-16803 CCD    GS4040 sCMOS
    Average QE 400-700 nm    50.7%    69.8%
    Dark Current    0.001 eps    0.15 eps
    Read Noise    10 e-    3.7 e-
    Throughput    1 MHz    800 MHz
    Full Well Capacity    100000 e-    70000 e-
    Dynamic Range    10000 : 1    18900 : 1
    SNR 900 sec    19.2    22.5
    SNR 5 x 180 sec    14.7    21.8
    SNR 10 x 90 sec    11.9    20.9
     

    Summary: A Paradigm Shift
    It is no surprise that the CCD’s best performance is with a single long exposure. What may be surprising is the Kepler KL4040 has a better signal-to-noise ratio than the PL16803 even with a single long exposure. The signal-to-noise ratio of the KL4040 is better than the PL16803 even when using short exposures that are stacked!

    The benefit of taking multiple short exposures is the option to discard a bad exposure ruined by satellite trails, tracking errors, or bad seeing (etc.). Incredible low-noise images are now possible with a single long exposure or many stacked short exposures. The KL4040’s superior performance allows it to be used for a wide range of applications and requirements.

  3. $21,649.85 USD
    Back Order / Waiting List

    Flight Lakes Instrumentation: The Kepler KL400 provides ultra-high sensitivity, ultra-low noise with high frame rates, all at a game-changing price to performance ratio. The back-illuminated sensor is available with TVISB coating for best performance in the visible and at 240 nm; the UV version is best at 280 nm.

    The KL400's Low Dynamic Range (LDR) mode reads the image once and digitizes it to 12-bits. The user has eight gains to select from in LDR mode. Adjusting the gain affects full well size, dark current growth, and linearity.

    The High Dynamic Range (HDR) mode reads the pixels twice, digitizing with different gains. (Unlike CCDs that only read the charge from each pixel once, CMOS sensors can measure the charge multiple times.) The two images are merged to create a 16 bit image with the linearity of a single image, thus allowing an HDR image to show detail in both low-count and high-count areas of an image. Because of the additional read time, the maximum HDR frame rate is half that of the LDR mode.

    The Kepler camera also features a Low Dark Current (LDC) options for both LDR and HDR. When used, the LDC option minimizes dark current at the expense of reduced full well capacity. For short exposures where dark current growth is not a problem, LDC is not generally used. Standard modes (not LDC) provide the highest full well capacity and widest dynamic range. On the other hand LDC mode is very useful for imaging dim objects that require very long exposures where dark current growth can be significant.

    The following may be useful in making the decision on which mode is most appropriate:

    Choose LDR mode for required frame rate greater than 24 FPS (exposures <42 ms).

    Choose HDR mode for a dynamic range greater than 0 – 4095 counts

    Choose LDC when your exposures are sufficiently long that dark current growth uses a significant percentage of full well capacity. (Also cool sensor to lowest possible operating temp.)

    Do not choose LDC for short exposures.

     
    A Signal to Noise Ratio Comparison: PL16803 CCD vs. KL4040 sCMOS
    The ProLine PL16803 has been the de facto standard for astrophotography since its release in 2006, and the Kepler KL4040 continues the tradition of excellence. Both cameras use a 4k x 4k sensor with 9 micron pixels. The difference is the ProLine uses a traditional CCD while the Kepler uses a Scientific CMOS sensor.

    The table below is a comparison of the ProLine PL16803 and the Kepler KL4040 cameras, using a low flux value of 1 photon/pixel/second.

    KAF-16803 vs GSense4040
    Sensor    KAF-16803 CCD    GS4040 sCMOS
    Average QE 400-700 nm    50.7%    69.8%
    Dark Current    0.001 eps    0.15 eps
    Read Noise    10 e-    3.7 e-
    Throughput    1 MHz    800 MHz
    Full Well Capacity    100000 e-    70000 e-
    Dynamic Range    10000 : 1    18900 : 1
    SNR 900 sec    19.2    22.5
    SNR 5 x 180 sec    14.7    21.8
    SNR 10 x 90 sec    11.9    20.9
     

    Summary: A Paradigm Shift
    It is no surprise that the CCD’s best performance is with a single long exposure. What may be surprising is the Kepler KL4040 has a better signal-to-noise ratio than the PL16803 even with a single long exposure. The signal-to-noise ratio of the KL4040 is better than the PL16803 even when using short exposures that are stacked!

    The benefit of taking multiple short exposures is the option to discard a bad exposure ruined by satellite trails, tracking errors, or bad seeing (etc.). Incredible low-noise images are now possible with a single long exposure or many stacked short exposures. The KL4040’s superior performance allows it to be used for a wide range of applications and requirements.

  4. $16,499.85 USD
    Back Order / Waiting List

    Flight Lakes Instrumentation:

    The KL4040 scientific CMOS camera has the same pixel size and imaging area as the popular KAF-16803 CCD, but with 1/3 the noise and 40% higher quantum efficiency. Kepler cooled sCMOS cameras provide ultra-high sensitivity, ultra-low noise, and high frame rates, all at game-changing price to performance ratio.

    The KL400's Low Dynamic Range (LDR) mode reads the image once and digitizes it to 12-bits. The user has eight gains to select from in LDR mode. Adjusting the gain affects full well size, dark current growth, and linearity.

    The High Dynamic Range (HDR) mode reads the pixels twice, digitizing with different gains. (Unlike CCDs that only read the charge from each pixel once, CMOS sensors can measure the charge multiple times.) The two images are merged to create a 16 bit image with the linearity of a single image, thus allowing an HDR image to show detail in both low-count and high-count areas of an image. Because of the additional read time, the maximum HDR frame rate is half that of the LDR mode.

    The Kepler camera also features a Low Dark Current (LDC) options for both LDR and HDR. When used, the LDC option minimizes dark current at the expense of reduced full well capacity. For short exposures where dark current growth is not a problem, LDC is not generally used. Standard modes (not LDC) provide the highest full well capacity and widest dynamic range. On the other hand LDC mode is very useful for imaging dim objects that require very long exposures where dark current growth can be significant.

    The following may be useful in making the decision on which mode is most appropriate:

    Choose LDR mode for required frame rate greater than 24 FPS (exposures <42 ms).

    Choose HDR mode for a dynamic range greater than 0 – 4095 counts

    Choose LDC when your exposures are sufficiently long that dark current growth uses a significant percentage of full well capacity. (Also cool sensor to lowest possible operating temp.)

    Do not choose LDC for short exposures.

     
    A Signal to Noise Ratio Comparison: PL16803 CCD vs. KL4040 sCMOS
    The ProLine PL16803 has been the de facto standard for astrophotography since its release in 2006, and the Kepler KL4040 continues the tradition of excellence. Both cameras use a 4k x 4k sensor with 9 micron pixels. The difference is the ProLine uses a traditional CCD while the Kepler uses a Scientific CMOS sensor.

    The table below is a comparison of the ProLine PL16803 and the Kepler KL4040 cameras, using a low flux value of 1 photon/pixel/second.

    KAF-16803 vs GSense4040
    Sensor    KAF-16803 CCD    GS4040 sCMOS
    Average QE 400-700 nm    50.7%    69.8%
    Dark Current    0.001 eps    0.15 eps
    Read Noise    10 e-    3.7 e-
    Throughput    1 MHz    800 MHz
    Full Well Capacity    100000 e-    70000 e-
    Dynamic Range    10000 : 1    18900 : 1
    SNR 900 sec    19.2    22.5
    SNR 5 x 180 sec    14.7    21.8
    SNR 10 x 90 sec    11.9    20.9


    Summary: A Paradigm Shift
    It is no surprise that the CCD’s best performance is with a single long exposure. What may be surprising is the Kepler KL4040 has a better signal-to-noise ratio than the PL16803 even with a single long exposure. The signal-to-noise ratio of the KL4040 is better than the PL16803 even when using short exposures that are stacked!

    The benefit of taking multiple short exposures is the option to discard a bad exposure ruined by satellite trails, tracking errors, or bad seeing (etc.). Incredible low-noise images are now possible with a single long exposure or many stacked short exposures. The KL4040’s superior performance allows it to be used for a wide range of applications and requirements.

  5. $46,369.85 USD
    Back Order / Waiting List

    Flight Lakes Instrumentation: The very large imaging area of the KL6060 FI scientific CMOS camera provides high sensitivity with low noise, even at multiple frames per second. The camera offers 4x the area of comparably priced 2K x 2K back illuminated CCD cameras.

    The Kepler KL400 provides ultra-high sensitivity, ultra-low noise with high frame rates, all at a game-changing price to performance ratio. The back-illuminated sensor is available with TVISB coating for best performance in the visible and at 240 nm; the UV version is best at 280 nm.

    The KL400's Low Dynamic Range (LDR) mode reads the image once and digitizes it to 12-bits. The user has eight gains to select from in LDR mode. Adjusting the gain affects full well size, dark current growth, and linearity.

    The High Dynamic Range (HDR) mode reads the pixels twice, digitizing with different gains. (Unlike CCDs that only read the charge from each pixel once, CMOS sensors can measure the charge multiple times.) The two images are merged to create a 16 bit image with the linearity of a single image, thus allowing an HDR image to show detail in both low-count and high-count areas of an image. Because of the additional read time, the maximum HDR frame rate is half that of the LDR mode.

    The Kepler camera also features a Low Dark Current (LDC) options for both LDR and HDR. When used, the LDC option minimizes dark current at the expense of reduced full well capacity. For short exposures where dark current growth is not a problem, LDC is not generally used. Standard modes (not LDC) provide the highest full well capacity and widest dynamic range. On the other hand LDC mode is very useful for imaging dim objects that require very long exposures where dark current growth can be significant.

    The following may be useful in making the decision on which mode is most appropriate:

    Choose LDR mode for required frame rate greater than 24 FPS (exposures <42 ms).

    Choose HDR mode for a dynamic range greater than 0 – 4095 counts

    Choose LDC when your exposures are sufficiently long that dark current growth uses a significant percentage of full well capacity. (Also cool sensor to lowest possible operating temp.)

    Do not choose LDC for short exposures.

     
    A Signal to Noise Ratio Comparison: PL16803 CCD vs. KL4040 sCMOS
    The ProLine PL16803 has been the de facto standard for astrophotography since its release in 2006, and the Kepler KL4040 continues the tradition of excellence. Both cameras use a 4k x 4k sensor with 9 micron pixels. The difference is the ProLine uses a traditional CCD while the Kepler uses a Scientific CMOS sensor.

    The table below is a comparison of the ProLine PL16803 and the Kepler KL4040 cameras, using a low flux value of 1 photon/pixel/second.

    KAF-16803 vs GSense4040
    Sensor    KAF-16803 CCD    GS4040 sCMOS
    Average QE 400-700 nm    50.7%    69.8%
    Dark Current    0.001 eps    0.15 eps
    Read Noise    10 e-    3.7 e-
    Throughput    1 MHz    800 MHz
    Full Well Capacity    100000 e-    70000 e-
    Dynamic Range    10000 : 1    18900 : 1
    SNR 900 sec    19.2    22.5
    SNR 5 x 180 sec    14.7    21.8
    SNR 10 x 90 sec    11.9    20.9
     

    Summary: A Paradigm Shift
    It is no surprise that the CCD’s best performance is with a single long exposure. What may be surprising is the Kepler KL4040 has a better signal-to-noise ratio than the PL16803 even with a single long exposure. The signal-to-noise ratio of the KL4040 is better than the PL16803 even when using short exposures that are stacked!

    The benefit of taking multiple short exposures is the option to discard a bad exposure ruined by satellite trails, tracking errors, or bad seeing (etc.). Incredible low-noise images are now possible with a single long exposure or many stacked short exposures. The KL4040’s superior performance allows it to be used for a wide range of applications and requirements.

  6. $169,975.00 USD
    Back Order / Waiting List

    Flight Lakes Instrumentation: The KL6060 BI scientific CMOS camera has the same sensitivity and imaging area as the back-illuminated CCD230-84 CCD, but with a fraction of the noise even at multiple frames per second. Kepler cooled sCMOS cameras provide ultra-high sensitivity, ultra-low noise, and high frame rates, all at game-changing price to performance ratio.

    The Kepler KL400 provides ultra-high sensitivity, ultra-low noise with high frame rates, all at a game-changing price to performance ratio. The back-illuminated sensor is available with TVISB coating for best performance in the visible and at 240 nm; the UV version is best at 280 nm.

    The KL400's Low Dynamic Range (LDR) mode reads the image once and digitizes it to 12-bits. The user has eight gains to select from in LDR mode. Adjusting the gain affects full well size, dark current growth, and linearity.

    The High Dynamic Range (HDR) mode reads the pixels twice, digitizing with different gains. (Unlike CCDs that only read the charge from each pixel once, CMOS sensors can measure the charge multiple times.) The two images are merged to create a 16 bit image with the linearity of a single image, thus allowing an HDR image to show detail in both low-count and high-count areas of an image. Because of the additional read time, the maximum HDR frame rate is half that of the LDR mode.

    The Kepler camera also features a Low Dark Current (LDC) options for both LDR and HDR. When used, the LDC option minimizes dark current at the expense of reduced full well capacity. For short exposures where dark current growth is not a problem, LDC is not generally used. Standard modes (not LDC) provide the highest full well capacity and widest dynamic range. On the other hand LDC mode is very useful for imaging dim objects that require very long exposures where dark current growth can be significant.

    The following may be useful in making the decision on which mode is most appropriate:

    Choose LDR mode for required frame rate greater than 24 FPS (exposures <42 ms).

    Choose HDR mode for a dynamic range greater than 0 – 4095 counts

    Choose LDC when your exposures are sufficiently long that dark current growth uses a significant percentage of full well capacity. (Also cool sensor to lowest possible operating temp.)

    Do not choose LDC for short exposures.

     
    A Signal to Noise Ratio Comparison: PL16803 CCD vs. KL4040 sCMOS
    The ProLine PL16803 has been the de facto standard for astrophotography since its release in 2006, and the Kepler KL4040 continues the tradition of excellence. Both cameras use a 4k x 4k sensor with 9 micron pixels. The difference is the ProLine uses a traditional CCD while the Kepler uses a Scientific CMOS sensor.

    The table below is a comparison of the ProLine PL16803 and the Kepler KL4040 cameras, using a low flux value of 1 photon/pixel/second.

    KAF-16803 vs GSense4040
    Sensor    KAF-16803 CCD    GS4040 sCMOS
    Average QE 400-700 nm    50.7%    69.8%
    Dark Current    0.001 eps    0.15 eps
    Read Noise    10 e-    3.7 e-
    Throughput    1 MHz    800 MHz
    Full Well Capacity    100000 e-    70000 e-
    Dynamic Range    10000 : 1    18900 : 1
    SNR 900 sec    19.2    22.5
    SNR 5 x 180 sec    14.7    21.8
    SNR 10 x 90 sec    11.9    20.9
     

    Summary: A Paradigm Shift
    It is no surprise that the CCD’s best performance is with a single long exposure. What may be surprising is the Kepler KL4040 has a better signal-to-noise ratio than the PL16803 even with a single long exposure. The signal-to-noise ratio of the KL4040 is better than the PL16803 even when using short exposures that are stacked!

    The benefit of taking multiple short exposures is the option to discard a bad exposure ruined by satellite trails, tracking errors, or bad seeing (etc.). Incredible low-noise images are now possible with a single long exposure or many stacked short exposures. The KL4040’s superior performance allows it to be used for a wide range of applications and requirements.

  7. $3,787.22 USD
    specialorder
    Scheduled Delivery

    CMOS sensor 6276 x 4176 pixels, ("consumer grade" intended for operation time max. 300 hours per year), USB 3.0 interface

    C3 cameras employ the latest generation of Sony IMX CMOS sensors, offering exceptional quantum efficiency thanks to back-illuminated design and very low dark current. Despite relatively small pixels, full-well capacity exceeding 50 ke-. Combined with full 16 bit digitization and perfectly linear response to light make these cameras suitable for both aesthetic astrophotography and astronomical research. Sensor formats from APS to photographic full-frame (24 × 36 mm) ensure wide field of view and optimally utilize the capabilities of the optical systems most commonly used by amateur astronomers.

  8. $4,052.22 USD
    specialorder
    Scheduled Delivery

    CMOS sensor 6276 x 4176 pixels, ("consumer grade" intended for operation time max. 300 hours per year), USB 3.0 interface

    C3 cameras employ the latest generation of Sony IMX CMOS sensors, offering exceptional quantum efficiency thanks to back-illuminated design and very low dark current. Despite relatively small pixels, full-well capacity exceeding 50 ke-. Combined with full 16 bit digitization and perfectly linear response to light make these cameras suitable for both aesthetic astrophotography and astronomical research. Sensor formats from APS to photographic full-frame (24 × 36 mm) ensure wide field of view and optimally utilize the capabilities of the optical systems most commonly used by amateur astronomers.

  9. $6,115.18 USD
    specialorder
    Scheduled Delivery

    CMOS sensor 9600 x 6388 pixels, ("consumer grade" intended for operation time max. 300 hours per year), USB 3.0 interface.

    C3 cameras employ the latest generation of Sony IMX CMOS sensors, offering exceptional quantum efficiency thanks to back-illuminated design and very low dark current. Despite relatively small pixels, full-well capacity exceeding 50 ke-. Combined with full 16 bit digitization and perfectly linear response to light make these cameras suitable for both aesthetic astro-photography as well as astronomical research. Sensor formats from APS to photographic full-frame (24 × 36 mm) ensure wide field of view and optimally utilize capabilities of the optical systems most commonly used by amateur astronomers.

  10. $6,380.18 USD
    specialorder
    Scheduled Delivery

    CMOS sensor 9600 x 6388 pixels, ("consumer grade" intended for operation time max. 300 hours per year), USB 3.0 interface.

    C3 cameras employ the latest generation of Sony IMX CMOS sensors, offering exceptional quantum efficiency thanks to back-illuminated design and very low dark current. Despite relatively small pixels, full-well capacity exceeding 50 ke-. Combined with full 16 bit digitization and perfectly linear response to light make these cameras suitable for both aesthetic astro-photography as well as astronomical research. Sensor formats from APS to photographic full-frame (24 × 36 mm) ensure wide field of view and optimally utilize capabilities of the optical systems most commonly used by amateur astronomers.

  11. $6,966.23 USD
    specialorder
    Scheduled Delivery

    C3-61000 PRO CMOS camera with "full frame" (36x24mm) format sensor Sony IMX455

    C3 cameras employ the latest generation of Sony IMX CMOS sensors, offering exceptional quantum efficiency thanks to back-illuminated design and very low dark current. Despite relatively small pixels, full-well capacity exceeding 50 ke-. Combined with full 16 bit digitization and perfectly linear response to light make these cameras suitable for both aesthetic astro-photography as well as astronomical research. Sensor formats from APS to photographic full-frame (24 × 36 mm) ensure wide field of view and optimally utilize capabilities of the optical systems most commonly used by amateur astronomers.

  12. $7,231.23 USD
    specialorder
    Scheduled Delivery

    C3-61000 PRO CMOS camera with "full frame" (36x24mm) format sensor Sony IMX455

    C3 cameras employ the latest generation of Sony IMX CMOS sensors, offering exceptional quantum efficiency thanks to back-illuminated design and very low dark current. Despite relatively small pixels, full-well capacity exceeding 50 ke-. Combined with full 16 bit digitization and perfectly linear response to light make these cameras suitable for both aesthetic astro-photography as well as astronomical research. Sensor formats from APS to photographic full-frame (24 × 36 mm) ensure wide field of view and optimally utilize capabilities of the optical systems most commonly used by amateur astronomers.

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