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Kepler KL6060 Scmos Camera Large Format Low Noise High Frame Rate Maximize Your Field of View with Our New Large Format Kepler KL6060 Scmos Camera

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Kepler KL6060 Scmos Camera Large Format Low Noise High Frame Rate Maximize Your Field of View with Our New Large Format Kepler KL6060 Scmos Camera Kepler KL6060 sCMOS Camera Large Format Low Noise High Frame Rate Maximize Your Field of View with our New Large Format Kepler KL6060 sCMOS Camera 86.8 mm DIAG HDR Extremely High Frame High High Dynamic Back-Illuminated (BI) High Performance Large Area Rate Sensitivity Range & Front-Illuminated (FI) & Reliability The New Low-Noise Cooled High Frame Rates The back-illuminated camera reads out at 14.288 microseconds per sCMOS Camera from Finger row (11 fps for full array). The front-illuminated camera reads at 8.533 microseconds per row (19 fps for full array). Faster imaging speed can Lakes Instrumentation (FLI) be achieved by selecting a smaller region of interest. For example, by selecting a sub-array of 1,000 rows, frame rate increases by 6x. Provides High Speed Imaging High Dynamic Range (HDR) with an Exceptional Field of View The KL6060 is able to capture bright and dim objects in a single image. It achieves a remarkable 90 dB dynamic range by reading a single exposure twice – once in high gain and once in low gain. Available with a front-illuminated sensor or high-QE FLI’s proprietary algorithms guarantee the merged 16-bit HDR back-illuminated sensor, the Kepler KL6060 camera image is exceptionally linear, enabling high-precision quantitative is capable of taking up to 19 frames per second, using analysis. FLI's Pilot software allows you to preserve the original 12-bit images for future scrutiny, ensuring that your original data the optional QSFP fiber interface. This affordable camera remains unchanged. is a game-changing solution for Space Debris Detection Optional QSFP Fiber Interface and Space Situational Awareness applications and is When combined with the optional QSFP Fiber Interface, the KL6060 ideal for universities or dedicated amateurs who want allows for long distance operation and isolation from electrical to capture every possible photon. interferences. It also provides the highest data rates possible on the Kepler platform. Our PCIE interface supports customizable on-the-fly correction for Dark Signal Non-Uniformity and Photo Response Non- SPECIFICATIONS Uniformity at full data rates, including the ability for you to add the algorithms of your choice. Please contact FLI for details. Back- Front- Illuminated (BI) Illuminated (FI) Reliable, Long-Life Performance Array Size 37.7 Megapixels The Kepler KL6060 is designed for use in the most remote locations and eliminates the need to periodically pump down the chamber or Resolution 6144 x 6144 with 10 micron pixels service desiccant cartridges. Our proprietary chamber design, coupled Array Diagonal 86.8 mm with decades of manufacturing experience, ensure that your camera will have a long lifespan, regardless of location. Full Well Capacity (e-) 102k 135k Support & Service Read Noise 3e- 4.6e- Each of our Kepler cameras are built for long-lasting sustainability Frame Rate (QSFP) 11 fps 19 fps and come standard with unrivaled service and support. They are field-programmable with the capacity to easily upgrade firmware Dynamic Range (HDR) 90 dB 89 dB and re-program from anywhere in the world. In addition, our shutters, Rolling power boards, and fans are simple field replacements, with no need Electronic Shutter Type Rolling with Global Reset for expensive, time-consuming transport back and forth from the QSFP Fiber Interface factory. Our cameras are installed in observatories worldwide — many Options 90 mm Shutter in remote mountaintop locations — from Antarctica to Fairbanks and Liquid Cooling Finland. See the back page of this brochure for a sampling of our satisfied customers. KL6060 FI KL6060 BI The KL6060 FI sensor has 3X the area With a diagonal of 86.8 mm, CCD230-42 KAF-16803 FIELD OFFIELD VIEW: of the KAF-16803 and 50% more FOV than a KAF-4320. CCD230-84. The KL6060 sensor has 4X the FOV of the CCD230-42 and 5X the FOV of the CCD42-40. the KL6060 BI is comparable to the massive FIELD OFFIELD VIEW: 1080 1080 1040 1040 1000 960 1000 920 960 880 920 840 880 800 840 d 760 800 720 (nm) 760 680 (nm) 640 TH 720 TH BI 0 600 680 606 CCD230 Midban 560 VELENG 640 VELENG FI 520 16803 WA 0 F- 600 WA 480 606 KA 560 440 520 400 360 480 320 At operating temperature, the KL6060 the dark has ~1/3 current : 440 280 The KL6060 of the noise BI has of ~1/4 the CCD230-42 running at 500 400 The read noise of the KL6060 FI is the 1/3 noise of the KAF-16803 running 240 360 200 0 0 320 80 60 40 20 0 10 20 40 60 80 ABSOLU ) (% QE TE ABSOLU ) (% QE QUANTUM EFFICIENCY: KL6060 FI VS. ON SEMI KAF-16803 TE QUANTUM EFFICIENCY: KL6060 BI VS. CCD230 BI MIDBAND of the popular CCD230-42 or CCD42-40 back-illuminated sensors. READ NOISE: kHz (about seconds 11 readout time), but the KL6060 BI delivers frames 11 per second. DARK CURRENT DARK Back-Illuminated sCMOS vs. Back-Illuminated CCD Back-Illuminated vs. sCMOS Back-Illuminated Front-Illuminated sCMOS vs. Front-Illuminated CCD READ NOISE: at 8 MHz (about 3 second readout time), but the KL6060 FI delivers frames 19 per second. IMAGE CREDIT: The Melotte imageIMAGE CREDIT: 15 used in this brochure is courtesy Gumusayak, Tolga taken with an Kepler FLI KL4040 camera. Our Customers Abastumani Observatory (Georgia) Food & Drug Administration Milkovo Observatory (Russia) Technical Universities of Darmstadt, Academia Sinica (China) Florida International University Mississippi State University Dresden, and Ilmenau (Germany) Adiyaman University (Turkey) Fordham University MIT Technion University (Israel) Adler Planetarium Freie Universität Berlin (Germany) MIT Lincoln Laboratory Tel Aviv University (Israel) Aerospace Corporation Fudan University (China) Mondy Observatory (Russia) Tenagra Observatories Aiglon College (Switzerland) Geneva Observatory (Switzerland) Montana State University Terskol Observatory (Russia) Air Force Research Laboratory George Washington University Mt. Sinai School of Medicine Texas A&M University AIX Marseille Universite (France) Georgia Institute of Technology NASA Ames Texas State University American Museum of Natural History Georgia Public Health Lab NASA Goddard The Ohio State University Anadolu University (Turkey) Getty Museum NASA Johnson Tiraspol Observatory (Moldova) Andor Technology (UK) Gissar Observatory (Tajikistan) National Astronomical Tubitak National Observatory (Turkey) Andrushivka Observatory (Ukraine) Goodrich Observatories of China Turksat University (Turkey) Appalachian State University Guang Xi University (China) National Astronomical Research Tuskegee University Institute of Thailand/NARIT Argonne National Lab Harvard University Universidad Nacional Autónoma National Institute of Aeronautics de México Arizona State University Hefei Institute (China) and Space (Indonesia) Universidad Nacional de La Plata Artem Observatory (Russia) Helmholtz Centrum Geesthacht National Institute of Health (Argentina) (Germany) Auburn University National Renewable Energy Laboratory Universita di Roma (Italy) Hitachi Austin College National Taiwan University Universitat de Barcelona (Spain) Horiba Australian Astronomical Observatory National University of Ireland Universitat de Valencia (Spain) Howard Hughes Medical Institute Australian Defence Science & Technology Nauchny Observatory (Ukraine) Université de Montreal (Canada) Organisation (DSTO) Humboldt University of Berlin (Germany) Naval Ordnance Test Unit Universiteit Leiden (Netherlands) Australian National University Institute of Molecular and Cell Biology Naval Research Laboratory Universities of Alabama, Alaska, Arizona, Azdeniz University (Turkey) (Singapore) New Mexico State University California, Central Florida, Chicago, Baader Planetarium (Germany) Institut d’Astrophysique de Hawaii, Illinois, Iowa, Kentucky, Maryland, l’Université de Liège (Belgium) New Mexico Tech Baku State University (Azerbaijan) Massachusetts, Minnesota, Nevada, Institut de Planetologie et New York State Dept. of Health New Mexico, North Carolina, North Ball Aerospace Astrophysique de Grenoble (France) New York University Dakota, Notre Dame, Pittsburgh, Ball State University Rochester, South Carolina, Texas, Institute of Astronomy, Hawaii Nikon Virginia, Washington, and Wisconsin Beijing Institute of Technology (China) Institute of Fluid Physics (China) NIST Universities of Bremen, Duisburg, Beijing University (China) Institute of Mechanics, Northrop Grumman Freiburg, Göttingen, Heidelberg, Binghamton University Chinese Academy of Sciences (CAS) Kiel, Konstanz, Magdeburg, Potsdam, Northwestern Polytechnical University and Würzburg (Germany) Boeing Institute of Physics (CAS) (China) University College Dublin (Ireland) Boston University Instituto de Astrofísica Northwestern University de Andalucía (Spain) University Observatory Munich (Germany) Brigham Young University Novosibirsk State University (Russia) Instituto de Astrofi sica University of Bern (Switzerland) Butler University Observatoire de Oukaimeden (Morocco) de Canarias (Spain) University of Bradford (UK) California Institute of Technology Instituto de Estudios Espaciales Observatorio Astronomico Nacional Carl Zeiss Jena de Cataluña (Spain) (Bolivia) University of Calgary (Canada) Carlton University (Canada) IPICYT (Mexico) Observatory Hamburg (Germany) University of Dresden (Germany) Carnegie Institution for Science ITT Space Systems Olympus University of Jena (Germany) Carnegie Observatories IUCAA Pune University (India) Oxford University (UK) University of Lethbridge (Canada) Catholic University of America Japan Aerospace Exploration Agency Palomar Observatory University of Munich (Germany) Centro de Estudios de Física (JAXA)
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