Astronomy is a field where various researches are being conducted to discover and explore unknown celestial bodies and astronomical phenomena. This brochure introduces examples of such applications and our cameras suitable for each application.
Large telescopes are used to observe exoplanets and protoplanetary systems, to search for signs of life, and to study the nature of dark energy by directly measuring the universe's expansion.
Large telescopes such as the Subaru Telescope, the Thirty Meter Telescope (TMT), the Keck Telescope, and the Gemini Telescope on the summit of Mauna Kea on the island of Hawaii, the Alma Telescope in the Atacama Desert in Chile, and the Canary Large Telescope on the island of La Palma in the Canary Islands have been installed in many parts of the world and continue to be used for observations.
Adaptive optics is a method where systems immediately correct the wavefront of incoming light which is disturbed by atmospheric fluctuations. This atmospheric turbulence can move the incoming light (think of stars twinkling) and therefore blur an image on a sensor. Adaptive optics allow astronomers to correct this and obtain the clearest image at the performance limit of the telescope. In order to perform real-time and highly accurate wavefront correction, a camera in this application must have high speed and high resolution. In addition, since the wavefront correction is performed in a very dark state using a laser artificial star, the camera also needs high sensitivity.
*Courtesy of Kodai Yamamoto, Ph.D., Department of Astronomy, Kyoto University
The sun has a great effect on the Earth. Imaging and understanding solar activity, such as researching flare generations from sunspots and magnetic field movements, is becoming more important as we strive to understand the cause and effect between the Earth and the sun. In order to closely track the internal structure of the solar flare and its evolution over time, a detector that simultaneously achieves high resolution, high speed, and high dynamic range is required.
The upper atmosphere is the atmosphere around 80 to 400 km high. This height corresponds to the boundary region between Earth's atmosphere and outer space. This part of the atmosphere is in a plasma state which is ionized. Due to the interaction between the plasma and the atmosphere, auroras are produced in the Arctic and Antarctic regions. During the night, a dim airglow is produced at this altitude. The dynamics of the upper atmosphere can be measured with a high-sensitivity, high-resolution, and high-speed camera.
*Courtesy of Yoshizumi Miyoshi, Ph.D., Institute for Space-Earth Environmental Research (ISEE), Nagoya University
The ORCA-Quest captures wide range of atmospheric changes with low noise (0.43e-), high speed (120 Hz), and high resolution (9.4 megapixels).
The ORCA-Fusion, a back-illuminated sCMOS, offers high QE (95 %) and low readout noise, enabling high sensitivity imaging.
The ORCA-Flash4.0 V3 digital CMOS camera captures auroras with high speed, high definition, and wide dynamic range.
ImagEM X2 is equipped with an EM gain of up to 1200×, making it possible to capture atmospheric changes with high sensitivity.
Hamamatsu Photonics has been providing various products for the field of astronomy, such as image sensors for large telescopes and infrared detectors for astronomical satellites. Below are examples of our collaborations with the astronomical community.
The Subaru Telescope is an extremely large telescope on the summit of Mauna Kea, Hawaii. One of the world's most powerful telescopes, it is used to measure the history of cosmic expansion and dark energy, and it directly observes the distribution of dark matter.
Our CCD image sensor is used in the Prime Focus Camera for the Subaru Telescope. The CCD sensor has a unique, full-depletion structure and high sensitivity at long wavelengths, making it possible to observe at high resolution a wide range of faint objects that had been impossible to observe with conventional sensors.
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