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Diagram highlighting ISIM. Integrated Science Instrument Module (ISIM) is a component of the James Webb Space Telescope, a large international infrared space telescope launched on 25 December 2021. [1] ISIM is the heart of the JWST, and holds the main science payload which includes four science instruments and the fine guidance sensor. [1]
Primary lens: The objective of a refracting telescope. Primary mirror: The objective of a reflecting telescope. Corrector plate: A full aperture negative lens placed before a primary mirror designed to correct the optical aberrations of the mirror. Schmidt corrector plate: An aspheric-shaped corrector plate used in the Schmidt telescope.
Afocal photography works with any system that can produce a virtual image of parallel light, for example telescopes and microscopes. Afocal photographic setups work because the imaging device's eyepiece produces collimated light and with the camera's lens focused at infinity, creating an afocal system with no net convergence or divergence in the light path between the two devices. [2]
The Infrared Array Camera (IRAC) was an infrared camera system on the Spitzer Space Telescope which operated in the mid-infrared spectrum. [1] It was composed of four detectors that operated simultaneously at different wavelengths; all four were in use until 2009 May 15 when the Spitzer cryostat ran out of liquid helium. [2]
A teleside converter lens attached in front of a camera. 2 - Camera lens 1 - Teleside converter. A teleside converter [1] (also known as a telephoto conversion lens or a front mount teleconverter) [2] is a secondary lens which is mounted on the front of a photographic lens to increase the effective focal length of the lens they are attached to.
Flat-field correction (FFC) is a digital imaging technique to mitigate the image detector pixel-to-pixel sensitivity and distortions in the optical path. It is a standard calibration procedure in everything from personal digital cameras to large telescopes.
Spectral imaging may use the infrared, the visible spectrum, the ultraviolet, x-rays, or some combination of the above. It may include the acquisition of image data in visible and non-visible bands simultaneously, illumination from outside the visible range, or the use of optical filters to capture a specific spectral range.
Aperture synthesis is possible only if both the amplitude and the phase of the incoming signal are measured by each telescope. For radio frequencies, this is possible by electronics, while for optical frequencies, the electromagnetic field cannot be measured directly and correlated in software, but must be propagated by sensitive optics and interfered optically.