{"dataset":{"slug":"observatory-instrumentation","title":"Observatory Instrumentation & Detectors","description":"The instrumentation frontier of ground-based astronomy — the adaptive-optics chain (laser guide stars, wavefront sensors, deformable mirrors), spectrographs, coronagraphs and starshades, and the detectors from CCDs to superconducting MKIDs and bolometers.","version":"1.0.0","lastGenerated":"2026-06-29","license":"CC BY-SA 4.0","entityCount":12,"sources":["eso","noirlab"]},"entities":[{"id":"detector_technology:bolometer","name":"Bolometer","type":"detector_technology","domain":"science","description":"A detector that measures light by the tiny rise in temperature it causes in an absorbing element — the standard way to detect the faint millimetre and submillimetre sky, including the cosmic microwave background. Cooled to a fraction of a degree above absolute zero; the South Pole Telescope's cameras use large bolometer arrays.","entryPath":"/observatory-frontier/bolometer"},{"id":"detector_technology:ccd","name":"CCD","type":"detector_technology","domain":"science","description":"The charge-coupled device, the detector that transformed optical astronomy — a silicon chip that converts light into electric charge with high efficiency and low noise, read out pixel by pixel. It replaced photographic plates and remains the standard optical detector; Rubin's camera is built from a mosaic of them.","entryPath":"/observatory-frontier/ccd"},{"id":"detector_technology:cmos","name":"CMOS Sensor","type":"detector_technology","domain":"science","description":"A detector in which each pixel has its own amplifier, allowing very fast, low-power readout. Increasingly used in astronomy for high-speed imaging and for techniques that need many frames per second, and ubiquitous in consumer cameras.","entryPath":"/observatory-frontier/cmos"},{"id":"instrument_technique:coronagraph","name":"Coronagraph","type":"instrument_technique","domain":"science","description":"An instrument that blocks the overwhelming light of a star so the far fainter objects beside it — a planet, a disc, the solar corona — can be seen. First built by Bernard Lyot to study the Sun, it is now central to directly imaging exoplanets; SPHERE on the VLT is a modern example.","entryPath":"/observatory-frontier/coronagraph"},{"id":"detector_technology:cryogenic-detector","name":"Cryogenic Detector","type":"detector_technology","domain":"science","description":"The broad family of detectors that must be cooled to cryogenic temperatures — sometimes thousandths of a degree above absolute zero — so that thermal noise does not swamp the faint astronomical signal. Bolometers and MKIDs are cryogenic detectors; the technique is essential across the infrared, millimetre, and X-ray.","entryPath":"/observatory-frontier/cryogenic-detector"},{"id":"instrument_technique:deformable-mirror","name":"Deformable Mirror","type":"instrument_technique","domain":"science","description":"A thin mirror whose surface is reshaped hundreds or thousands of times a second by an array of actuators, cancelling the distortion the atmosphere imposes on starlight in real time. The active heart of adaptive optics — the ELT's M4 is one of the largest ever built.","entryPath":"/observatory-frontier/deformable-mirror"},{"id":"instrument_technique:echelle-spectrograph","name":"Echelle Spectrograph","type":"instrument_technique","domain":"science","description":"A high-resolution spectrograph that uses a coarse, steeply-ruled grating (an échelle) to spread light into many overlapping orders, then a second disperser to separate them — packing very high spectral resolution onto a single detector. The workhorse of precision radial-velocity and stellar-abundance work; HIRES is a classic example.","entryPath":"/observatory-frontier/echelle-spectrograph"},{"id":"instrument_technique:integral-field-spectrograph","name":"Integral-Field Spectrograph","type":"instrument_technique","domain":"science","description":"A spectrograph that records a full spectrum at every point in a two-dimensional field of view at once, producing a 'data cube' of the sky — an image where every pixel is a spectrum. It maps how motion and composition vary across a galaxy or nebula in a single exposure; MUSE on the VLT is a leading example.","entryPath":"/observatory-frontier/integral-field-spectrograph"},{"id":"instrument_technique:laser-guide-star","name":"Laser Guide Star","type":"instrument_technique","domain":"science","description":"An artificial star created by shining a laser into the upper atmosphere, exciting sodium atoms ~90 km up to glow. It gives adaptive optics a bright reference point anywhere on the sky — not just near a real bright star — so the shape of the atmosphere's blur can be measured and corrected.","entryPath":"/observatory-frontier/laser-guide-star"},{"id":"detector_technology:mkid","name":"MKID","type":"detector_technology","domain":"science","description":"A superconducting detector that records not just the arrival of a photon but its energy and precise time, with no read noise. Operating at temperatures near absolute zero, MKIDs are a frontier technology for the millimetre, submillimetre, and optical sky, and scale to large arrays.","entryPath":"/observatory-frontier/mkid"},{"id":"instrument_technique:starshade","name":"Starshade","type":"instrument_technique","domain":"science","description":"A concept for blocking a star's light not inside the instrument but far in front of the telescope — a large, precisely-shaped screen flown tens of thousands of kilometres away, casting a deep shadow so an orbiting planet stands clear. A proposed external alternative to the coronagraph for future exoplanet-imaging missions.","entryPath":"/observatory-frontier/starshade"},{"id":"instrument_technique:wavefront-sensor","name":"Wavefront Sensor","type":"instrument_technique","domain":"science","description":"The eye of an adaptive-optics system — it measures, hundreds or thousands of times a second, exactly how the atmosphere has distorted the incoming light, so a correction can be computed and applied. Common designs are the Shack–Hartmann and pyramid sensors.","entryPath":"/observatory-frontier/wavefront-sensor"}]}