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... > Instruments > Earth Remote Sensing Instruments > Passive Remote Sensing > Spectrometers/Radiometers > Imaging Spectrometers/Radiometers > Sentinel-2 MSI

Preferred term

Sentinel-2 MSI  

Definition

  • The instrument is based on the pushbroom observation concept. The telescope features a TMA (Three Mirror Anastigmat) design with a pupil diameter of 150 mm, providing a very good imaging quality all across its wide FOV (Field of View). The equivalent swath width is 290 km. The telescope structure and the mirrors are made of silicon carbide (SiC) which allows to minimize thermoelastic deformations. The VNIR focal plane is based on monolithic CMOS (Complementary Metal Oxide Semiconductor) detectors while the SWIR focal plane is based on a MCT (Mercury Cadmium Telluride) detector hybridized on a CMOS read-out circuit. A dichroic beamsplitter provides the spectral separation of VNIR and SWIR channels. EADS Astrium SAS of Toulouse is prime for the instrument. The industrial core team also comprises Jena Optronik (Germany), Boostec (Bazet, France), Sener and GMV (Spain), and AMOS, Belgium. The VNIR detectors are built by Astrium-E2V, while the French company Sofradir received a contract to provide the SWIR detectors for MSI. Calibration: A combination of partial on-board calibration with a sun diffuser and vicarious calibration with ground targets is foreseen to guarantee a high quality radiometric performance. State-of-the-art lossy compression based on wavelet transform is applied to reduce the data volume. The compression ratio will be fine tuned for each spectral band to ensure that there is no significant impact on image quality. The observation data are digitized on 12 bit. A shutter mechanism is implemented to prevent the instrument from direct viewing of the sun in orbit and from contamination during launch. The average observation time per orbit is 16.3 minutes, while the peak value is 31 minutes (duty cycle of about 16-31%). Imager type Pushbroom instrument Spectral range (total of 13 bands) 0.4-2.4 µm (VNIR + SWIR) Spectral dispersion technique Dichroic for VNIR and SWIR split In field separation within focal plane Mirror dimensions of telescope M1 = 440 mm x 190 mm M2 = 145 mm x 118 mm M3 = 550 mm x 285 mm SSD (Spatial Sampling Distance) 10 m: (VNIR) B2, B3, B4, B8 (4 bands) 20 m: B5, B6, B7, B8a, B11, B12 (6 bands) 60 m: B1, B9, (3 bands) Swath width 290 km, FOV= 20.6º Detector technologies Monolithic Si (VNIR); hybrid HgCdTe CMOS (SWIR) Detector cooling Cooling of SWIR detector to < 210 K Data quantization 12 bit Instrument mass, power ~ 290 kg, < 266 W Data rate 450 Mbit/s after compression (en)

Broader concept

Change note

  • 2018-07-10 12:30:52.0 [mmorahan] Insert Concept add broader relation (Sentinel-2 MSI [fc57a9a0-a287-4bcf-a517-20811b55596b,367807] - Imaging Spectrometers/Radiometers [944b7691-af37-4fb4-9393-c114e7997829,347979]);
  • 2018-07-10 12:34:37.0 [mmorahan] insert AltLabel (id: null category: primary text: Sentinel-2 Multispectral Imager language code: en); insert Definition (id: null text: The instrument is based on the pushbroom observation concept. The telescope features a TMA (Three Mirror Anastigmat) design with a pupil diameter of 150 mm, providing a very good imaging quality all across its wide FOV (Field of View). The equivalent swath width is 290 km. The telescope structure and the mirrors are made of silicon carbide (SiC) which allows to minimize thermoelastic deformations. The VNIR focal plane is based on monolithic CMOS (Complementary Metal Oxide Semiconductor) detectors while the SWIR focal plane is based on a MCT (Mercury Cadmium Telluride) detector hybridized on a CMOS read-out circuit. A dichroic beamsplitter provides the spectral separation of VNIR and SWIR channels. EADS Astrium SAS of Toulouse is prime for the instrument. The industrial core team also comprises Jena Optronik (Germany), Boostec (Bazet, France), Sener and GMV (Spain), and AMOS, Belgium. The VNIR detectors are built by Astrium-E2V, while the French company Sofradir received a contract to provide the SWIR detectors for MSI. Calibration: A combination of partial on-board calibration with a sun diffuser and vicarious calibration with ground targets is foreseen to guarantee a high quality radiometric performance. State-of-the-art lossy compression based on wavelet transform is applied to reduce the data volume. The compression ratio will be fine tuned for each spectral band to ensure that there is no significant impact on image quality. The observation data are digitized on 12 bit. A shutter mechanism is implemented to prevent the instrument from direct viewing of the sun in orbit and from contamination during launch. The average observation time per orbit is 16.3 minutes, while the peak value is 31 minutes (duty cycle of about 16-31%). Imager type Pushbroom instrument Spectral range (total of 13 bands) 0.4-2.4 µm (VNIR + SWIR) Spectral dispersion technique Dichroic for VNIR and SWIR split In field separation within focal plane Mirror dimensions of telescope M1 = 440 mm x 190 mm M2 = 145 mm x 118 mm M3 = 550 mm x 285 mm SSD (Spatial Sampling Distance) 10 m: (VNIR) B2, B3, B4, B8 (4 bands) 20 m: B5, B6, B7, B8a, B11, B12 (6 bands) 60 m: B1, B9, (3 bands) Swath width 290 km, FOV= 20.6º Detector technologies Monolithic Si (VNIR); hybrid HgCdTe CMOS (SWIR) Detector cooling Cooling of SWIR detector to < 210 K Data quantization 12 bit Instrument mass, power ~ 290 kg, < 266 W Data rate 450 Mbit/s after compression language code: en);
  • 2018-10-23 06:29:58.0 [mmorahan] insert WeightedRelation (id: null related concept uuid: 2ce20983-98b2-40b9-bb0e-a08074fb93b3 relationship type: null relationship value: null generated by: null);

URI

https://gcmd.earthdata.nasa.gov/kms/concept/fc57a9a0-a287-4bcf-a517-20811b55596b

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