ESA Data Ontology: ESADO: LPSP

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LPSP

The LPSP multichannel High Resolution UV and visible spectometer was launched June 21, 1975 and was in operation until September 30, 1978 with 6 channels covering the most intense optically thick chromospheric lines (H and K CaII, h and k MgII, Lymann alpha and Lymann beta HI) The imaging system is a cassegranian telescope, with a collecting area of 170 cm2 and an aperture f/16. The solar image can be scanned by moving the secondary mirror in azimuth and elevation. Each step increment is either 1' or .5'. The size of the raster in azimuth and elevation is chosen between 1' to 64' by binary increments. The slit defines the focus of the telescope and is formed of two parts : -a narrow one of 1'x60' which optimizes the spectrometer resolution -a large one of 6'x6' -a rotating disk actuated by a stepping motor allows the selection of several spatial resolution. The dispersing system is a 6 channel polychromator of the Czerny-Turner type. The main dispersor is a 1200 grooves (1/mm) plane grating. The scan in wavelength is performed by rotation of the grating. Raw data are on 1600 bpi magnetic tapes and saved on 6250 bpi tapes, all created on CDC computer running NOS-BE system. [Summary provided by NASA] (en)

https://gcmd.earthdata.nasa.gov/kms/concept/e999ce1b-d55c-40b8-a3c3-c4e93b34529d

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ESA Data Ontology