The absolute solar spectral irradiance from 200 to 2500nm as measured by the SOLSPEC spectrometer with the ATLAS and EURECA missions

International audienceThe SOLSPEC instrument measures the absolute solar spectral irradiance from 200 to 2500 nm. The instrument flew in March 1992, March 1993 and November 1994 with the three ATLAS missions during 10 days. SOSP is the spare unit of SOLSPEC. It flew on the EURECA platform from 11 August 1992 to May 1993. SOLSPEC and SOSP are made of three spectrometers and contains several lamps allowing to check in flight, the instrument stability and its wavelength scale.These two units have an identical design and are made of the same components. However, their detectors have different performance leading to a SOSP responsivity smaller than the SOLSPEC responsivity. As during the ATLAS missions two other spectrometers were also observing in the UV and near visible domain, we took advantage of this situation by choosing SOLSPEC for the three ATLAS missions. Afterward, it appeared that it was also the good choice for the IR channel of SOSP on board EURECA.The calibration of the instrument is performed with the blackbody of the Heidelberg observatory (Mandel et al., 1998). Its temperature is adjusted as a function of the wavelength domain, ranging from 3000 K for UV calibration, down to 2700 K for the IR spectrometer calibration. The blackbody temperature is measured with a pyrometer calibrated by the Physikalisch-Technische Bundesanstalt (PTB) of Berlin (Germany). The mean accuracy of the solar irradiance is estimated to be 2 to 3% in UV and 2% in the visible and infrared domains. In details, it depends on the spectral interval being better in the middle of each spectral domain.We shall present the best data obtained during the ATLAS and EURECA missions, e.g., UV and visible spectra from the three ATLAS missions and the IR results from EURECA.The duration of each ATLAS mission does not allow study of the solar variability. This is why the best spectra are selected. This selection is based on several criteria including the thermal conditions, stability of the pointing, linearity of the measurements, stability of the wavelength scale, position of the Sun in the field of view and tangent height of the line of slight observations greatern than 100 km. The selected spectra are averaged afterward. A similar procedure was also applied to the SOSP infrared data because the solar variability in this domain is very small and is not detectable with SOSP. Special care was dedicated to this channel due to the variable responsivity in the field of view. Spectra which were not measured in the condition of the laboratory calibration, were eliminated