Here we describe scientific processing pipeline of ASPIICS. The ASPIICS coronagraph onboard the formation ying PROBA-3 mission will deliver unprecedented observations of the solar corona starting from 1:1Rꙩ with low straylight. The Science Operations Center (SOC) of ASPIICS, to be installed at the Royal Observatory of Belgium, is responsible for delivering the raw and radiometrically calibrated data products to the science community. Among other processes, the SOC hosts the ASPIICS science data pipeline. The science processing of the ASPIICS data is required to account for the optical and detector effects correctly, convert the data into physical units, merge individual exposures into full field of view images, and calculate the polarized and spectral data products. The general architecture of the SOC is discussed and a particular attention is paid to the science data pipeline.
PROBA2 is an ESA technology demonstration mission to be launched in early 2007. The two primary scientific instruments on board of PROBA2 are SWAP (Sun Watcher using Active Pixel System detector and Image Processing) and the LYRA VUV radiometer. SWAP provides a full disk solar imaging capability with a bandpass filter centred at 17.5 nm (FeIX-XI) and a fast cadence of ≈1 min. The telescope is based on an off-axis Ritchey Chretien design while an extreme ultraviolet (EUV) enhanced APS CMOS will be used as a detector. As the prime goal of the SWAP is solar monitoring and advance warning of Coronal Mass Ejections (CME), on-board intellige nce will be implemented. Image recognition software using experimental algorithms will be used to detect CMEs during the first phase of eruption so the event can be tracked by the spacecraft without huma n intervention. LYRA will monitor solar irradiance in four different VUV passbands with a cadence of up to 100 Hz. The four channels were chosen for their relevance to solar physics, aeronomy and space weather: 115-125 nm (Lyman-α), 200-220 nm Herzberg continuum, the 17-70 nm Aluminium filter channel (that includes the HeII line at 30.4 nm) and the 1-20 nm Zirconium filter channel. On-board calibration sources will monitor the stability of the detectors and the filters throughout the duration of the mission.