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Fig. 3


Examples of the contamination of Euclid FOV by SSOs. Left: survey field 15117 centered on (RA, Dec) = (167.218°, +12.740°) and starting on 2022 June 16 at 20:26:05 UTC. The successive trails impressed by the 6 known SSOs during the Euclid hour-long sequence of VIS-NISP imaging observations are drawn in different colors, one for each filter (VIS, Y, J, and H). We can expect about a hundred times more SSOs at the limiting magnitude of Euclid (e.g., Fig. 4). The inset is a magnified view of 2014 WQ501, a main-belt asteroid, illustrating the highly elongated shape of an SSO in Euclid frames. The scale bar of 6′′ corresponds to 60 pixels in VIS frames and 20 pixels in NISP. The timings reported are the starting time of the VIS exposures. The slitless spectra will be acquired by NISP simultaneously with the VIS images. Right: calibration field 13 165 centered on (RA, Dec) = (76.785°, +23.988°) and starting on 2022 March 9° at 20:37:37 UTC. There are 117 known SSOs in the field, and here also, a hundred times more SSOs will be detected at the limiting magnitude of Euclid.

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