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Proceedings Paper • Open Access

Atise: a miniatureFourier-transform spectro-imaging concept for surveying auroras and airglow monitoring from a 6/12u cubesat
Author(s): E. Le Courer; M. Barthelemy; A. Vialatte; M. Prugniaux; G. Bourdarot; T. Sequies; P. Monsinjon; R. Puget; N. Guerineau

Paper Abstract

The nanosatellite ATISE is a mission dedicated to the observation of the emission spectra of the upper atmosphere (i.e. Airglow and Auroras) mainly related to both the solar UV flux and the precipitation of suprathermal particles coming from the solar wind through the magnetosphere. ATISE will measure specifically the auroral emissions, and the airglow (day- and night) in the spectral range between 380 and 900 nm at altitudes between 100 and 350 km. The exposure time will be 1 second in auroral region and 20 s at low latitude regions. The 5 year expected lifetime of this mission should cover almost a half of solar cycle (2 years nominal). This instrument concept is based on an innovative miniaturized Fourier-transform spectrometer (FTS) allowing simultaneous 1 Rayleigh sensitivity detection along six 1.5°x1° limb lines of sight. This 1-2kg payload instrument is hosted in a 12U cubeSat where 6U are allocated to the payload and 6U to the plateform subsystems. This represents a miniaturisation by a factor of 500 on weight and volume compared to previous Arizona-GLO instrument for equivalent performances in the visible. The instrument is based on microSPOC concept developed by ONERA and IPAG using one Fizeau interferometer per line of sight directly glued on top of the half of a very sensitive CMOS Pyxalis HDPYX detector. Three detectors are necessary with a total electrical consumption compatible with a 6U nanoSat. Each interferometer occupies a 1.4 M pixel part of detector, each is placed on an image of the entrance pupil corresponding to a unique direction of the six lines of sight, this in order to have a uniform illumination permitting good spectral Fourier reconstruction from fringes created between the Fizeau plate and the detector itself. Despite a limited 8x6 cm telescope, this configuration takes advantage of FTS multiplex effect and permits us to maximize the throughput and to integrate very faint emission lines over a wide field of view even if the 1 second integrated signal is comparable to the detector noise.

Paper Details

Date Published: 25 September 2017
PDF: 9 pages
Proc. SPIE 10562, International Conference on Space Optics — ICSO 2016, 105620W (25 September 2017); doi: 10.1117/12.2296214
Show Author Affiliations
E. Le Courer, Univ. Grenoble Alpes, CNRS (France)
Ctr. Spatial Univ. de Grenoble (France)
M. Barthelemy, Univ. Grenoble Alpes, CNRS (France)
Ctr. Spatial Univ. de Grenoble (France)
A. Vialatte, Univ. Grenoble Alpes, CNRS (France)
Ctr. Spatial Univ. de Grenoble (France)
M. Prugniaux, Ctr. Spatial Univ. de Grenoble (France)
G. Bourdarot, Univ. Grenoble Alpes, CNRS (France)
Ctr. Spatial Univ. de Grenoble (France)
T. Sequies, Ctr. Spatial Univ. de Grenoble (France)
Institut Univ. Technologique de Grenoble (France)
P. Monsinjon, Pyxalis Ctr. Alp (France)
R. Puget, RESOLUTION Spectra Systems (France)
N. Guerineau, ONERA (France)

Published in SPIE Proceedings Vol. 10562:
International Conference on Space Optics — ICSO 2016
Bruno Cugny; Nikos Karafolas; Zoran Sodnik, Editor(s)

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