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EyeSat has been a tremendous, challenging and successful student project. With 250 students over 7 years, CNES has achieved to put in orbit a 3U CubeSat that carries tens of state-of-the art innovative nanosatellite subsystems resulting from R&D programs carried out within the French space ecosystem. Launched in December 18, 2019, EyeSat has proved to be fully functional in orbit and has started its mission to map the intensity and the polarization direction of the zodiacal light. Housekeeping data, acquired over the past 5 months, has been analyzed by the team. Precious comparisons have been made between design and simulation results on the one hand and actual data on the other. Now, the private company U-Space, created in 2018, leverages those lessons learned from EyeSat and provides space missions based on high-performance nanosatellites.

AGU Fall Meeting 2019 in San Francisco , 9-13 December 2019, EIS/InSIght team, InSight is the first planetary mission with a seismometer package, SEIS, since the Apollo Lunar Surface Experiments Package. SEIS is complimented by APSS, which has as a goal to document the atmospheric source of seismic noise and signals. Since June 2019, SEIS has been delivering 6 axis 20 sps continuous seismic data, a rate one order of magnitude larger originally planned. More than 50 events have been detected by the end of July 2019 but only three have amplitudes significantly above the SEIS instrument requirement. Two have clear and coherent arrivals of P and S waves, enabling location, diffusion/attenuation characterization and receiver function analysis. The event¿s magnitudes are likely ¿ 3 and no clear surface waves nor deep interior phases have been identified. This suggests deep events with scattering along their final propagation paths and with large propagation differences as compared to Earth and Moon quakes. Most of the event¿s detections are made possible due to the very low noise achieved by the instrument installation strategy and the very low VBB self-noise. Most of the SEIS signals have amplitudes of spectral densities in the 0.03-5Hz frequency bandwidth ranging from 10-10 m/s2/Hz1/2 to 5 10-9 m/s2/Hz1/2. The smallest noise levels occurs during the early night, with angstrom displacements or nano-radian tilts. This monitors the elastic and seismic interaction of a planetary surface with its atmosphere, illustrated not only by a wide range of SEIS signals correlated with pressure vortexes, dust devils or wind activity but also by modulation of resonances above 1 Hz, amplified by ultra-low velocity surface layers. After about one half of a Martian year, clear seasonal changes appear also in the noise, which will be discussed. One year after landing, the seismic noise is therefore better and better understood, and noise correction techniques begun to be implemented, either thanks to the APSS wind and pressure sensors, or by SEIS only data processing techniques. These data processing techniques open not only the possibility of better signal to noise ratio of the events, but are also used for various noise auto-correlation techniques as well as searches of long period signals. Noise and seismic signals on Mars are therefore completely different from what seismology encountered previously on Earth and Moon.

L'institut géographique national d'Espagne a publié en 2008 un très bel Atlas en couleurs in folio de démographie de l'Espagne. L'aspect matériel en est absolument impeccable. Au-delà des problèmes de recensement, on rêve pour la France de telles publications. L'ouvrage compte 420 cartes en couleurs, dont 1/4 sont à l'échelle communale. De très nombreux tableaux et graphiques ainsi que des photos illustrent les textes. Il offre donc une vision très détaillée de la démographie actuelle de l'Es...