A new numerical inversion scheme of m sin i exo-planet mass distribution: its double peak remains after inversion.

International audienceThe use of radial velocity (RV) measurements of stars has proven very successful at the indirect detection of planets orbiting other stars, since both the planet (unseen) and the star are orbiting around their common center of mass. Unfortunately the mass m of the exo-planet cannot be retrieved: only the product m sin i is derived from the amplitude of the RV wobble, where i is the inclination of the polar axis of the orbit on the line of sight (LOS) from the observer to the star.However, when a reasonable number of exo-planets are detected, giving an observed distribution of m sin i it is possible to retrieve the distribution function of planetary masses f(m) that will give the observed distribution fO(m sin i). One has to make the assumption that the orientations of orbital polar axis are isotropically distributed in space, and independent of the distribution f(m). We have developed a new representation of exo-planets in a 3D space, and established a formally exact solution to the inversion problem, based on spheres and cylinders. We have applied this method to the more than 700 known exo-planets masses. The observed distribution of m sin i shows two peaks, one around 0.025 Mjup (Jupiter mass) and one around 2 Mjup. After inversion, the true distribution of masses still present a double peak, showing that this double peak is not an artefact or shortcoming of the RV method. Our new inversion scheme will be presented and the double peak discussed. Coauthors from IKI acknowledge support from the Russian Government Grant #14.W03.31.0017

Improved near-infrared high-resolution solar spectrum from ACS NIR onboard TGO

International audienceHere we present solar spectrum obtained from solar observations by ACS NIR instrument. We have found difference between Continuum Absorption at Visible and Infrared Wavelengths and its Atmospheric Relevance (CAVIAR) and spectrum observed by NIR

Near-infrared high-resolution solar spectrum from ACS NIR onboard TGO

International audienceThe Atmospheric Chemistry Suite (ACS) is Russian contribution to ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter (TGO) mission. It arrived at Mars in October 2016. In this work, we present preliminary results for high-resolution solar spectra observed by ACS NIR instrument in the near-infrared range

Near-infrared high-resolution solar spectrum from ACS NIR onboard TGO

International audienceThe Atmospheric Chemistry Suite (ACS) is Russian contribution to ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter (TGO) mission. It arrived at Mars in October 2016. In this work, we present preliminary results for high-resolution solar spectra observed by ACS NIR instrument in the near-infrared range

Performance of the ACS NIR channel in nadir

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Near-infrared high-resolution solar spectrum from ACS NIR onboard TGO

International audienceThe Atmospheric Chemistry Suite (ACS) is Russian contribution to ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter (TGO) mission [1, 2]. It arrived at Mars in October 2016. ACS is a package of three highly sensitive infrared spectrometers with high resolve power (>10,000) and covers from 0.7 to 17µm-the visible to thermal infrared range. In this work, we present results for high-resolution solar spectra observed by ACS NIR instrument in the near-infrared range

Performance of the ACS NIR channel and O 2 profiles

International audienceThe Atmospheric Chemistry Suite (ACS) is a set of three spectrometers (-NIR,-MIR, and-TIRVIM) intended to observe Mars atmosphere onboard the ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter(TGO) mission