https://hal-insu.archives-ouvertes.fr/insu-02543065Ananyeva, Vladislava I.Vladislava I.AnanyevaIKI - Space Research Institute of the Russian Academy of Sciences - RAS - Russian Academy of Sciences [Moscow]Ivanova, Anastasiia E.Anastasiia E.IvanovaIKI - Space Research Institute of the Russian Academy of Sciences - RAS - Russian Academy of Sciences [Moscow]Venkstern, Alla A.Alla A.VenksternIKI - Space Research Institute of the Russian Academy of Sciences - RAS - Russian Academy of Sciences [Moscow]Shashkova, Inna A.Inna A.ShashkovaIKI - Space Research Institute of the Russian Academy of Sciences - RAS - Russian Academy of Sciences [Moscow]Yudaev, Andrey V.Andrey V.YudaevMIPT - Moscow Institute of Physics and Technology [Moscow]Tavrov, Alexander V.Alexander V.TavrovIKI - Space Research Institute of the Russian Academy of Sciences - RAS - Russian Academy of Sciences [Moscow]Korablev, Oleg I..Oleg I..KorablevIKI - Space Research Institute of the Russian Academy of Sciences - RAS - Russian Academy of Sciences [Moscow]Bertaux, Jean-LoupJean-LoupBertauxIKI - Space Research Institute of the Russian Academy of Sciences - RAS - Russian Academy of Sciences [Moscow]HELIOS - LATMOS - LATMOS - Laboratoire Atmosphères, Milieux, Observations Spatiales - UVSQ - Université de Versailles Saint-Quentin-en-Yvelines - INSU - CNRS - Institut national des sciences de l'Univers - SU - Sorbonne Université - CNRS - Centre National de la Recherche ScientifiqueMass distribution of exoplanets considering some observation selection effects in the transit detection techniqueHAL CCSD2020Transiting exoplanetsPlanetary formationExoplanet mass distribution[SDU] Sciences of the Universe [physics]Cardon, Catherine2020-04-15 09:49:252021-12-03 11:42:522020-04-15 09:49:25enJournal articles10.1016/j.icarus.2020.1137731While the radial velocity technique (RV) allows to determine only the product m·sin i of the mass m of one exoplanet by sin i (i, angle of inclination of orbital pole to the observer), when it is applied to a planet already detected while transiting its host star, the true mass m is determined, since angle i is near 90° and sin i ~ 1. Therefore, the mass distribution of transiting exoplanets discovered by photometric observations is of particular interest. However, there are some selection effects that distort the true (original) mass distribution into the observed mass distribution. We have studied the whole observed mass distribution of transiting exoplanets that were discovered from space-borne and ground-based surveys (NASA Exoplanet Archive 2019) and corrected them from some selection effects to retrieve a de-biased true mass distribution. For this, we take into account two factors: the probability of mass determination and the probability of transit configurations. The first factor is a bias introduced by a number of effects inherent to the RV method. The bias factor could be estimated by computing the fraction of transiting planets for which the mass was determined from the RV or TTV (Transit Timing Variations) methods. Photometric surveys for transit detection allow determining the planetary radii, and the bias factor was estimated for various bins of planetary sizes. The second factor is the transit probability, a geometrical factor which is precisely known for each detected transiting planet and therefore easy to account for. The mass distribution of exoplanets corrected for the first factor (de-biased) was analyzed, and it is found that this distribution can be well approximated by a power law: dN/dm ∝ m−2. When both factors of observation selection are taken into account, a flat statistically significant area (plateau) in the mass interval of 0.3–2 mJ appears on the mass distribution. The mass distributions derived from transiting planets is preliminary and can be updated after the RV follow-up of K2 planets will be more complete and the number of Kepler1 confirmed planets definitive. The significances of the local minima (plateau) in the retrieved mass distribution have been estimated by the Kolmogorov-Smirnov test.Our de-biased mass distribution was compared to the theoretical model of Mordasini (2018). The slopes are similar, but a plateau present in the model in the range 0.1–5 Jupiter mass is appearing in the data if one considers the probability of transit configuration and considers the lower sensitivity of transit method (with follow-up mass measurement by RV) to planets with long periods and large orbits. In fact, Mordasini (2018) included exoplanets on all orbits. The Gaia2 astrometric method should be able to clarify this discrepancy.Radial velocity surveys are more complete than transits for long period planets. And though the sin i effect is present, its amplitude is indeed not strongly relevant from a statistical point of view (and can actually be taken into account). However RV-database is formed by surveys with substantially different durations, sensitivities, and other sources of inhomogeneities. Some examples of regularization of RV data are shown by e.g. (Mordasini, 2018; Ananyeva et al., 2019; Tuomi et al., 2019), but it is hoped that more biases/inhomogeneities may be dealt with in the future.