2023, Bourrier, V., Attia, O., Mallonn, M., Marret, A., Lendl, M., Konig, P.-C., Krenn, A., Cretignier, M., Allart, R., Henry, G., Bryant, E., Leleu, A., Nielsen, L., Hebrard, G., Hara, N., Ehrenreich, D., Seidel, J., Dos Santos, L., Lovis, C., Bayliss, D., Cegla, H.M., Dumusque, X., Boisse, I., Boucher, A., Bouchy, F., Pepe, F., Lavie, B., Rey Cerda, J., Ségransan, D., Udry, S., Vrignaud, T.

The distribution of close-in exoplanets is shaped by a complex interplay between atmospheric and dynamical processes. The Desert-Rim Exoplanets Atmosphere and Migration (DREAM) program aims at disentangling those processes through the study of the hot Neptune desert, whose rim hosts planets that are undergoing, or survived, atmospheric evaporation and orbital migration. In this first paper, we use the Rossiter-McLaughlin revolutions (RMR) technique to investigate the orbital architecture of 14 close-in planets ranging from mini-Neptune to Jupiter-size and covering a broad range of orbital distances. While no signal is detected for the two smallest planets, we were able to constrain the sky-projected spin-orbit angle of six planets for the first time, to revise its value for six others, and, thanks to constraints on the stellar inclination, to derive the 3D orbital architecture in seven systems. These results reveal a striking three-quarters of polar orbits in our sample, all being systems with a single close-in planet but of various stellar and planetary types. High-eccentricity migration is favored to explain such orbits for several evaporating warm Neptunes, supporting the role of late migration in shaping the desert and populating its rim. Putting our measurements in the wider context of the close-in planet population will be useful to investigate the various processes shaping their architectures.

2018, Deleuil, M., Aigrain, S., Moutou, C., Cabrera, J., Bouchy, F., Deeg, H. J., Almenara, J.-M., Hébrard, G., Santerne, A., Alonso, R., Bonomo, A.S., Bordé, P., Csizmadia, S., Dìaz, R.F., Erikson, A., Fridlund, M., Gandolfi, D., Guenther, E., Guillot, T., Guterman, P., Grziwa, S., Hatzes, A., Léger, A., Mazeh, T., Ofir, A., Ollivier, M., Pätzold, M., Parviainen, H., Rauer, H., Rouan, D., Schneider, J., Titz-Weider, R., Tingley, B., Weingrill, J.

The CoRoT space mission observed 163 665 stars over 26 stellar fields in the faint star channel. The exoplanet teams detected a total of 4123 transit-like features in the 177 454 light curves. We present the complete re-analysis of all these detections carried out with the same softwares so that to ensure their homogeneous analysis. Although the vetting process involves some human evaluation, it also involves a simple binary flag system over basic tests: Detection significance, presence of a secondary, difference between odd and even depths, colour dependence, V-shape transit, and duration of the transit. We also gathered the information from the large accompanying ground-based programme carried out on the planet candidates and checked how useful the flag system could have been at the vetting stage of the candidates. From the initial list of transit-like features, we identified and separated 824 false alarms of various kind, 2269 eclipsing binaries among which 616 are contact binaries and 1653 are detached ones, 37 planets and brown dwarfs, and 557 planet candidates. We provide the catalogue of all these transit-like features, including false alarms. For the planet candidates, the catalogue gives not only their transit parameters but also the products of their light curve modelling: Reduced radius, reduced semi-major axis, and impact parameter, together with a summary of the outcome of follow-up observations when carried out and their current status. For the detached eclipsing binaries, the catalogue provides, in addition to their transit parameters, a simple visual classification. Among the planet candidates whose nature remains unresolved, we estimate that eight (within an error of three) planets are still to be identified. After correcting for geometric and sensitivity biases, we derived planet and brown dwarf occurrences and confirm disagreements with Kepler estimates, as previously reported by other authors from the analysis of the first runs: Small-size planets with orbital period less than ten days are underabundant by a factor of three in the CoRoT fields whereas giant planets are overabundant by a factor of two. These preliminary results would however deserve further investigations using the recently released CoRoT light curves that are corrected of the various instrumental effects and a homogeneous analysis of the stellar populations observed by the two missions.