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Fig. 12


a) Height to the Galactic plane of symmetry (ZGC) as a function of the Galactic radius (RGC) for the whole sample. Blue crosses represent stars from the LRc01 direction, green circles stars from the SRc01 direction, and red plus stars from the LRa01 direction. Planet-hosting stars are represented with black thick uncertainty bars. The dotted lines correspond to the typical scale height of the thin and thick discs reported by Veltz et al. (2008). b) Toomre diagram representing the different Galactic populations in our sample: thin disc (cyan △ ), thick disc (yellow ∗) and halo stars, (orange ⋄ ). Dotted lines represent circles with radius every 50 km s-1. c) Bottlinger diagram: U versus V velocities. The symbols are the same as in the Toomre diagram. The thin disc stars are focussed at U = 0 km s-1 and V = 0 km s-1. d) Kinematical heat diagram of W velocities. The symbols are the same as in the Toomre diagram. The separation between the stellar populations is clear with the kinematically hottest stars being the halo stars and the coolest ones corresponding to the thin disc. e) Peculiar velocity () as a function of the overall metallicity. The symbols are the same as in f). We represented in thick black the planet-hosting stars for a) to e). f) α-enhancement as a function of the metallicity. The solid line corresponds to the standard law we used in our grid, the dashed line corresponds to 1σ deviation from this law.

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