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Published online by Cambridge University Press: 15 February 2011
The resonances of the bar and the spiral arms of the Milky Way (MW) can induce kinematicgroups in the local stellar velocity distribution. The Gaia mission is going to provide uswith accurate information on the velocity distribution for an extended region of theGalactic disc. Here we aim to evaluate the Gaia capabilities to constrain thenon-axisymmetric large-scale structure of the MW from the observed velocitydistributions.