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The Rossiter-McLaughlin effect observed for transiting exoplanets oftenrequires prior knowledge of the stellar projected equatorial rotationalvelocity. This is usually provided by measuring the broadening of spectrallines, however this method has uncertainties as lines are also broadened byvelocity fields in the stellar photosphere known as macroturbulence. We haveestimated accurate rotational velocity values from asteroseismic analyses ofmain sequence stars observed by Kepler. The rotational frequency splittings ofthe detected solar-like oscillations of these stars are determined largely bythe near-surface rotation. These estimates have been used to infer themacroturbulence values for 28 Kepler stars. Out of this sample, 26 stars wereused along with the Sun to obtain a new calibration between macroturbulence,effective temperature and surface gravity. The new calibration is valid for thetemperature range 5200 to 6400 K and the gravity range 4.0 to 4.6 dex. Acomparison is also provided with previous macroturbulence calibrations. As aresult of this work, macroturbulence, and thus rotational velocity, can now bedetermined with confidence for stars that do not have asteroseismic dataavailable. We present new spectroscopic rotational velocity values for the WASPplanet host stars, using high resolution HARPS spectra.

Determining stellar macroturbulence using asteroseismic rotational velocities from Kepler