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We reconsider the problem of a slowly rotating homogeneous star, orSchwarzschild star, when its compactness goes beyond the Buchdahl bound andapproaches the gravastar limit $R\to 2M$. We compute surface and integralproperties of such configuration by integrating the Hartle-Thorne structureequations for slowly rotating relativistic masses, at second order in angularvelocity. In the gravastar limit, we show that the metric of a slowly rotatingSchwarzschild star agrees with the Kerr metric, thus, within thisapproximation, it is not possible to tell a gravastar from a Kerr black hole byany observations from the spacetime exterior to the horizon.

Slowly rotating ultracompact Schwarzschild star in the gravastar limit