  Context. The interaction of solar oscillations with near surface convection
is poorly understood. These interactions are likely the cause of several
problems in helio- and astero-seismology, including the so-called surface
effect and apparently unphysical travel time shifts as a function of center to
limb distance. There is thus a clear need for further theoretical understanding
and observational tests.
  Aims. The aim is to determine how the observed modes are affected by the
convection.
  Methods. I use HMI velocity and intensity images to construct k-$\omega$
diagrams showing how the oscillation amplitude and phase depend on the local
granulation intensity.
  Results. There is a clear and significant dependence of the observed
properties of the oscillations on the local convection state.
