  Rotating accretion flow may undergo centrifugal pressure mediated shock
transition even in presence of various dissipative processes, such as viscosity
and cooling mechanism. The extra thermal gradient force along the vertical
direction in the post shock flow drives a part of the accreting matter as
bipolar outflows which are believed to be the precursor of relativistic jets.
We compute mass loss rates from a viscous accretion disc in presence of
synchrotron cooling in terms of the inflow parameters. We show cooling
significantly affects the mass outflow rate, to the extent that, jets may be
generated from flows with higher viscosity. We discuss that our formalism may
be employed to explain observed jet power for a couple of black hole
candidates. We also indicate that using our formalism, it is possible to
connect the spectral properties of the disc with the rate of mass loss.
