  The broadband spectral energy distribution(SED) of blazars is generally
interpreted as radiation arising from synchrotron and inverse Compton
mechanisms.Traditionally, the underlying source parameters responsible for
these emission processes,like particle energy density, magnetic field, etc.,
are obtained through simple visual reproduction of the observed fluxes.
However, this procedure is incapable of providing the confidence range on the
estimated parameters. In this work, we propose an efficient algorithm to
perform a statistical fit of the observed broadband spectrum of blazars using
different emission models. Moreover, in this work we use the the observable
quantities as the fit parameters, rather than the direct source parameters
which govern the resultant SED. This significantly improves the convergence
time and eliminates the uncertainty regarding the initial guess parameters.
This approach also has an added advantage of identifying the degenerate
parameters, which can be removed by including more observable information
and/or additional constraints. A computer code developed based on this
algorithm is implemented as an user-defined routine in the standard X-ray
spectral fitting package, XSPEC. Further, we demonstrate the efficacy of the
algorithm by fitting the well sampled SED of the blazar, 3C 279, during its
gamma ray flare in 2014.
