  From the early days in gamma-ray astronomy, locating the origin of GeV
emission within the core of an active galactic nucleus (AGN) persisted as an
open question; the problem is to discern between near- and far-site scenarios
with respect to the distance from the super massive central engine. We
investigate this question under the light of a complete sample of low
synchrotron peak (LSP) blazars which is fully characterized along many decades
in the electromagnetic spectrum, from radio up to tens of GeV. We consider the
high-energy emission from bright radio blazars and test for synchrotron
self-Compton (SSC) and external Compton (EC) scenarios in the framework of
localizing the $\gamma$-ray emission sites. Given that the inverse Compton (IC)
process under the EC regime is driven by the abundance of external seed
photons, these photons could be mainly ultraviolet (UV) to X-rays coming from
the accretion disk region and the broad-line region (BLR), therefore close to
the jet launch base; or infrared (IR) seed photons from the dust torus and
molecular cloud spine-sheath, therefore far from jet launch base. We use
enhanced SED information from recent works (including new $\gamma$-ray
detections) to refine the study of Syn to IC peak correlations, which points to
a particular $\gamma$-ray emission site. We show that SSC alone is not enough
to account for the observed SEDs. Our analysis favors an EC scenario under the
Thomson scattering regime, with a dominant IR external photon field. Therefore,
the far-site (i.e., far from the jet launch) is probably the most reasonable
scenario to account for the population properties of bright LSP blazars in
cases modeled with a pure leptonic component. We calculate the photon energy
density associated with the external field at the jet comoving frame to be $\rm
U'_{ext}=1.69 \times 10^{-2}$ erg/cm$^3$, finding good agreement to other
correlated works.
