  Accretion on length-scales of interstellar or even intergalactic is
particularly relevant, in the context of spherical or quasi-spherical hot mode
accretion, supposedly powering low excitation radio galaxies in the
maintenance-mode feedback paradigm. In the present study, we aim to analyze
such a spherical-type flow around the host active nucleus in the backdrop of a
five-component galactic system (SMBH, stellar, dark matter, diffuse hot gas,
$\Lambda$), with the principal intent to address the issue of {\it galactic
potential induced shock} formation in the flow, that may contain (dissipative)
isothermal standing shocks. The present paper is an extension of Raychaudhuri
et al. (2018), who conducted a preliminary investigation of such a problem. The
galactic potential, not only renders the flow to be multi-transonic in nature,
the flow topology resembles `$X\alpha$' and `$\alpha X$' type trajectories of
advective flows in the vicinity of the BHs/compact objects. Owing to the
influence of the galactic potential, the entire range of galactic mass-to-light
ratio ($\Upsilon_B$) allows shock formation in central to the outer radial
regions of our wind-type flows, with the strength of those galactic induced
shocks found to be comparable to that of the shocks one would expect in the
advective flows in the vicinity of a BH. We also observe that the shock
parameters remain sensitive to $\Upsilon_B$. We discussed the possible
implication of these shocks in the context of radio source dynamics as well as
their potential association with flaring in radio jets. Our study also reveals
that galactic potential could substantially augment the mass inflow rate.
