  The angular distribution of GRB jets is not yet clear. The observed
luminosity of GRB 170817A is the lowest among all known short GRBs, which is
best explained by the fact that our line of sight is outside of the jet opening
angle, $\theta_{obs}$ $>$ $\theta_j$, where $\theta_{obs}$ is the angle between
our line of sight and jet axis. Inferred by gravitational wave observations, as
well as radio and X-ray afterglow modeling of GRB 170817A, it is likely that
$\theta_{obs}$ $\sim$ 20$^{\circ}$ -- 28$^{\circ}$. In this work, we
quantitatively consider two scenarios of angular energy distribution of GRB
ejecta: top-hat jet, and structured jet with a power law index $s$. For top-hat
jet model, we get a large $\theta_j$ (e.g., $\theta_{j}$$>$$10^{\circ}$), a
rather high local (i.e., z$<$0.01) short GRB rate $\sim$8--15$\times10^3$
$Gpc^{-3}$$yr^{-1}$ (estimated 90$\sim$1850 $ Gpc^{-3}$$yr^{-1}$ in Fong et al.
2015) and an extremely high
$E_{peak,0}$(on-axis,rest-frame)$>$7.5$\times10^4$keV($\sim$500keV for typical
short GRB). For structured jet model, we use $\theta_{obs}$ to give limits on
$s$ and $\theta_{j}$ for a typical on-axis luminosity short GRB (e.g.,
$10^{49}$ erg s$^{-1}$$\sim$$10^{51}$ erg s$^{-1}$), and a low on-axis
luminosity case (e.g., $10^{49}$ erg s$^{-1}$) gives more reasonable values of
$s$. A structured jet model is more feasible for GRB 170817A than a top-hat jet
model, due to the rather high local short GRB rate and the extremely high
on-axis $E_{peak,0}$ almost rules out the top-hat jet model. GRB 170817A is
likely a low on-axis luminosity GRB ($10^{49}$ erg s$^{-1}$) with a structured
jet.
