$against$ $localization$ $of$ $events$  [@DFR],  [@BDMP]. This principle implies Spacetime Uncertainty Relations $$\Delta q_0 \cdot \sum \limits_{j = 1}^3 \Delta q_j \gtrsim 1 ; \sum   
\limits_{1 \leq j < k \leq 3 } \Delta q_j  \Delta q_k \gtrsim 1 .$$ for the coordinates $q_\mu$ of an event, which must be implemented by Spacetime commutation relations $$[q_\mu  ,q_\nu  ]   =   i \lambda_P^2   Q_{\mu \nu}$$ where $\lambda_P$ is the Planck length and where $Q_{\mu \nu}$ satisfies appropriate Quantum Conditions.

The simplest solution is given by: $$\begin{aligned}
[q^\mu , Q^{\nu \lambda}]  &=  0,\\
\label{dopleq14}
Q_{\mu \nu} Q^{\mu \nu}  &=  0,\\
((1/2) \left[q_0  ,\dots,q_3 \right] )^2 &= I,\end{aligned}$$ where $$\begin{aligned}
\left[q_0  ,\dots,q_3 \right]  &\equiv  \det \left(
\begin{array}{ccc}
q_0 & \cdots  & q_3 \nonumber\\
\vdots  & \ddots  & \vdots  \\
q_0 & \cdots  & q_3
\end{array}
\right)\\&\equiv  \varepsilon^{\mu \nu \lambda \rho} q_\mu q_\nu q_\lambda 
q_\rho =\nonumber\\&= - (1/2) Q_{\mu \nu}  (*Q)^{\mu \nu}\end{aligned}$$ (notice that $Q_{\mu \nu} Q^{\mu \nu}$ is a scalar and $ Q_{\mu \nu}  (*Q)^{\mu \nu}$ is a pseudoscalar, hence we square it in the Quantum Conditions).

Called for brevity *the Basic Model of Quantum Spacetime*, this model implements exactly the Space Time Uncertainty Relations and is fully Poincaré covariant.

The $noncommutative$ C\* algebra 