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Using the IRAM 30m telescope we have surveyed a $1\times0.8^{\circ}$ part ofthe Orion molecular cloud in the $^{12}$CO and $^{13}$CO (2-1) lines with amaximal spatial resolution of $\sim$11" and spectral resolution of $\sim$ 0.4km~s$^{-1}$. The cloud appears filamentary, clumpy and with a complexkinematical structure. We derive an estimated mass of the cloud of 7700M$_{\text{Sun}}$ (half of which is found in regions with visual extinctions$A_V$ below $\sim$10) and a dynamical age for the nebula of the order of 0.2Myrs. The energy balance suggests that magnetic fields play an important rolein supporting the cloud, at large and small scales. According to our analysis,the turbulent kinetic energy in the molecular gas due to outflows is comparableto turbulent kinetic energy resulting from the interaction of the cloud withthe HII region. This latter feedback appears negative, i.e. the triggering ofstar formation by the HII region is inefficient in Orion. The reduced data aswell as additional products such as the column density map are made availableonline at http://userpages.irap.omp.eu/~oberne/Olivier_Berne/Data.

IRAM-30m large scale survey of $^{12}$CO(2-1) and $^{13}$CO(2-1) emission in the Orion molecular cloud