at the CO(2-1) frequency of 230GHz is 23$\arcsec$, which corresponds to a projected size of 5.6pc at the distance to the LMC.

Observations were conducted in position switching mode using a reference point free of CO(2-1) (at $\alpha$=05$^{h}$37$^{m}$54$^s$, $\delta$=$-69^{\rm \circ}$04$'24''$) for sky subtraction. The backend narrow-band high-resolution spectrometer (HRS) was used with a bandwidth of 80MHz, and a frequency resolution of 41.7kHz, which translates to a velocity resolution of 0.054kms$^{-1}$ at the frequency of CO(2-1). The data were reduced using the GILDAS software [^1], with linear or third-order polynomial for baseline fitting. The resultant spectra were smoothed to a velocity resolution of 0.25kms$^{-1}$. The rms noise achieved in a single channel is 0.07K after 240s of integration. We mapped the 30 Doradus region with 10$\arcsec$ spacings and detected CO(2-1) emission across 30 Doradus, including the stapler nebula where CO(1-0) emission had not been previously detected (Pineda et al. 2009; Johansson et al. 1998). In Fig.1, the CO(2-1) contours are overlaid on a [*Hubble space telescope*]{} (HST) three colour optical $BVI$H$\alpha$ image of 30 Doradus, where the position of CO(2-1) emission with respect to the R136 cluster, and its ionized surroundings can be visualized. Our observations represent a five-fold increase in 