We have carried out a survey of the NGC 2068 region in the Orion B molecular cloud using HARP on the JCMT , in the ^ { 13 } CO and C ^ { 18 } O ( J = 3 – 2 ) and H ^ { 13 } CO ^ { + } ( J = 4 – 3 ) lines .
We used ^ { 13 } CO to map the outflows in the region , and matched them with previously defined SCUBA cores .
We decomposed the C ^ { 18 } O and H ^ { 13 } CO ^ { + } into Gaussian clumps , finding 26 and 8 clumps respectively .
The average deconvolved radii of these clumps is 6200 \pm 2000 AU and 3600 \pm 900 AU for C ^ { 18 } O and H ^ { 13 } CO ^ { + } respectively .
We have also calculated virial and gas masses for these clumps , and hence determined how bound they are .
We find that the C ^ { 18 } O clumps are more bound than the H ^ { 13 } CO ^ { + } clumps ( average gas mass to virial mass ratio of 4.9 compared to 1.4 ) .
We measure clump internal velocity dispersions of 0.28 \pm 0.02 km s ^ { -1 } and 0.27 \pm 0.04 km s ^ { -1 } for C ^ { 18 } O and H ^ { 13 } CO ^ { + } respectively , although the H ^ { 13 } CO ^ { + } values are heavily weighted by a majority of the clumps being protostellar , and hence having intrinsically greater linewidths .
We suggest that the starless clumps correspond to local turbulence minima , and we find that our clumps are consistent with formation by gravoturbulent fragmentation .
We also calculate inter-clump velocity dispersions of 0.39 \pm 0.05 km s ^ { -1 } and 0.28 \pm 0.08 km s ^ { -1 } for C ^ { 18 } O and H ^ { 13 } CO ^ { + } respectively .
The velocity dispersions ( both internal and external ) for our clumps match results from numerical simulations of decaying turbulence in a molecular cloud .
However , there is still insufficient evidence to conclusively determine the type of turbulence and timescale of star formation , due to the small size of our sample .