We present maps of the first-ranked HII region complex Hubble V in the metal-poor Local Group dwarf galaxy NGC 6822 in the first four transitions of { { } ^ { 12 } CO } , the 158 \mu m transition of C ^ { + } , the 21-cm line of HI , the Pa \beta line of HII , and the continuum at 21 cm and 2.2 \mu m wavelengths .
We have also determined various integrated intensities , notably of HCO ^ { + } and near-IR { H _ { 2 } } emission .
Although Hubble X is located in a region of relatively strong HI emission , our mapping failed to reveal any significant CO emission from it .
The relatively small CO cloud complex associated with Hubble V is comparable in size to the ionized HII region .
The CO clouds are hot ( T _ { kin } = 150 K ) and have high molecular gas densities ( n ( { H _ { 2 } } ) \approx 10 ^ { 4 } { cm ^ { -3 } } ) .
Molecular hydrogen probably extends well beyond the CO boundaries .
C ^ { + } column densities are more than an order of magnitude higher than those of CO .
The total mass of the complex is about 10 ^ { 6 } M _ { \odot } and molecular gas account for more than half of this .
The complex is excited by luminous stars reddened or obscured at visual , but apparent at near-infrared wavelengths .
The total embedded stellar mass may account for about 10 \% of the total mass , and the mass of ionized gas for half of that .
Hubble V illustrates that modest star formation efficiencies may be associated with high CO destruction efficiencies in low-metallicity objects .
The analysis of the Hubble V photon-dominated region ( PDR ) confirms in an independent manner the high value of the CO-to- { H _ { 2 } } conversion factor X found earlier , characteristic of starforming low-metallicity regions .