THE DISTRIBUTION OF FAR-INFRARED LIGHT IN THE DUSTY-HAND GALAXY NGC-2146

The Kuiper Airborne Observatory has been used to obtain high spatial r esolution 50 and 100 mu m observations of the peculiar galaxy NGC 2146 . We find that the far-infrared luminosity of NGC 2146 arises in a 21 '' x less than or equal to 16 '' (1.5 kpc x less than or equal to 1.1 kpc) region (FWHM) elongated along the major axis. This limit is consi stent with the size of the central radio continuum and (CO)-C-12 (1-0) sources. The far-infrared distribution is slightly more compact than that of the H alpha; this difference is consistent with the observed p attern of extinction in this galaxy. From a study of the energetics in this galaxy, we conclude that young massive stars are largely respons ible for powering the far-infrared luminosity of NGC 2146. The far-inf rared and CO (1-0) distributions differ from the reddening morphology as seen in optical images and in the Br gamma/H alpha ratio. The starl ight and the ionized gas appear most highly reddened at the prominent dust lane 15 '' to the west of the nucleus, while the CO and far-infra red emission peak near the nucleus. This result can be explained by ei ther a high proportion of cold dust and gas at the dust lane, or a geo metry in which the dust lane lies in front of the main body of the gal axy.