THE NATURE OF OH IR SEARS IN THE GALACTIC-CENTER/

We report on infrared observations of stars in a field of 30' near the galactic centre. All these objects were previously detected as OH (16 12 MHz) maser sources. For a large fraction of these stars variability data are available from a VLA monitor programme. This makes it possib le to correct the IR measurements for variability. Corrections for int erstellar extinction are also applied. The resulting infrared colours, periods and luminosities are compared with results for other samples of OH/IR stars and it is shown that the galactic centre stars are simi lar to the same type of objects in the bulge of the Galaxy but that mo re luminous (and thus younger) stars exist in the centre. The question of the existence of two distinct populations of OH/IR stars near the galactic centre is addressed, but the limited number of stars inhibits a firm conclusion. We do find that when the sample is divided accordi ng to OH expansion velocity, the dust-to-gas mass loss ratio, which de pends on metallicity, is on average twice as high for the high expansi on velocity group as for the low expansion velocity stars. The luminos ities and the number density of the low expansion velocity stars are c onsistent with them being an extension of the bulge population, wherea s the high expansion velocity group contains brighter sources and is m ore likely to be a population intrinsic to the galactic centre. The pr eviously proposed period-luminosity (PL-) relation for OH/IR stars can be studied with this sample. We find that the OH/IR stars significant ly deviate from the PL-relation and argue that the OH/IR stars have ev olved away from the PL-relation. It was found that non-variable OH/IR stars are often associated with peculiar IR sources.