The association surrounding NGC 2439

The structure of the field surrounding the Galactic cluster NGC 2439 is stu died utilizing uvby beta photometry of bright OB stars. We collate all phot ometric and kinematic data available to identify possible groupings. The st ars of our sample show a large scatter in their distances, radial velocitie s, proper motions and reddenings. We conclude that they do not belong to a single stellar association. We find evidence of the existence of three cohe rent structures at distances of 370 pc, 1 kpc, and 2.6-3.2 kpc. The high st ellar density toward NGC 2439 is very likely due to a decreased absorption in this direction, which poses some doubt on the reality of the cluster. A comprehensive uvby beta study of NGC 2439 is required to clarify its nature . The spatial distribution of the stars and their reddening are used to cha racterise the spatial distribution of the visual extinction in the region. The results obtained confirm previously determined constraints on the forma tion mechanism of interstellar CH+ towards the NGC 2439 field.