A full paper will be published in a refereed journal later. We obtained 179 frames of one 11.5 by 11.5 arcmin field in M 34 using a filter, which we shall call g', whose effective wavelength is 4825 Angstr m. For the purpose of frequency analysis of data from the whole observing run we needed to do some averaging. These transformations are only necessary in the context of this paper to estimate the spectral types of some stars in M 34. The large open squares represent stars too bright for photometric analysis.
North is up.
East is to the left. The dotted region is the area of overlap between the two fields. 1 we give an identification chart of the parts of M 34 which were imaged. Since non-linear effects begin with the USNO camera when one obtains more than 16,000 ADUs per pixel, some of the stars were too bright for accurate photometric analysis. These are indicated by open squares in the figure.