The observations were carried out in January 1995, at the ESO 3.5 m NTT using EMMI in its multi-object spectroscopy mode. Grism #5 was employed yielding a dispersion of 1.3 Å/pix on a Tektronix pixel CCD detector.
A total of seven starplates were produced using the punching machine mounted inside EMMI from a direct image of the region previously obtained. This provides an excellent accuracy in the slit positions without need for accurate astrometry prior to mask construction. Each starplate contained an average of 30 slitlets thus producing more than 200 spectra in total. The slitlets were 1.1'' wide and 8'' long.
The stars included in each starplate were chosen from the direct images in groups of similar brightness and minimum overlapping. Thus, the number of stars and the exposure times differ from plate to plate. Figures 1 and 2 show the slit positions together with the identification numbers from [Parker (1993)].
He-Ar lamp exposures were taken for wavelength calibration, and halogen lamp exposures were obtained for flat-fielding the images.
|Figure 1: Finding chart for observed stars north of R136. Stars observed are enclosed by the slit position, drawn to scale. Numbers correspond to the ones listed in Tables 1 and 2. North is to the top, East to the left|
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