General remarks

The observer should be familiar with the techniques of near infrared observation:

• Sky-subtraction: For every frame of the astronomical object one sky frame should be recorded (pointing sequence programmable)
• Flat field correction: For every image scale and wavelength a flat-field should be generated (dome-flats, twilight-flats, etc.)
• Photometric calibration: Several photometric reference stars nearby the object of interest should be observed simultaneously

Because the correction of the atmospheric aberrations by adaptive optics is incomplete, full advantage from adaptive optics observations can be achieved only by deconvolution (Lucy-Richardson algorithm, maximum entropy deconvolution, etc.) with the point spread function. This point spread function is highly depending on the seeing conditions and the brightness of the reference star. Therefore, if there is no well separated reference star within the observed field, a separate observation of a nearby reference star of similar brightness is necessary.