By Allington-Smith J.
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2004 for details). A critical step in the data reduction is the spatial rectiﬁcation, in which the ﬂux received in each detector pixel is associated with the lenslets. Since the individual spectra are separated by only two pixels on the detector, cross-talk between them has to be taken into account properly. We have developed a procedure that distributes the light received at each detector pixel among all lenslets that contribute to the illumination of that pixel in a consistent way (Quirrenbach et al.
2 Proposed Method: The potential of IFS in observations of planet transits Here we want to highlight three main advantages of IFS when performing high S/N time series spectrophotometric observations: i) Ability to gather photons during the transit: S/N enhancement. Gilliland, Goudfrooij, and Kimble (1999) proposed to increase the photometric accuracy of very high S/N observations by using the spectroscopic mode of STIS. By distributing the star light along the dispersion direction it was possible to increase the total number of photons collected before the detector reaches the saturation limit.
Scanning long–slit spectroscopy does not require a new instrument, but uses a normal long-slit spectrograph. It does not simultaneously ﬁll the data cube, but can be used for very elongated objects, like edge-on galaxies, when only coarse information is required in the second spatial direction. 4 Selection of the Most Suitable Technique Although advantages and disadvantages can be found (see Table 1), it is hard to say which technique is best. One has rather to ﬁnd the technique which most eﬃciently ﬁlls the (x,y,λ) data cube for each speciﬁc application.
3D Instrumentation by Allington-Smith J.