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23.2 STIS-Specific Reduction and Analysis Tasks
In Chapter 21 we discussed the components of the STIS pipeline that can be run as individual tasks. Observers may find that they wish to perform parts of the pipeline reduction again on their data using these tasks. Typical examples will be to re-perform cosmic ray rejection, altering the input parameters or using data from separate datasets, or to perform one-dimensional spectral extraction on long-slit data or to modify the input parameters (e.g., aperture extraction box, or background region) when doing one-dimensional spectral extraction for echelle data. For completeness we list the tasks again below. To run these tasks you need to retrieve the calibration reference files they require from the Archive and set the oref parameter appropriately (see "Mechanics of Full Recalibration" on page 21-31). An example of using x1d with a user specified extraction box (11 pixels high) and a user specified center (line=500) is given below:
cl> x1d o3s41301o_flt.fits 3s41301o_x1d.fits center=500 \
>>> size=11
Table 23.2 lists some of the stand-alone tasks for working with STIS data. Consult the on-line help for more information about all these tasks. We expect additional options to become available within the stand-alone (i.e., outside the pipeline) versions of these tasks as we increase the number of parameters which can be changed through epar and as we add new functions, such as background subtraction correction for echelle modes and optimal extraction for echelle and first order spectra to x1d. Stay tuned to the STANs and WWW.
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Last updated: 11/13/97 17:47:14