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Purpose: To create light curves binned on 30-s intervals for the seven bands. The output is used in conjunction with the output of the program AO in the program RATE_FIT to fit the scattered solar X-ray and long-term enhancement background contamination. The capability now exists to mask out the contributions of bright point sources or extended sources to the light curves. This can become important when, for instance, a strong flaring source affects the modelling process. In practice this has not been much of a problem, but the possibility should be kept in mind. The most noticeable affect comes when a bright source is found near the window support structure or the edge of the field and is wobbled in and out of the open area. In this case, there will be strong variations in the light curve with the wobble period. The light-curve described below is in general not sensitive to that frequency of variation so the fitted parameters remain reasonable while the reduced value can be very large (e.g., 5-10). Note that if a mask is used in RATE, the same mask must be used in CAST_SSX.
1) Observation data set fits files - xxx_EVENTRATES.FITS and
xxx_EVENTS.FITS for German and US data or xxx_ANC.FITS and
xxx_BAS.FITS for RDF data
2) Other fixed input - valid_times_all.dat 3) Mask - if desired, same format as the output of DETECT.
1) Observation control - the eight or fewer character string listed above as xxx.
2) Data format control - 1 for German data, 2 for US data, 3 for RDF data.
3) Gain control - 1 for high gain, 2 for low gain, 3 for low gain pulse-height range, high gain area (the latter is for processing high-gain data and using the R1L band). The gain was reduced on 11 October 1991 (S/C clock 42910000).
4) Mask control - 1 for masking, 0 for no masking. If masking is chosen, the program will next query for the mask name.
4a) Mask name - name of fits file containing mask.
1&2) RATE1.DAT, RATE2.DAT - files containing light-curve count rates, count-rate uncertainties, and particle background count rates.