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Subsections



E..4 TIMING Stage

This stage is run for each observation to perform timing analyses, as shown in Figure 8.

BEWARE: none of AE's timing analysis (light curves, median energy time series, variability measures) currently takes the background into account! This can produce misleading results in some cases, e.g. a spurious indication of variability between two ObsIds that have very different backgrounds.

E..4.1 Actions

E..4.2 Usage and Inputs

acis_extract, srclist_filename, obsname, /TIMING, ENERGY_RANGE=[energy,energy], SNR_RANGE=[value,value], NUM_GROUPS_RANGE=[value,value]


EXAMPLE:
idl $\vert\&$ tee timing_1875.log


acis_extract, 'all.srclist', '1875', /TIMING, ENERGY_RANGE=[0.5,8], SNR_RANGE=[2,20], NUM_GROUPS_RANGE=[2,100]

E..4.3 Data Products

For each source the following files are produced:
{sourcename}/{obsname}/source.lc:
a FITS table containing the grouped light curve, grouped median energy time-series, exposure time series, and adaptively smoothed light curve. The exposure values in this table attempt to account for both the integration time within each time bin (obtained from the GTI tables) and the ARF value (effective area and PSF fraction) associated with this ObsId. This facilitates testing for variability across ObsIds in the MERGE stage.

{sourcename}/{obsname}/source.evt.ps:
a PostScript file containing a scatter plot of event arrival times and energies, and a plot of the observed and uniform cumulative distribution functions used to compute KS probability.

To accommodate multiple observations, the binned and smoothed light curves are plotted in the MERGE_OBSERVATIONS stage.


next up previous contents pdf.png
Next: E..5 EXTRACT_BACKGROUNDS Stage Up: E. Obsolete Stages Previous: E..3 EXTRACT_SPECTRA Stage
Patrick Broos
Penn State Department of Astronomy
2013-05-09