2002 Chandra Calibration Workshop

GX 5-1

This example concerns the HETGS observation (obsid_716) of GX 5-1 by Alan Levine in July 2000.

The first figure shows the result of flux-correcting using the standard technique. In this figure the dashed black line indicates the best guess of the correct flux based upon the use of the pileup model.

Figure showing result of standard technique

Here is the result of the pileup model:

Figure showing result of the pileup
model

As can be seen from the figure, the agreement between HEG+1, HEG-1, and MEG+1 orders is good for wavelengths longer than about 3.5 angstroms. Note how the MEG-1 agrees with the MEG+1 for wavelengths less than 2.9 angstroms, which is where the MEG-1 dispersion arm changes from the S2 (frontside) to the S3 (backside chip).

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This page was last updated Dec 16, 2002 by John E. Davis. To comment on it or the material presented here, send email to davis (at) space.mit.edu.