Data Preparation
When Chandra data goes through Standard Data Processing (SDP), the most recently available calibration is applied to it. Since this calibration is continuously being improved, one should check whether there are newer files available. Similarly, some science decisions are made during SDP; every user has the option to reprocess the data with different parameters.
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See the current
Calibration Status Report
Analysis Guides:
General:
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Setting the Observation-specific Bad Pixel Files
Uses: the acis_set_ardlib script - Filtering Data (S-Lang or Python)
- Filtering Lightcurves (S-Lang or Python)
Uses: the lightcurves.sl S-Lang script; the lightcurves.py script
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Setting the Observation-specific Bad Pixel Files
Coordinates, Astrometry, & Spatial Filtering:
ACIS:
- Check the ACIS Data Caveats
- Why topic: -110 C Observations
- Why topic: Continuous Clocking Mode Data
Removing Cosmic-Ray Afterglows:
acis_process_events:
- Reprocessing Data to Create a New Level=2 Event File thread: apply the newest calibration (CTI, TGAIN); includes CC mode times of arrival calculation.
- Clean ACIS Background in VFAINT Mode
- The ACIS "Blank-Sky" Background Files (S-Lang or Python)
Uses: the acis_bkgrnd_lookup script; the lightcurves.sl S-Lang script; the lightcurves.py script - Remove the ACIS Readout Streak
HRC:
- New Observation-Specific HRC Bad Pixel File
- Reprocessing Data to Create a New Level=2 Event File thread: applies the newest calibration (degap, AMP_SF/tapringing).
- Computing Average HRC Dead Time Corrections (S-Lang or Python)
![[New]](../imgs/new.gif)
(19 Jan 2010)
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