Pipeline Stages¶
End-to-end calibration of Roman data is divided into levels of processing:
The exposure level processing consists of detector-level corrections that are performed on a group-by-group basis, followed by ramp fitting. The output of the exposure level processing is a count rate image per exposure, or per integration for some modes that is aligned to the Gaia reference system. Details of this pipeline can be found at:
Exposure level processing consists of additional instrument-level and observing-mode corrections and calibrations to produce fully calibrated exposures. The details differ for imaging and spectroscopic exposures, and there are some corrections that are unique to certain instruments or modes. Details are at: Exposure Level Processing
The High Level level processing uses overlapping exposures to match the sky background, detect aberrant data values and resample the image to produce a single undistorted product. Details are at: High Level Image Processing
The table below represents the same information as described above, but alphabetically ordered by pipeline class.
Pipeline Class |
Alias |
Used For |
|---|---|---|
roman_elp |
Exposure Level: |
|
roman_hlp |
High Level: |
Pipelines and Exposure Type¶
The data from different observing modes needs to be processed with the proper pipeline levels listed above. The proper pipeline selection is usually based solely on the exposure type (exposure.type attribute).