iris_pipeline Documentation¶
The IRIS Data Reduction System is based on the stpipe
package released by Space Telescope
for the James Webb Space Telescope.
With stpipe
we can configure each step of a pipeline through one or more text based .INI style files,
then we provide one input FITS file or a set of multiple inputs defined in JSON (named Associations).
Custom analysis steps and pipelines for IRIS are defined as classes in the current repository iris_pipeline
Then execute the pipeline from the command line using the tmtrun
executable or using
directly the Python library.
The pipeline also dynamically interfaces to the CRDS
the Calibration References Data System,
to retrieve the best calibration datasets given the metadata in the headers of the input FITS files.
The CRDS
client can also load data from a local cache, so for now we do not have a actual
CRDS
server and we only rely on a local cache.
The CRDS
is not under our control, the Thirty Meter Telescope will deliver a database system
to replace the CRDS
and we can adapt our code to that in the future.
Getting Started¶
Example run¶
Design¶
Calibration¶
Reference/API¶
iris_pipeline Package¶
Classes¶
|
BackgroundStep: Subtract background exposures from target exposures. |
|
Initialize the Data Quality extension from the mask reference file. |
|
Flat-field a science image using a flatfield reference image. |
|
Image2Pipeline: Processes JWST imaging-mode slope data from Level-2a to Level-2b. |
|
DarkCurrentStep: Performs dark current correction by subtracting dark current reference data from the input science data model. |
|
PreprocessFlatfield: Remove dark and normalize exposure to create a flat field to be later added to the CRDS. |
|
SubtractImagesStep: Subtract two exposures from one another to accomplish background subtraction. |