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spacetelescope · Feb 5, 2025 · c1f751d · c1f751d
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diff --git a/docs/jwst/dark_current/description.rst b/docs/jwst/dark_current/description.rst
@@ -49,8 +49,6 @@ subtracted from the corresponding first few integrations of the science exposure
 The data in the last integration of the dark reference file is applied to all
 remaining science integrations.
 
-The ERR arrays of the science data are currently not modified by this step.
-
 The DQ flags from the dark reference file are propagated into the science
 exposure PIXELDQ array using a bitwise OR operation.
 

diff --git a/docs/jwst/linearity/description.rst b/docs/jwst/linearity/description.rst
@@ -63,8 +63,6 @@ Special Handling
    applied to that group. Any groups for that pixel that are not flagged as
    saturated will be corrected.
 
-The ERR array of the input science exposure is not modified.
-
 The flags from the linearity reference file DQ array are propagated into the
 PIXELDQ array of the science exposure using a bitwise OR operation.
 

diff --git a/docs/jwst/pipeline/calwebb_detector1.rst b/docs/jwst/pipeline/calwebb_detector1.rst
@@ -127,7 +127,7 @@ input will be in the form of a `~jwst.datamodels.Level1bModel`, which only
 contains the 4D array of detector pixel values, along with some optional
 extensions. When such a file is loaded into the pipeline, it is immediately
 converted into a `~jwst.datamodels.RampModel`, and has all additional data arrays
-for errors and Data Quality flags created and initialized to zero.
+for Data Quality flags created and initialized to zero.
 
 The input can also contain a 3D cube of NIRCam "Frame 0" data, where
 each image plane in the 3D cube is the initial frame for each integration in