text changes to notebook

notebooks/niriss_imaging/niriss-imaging-tutorial.ipynb

@@ -45,11 +45,11 @@
    "id": "9c5b415a-f0f4-4c48-a038-d319e825ee4f",
    "metadata": {},
    "source": [
-    "Make sure the [latest version of the pipeline is installed](https://jwst-pipeline.readthedocs.io/en/stable/index.html) and that the [Calibration Reference Data System (CRDS)](https://jwst-crds.stsci.edu/static/users_guide/index.html) is configured so the most up-to-date calibration files are used to process the dataset. This notebook was created with pipeline version `1.12.3`. \n",
-    "\n",
-    "This notebook uses the [`jdaviz` package](https://jdaviz.readthedocs.io/en/latest/index.html) to visualize the datasets. To [install `jdaviz`](https://jdaviz.readthedocs.io/en/latest/installation.html) in your current environment:\n",
+    "To make sure that the pipeline version is compatabile with the steps discussed below and the required dependencies and packages are installed, you can create a fresh conda environment and install the provided `requirements.txt` file:\n",
     "```\n",
-    "pip install jdaviz --upgrade\n",
+    "conda create -n niriss_imaging_pipeline python=3.11\n",
+    "conda activate niriss_imaging_pipeline\n",
+    "pip install -r requirements.txt\n",
     "```\n",
     "\n",
     "### Imports"
@@ -540,7 +540,7 @@
     "By default, the `Image3` stage of the pipeline performs the following steps on NIRISS data: \n",
     "- [tweakreg](https://jwst-pipeline.readthedocs.io/en/latest/jwst/tweakreg/index.html#tweakreg-step) - creates source catalogs of pointlike sources for each input image. The source catalog for each input image is compared to each other to derive coordinate transforms to align the images relative to each other.\n",
     "   - As of CRDS context `jwst_1156.pmap` and later, the `pars-tweakreg` parameter reference file for NIRISS performs an absolute astrometric correction to GAIA data release 3 by default (i.e., the `abs_refcat` parameter is set to `GAIADR3`). Though this default correction generally improves results compared with not doing this alignment, it can sometimes result in poor performance in crowded or sparse fields, so users are encouraged to check astrometric accuracy and revisit this step if necessary.\n",
-    "   - As of pipeline version 1.12.5, the default source finding algorithm is `DAOStarFind` which can result in up to 0.5 pix uncertainties in the centroids for undersampled PSFs, like the NIRISS PSFs at short wavelengths [(Goudfrooij 2022)](https://www.stsci.edu/files/live/sites/www/files/home/jwst/documentation/technical-documents/_documents/JWST-STScI-008116.pdf). There are plans to update the default algorithm to `IRAFStarFind` in future pipeline versions.\n",
+    "   - As of pipeline version 1.12.5, the default source finding algorithm is `DAOStarFinder` which can result in up to 0.5 pix uncertainties in the centroids for undersampled PSFs, like the NIRISS PSFs at short wavelengths [(Goudfrooij 2022)](https://www.stsci.edu/files/live/sites/www/files/home/jwst/documentation/technical-documents/_documents/JWST-STScI-008116.pdf). There are plans to update the default algorithm to `IRAFStarFinder` in future pipeline versions.\n",
     "- [skymatch](https://jwst-pipeline.readthedocs.io/en/latest/jwst/skymatch/index.html#skymatch-step) - measures the background level from the sky to use as input into the subsequent `outlier detection` and `resample` steps.\n",
     "- [outlier detection](https://jwst-pipeline.readthedocs.io/en/latest/jwst/outlier_detection/index.html#outlier-detection-step) - flags any remaining cosmic rays, bad pixels, or other artifacts not already flagged during the `DETECTOR1` stage of the pipeline, using all input images to create a median image so that outliers in individual images can be identified.\n",
     "- [resample](https://jwst-pipeline.readthedocs.io/en/latest/jwst/resample/index.html#resample-step) - resamples each input image based on its WCS and distortion information and creates a single undistorted image.\n",
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+}