Add IFU+datacubes docs page.

docs/index.rst

@@ -61,6 +61,7 @@ Contents
    jwst_measured_opds.ipynb
    jwst_detector_effects.ipynb
    jwst_matching_psfs_to_data.ipynb
+   jwst_ifu_datacubes.ipynb
    jwst_large_psf.ipynb
    jwst_optical_budgets.ipynb
    jwst_psf_subtraction.ipynb

docs/jwst_matching_psfs_to_data.ipynb

@@ -27,7 +27,9 @@
    "id": "42ce87d3",
    "metadata": {},
    "source": [
-    "Often one wants to generate PSFs matched to some particular science dataset or file. The convenience function `webbpsf.setup_sim_to_match_data` helps with this, using the file's FITS header to set up a simulated instrument matched to the appropriate instrument setup and date of observation.  "
+    "Often one wants to generate PSFs matched to some particular science dataset or file. The convenience function `webbpsf.setup_sim_to_match_file` helps with this, using the file's FITS header to set up a simulated instrument matched to the appropriate instrument setup and date of observation. \n",
+    "\n",
+    "Let's call that function, providing a filename of a data file already downloaded in the current directory:"
    ]
   },
   {
@@ -91,6 +93,7 @@
    "metadata": {},
    "source": [
     "This function will:\n",
+    "\n",
     " * Create a webbpsf instrument object for the relevant instrument\n",
     " * Configure it to have the correct filter, detector, and other relevant instrument parameters for that science data file (e.g. coronagraph masks and so on). \n",
     " * Load the measured telescope mirror alignment data from the closest-in-time wavefront sensing visit to that science data. "
@@ -160,6 +163,7 @@
    "metadata": {},
    "source": [
     "The difference between the oversampled and detector-sampled output products is readily apparent. The distortion effects are generally more subtle: \n",
+    "\n",
     " * In this example case, note the slightly blurred softer look of the DET_DIST output compared to DET_SAMP, or of OVERDIST compared to OVERSAMP. This aspect of the simulation is a model for charge transfer physics and inter-pixel capacitance within the detector which result in crosstalk between adjacent pixels.\n",
     " * Also included as part of the distortion is a model for optical geometric distortions (including for instance slight differences between X and Y pixel scales, small rotations and skews of the detector pixel axes, the very-slightly-different position angles for each NIRCam detector, etc.). This attempts to forward-model the distortions which the \"drizzle\" pipeline algorithm corrects for, using the same astrometric calibration information for the instruments recorded in the [science instrument aperture file](https://pysiaf.readthedocs.io/en/latest/). \n",
     "\n",
@@ -488,7 +492,7 @@
    "name": "python",
    "nbconvert_exporter": "python",
    "pygments_lexer": "ipython3",
-   "version": "3.11.7"
+   "version": "3.12.5"
   }
  },
  "nbformat": 4,