diff --git a/notebooks/ACS/acs_saturation_trails/acs_saturation_trails.ipynb b/notebooks/ACS/acs_saturation_trails/acs_saturation_trails.ipynb
index dbed8b8f9..731f036fa 100644
--- a/notebooks/ACS/acs_saturation_trails/acs_saturation_trails.ipynb
+++ b/notebooks/ACS/acs_saturation_trails/acs_saturation_trails.ipynb
@@ -29,9 +29,10 @@
     "\n",
     "However, accurate relative photometry can be obtained as long as a large enough aperture is selected to contain the spilled flux ([ACS ISR 2004-01](http://www.stsci.edu/files/live/sites/www/files/home/hst/instrumentation/acs/documentation/instrument-science-reports-isrs/_documents/isr0401.pdf)). While one could simply use a larger circular aperture, that may introduce error when working with a crowded field (where bright stars are often located).\n",
     "\n",
-    "Here we present a method to identify and perform photometry on saturated sources by defining a custom aperture that is a combination of a standard 0.5\" arcsecond circular aperture and the pixels affected by saturation trails. This method has been tested on ACS/WFC observations of 47 Tuc in the F660W band. The plot below shows the results of using this alternative method to recover flux.\n",
+    "Here we present a method to identify and perform photometry on saturated sources by defining a custom aperture that is a combination of a standard 0.5\" arcsecond circular aperture and the pixels affected by saturation trails. This method has been tested on ACS/WFC observations of 47 Tuc in the F606W band. The plot below shows the results of using this alternative method to recover flux.\n",
+    "\n",
+    "<img src=photometry_recovery.png width =\"900\" title=\"\" alt=\"\">\n",
     "\n",
-    "![title](photometry_plot.png)\n",
     "\n",
     "### This tutorial will show you how to...\n",
     "\n",
@@ -1193,7 +1194,7 @@
    "name": "python",
    "nbconvert_exporter": "python",
    "pygments_lexer": "ipython3",
-   "version": "3.9.13"
+   "version": "3.8.12"
   }
  },
  "nbformat": 4,
diff --git a/notebooks/ACS/acs_saturation_trails/p_module/plot.py b/notebooks/ACS/acs_saturation_trails/p_module/plot.py
index c50038091..962395944 100644
--- a/notebooks/ACS/acs_saturation_trails/p_module/plot.py
+++ b/notebooks/ACS/acs_saturation_trails/p_module/plot.py
@@ -3,6 +3,7 @@
 from astropy.visualization import (ZScaleInterval, LinearStretch,
                                    ImageNormalize)
 
+
 def ds9_imitate(ax, image, extent=None):
     norm = ImageNormalize(image,
                           interval=ZScaleInterval(),
@@ -15,8 +16,8 @@ def triple_pam_plot(flt_file, pam_file, figtitle):
     fl_img = fits.getdata(flt_file, ext=1)
     pam_img = fits.getdata(pam_file)
 
-    fig = plt.figure(figsize=(20,4))
-    fig.suptitle(figtitle,fontsize=20)
+    fig = plt.figure(figsize=(20, 4))
+    fig.suptitle(figtitle, fontsize=20)
 
     ax = fig.add_subplot(1, 3, 1)
     ds9_imitate(ax, fl_img)
@@ -36,13 +37,12 @@ def triple_pam_plot(flt_file, pam_file, figtitle):
 
 
 def calib_compare_plot(raw_image, cal_image):
-    fig = plt.figure(figsize=(14,14))
+    fig = plt.figure(figsize=(14, 14))
 
-    ax = fig.add_subplot(2,1,1)
+    ax = fig.add_subplot(2, 1, 1)
     ds9_imitate(ax, raw_image)
     ax.set_title('Raw')
 
-    ax2 = fig.add_subplot(2,1,2)
+    ax2 = fig.add_subplot(2, 1, 2)
     ds9_imitate(ax2, cal_image)
     ax2.set_title('Flat-Fielded')
-
diff --git a/notebooks/ACS/acs_saturation_trails/photometry_recovery.png b/notebooks/ACS/acs_saturation_trails/photometry_recovery.png
new file mode 100644
index 000000000..26b92ef79
Binary files /dev/null and b/notebooks/ACS/acs_saturation_trails/photometry_recovery.png differ