diff --git a/Lab_5/Lab_5.ipynb b/Lab_5/Lab_5.ipynb
index de4bfeb..246124b 100644
--- a/Lab_5/Lab_5.ipynb
+++ b/Lab_5/Lab_5.ipynb
@@ -4,14 +4,14 @@
    "cell_type": "markdown",
    "metadata": {},
    "source": [
-    "# <p style=\"text-align: center;\">PHYS 134L Spring 2022 Lab 5</p>"
+    "# <p style=\"text-align: center;\">PHYS 134L Spring 2024 Lab 5</p>"
    ]
   },
   {
    "cell_type": "markdown",
    "metadata": {},
    "source": [
-    "<div class=\"alert alert-block alert-danger\"><b>Due date:</b> Sunday, May 8th, 2022 by 11:59pm, submitted through Gradescope.</div>"
+    "<div class=\"alert alert-block alert-danger\"><b>Due date:</b> Sunday, May 12th, 2024 by 11:59pm, submitted through Gradescope.</div>"
    ]
   },
   {
@@ -47,7 +47,7 @@
    "cell_type": "markdown",
    "metadata": {},
    "source": [
-    "The first part of this lab will be an introduction to spectra.  Astronomical data comes in two basic forms: images and spectra.  You have already seen images.  Spectra are a bit different: we lose at least some of our ability to resolve an object and see its shape, but we spread out its light into its colors, or wavelengths.  The intro slides to this lab included a spectrum as it appears on a detector.  It is a colored spectrum of the Sun, showing many black parts where there is less light.  These are absorption lines and give a whole lot of information about the physics of the Sun. \n",
+    "The first part of this lab will be an introduction to spectra.  Astronomical data typically comes in two basic forms: images and spectra.  You have already seen images.  Spectra are a bit different: we lose at least some of our ability to resolve an object and see its shape, but we spread out its light into its wavelengths.  The intro slides to this lab included a spectrum as it appears on a detector.  It is a colored spectrum of the Sun, showing many black parts where there is less light.  These are absorption lines and give a whole lot of information about the physics of the Sun. \n",
     "\n",
     "Just like Source Extractor takes the images and extracts the positions and brightnesses of stars, we can extract the flux of a star as a function of wavelength.  "
    ]
@@ -343,7 +343,7 @@
    "cell_type": "markdown",
    "metadata": {},
    "source": [
-    "Now you can image that only using images of a star in two filters, we can learn a lot about its fundamental properties! "
+    "Now you can imagine that only using images of a star in two filters, we can learn a lot about its fundamental properties! "
    ]
   },
   {
diff --git a/Lab_6/Lab_6.ipynb b/Lab_6/Lab_6.ipynb
index a1ac3d8..f46a81d 100644
--- a/Lab_6/Lab_6.ipynb
+++ b/Lab_6/Lab_6.ipynb
@@ -51,7 +51,7 @@
    "source": [
     "For a quick introduction to (or refresher on) many of the basic notions, see [here](http://www.tim-thompson.com/hr.html). \n",
     "\n",
-    "For a more quantitative picture of stellar evolution, consider the files ```evol_M0.8.dat```, ```evol_M1.0.dat```, ```evol_M1.3.dat```,```evol_M1.8.dat```, and ```evol_M2.6.dat. These contain evolutionary tracks for stars with compositions similar to the Sun's and with masses of 0.8, 1.0, 1.3, 1.8, and 2.5 times the mass of the\n",
+    "For a more quantitative picture of stellar evolution, consider the files ```evol_M0.8.dat```, ```evol_M1.0.dat```, ```evol_M1.3.dat```,```evol_M1.8.dat```, and ```evol_M2.6.dat```. These contain evolutionary tracks for stars with compositions similar to the Sun's and with masses of 0.8, 1.0, 1.3, 1.8, and 2.5 times the mass of the\n",
     "Sun. The columns of the tables contain $\\log_{10}(Temperature~(K))$, $\\log_{10}(Luminosity~(solar~units)$), and Age (in Gyr). Notice (by opening one of the files in a text editor) that the range of ages in the various tables is fairly wide -- massive stars live for much shorter times than low-mass ones, though they are much more luminous.  They burn brightly but burn out quickly."
    ]
   },