update notebooks to lcviz 0.2.0 (#4)

kecnry · Mar 7, 2024 · 4510ba7 · 4510ba7
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diff --git a/mult_ephem_RR-Lyr.ipynb b/mult_ephem_RR-Lyr.ipynb
@@ -9,8 +9,8 @@
     "\n",
     "[RR Lyrae](https://en.wikipedia.org/wiki/RR_Lyrae) is the prototype of a class of variable stars with radial pulsations. The pulsation period is related to the stellar luminosity, and a second, lower frequency variation can be seen on longer timescales, known as the [Blazkho effect](https://en.wikipedia.org/wiki/Blazhko_effect). \n",
     "\n",
-    "* **Last Updated**: Dec 6, 2023\n",
-    "* **lcviz version**: unreleased (Dec 6, 2023)\n",
+    "* **Last Updated**: March 7, 2024\n",
+    "* **lcviz version**: 0.2.0\n",
     "\n",
     "RR Lyrae itself was in the Kepler field, so let's load one Kepler Quarter of long-cadence observations, and inspect the periods:"
    ]
@@ -158,6 +158,14 @@
     "    plot_options.marker_colormap = 'Viridis'\n",
     "    plot_options._obj.marker_color_col_value = 'phase:blazkho'"
    ]
+  },
+  {
+   "cell_type": "code",
+   "execution_count": null,
+   "id": "538d7a6b-9b31-41e8-9d59-f2a0f9fc34f8",
+   "metadata": {},
+   "outputs": [],
+   "source": []
   }
  ],
  "metadata": {
@@ -176,7 +184,7 @@
    "name": "python",
    "nbconvert_exporter": "python",
    "pygments_lexer": "ipython3",
-   "version": "3.11.4"
+   "version": "3.11.3"
   }
  },
  "nbformat": 4,

diff --git a/mult_ephem_kic_2835289.ipynb b/mult_ephem_kic_2835289.ipynb
@@ -9,8 +9,8 @@
     "\n",
     "This notebook loads the Kepler light curve for a eclipsing triple system (KIC 2835289) containing a binary with ellipsoidal variations and a third star on an eccentric orbit.  We use lcviz to flatten the light curve, and phase-fold on both orbital periods.\n",
     "\n",
-    "* **Last Updated**: Dec 6, 2023\n",
-    "* **lcviz version**: unreleased (Dec 6, 2023)"
+    "* **Last Updated**: March 7, 2024\n",
+    "* **lcviz version**: 0.2.0"
    ]
   },
   {

diff --git a/short_cadence_phase_curve_HAT-P-7.ipynb b/short_cadence_phase_curve_HAT-P-7.ipynb
@@ -9,8 +9,8 @@
     "\n",
     "HAT-P-7 b ([Pál et al. 2008](https://ui.adsabs.harvard.edu/abs/2008ApJ...680.1450P/abstract)) is a hot Jupiter orbiting a bright F6V host in the Kepler field. Let's take a look at short cadence (one-minute) Kepler observations from the first three Kepler quarters to see the secondary eclipse of the planet, when the planet's flux disappears as the planet is eclipsed by the host star.\n",
     "\n",
-    "* **Last Updated**: Dec 11, 2023\n",
-    "* **lcviz version**: unreleased (Dec 11, 2023)\n",
+    "* **Last Updated**: March 7, 2024\n",
+    "* **lcviz version**: 0.2.0\n",
     "\n",
     "First we download the observations with `lightkurve`:"
    ]
@@ -162,11 +162,11 @@
     "\n",
     "plot_options = lcviz.plugins['Plot Options']\n",
     "plot_options.viewer = 'flux-vs-phase:default'\n",
-    "plot_options.layer = 'HAT-P-7[pdcsap_flux]'\n",
+    "plot_options.layer = 'HAT-P-7'\n",
     "plot_options.marker_opacity = 0.1\n",
     "plot_options.marker_size = 1\n",
     "\n",
-    "plot_options.layer = 'binned HAT-P-7[pdcsap_flux]:default'\n",
+    "plot_options.layer = 'binned HAT-P-7:default'\n",
     "plot_options.marker_size = 50\n",
     "plot_options.marker_color = 'r'"
    ]
@@ -196,7 +196,7 @@
    "name": "python",
    "nbconvert_exporter": "python",
    "pygments_lexer": "ipython3",
-   "version": "3.11.4"
+   "version": "3.11.3"
   }
  },
  "nbformat": 4,