Edits in response to review

Author: jeffcarlin

DP1/300_Science_Demos/305_Galactic_variables_and_transients/305_2_Stellar_Variability_Characterization.ipynb

@@ -19,7 +19,7 @@
     "Data Release: <a href=\"https://dp1.lsst.io/\">Data Preview 1</a> <br>\n",
     "Container Size: large <br>\n",
     "LSST Science Pipelines version: Release r29.2.0 <br>\n",
-    "Last verified to run: 2026-01-22 <br>\n",
+    "Last verified to run: 2026-01-29 <br>\n",
     "Repository: <a href=\"https://github.com/lsst/tutorial-notebooks\">github.com/lsst/tutorial-notebooks</a> <br>"
    ]
   },
@@ -170,7 +170,7 @@
     "\n",
     "### 2.1. Get a sample of DiaObjects\n",
     "\n",
-    "To identify candidates such as the periodic variable star from the first notebook in the 305-series, we wish to select stars that are varying in brightness significantly (by using, e.g., `[f]_psfFluxSigma`, or some combination of the flux value percentiles from `[f]_psfFluxPercentile05, 25, 50, 75, 95`). We will also use `r_psfFluxStetsonJ`, which reports the Stetson J-index, an indicator of periodic variability.\n",
+    "To identify candidates such as the periodic variable star from the first notebook in the 305-series, we wish to select stars that are varying in brightness significantly. We will do so by using `[f]_psfFluxSigma` and the inter-quartile range (IQR) of the fluxes derived from the percentiles `[f]_psfFluxPercentile25` and `[f]_psfFluxPercentile75`. We will also use `r_psfFluxStetsonJ`, which reports the Stetson J-index, an indicator of periodic variability.\n",
     "\n",
     "For this tutorial, we will focus on the *r*-band measurements. Note that the statistics selected below are all based on the difference-image point source flux values, except for `r_scienceFlux*`, which are based on the calibrated `visit_image`.\n",
     "\n",
@@ -340,7 +340,7 @@
     "In addition to the `nDiaSources` > 40 and S/N > 5 cuts applied in the TAP query above, filter the `DiaObject` results (defined as `DiaObjsFull`) with the following conditions:\n",
     "\n",
     "* `nDiaSources` > 40: Candidate has more than 40 `DiaSource` detections (in all bands); applied in TAP query.\n",
-    "* `r_scienceFluxMean` S/N > 5: Candidate has signal-to-noise larger than 5 in the `visit_image`s.\n",
+    "* `r_scienceFluxMean` S/N > 5: Candidate has signal-to-noise larger than 5 in the `visit_image`s; applied in TAP query.\n",
     "* `r_psfFluxSigma` > 0.02: Candidate has flux variations with sigma larger than 2 percent.\n",
     "* `r_psfFluxIQRFrac` > 0.05: Candidate has IQR flux variations with larger than 5 percent.\n",
     "* `r_psfFluxStetsonJ` > 10: Candidate has Stetson J index larger than 10.\n",
@@ -524,8 +524,6 @@
     "\n",
     "The lightcurves above show that these objects clearly vary in brightness, but it is unclear whether there is a pattern (for example a periodic signal) in that variability.\n",
     "\n",
-    "Describe how we measure the period via Lomb-Scargle, and how the LC is phased.\n",
-    "\n",
     "Loop over the candidates, extracting the frequency of the highest peak in the Lomb-Scargle results, and placing each measurement into the correct phase of the star's variability period."
    ]
   },
@@ -773,6 +771,14 @@
    "source": [
     "tab"
    ]
+  },
+  {
+   "cell_type": "code",
+   "execution_count": null,
+   "id": "17b494c9-9a90-49f3-a57d-2673378d53ce",
+   "metadata": {},
+   "outputs": [],
+   "source": []
   }
  ],
  "metadata": {