diff --git a/assets/profiles_demo.png b/assets/profiles_demo.png
new file mode 100644
index 0000000..0c78409
Binary files /dev/null and b/assets/profiles_demo.png differ
diff --git a/beorn.typ b/beorn.typ
index 755372b..a878b48 100644
--- a/beorn.typ
+++ b/beorn.typ
@@ -1,9 +1,6 @@
 #import "globals.typ": *
 
-= #beorn
-
-
-== Procedure
+== The "painting" procedure
 
 #let notebook = json("../workdir/11_visualization/simplified_visualization_of_procedure.ipynb")
 
@@ -74,8 +71,7 @@
     image_cell(notebook, cell_id: "step_profile_3d_overlap"),
   ),
   [],
-  // [],
-  // [],
+
 
   [#h(3em) Multiple contributions $==>$],
   [
@@ -83,18 +79,17 @@
 
     (overlaps, normalization, ...)
   ],
-  // [],
-  // [],
 
   image_cell(notebook, cell_id: "step_profile_3d_second"),
   [],
-  // [],
-  // [],
 )
+
 #pagebreak()
 
 == Postprocessing
+
 - ionization overlaps
+
 - corrections due to RSD
 - computation of derived quantities
 - summary statistics
diff --git a/halo_model.typ b/halo_model.typ
index aa45c81..c469fd0 100644
--- a/halo_model.typ
+++ b/halo_model.typ
@@ -1,7 +1,6 @@
 #import "globals.typ": *
 
 
-
 == The halo model of reionization
 Following @Schneider_2021 @schneider2023cosmologicalforecast21cmpower, the halo model describes (#link(<backup_full_profiles>, "derivation")):
 #line(length: 100%, stroke: color.white.transparentize(100%))
@@ -32,7 +31,8 @@ $
 #pagebreak()
 Visually:
 
-#image("assets/profiles.png")
+#image("assets/profiles_demo.png", height: 70%)
+(from @Schaeffer_2023)
 // COMMENTS:
 // - contribution from the lyman lines
 // - 1/r^2 decrease from spreading photons
@@ -55,9 +55,9 @@ $ <eq:dTb>
 #pinit-point-from((1, 2))[from $x_"HII"$]
 #pause
 
-#pinit-point-from((3, 4))[From $rho_alpha$]
+#pinit-point-from((3, 4))[from $rho_alpha$]
 #pause
 
-#pinit-point-from((5, 6))[From $rho_"h"$]
+#pinit-point-from((5, 6))[from $rho_"h"$]
 
 #pagebreak()
diff --git a/implementation.typ b/implementation.typ
index bcfe96b..fff3448 100644
--- a/implementation.typ
+++ b/implementation.typ
@@ -20,13 +20,8 @@
 // usage of HDF5
 // solid caching mechanisms -> resume simulations, etc...
 
-// #v(5em)
-// #text(
-//   size: .7em,
-// )[
-//   (#link(<backup_validation>, "Validated"))
-// ]
-
+#pause
+$->$ #link(<backup_validation>, "Validated") ✅
 
 == Simplified usage
 
@@ -44,12 +39,10 @@
       code_cell(notebook, cell_id: "code_for_run"),
     )
   ]
+// sadly didn't work:
 // #pinit-point-to(1)[Hello]
 // #pinit-point-to(2)[Hello]
 // #pinit-point-to(3)[Hello]
 // #pinit-point-to(4)[Hello]
 // #pinit-point-to(5)[Hello]
-
 ]
-
-
diff --git a/introduction.typ b/introduction.typ
index b5251ff..9539f2e 100644
--- a/introduction.typ
+++ b/introduction.typ
@@ -19,7 +19,7 @@
 == The 21-cm signal
 
 
-The brigthtness temperature describes the difference between the CMB temperature and the spin temperature of neutral hydrogen
+The _brigthtness temperature_ describes the intensity of the 21-cm line
 
 #v(1em)
 
@@ -28,11 +28,11 @@ The brigthtness temperature describes the difference between the CMB temperature
 ][
   #pause
   #set text(size: 0.8em)
-  remove contribution from the BB spectrum:
+  remove contribution from the BB spectrum
 
   _differential brightness temperature_
 
-  $==>$ the actual 21-cm signal
+  $==>$ the actual reionization signal
 
   #image("assets/brighness_temperature.png", fit: "contain")
   from @Schaeffer_2023
@@ -41,19 +41,13 @@ The brigthtness temperature describes the difference between the CMB temperature
 #pagebreak()
 
 
+== Expression the 21-cm signal @Pritchard2012 @Furlanetto_2006
 
 #align(center)[
-  #image("assets/evolution_of_dtb.png", height: 85%, fit: "contain")
-  #text(size: 0.8em)[from @Pritchard2012]
+  #image("assets/evolution_of_dtb.png", height: 70%, fit: "contain")
+  // #text(size: 0.8em)[from @Pritchard2012]
 ]
-
-// COMMENTS:
-
-
-
-== Expression the 21-cm signal
-Expressing the _differential brightness temperature_ (e.g @Pritchard2012):
-
+#pause
 $
   d T_"b" (bold(x), z) tilde.eq T_0 (z) dot
   #pin(1) x_"HI" (bold(x), z) #pin(2) dot
@@ -62,8 +56,6 @@ $
   ((1 - T_"CMB" (z)) / (#pin(5) T_"gas" (bold(x), z) #pin(6)))
 $ <eq:dTb>
 
-// Explanation
-- further modulation by _RSD_
 
 
 == The current state of simulations
@@ -73,11 +65,14 @@ $ <eq:dTb>
   [
     *Traditional approaches*
     // From first principles
-    - need to cover large dynamic range
+
+    $->$ need to cover large dynamic range
+
     // small scales to resolve sources + sinks + feedback
     // large scales to capture statistics
-    - hydrodynamics & radiative transfer
-    - hard to scale
+    $->$ hydrodynamics & radiative transfer
+
+    $->$ hard to scale
 
     $=>$ no reproducibility
     #pause
@@ -85,7 +80,7 @@ $ <eq:dTb>
   [
     #pad(1em)[
       #align(left)[
-        #text(weight: "bold")[semi-numerical approaches]
+        #text(weight: "bold")[Semi-numerical approaches]
 
         such as #beorn @Schaeffer_2023, `21cmFAST` @21cmfast
 
@@ -94,7 +89,8 @@ $ <eq:dTb>
 
         $->$ approximative treatment
 
-        $->$ link
+        $->$ prediction of global signals
+        // and statisticical properties
 
         $->$ scalable + efficient
 
@@ -105,4 +101,3 @@ $ <eq:dTb>
     ]
   ]
 )
-
diff --git a/main.pdf b/main.pdf
index 205a9eb..c80a9c8 100644
Binary files a/main.pdf and b/main.pdf differ
diff --git a/main.typ b/main.typ
index c421532..fd75183 100644
--- a/main.typ
+++ b/main.typ
@@ -107,15 +107,19 @@
     institution: [ETH Zürich, University of Zürich],
     // logo: brand.logo,
   ),
-  config-common(handout: true)
+  // config-common(handout: true)
   // footer-left: self => [..#padded_logos],
 )
 
 #title-slide()
 
 #include "introduction.typ"
+
+= #beorn
 #include "halo_model.typ"
 #include "beorn.typ"
+
+
 #include "refinements.typ"
 
 #include "implementation.typ"
diff --git a/references.bib b/references.bib
index 0d725bb..bce21cb 100644
--- a/references.bib
+++ b/references.bib
@@ -447,3 +447,15 @@ archivePrefix = {arXiv},
 
 
 
+@article{Furlanetto_2006,
+   title={Cosmology at low frequencies: The 21cm transition and the high-redshift Universe},
+   volume={433},
+   ISSN={0370-1573},
+   url={http://dx.doi.org/10.1016/j.physrep.2006.08.002},
+   DOI={10.1016/j.physrep.2006.08.002},
+   number={4–6},
+   journal={Physics Reports},
+   publisher={Elsevier BV},
+   author={Furlanetto, Steven R. and Peng Oh, S. and Briggs, Frank H.},
+   year={2006},
+   month=oct, pages={181–301} }
diff --git a/refinements.typ b/refinements.typ
index 06b50cc..ab88a0d 100644
--- a/refinements.typ
+++ b/refinements.typ
@@ -26,7 +26,7 @@
     $->$ #text(weight: "bold")[inconsistent] with the N-body output
 
     #pause
-    $->$ stochasticity for a more realistic description?
+    $->$ how to implement #text(weight: "bold")[consistent] growth?
   ]
 )
 
diff --git a/results.typ b/results.typ
index 39536af..0a6ca76 100644
--- a/results.typ
+++ b/results.typ
@@ -9,7 +9,12 @@
 )[
   #image_cell(notebook, cell_id: "presentation_x_alpha_map")
 ][
-  #lorem(20)
+  - stronger coupling in dense regions
+  // the ones where the accretion rate is likely higher
+
+  - nearly no effect in voids
+  // in particular: no values where the coupling has become weaker
+  // will become apparent in the signal as well
 ]
 
 #pagebreak()
@@ -19,7 +24,10 @@
 )[
   #image_cell(notebook, cell_id: "presentation_temperature_map")
 ][
-  #lorem(20)
+  - delayed heating $<=>$ colder halos
+
+  - highest accreting halos catch up
+  // those are the ones where the diff vanishes: e.g. top right
 ]
 
 #pagebreak()
@@ -29,23 +37,39 @@
 )[
   #image_cell(notebook, cell_id: "presentation_xHII_map")
 ][
-  #lorem(20)
+  - high contrast due to sharp cutoffs
+
+  - clearly increased dynamic range
+  // more variation due to the different accretion rates
+  // globally the morphology is more diversified now: previously all the bubbles had similar sizes due to their similar size -> this degeneracy is removed here.
 ]
 
 #pagebreak()
+// Globally:
+// more dynamic range while the mean systematically shifts towards the (biased) lower accretion rates
+
+// Intermezzo - compare with lower alpha range - mostly similar but occasional contributions from higher alpha values
+// => recommend keeping a wide range since it does not affect performance (if the bins are empty anyway)
+// the more intersting discussion to be had is the effect of a more fine binning - thesan data already gives an indication which values will be most frequent
+// => the implementation to test that is there
 
 #grid(
   columns: (auto, 10em)
 )[
   #image_cell(notebook, cell_id: "presentation_dtb_map")
 ][
-  #lorem(20)
+  - richer structures due to combined effects
+
+  - clear distinction between "foreground" and "background" effects
+  // the halos themselves produce a stronger singal while the background is usually
 ]
 
 
 
 
+
+
 == Signals
 #let notebook = json("../workdir/11_visualization/simulation_signals.ipynb")
-#image_cell(notebook, cell_id: "signal_comparison")
+#image_cell(notebook, cell_id: "presentation_signal")
 #image_cell(notebook, cell_id: "power_spectra_comparison")
diff --git a/talking_points.md b/talking_points.md
new file mode 100644
index 0000000..d3ba730
--- /dev/null
+++ b/talking_points.md
@@ -0,0 +1,205 @@
+# Comments for the presentation
+
+
+## Introduction
+
+---
+
+---
+
+
+---
+
+
+// COMMENTS:
+
+
+---
+
+// Explanation
+- further modulation by _RSD_
+
+
+    // From first principles
+    // small scales to resolve sources + sinks + feedback
+    // large scales to capture statistics
+
+        // IF ASKED: difference with `21cmFAST`:
+        // based on excursion formalistm -> only valid >= 1Mpc, which is ideal for large volumes + statistics => 21-cm forecasts
+
+        // interesting to build emulators for instance
+
+
+---
+
+
+// From the xray emission
+// primordial + heating term
+// expansion + deposition by xrays
+// => xrays are assumed to be the only source of heating
+
+
+// $
+//   x_("HII")(r bar M, z) = theta_"H" lr([R_b (M, z) - r], size: #150%)
+// $
+
+---
+
+// COMMENTS:
+// - contribution from the lyman lines
+// - 1/r^2 decrease from spreading photons
+// - more steep outwards + sharp drop due to redshifting out of line
+
+
+---
+
+== Revisiting the 21cm signal
+
+
+---
+
+
+### Procedure
+Painting using all halos that match in a SINGLE step
+
+
+
+---
+
+OVERLAP EXPLICITLY ALLOWED
+
+
+---
+### Postprocessing
+- ionization overlaps
+- corrections due to RSD
+- computation of derived quantities
+- summary statistics
+
+---
+### Maps
+
+---
+
+### Signal
+
+---
+
+## Halo growth
+
+### Motivation
+
+
+
+### Effect on the flux profiles
+
+// COMMENTS
+// That will be directly affect the global signal as well
+// shifting
+//
+// Yu-Siu already investigated the more nuanced effect of stochasticity but the approach we propose should supersede that
+
+
+### Inferring growth from #smallcaps[Thesan] data
+// ideal for rapid iterations
+
+// in a parallelized fashion => want to stay fast
+// fix the original mass for max. consistency
+// fix the allowed dynamic range
+
+// this sort of "breaks the degeneracy" between halos of the same mass but different growth histories
+
+
+---
+
+RESULT OF LOADING:
+// COMMENTS:
+// no clear trend between mass and growth rate
+
+---
+
+## Adaptations
+---
+
+### Central changes
+
+
+// important since the bins are more now
+
+
+// largely through vectorization -> still "native" python
+// usage of HDF5
+// solid caching mechanisms -> resume simulations, etc...
+
+
+### Simplified usage
+
+In a page or less
+
+---
+
+## Results
+### Map outputs
+  // the ones where the accretion rate is likely higher
+
+  // in particular: no values where the coupling has become weaker
+  // will become apparent in the signal as well
+
+
+---
+
+  // those are the ones where the diff vanishes: e.g. top right
+
+---
+
+  // more variation due to the different accretion rates
+
+---
+// Globally:
+// more dynamic range while the mean systematically shifts towards the (biased) lower accretion rates
+
+// Intermezzo - compare with lower alpha range - mostly similar but occasional contributions from higher alpha values
+// => recommend keeping a wide range since it does not affect performance (if the bins are empty anyway)
+// the more intersting discussion to be had is the effect of a more fine binning - thesan data already gives an indication which values will be most frequent
+// => the implementation to test that is there
+
+
+  // the halos themselves produce a stronger singal while the background is usually
+
+
+
+
+---
+
+### Signals
+
+---
+
+## Conclusion
+
+---
+### Summary
+
+  // since it affects the SFR and thus the emissivity
+
+
+  // change in profiles trivially
+
+  // which could in theory be absorbed by shifting other paremeters
+
+  // which we can hope to observe (although many are subtle)
+
+// unique position of 21-cm cosmology -> cannot discuss observational constraints
+
+
+  // invite you to check out
+
+
+### Outlook
+// finally ready for direct comparison with c2ray? now that parameters and loading have been properly implemented
+
+// Assuming other relations related to production of photons is (hopefully by now well motivated) complex
+// these cannot directly be inferred => expressed as a distribution as a function of another halo property
+
+// the scale-up -> large volumes with usable merger trees
+// comitting to reserving some 100s of node hours (which I would still quantify as fast)