diff --git a/paper.md b/paper.md
index 489ba35..7515420 100644
--- a/paper.md
+++ b/paper.md
@@ -90,7 +90,7 @@ The ``py-EnBiD-ananke`` submodule handles the installation of ``EnBiD`` and inte
 
 The full description of ``Galaxia`` is detailed in @Galaxia:2011, but to summarize, ``Galaxia`` uses a given galactic model to generate a population of synthetic stars that composes it, with its associated astrometric and photometric catalog. The original pipeline had a more general purpose as the input galactic model can be generated via an N-Body simulation as much as it can be specified as a set of density distributions. However, for our purpose with our modified version ``galaxia-ananke``, the pipeline uses cosmological simulation star particle data provided by the user, specifically the mass, position, velocity, age, metallicity & abundances, as well as phase space densities for each star particle.
 
-``galaxia-ananke`` generates the synthetic stars by sampling phase space to reproduce the distribution representing overlapping phase space kernels centered at each particle, invertly scaled with the particle density, and by sampling mass to reproduce a @Kroupa:2001 initial mass function. Each synthetic star carries the other properties of the parent particle such as age and metallicity, with which the masses are used to interpolate photometry from pre-computed isochrone tracks (details on those are described in the section \autoref{sec:dependencies}). Finally, astrometry is determined by converting the phase space coordinates to celestial coordinates given a user-specified observer phase space position.
+``galaxia-ananke`` generates the synthetic stars by sampling phase space to reproduce the distribution representing overlapping phase space kernels centered at each particle, invertly scaled with the particle density, and by sampling mass to reproduce a @Kroupa:2001 initial mass function. Each synthetic star carries the other properties of the parent particle such as age and metallicity, with which the masses are used to interpolate photometry from pre-computed isochrone tracks (details on those are described in \autoref{sec:dependencies} Dependencies). Finally, astrometry is determined by converting the phase space coordinates to celestial coordinates given a user-specified observer phase space position.
 
 The ``py-Galaxia-ananke`` submodule handles the installation of ``galaxia-ananke``, a modified version of ``Galaxia``, and interfaces with its pipeline. The ``galaxia-ananke`` source code lives in a separate repository which is linked as a ``git`` submodule in the repository of ``py-Galaxia-ananke``. At installation, ``py-Galaxia-ananke`` builds and packages the executable of ``galaxia-ananke`` from its source code directly from its ``git`` submodule, as well as the operational data for ``galaxia-ananke`` which includes the collections of isochrones sets. All the resulting ``galaxia-ananke`` packaged data is eventually placed in a dedicated cache folder that is created in the site-specific directory of the running ``Python`` installation.
 
diff --git a/py-EnBiD-ananke b/py-EnBiD-ananke
index 7ceff38..45cdca3 160000
--- a/py-EnBiD-ananke
+++ b/py-EnBiD-ananke
@@ -1 +1 @@
-Subproject commit 7ceff384c4b71df113e8e3b368a7649611092421
+Subproject commit 45cdca3d45ebb397fc0699428beb5b9962b282e1
diff --git a/py-Galaxia-ananke b/py-Galaxia-ananke
index c8b2d37..2c42b5d 160000
--- a/py-Galaxia-ananke
+++ b/py-Galaxia-ananke
@@ -1 +1 @@
-Subproject commit c8b2d37a5fbafd682ff192e376c5bbb34b75b4ce
+Subproject commit 2c42b5d54db1db5ccbb4eb26321995978c108e8b