diff --git a/a-short-survey-mdpi.tex b/a-short-survey-mdpi.tex
index 0ef2e23..e2ba869 100644
--- a/a-short-survey-mdpi.tex
+++ b/a-short-survey-mdpi.tex
@@ -100,7 +100,7 @@ \section{Timeline of Particles and Plasmas in the Universe}\label{sec:Intro}
 \subsection{Guide to \texorpdfstring{$130\GeV>T>20\keV$}{130\GeV>T>20\keV}}\label{sec:Guide}
 \noindent This survey of the early Universe begins with quark-gluon plasma (QGP) at a temperature of $T=130\GeV$. It then ends at a temperature of $T=20\keV$ with the electron-positron epoch which was the final phase of the Universe to contain significant quantities of antimatter. This defines the \lq\lq short\rq\rq\ $t\approx1/2$ hour time-span that will be covered. This work presumes that the Universe is homogeneous and that in our casual domain, the Universe's baryon content is matter dominated. Our work is rooted in the Universe as presented by Lizhi Fang and Remo Ruffini~\cite{fang1984cosmology,fang1985galaxies,fang1987quantum}. Within the realm of the Standard Model, we coherently connect the differing matter-antimatter plasmas as each transforms from one phase into another.
 
-A more detailed description of particles and plasmas follows in \rsec{sec:Timeline}. We have adopted the standard $\Lambda$CDM model of a cosmological constant ($\Lambda$) and cold dark matter (CDM) where the Universe undergoes dynamical expansion as described in the Friedmann–Lemaître–Robertson–Walker (FLRW) metric. The contemporary history of the Universe in terms of energy density as a function of time and temperature is shown in \rf{CosmicDensity}. The Universe's past is obtained from integrating backwards the proposed modern composition of the Universe which contains $69\%$ dark energy, $26\%$ dark matter, $5\%$ baryons, and $<1\%$ photons and neutrinos in terms of energy density. The method used to obtain these results are found in \rsec{sec:Cosmo}.
+A more detailed description of particles and plasmas follows in \rsec{sec:Timeline}. We have adopted the standard $\Lambda$CDM model of a cosmological constant ($\Lambda$) and cold dark matter (CDM) where the Universe undergoes dynamical expansion as described in the Friedmann-Lema\^itre-Robertson-Walker (FLRW) metric. The contemporary history of the Universe in terms of energy density as a function of time and temperature is shown in \rf{CosmicDensity}. The Universe's past is obtained from integrating backwards the proposed modern composition of the Universe which contains $69\%$ dark energy, $26\%$ dark matter, $5\%$ baryons, and $<1\%$ photons and neutrinos in terms of energy density. The method used to obtain these results are found in \rsec{sec:Cosmo}.
 
 After the general overview, we take the opportunity to enlarge in some detail our more recent work in special topics. In \rsec{sec:QGP}, we describe the chemical potentials of the QGP plasma species leading up to hadronization, Hubble expansion of the QGP plasma, and the abundances of heavy quarks. In \rsec{sec:Hadrons} we discuss the formation of matter during hadronization, the role of strangeness, and the unique circumstances which led to pions remaining abundant well after all other hadrons were diluted or decayed. We review the roles of muons and neutrinos in the leptonic epoch in \rsec{sec:Leptonic}. The $e^{\pm}$ plasma epoch is described in \rsec{sec:ElectronPositron} which is the final stage of the Universe where antimatter played an important role. Here we introduce the statistical physics description of electrons and positron gasses, their relation to the baryon density, and the magnetization of the $e^{\pm}$ plasma prior to the disappearance of the positrons shortly after Big Bang Nucleosynthesis (BBN). A more careful look at the effect of the dense $e^{\pm}$ plasma on BBN is underway. One interesting feature of having an abundant $e^{\pm}$ plasma is the possibility of magnetization in the early Universe. We begin to address this using spin-magnetization and mean-field theory where all the spins respond to the collective bulk magnetism self generated by the plasma. We stop our survey at a temperature of $T=20\keV$ with the disappearance of the positrons signifying the end of antimatter dynamics at cosmological scales.
 
@@ -298,7 +298,7 @@ \subsection{Conservation laws in QGP}\label{sec:Conservation}
 \begin{align}\label{QGP_sB}
 \frac{S}{B}=\frac{s}{n_B}=\frac{\sum_fs_f(\mu_f,T)}{\sum_fB_fn_f(\mu_f,T)}=\mathrm{const}
 \end{align}
-where $s_f$ is the entropy density of given species $f$. As the expanding Universe remains in thermal equilibrium, the entropy is conserved within a co-moving volume. The baryon number within a co-moving volume is also conserved. As both quantities dilute with $1/a(t)^{3}$ within a normal volume, the ratio of the two is constant. This constraint does not become broken until spatial inhomogeneitiess from gravitational attraction becomes significant, leading to increases in local entropy.
+where $s_f$ is the entropy density of given species $f$. As the expanding Universe remains in thermal equilibrium, the entropy is conserved within a co-moving volume. The baryon number within a co-moving volume is also conserved. As both quantities dilute with $1/a(t)^{3}$ within a normal volume, the ratio of the two is constant. This constraint does not become broken until spatial inhomogeneities from gravitational attraction becomes significant, leading to increases in local entropy.
 \end{enumerate}
 At each temperature $T$, the above three conditions form a system of three coupled, nonlinear equations of the three chosen unknowns (here we have $\mu_d$, $\mu_e$, and $\mu_\nu$). In \rf{QGPchem1} we present numerical solutions to the conditions \req{QGP_Q}-\req{QGP_sB} and plot the chemical potentials as a function of time. As seen in the figure, the three potentials are in alignment during the QGP phase until the hadronization epoch where the down quark chemical potential diverges from the leptonic chemical potentials before reaching an asymptotic value at late times. This asymptotic value is given as approximately $\mu_{q}\approx m_{N}/3$ the mass of the nucleons and represents the confinement of the quarks into the protons and neutrons at the end of hadronization.
 
@@ -688,7 +688,7 @@ \subsection{Neutrino masses and oscillation} \label{sec:Neutrinos}
 where $\nu^{c} = \hat{C}(\bar{\nu})^{T}$ is the charge conjugate of the neutrino field. The operator $\hat{C} = i\gamma^{2}\gamma^{0}$ is the charge conjugation operator. {\xblue An interesting consequence of neutrinos being Majorana particles is that they would be their own antiparticles like photons allowing for violations of total lepton number. Neutrinoless double beta decay is an important, yet undetected, evidence for Majorana nature of neutrinos~\cite{Dolinski:2019nrj}.} Majorana neutrinos with small masses can be generated from some high scale via the See-Saw mechanism~\cite{Arkani-Hamed:1998wuz,Ellis:1999my,Casas:2001sr} which ensures that the degrees of freedom separate into heavy neutrinos and light nearly massless Majorana neutrinos. The See-Saw mechanism then provides an explanation for the smallness of the neutrino masses as has been experimentally observed.
 
 
-A flavor eigenstate $\nu^{\alpha}$ can be described as a superposition of mass eigenstates $\nu^{k}$ with coefficients given by the Pontecorvo–Maki–Nakagawa–Sakata (PMNS) mixing matrix~\cite{King:2013eh,FernandezMartinez:2016lgt} which are both in general  complex and unitary. This is given by
+A flavor eigenstate $\nu^{\alpha}$ can be described as a superposition of mass eigenstates $\nu^{k}$ with coefficients given by the Pontecorvo-Maki-Nakagawa-Sakata (PMNS) mixing matrix~\cite{King:2013eh,FernandezMartinez:2016lgt} which are both in general  complex and unitary. This is given by
 \begin{align}\label{NuFlavors}
 	\nu^{\alpha}=\sum_k^nU^\ast_{\alpha k}\nu^{k}, \qquad\alpha=e,\mu,\tau,\qquad k=1,2,3,\dots,n
 \end{align}
@@ -708,14 +708,14 @@ \subsection{Neutrino masses and oscillation} \label{sec:Neutrinos}
 	\end{alignat}
 where $c_{ij} = \mathrm{cos}(\theta_{ij})$ and $s_{ij} = \mathrm{sin}(\theta_{ij})$. In this convention, the three mixing angles $(\theta_{12}, \theta_{13}, \theta_{23})$, are understood to be the Euler angles for generalized rotations.
 
-The neutrino eigenmasses are generally considered to be small with values no more than $0.1\eV$. Because of this, neutrinos produced during fusion within the Sun or radioactive fission in terrestrial reactors on Earth propagate relativistically. Evaluating freely propagating plane waves in the relativistic limit yields the vacuum oscillation probability between flavors $\nu_\alpha$ and $\nu_\beta$ written as~\cite{ParticleDataGroup:2022pth}
+The neutrino proper masses are generally considered to be small with values no more than $0.1\eV$. Because of this, neutrinos produced during fusion within the Sun or radioactive fission in terrestrial reactors on Earth propagate relativistically. Evaluating freely propagating plane waves in the relativistic limit yields the vacuum oscillation probability between flavors $\nu_\alpha$ and $\nu_\beta$ written as~\cite{ParticleDataGroup:2022pth}
 \begin{align}\label{NuOscillation}
   P_{\alpha\rightarrow\beta}
  =&\delta_{\alpha\beta}-4\sum_{i<j}^n \mathrm{Re}\left[U_{\alpha i}U^\ast_{\beta i}U^\ast_{\alpha j}U_{\beta j}\right]\sin^2\!\!\left(\frac{\Delta m^2_{ij}L}{4E}\right)\notag\\
  &+2\sum_{i<j}^n \mathrm{Im}\left[U_{\alpha i}U^\ast_{\beta i}U^\ast_{\alpha j}U_{\beta j}\right]\sin\!\!\left(\frac{\Delta m^2_{ij}L}{2E}\right)
  ,\qquad\Delta m^2_{ij}\equiv{m^2_i-m^2_j}
 \end{align}
-where $L$ is the distance traveled by the neutrino between production and detection. The square mass difference $\Delta m^2_{ij}$ has been experimentally measured~\cite{ParticleDataGroup:2022pth}. As oscillation only restricts the differences in mass squares, the precise values of the masses cannot be determined from oscillation experiments alone. It is also unknown under what hierarchical scheme (normal or inverted)~\cite{Avignone:2007fu,Esteban:2020cvm} the masses are organized as two of the three neutrino eigenmasses are close together in value. 
+where $L$ is the distance traveled by the neutrino between production and detection. The square mass difference $\Delta m^2_{ij}$ has been experimentally measured~\cite{ParticleDataGroup:2022pth}. As oscillation only restricts the differences in mass squares, the precise values of the masses cannot be determined from oscillation experiments alone. It is also unknown under what hierarchical scheme (normal or inverted)~\cite{Avignone:2007fu,Esteban:2020cvm} the masses are organized as two of the three neutrino proper masses are close together in value. 
 
 It is important to point out that oscillation does not represent any physical interaction (except when neutrinos must travel through matter which modulates the $\nu_{e}$ flavor~\cite{NuSTEC:2017hzk,DUNE:2020ypp}) or change in the neutrino during propagation. Rather, for a given production energy, the superposition of mass eigenstates each have unique momentum and thus unique group velocities. This mismatch in the wave propagation leads to the oscillatory probability of flavor detection as a function of distance.
 
@@ -777,7 +777,7 @@ \subsection{Neutrino freeze-out}\label{sec:Freezeout}
 
 After neutrinos freeze-out, the neutrino co-moving entropy is independently conserved. However, the presence of electron-positron rich plasma until $T=20\keV$ provides the reaction $\gamma\gamma\to e^-e^+\to\nu\bar{\nu}$ to occur even after neutrinos decouple from the cosmic plasma. This suggests the small amount of $e^\pm$ entropy can still transfer to neutrinos until temperature $T=20\keV$ and can modify free streaming distribution and the effective number of neutrinos.
 
-We expect that incorporating oscillations into the freeze-out calculation would yield a smaller freeze-out temperature difference between neutrino flavors as oscillation provides a mechanism in which the heavier flavors remain thermally active despite their direct production becoming suppressed. In work by Mangano et. al.~\cite{Mangano:2005cc}, neutrino freeze-out including flavour oscillations is shown to be a negligible effect.
+We expect that incorporating oscillations into the freeze-out calculation would yield a smaller freeze-out temperature difference between neutrino flavors as oscillation provides a mechanism in which the heavier flavors remain thermally active despite their direct production becoming suppressed. In work by Mangano et. al.~\cite{Mangano:2005cc}, neutrino freeze-out including flavor oscillations is shown to be a negligible effect.
 
 %%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%%
 \subsection{Effective number of neutrinos}\label{sec:EffectiveNeutrino}
@@ -949,7 +949,7 @@ \subsection{Electron-positron statistical physics}\label{sec:Partition}
 \end{align}
 where $\eta_{e}$ is the electron chemical potential and $\eta_s$ is the spin chemical potential for the generalized fugacity $\lambda_{\sigma}^{s}$. The parameter $\gamma(x)$ is a spatial field which controls the distribution inhomogeneity of the Fermi gas. Inhomogeneities can arise from the influence of other forces on the gas such as gravitational forces. Deviations of $\gamma\neq1$ represent configurations of reduced entropy (maximum entropy yields the normal Fermi distribution itself with $\gamma=1$) without pulling the system off a thermal temperature.
 
-This situation is similar to that of the quarks during QGP, but instead the deviation is spatial rather than in time. This is precisely the kind of behavior that may arise in the $e^{\pm}$ epoch as the dominant photon thermal bath keeps the Fermi gas in thermal equilibrium while spatial inequilibria could spontaneously develop. For the remainder of this work, we will retain $\gamma(x)=1$. The energy $E_{n}^\pm$ can be written as
+This situation is similar to that of the quarks during QGP, but instead the deviation is spatial rather than in time. This is precisely the kind of behavior that may arise in the $e^{\pm}$ epoch as the dominant photon thermal bath keeps the Fermi gas in thermal equilibrium while spatial inhomogeneity could spontaneously develop. For the remainder of this work, we will retain $\gamma(x)=1$. The energy $E_{n}^\pm$ can be written as
 \begin{align}
 E_{n}^\pm&=\sqrt{p^2_z+\tilde m^2_\pm+2eBn},\qquad\tilde{m}^2_\pm=m^2_e+eB\left(1\mp\frac{g}{2}\right)\,,
 \end{align}
@@ -1052,7 +1052,7 @@ \section{Looking in the Cosmic Rear-view Mirror}\label{sec:Summary}
 
 We explored several major epochs in the Universe evolution where antimatter, in all its diverse forms, played a large roll. Emphasis was placed on understanding the thermal and chemical equilibria arising within the context of the Standard Model of particle physics. We highlighted that primordial quark-gluon plasma (QGP, which existed for $\approx 25\;\mu$sec) is an important antimatter laboratory with its gargantuan antimatter content. Study of the QGP fireballs created in heavy-ion collisions performed today informs our understanding of the early Universe and vice versa~\cite{Borsanyi:2016ksw,Rafelski:2013qeu,Petran:2013lja,Philipsen:2012nu}, even though the primordial quark-gluon plasma under cosmic expansion explores a location in the phase diagram of QCD inaccessible to relativistic collider experiments considering both net baryon density, see \rf{phaseQGP}, and longevity of the plasma. We described (see \rsec{sec:BottomCharm}) that the QGP epoch near to hadronization condition possessed bottom quarks in a non-equilibrium abundance: This novel QGP-Universe feature may be of interest in consideration of the QGP epoch as possible source for baryon asymmetry~\cite{Yang:2020nne}. 
 
-Bottom nonequilibrium is one among a few interesting results presented bridging the temperature gap between QGP hadronization at temperature $T\simeq150\MeV$ and neutrino freeze-out. Specifically we shown {\bf persistence of:}
+Bottom non-equilibrium is one among a few interesting results presented bridging the temperature gap between QGP hadronization at temperature $T\simeq150\MeV$ and neutrino freeze-out. Specifically we shown {\bf persistence of:}
  \begin{itemize}
  \item Strangeness abundance, present beyond the loss of the antibaryons at $T=38.2\MeV$.
  \item Pions, which are equilibrated via photon production long after the other hadrons disappear; these lightest hadrons are also dominating the Universe baryon abundance down to $T=5.6\MeV$.
diff --git a/revisions-letter/revisions-letter.bbl b/revisions-letter/revisions-letter.bbl
deleted file mode 100644
index edcd955..0000000
--- a/revisions-letter/revisions-letter.bbl
+++ /dev/null
@@ -1,93 +0,0 @@
-\begin{thebibliography}{10}
-
-\bibitem{KamLAND:2002uet}
-K.~Eguchi {\em et~al.}, ``{First results from KamLAND: Evidence for reactor
-  anti-neutrino disappearance},'' {\em Phys. Rev. Lett.}, vol.~90, p.~021802,
-  2003.
-
-\bibitem{Fogli:2005cq}
-G.~L. Fogli, E.~Lisi, A.~Marrone, and A.~Palazzo, ``{Global analysis of
-  three-flavor neutrino masses and mixings},'' {\em Prog. Part. Nucl. Phys.},
-  vol.~57, pp.~742--795, 2006.
-
-\bibitem{SuperKamiokande:1998kpq}
-Y.~Fukuda {\em et~al.}, ``{Evidence for oscillation of atmospheric
-  neutrinos},'' {\em Phys. Rev. Lett.}, vol.~81, pp.~1562--1567, 1998.
-
-\bibitem{King:2013eh}
-S.~F. King and C.~Luhn, ``{Neutrino Mass and Mixing with Discrete Symmetry},''
-  {\em Rept. Prog. Phys.}, vol.~76, p.~056201, 2013.
-
-\bibitem{FernandezMartinez:2016lgt}
-E.~Fernandez-Martinez, J.~Hernandez-Garcia, and J.~Lopez-Pavon, ``{Global
-  constraints on heavy neutrino mixing},'' {\em JHEP}, vol.~08, p.~033, 2016.
-
-\bibitem{Pascoli:2006ci}
-S.~Pascoli, S.~T. Petcov, and A.~Riotto, ``{Leptogenesis and Low Energy CP
-  Violation in Neutrino Physics},'' {\em Nucl. Phys. B}, vol.~774, pp.~1--52,
-  2007.
-
-\bibitem{schwartz2014quantum}
-M.~D. Schwartz, {\em Quantum field theory and the standard model}.
-\newblock Cambridge university press, 2014.
-
-\bibitem{Fritzsch:2015gxa}
-H.~Fritzsch, ``{Neutrino Masses and Flavor Mixing},'' {\em Mod. Phys. Lett. A},
-  vol.~30, no.~16, p.~1530012, 2015.
-
-\bibitem{Fritzsch:1999ee}
-H.~Fritzsch and Z.-z. Xing, ``{Mass and flavor mixing schemes of quarks and
-  leptons},'' {\em Prog. Part. Nucl. Phys.}, vol.~45, pp.~1--81, 2000.
-
-\bibitem{giunti2007fundamentals}
-C.~Giunti and C.~W. Kim, {\em Fundamentals of neutrino physics and
-  astrophysics}.
-\newblock Oxford university press, 2007.
-
-\bibitem{Casas:2001sr}
-J.~A. Casas and A.~Ibarra, ``{Oscillating neutrinos and $\mu \to e, \gamma$},''
-  {\em Nucl. Phys. B}, vol.~618, pp.~171--204, 2001.
-
-\bibitem{Arkani-Hamed:1998wuz}
-N.~Arkani-Hamed, S.~Dimopoulos, G.~R. Dvali, and J.~March-Russell, ``{Neutrino
-  masses from large extra dimensions},'' {\em Phys. Rev. D}, vol.~65,
-  p.~024032, 2001.
-
-\bibitem{Ellis:1999my}
-J.~R. Ellis and S.~Lola, ``{Can neutrinos be degenerate in mass?},'' {\em Phys.
-  Lett. B}, vol.~458, pp.~310--321, 1999.
-
-\bibitem{Avignone:2007fu}
-F.~T. Avignone, III, S.~R. Elliott, and J.~Engel, ``{Double Beta Decay,
-  Majorana Neutrinos, and Neutrino Mass},'' {\em Rev. Mod. Phys.}, vol.~80,
-  pp.~481--516, 2008.
-
-\bibitem{Esteban:2020cvm}
-I.~Esteban, M.~C. Gonzalez-Garcia, M.~Maltoni, T.~Schwetz, and A.~Zhou, ``{The
-  fate of hints: updated global analysis of three-flavor neutrino
-  oscillations},'' {\em JHEP}, vol.~09, p.~178, 2020.
-
-\bibitem{DUNE:2020ypp}
-B.~Abi {\em et~al.}, ``{Deep Underground Neutrino Experiment (DUNE), Far
-  Detector Technical Design Report, Volume II: DUNE Physics}.'' 2 2020.
-
-\bibitem{NuSTEC:2017hzk}
-L.~Alvarez-Ruso {\em et~al.}, ``{NuSTEC White Paper: Status and challenges of
-  neutrino\textendash{}nucleus scattering},'' {\em Prog. Part. Nucl. Phys.},
-  vol.~100, pp.~1--68, 2018.
-
-\bibitem{Rafelski:2017hce}
-J.~Rafelski, M.~Formanek, and A.~Steinmetz, ``{Relativistic Dynamics of Point
-  Magnetic Moment},'' {\em Eur. Phys. J. C}, vol.~78, no.~1, p.~6, 2018.
-
-\bibitem{Formanek:2021mcp}
-M.~Formanek, A.~Steinmetz, and J.~Rafelski, ``{Motion of classical charged
-  particles with magnetic moment in external plane-wave electromagnetic
-  fields},'' {\em Phys. Rev. A}, vol.~103, no.~5, p.~052218, 2021.
-
-\bibitem{Formanek:2020zwc}
-M.~Formanek, A.~Steinmetz, and J.~Rafelski, ``{Radiation reaction friction:
-  Resistive material medium},'' {\em Phys. Rev. D}, vol.~102, no.~5, p.~056015,
-  2020.
-
-\end{thebibliography}
diff --git a/revisions-letter/revisions-letter.tex b/revisions-letter/revisions-letter.tex
index e810595..06a2df4 100644
--- a/revisions-letter/revisions-letter.tex
+++ b/revisions-letter/revisions-letter.tex
@@ -2,10 +2,12 @@
 \usepackage{fullpage}
 
 \name{Johann Rafelski, Jeremiah Birrell, Andrew Steinmetz, Cheng Tao Yang}
-\signature{Johann Rafelski\\ Jeremiah Birrell\\ Andrew Steinmetz\\ Cheng Tao Yang}
+\signature{Andrew Steinmetz}
 
 \address
 {
+    Prof. Johann Rafelski,\\
+    Andrew Steinmetz,\\
     Department of Physics,\\
     The University of Arizona,\\
     Tucson, AZ 85721, USA
@@ -14,29 +16,32 @@
 \longindentation=0pt
 \begin{document}
 
-\begin{letter}{MDPI Universe}
+\begin{letter}
+{Re: MDPI Universe Festschrift for Remo Ruffini}
 
-\opening{Dear Editors,}
+\opening{Dear Dr. Vereshchagin,}
 
-Thank you for reviewing our submission to Dr. Remo Ruffini's Festschrift. With this letter, we submit our revised manuscript with changes requested by the reviewers and minor changes we ourselves wished to make. Within the revised manuscript, added or revised text has been highlighted in blue. Minor grammatical changes or corrections remain unmarked. Below we provide a list of relevant changes with the Section denoted:
+With this letter we bring to your attention our expanded and updated contribution to Dr. Remo Ruffini's Festschrift following on the review round, which I have prepared with active assistance of Prof. Rafelski. In our revised manuscript we mark in blue our response to  requests made by the reviewers and some changes we ourselves wished to make. Trivial grammatical changes or corrections remain unmarked. This is a brief summary of relevant changes made:
 
 \begin{itemize}
     \item Sect. 1 - Revised to discuss the origin of baryon asymmetry and the application of the Sakharov conditions in more detail as recommended by Reviewers \#1 and \#2.
-    \item Sect. 1.3 - Added references to dynamical or phantom dark energy which are alternatives to the $\Lambda$ DE model as recommended by Reviewer \#2.
-    \item Sect. 3 - Emphasized mesons as a critical participant in antimatter evolution as requested by Reviewer \#1.
-    \item Sect. 4 - Section is revised for clarity as well as to emphasize antimatter presence as recommended by Reviewer \#1.
-    \item Sect. 5.2 - Emphasis is added that the unique situation of hot dense matter and antimatter in large quantities makes the $e^{\pm}$ epoch uniquely interesting in terms of magnetization as recommended by Reviewer \#1.
-    \item Sect. 6 - The photographs honoring Remo Ruffini and Lizhi Fang have been grouped together and moved to the acknowledgements in coordination with editors. The first line of the abstract, as well as the last paragraph of the conclusions have also been moved to acknowledgements with slight revision.
+    \item Sect. 1.3 - Added references to dynamical or phantom dark energy which are alternatives to the $\Lambda$CDM model as recommended by Reviewer \#2.
+    \item Sect. 3 - Emphasized mesons as a participant in antimatter evolution as requested by Reviewer \#1.
+    \item Sect. 4 - Section is sprinkled with remarks to emphasize antimatter presence as recommended by Reviewer \#1. (Some language revisions are also present here.)
+    \item Sect. 5 - Emphasis is added that the unique situation of hot dense matter and antimatter in large quantities makes the $e^{\pm}$ epoch uniquely interesting in terms of magnetization as recommended by Reviewer \#1.
+    \item Sect. 6 - The photographs honoring Remo Ruffini and Lizhi Fang have been grouped together and moved to the acknowledgements. The first line of the abstract, as well as the last paragraph of the conclusions have also been grouped within the acknowledgements with slight revision.
 \end{itemize}
 
 The following figures were changed or modified:
 \begin{itemize}
     \item Fig. 16 - Caption has been expanded to explain all curves.
-    \item Fig. 19 - Figure has been replaced with an corrected value for the Solar core density.
+    \item Fig. 19 - Figure has been replaced with a corrected value for the Solar core density.
     \item Fig. 23 - Caption rewritten for clarity.
+    \item Fig. 25 - Photo of Lizhi Fang has been added.
 \end{itemize}
 
-The following references were added to support above revisions or otherwise support statements already present in the work:
+The following references were added to support above revisions or otherwise support statements already present in the work (some as requested by referees added/omitted):\\
+ADDED
 \begin{itemize}
     \item K.~Eguchi {\em et~al.}, ``{First results from KamLAND: Evidence for reactor anti-neutrino disappearance},'' {\em Phys. Rev. Lett.}, vol.~90, p.~021802, 2003.
     \item G.~L. Fogli, E.~Lisi, A.~Marrone, and A.~Palazzo, ``{Global analysis of three-flavor neutrino masses and mixings},'' {\em Prog. Part. Nucl. Phys.}, vol.~57, pp.~742--795, 2006.
@@ -71,15 +76,16 @@
     \item M.~J.~Dolinski, A.~W.~P.~Poon and W.~Rodejohann, {Neutrinoless Double-Beta Decay: Status and Prospects}, Ann. Rev. Nucl. Part. Sci. 69, 219-251. 2019.
 \end{itemize}
 
-The following references were removed:
+REMOVED/REGROUPED
 \begin{itemize}
-    \item Yang, C.T.; Rafelski, J. {Bottom quark chemical nonequilibrium in primordial QGP}. Update in preparation, {\bf 2023}.
+    \item Yang, C.T.; Rafelski, J. {Bottom quark chemical nonequilibrium in primordial QGP}. Update in preparation, {\bf 2023}; added to another reference
     \item Demia\'nski, M.; Doroshkevich, A.G. {Beyond the standard $\Lambda$CDM cosmology: the observed structure of DM halos and the shape of the power spectrum}, arXiv:astro-ph.CO/1511.07989. {\bf 2015}.
 \end{itemize}
 The first removed reference (Yang, 2023, in preparation) was a duplicate of another article included in the citations which is on arXiv, and will be submitted for publication once updated. The second (Demia\'nski, 2015) was replaced with a more relevant reference which has been fully published as requested by Reviewer \#2. Additionally, a note was added in the bibliography justifying the arXiv reference (Fromerth and Rafelski, 2002) which was published in part in Acta Phys. Polon. B (Fromerth et. al., 2012) and in full in Eur. Phys. J. ST (Rafelski, 2019) as requested by Reviewer \#2.
 
+After these changes the number of references grew to a total of 164. 
 
-We look forward to having our work accepted for publication.
+We look forward to having our work accepted for publication. 
 
 \closing{Sincerely,}
 
diff --git a/revisions-letter/revisions-refs.bib b/revisions-letter/revisions-refs.bib
deleted file mode 100644
index 9bca42a..0000000
--- a/revisions-letter/revisions-refs.bib
+++ /dev/null
@@ -1,236 +0,0 @@
-@article{KamLAND:2002uet,
-    author = "Eguchi, K. and others",
-    collaboration = "KamLAND",
-    title = "{First results from KamLAND: Evidence for reactor anti-neutrino disappearance}",
-    eprint = "hep-ex/0212021",
-    archivePrefix = "arXiv",
-    doi = "10.1103/PhysRevLett.90.021802",
-    journal = "Phys. Rev. Lett.",
-    volume = "90",
-    pages = "021802",
-    year = "2003"
-}
-@article{Fogli:2005cq,
-    author = "Fogli, G. L. and Lisi, E. and Marrone, A. and Palazzo, A.",
-    title = "{Global analysis of three-flavor neutrino masses and mixings}",
-    eprint = "hep-ph/0506083",
-    archivePrefix = "arXiv",
-    doi = "10.1016/j.ppnp.2005.08.002",
-    journal = "Prog. Part. Nucl. Phys.",
-    volume = "57",
-    pages = "742--795",
-    year = "2006"
-}
-@article{SuperKamiokande:1998kpq,
-    author = "Fukuda, Y. and others",
-    collaboration = "Super-Kamiokande",
-    title = "{Evidence for oscillation of atmospheric neutrinos}",
-    eprint = "hep-ex/9807003",
-    archivePrefix = "arXiv",
-    reportNumber = "BU-98-17, ICRR-REPORT-422-98-18, UCI-98-8, KEK-PREPRINT-98-95, LSU-HEPA-5-98, UMD-98-003, SBHEP-98-5, TKU-PAP-98-06, TIT-HPE-98-09",
-    doi = "10.1103/PhysRevLett.81.1562",
-    journal = "Phys. Rev. Lett.",
-    volume = "81",
-    pages = "1562--1567",
-    year = "1998"
-}
-@article{King:2013eh,
-    author = "King, Stephen F. and Luhn, Christoph",
-    title = "{Neutrino Mass and Mixing with Discrete Symmetry}",
-    eprint = "1301.1340",
-    archivePrefix = "arXiv",
-    primaryClass = "hep-ph",
-    reportNumber = "IPPP-12-100, DCPT-12-200",
-    doi = "10.1088/0034-4885/76/5/056201",
-    journal = "Rept. Prog. Phys.",
-    volume = "76",
-    pages = "056201",
-    year = "2013"
-}
-@article{FernandezMartinez:2016lgt,
-    author = "Fernandez-Martinez, Enrique and Hernandez-Garcia, Josu and Lopez-Pavon, Jacobo",
-    title = "{Global constraints on heavy neutrino mixing}",
-    eprint = "1605.08774",
-    archivePrefix = "arXiv",
-    primaryClass = "hep-ph",
-    doi = "10.1007/JHEP08(2016)033",
-    journal = "JHEP",
-    volume = "08",
-    pages = "033",
-    year = "2016"
-}
-@article{Pascoli:2006ci,
-    author = "Pascoli, S. and Petcov, S. T. and Riotto, Antonio",
-    title = "{Leptogenesis and Low Energy CP Violation in Neutrino Physics}",
-    eprint = "hep-ph/0611338",
-    archivePrefix = "arXiv",
-    reportNumber = "DCPT-06-166, CERN-PH-TH-2006-213, IPPP-06-83, SISSA-71-2006-EP",
-    doi = "10.1016/j.nuclphysb.2007.02.019",
-    journal = "Nucl. Phys. B",
-    volume = "774",
-    pages = "1--52",
-    year = "2007"
-}
-@book{schwartz2014quantum,
-  title={Quantum field theory and the standard model},
-  author={Schwartz, Matthew D},
-  year={2014},
-  publisher={Cambridge university press}
-}
-@article{Fritzsch:2015gxa,
-    author = "Fritzsch, Harald",
-    title = "{Neutrino Masses and Flavor Mixing}",
-    eprint = "1503.01857",
-    archivePrefix = "arXiv",
-    primaryClass = "hep-ph",
-    doi = "10.1142/S0217732315300128",
-    journal = "Mod. Phys. Lett. A",
-    volume = "30",
-    number = "16",
-    pages = "1530012",
-    year = "2015"
-}
-@article{Fritzsch:1999ee,
-    author = "Fritzsch, Harald and Xing, Zhi-zhong",
-    title = "{Mass and flavor mixing schemes of quarks and leptons}",
-    eprint = "hep-ph/9912358",
-    archivePrefix = "arXiv",
-    reportNumber = "LMU-99-16",
-    doi = "10.1016/S0146-6410(00)00102-2",
-    journal = "Prog. Part. Nucl. Phys.",
-    volume = "45",
-    pages = "1--81",
-    year = "2000"
-}
-@book{giunti2007fundamentals,
-  title={Fundamentals of neutrino physics and astrophysics},
-  author={Giunti, Carlo and Kim, Chung W},
-  year={2007},
-  publisher={Oxford university press}
-}
-@article{Casas:2001sr,
-    author = "Casas, J. A. and Ibarra, A.",
-    title = "{Oscillating neutrinos and $\mu \to e, \gamma$}",
-    eprint = "hep-ph/0103065",
-    archivePrefix = "arXiv",
-    reportNumber = "IEM-FT-211-01, OUTP-01-11P, IFT-UAM-CSIC-01-08",
-    doi = "10.1016/S0550-3213(01)00475-8",
-    journal = "Nucl. Phys. B",
-    volume = "618",
-    pages = "171--204",
-    year = "2001"
-}
-@article{Arkani-Hamed:1998wuz,
-    author = "Arkani-Hamed, Nima and Dimopoulos, Savas and Dvali, G. R. and March-Russell, John",
-    title = "{Neutrino masses from large extra dimensions}",
-    eprint = "hep-ph/9811448",
-    archivePrefix = "arXiv",
-    reportNumber = "SLAC-PUB-8014, SU-ITP-98-64",
-    doi = "10.1103/PhysRevD.65.024032",
-    journal = "Phys. Rev. D",
-    volume = "65",
-    pages = "024032",
-    year = "2001"
-}
-@article{Ellis:1999my,
-    author = "Ellis, John R. and Lola, Smaragda",
-    title = "{Can neutrinos be degenerate in mass?}",
-    eprint = "hep-ph/9904279",
-    archivePrefix = "arXiv",
-    reportNumber = "CERN-TH-99-87",
-    doi = "10.1016/S0370-2693(99)00545-6",
-    journal = "Phys. Lett. B",
-    volume = "458",
-    pages = "310--321",
-    year = "1999"
-}
-@article{Avignone:2007fu,
-    author = "Avignone, III, Frank T. and Elliott, Steven R. and Engel, Jonathan",
-    title = "{Double Beta Decay, Majorana Neutrinos, and Neutrino Mass}",
-    eprint = "0708.1033",
-    archivePrefix = "arXiv",
-    primaryClass = "nucl-ex",
-    reportNumber = "LA-UR-07-3577",
-    doi = "10.1103/RevModPhys.80.481",
-    journal = "Rev. Mod. Phys.",
-    volume = "80",
-    pages = "481--516",
-    year = "2008"
-}
-@article{Esteban:2020cvm,
-    author = "Esteban, Ivan and Gonzalez-Garcia, M. C. and Maltoni, Michele and Schwetz, Thomas and Zhou, Albert",
-    title = "{The fate of hints: updated global analysis of three-flavor neutrino oscillations}",
-    eprint = "2007.14792",
-    archivePrefix = "arXiv",
-    primaryClass = "hep-ph",
-    reportNumber = "IFT-UAM/CSIC-112, YITP-SB-2020-21",
-    doi = "10.1007/JHEP09(2020)178",
-    journal = "JHEP",
-    volume = "09",
-    pages = "178",
-    year = "2020"
-}
-@unpublished{DUNE:2020ypp,
-    author = "Abi, Babak and others",
-    collaboration = "DUNE",
-    title = "{Deep Underground Neutrino Experiment (DUNE), Far Detector Technical Design Report, Volume II: DUNE Physics}",
-    eprint = "2002.03005",
-    archivePrefix = "arXiv",
-    primaryClass = "hep-ex",
-    reportNumber = "FERMILAB-PUB-20-025-ND, FERMILAB-DESIGN-2020-02",
-    month = "2",
-    year = "2020"
-}
-@article{NuSTEC:2017hzk,
-    author = "Alvarez-Ruso, L. and others",
-    collaboration = "NuSTEC",
-    title = "{NuSTEC White Paper: Status and challenges of neutrino\textendash{}nucleus scattering}",
-    eprint = "1706.03621",
-    archivePrefix = "arXiv",
-    primaryClass = "hep-ph",
-    reportNumber = "FERMILAB-PUB-17-195-ND-T, INT-PUB-17-020",
-    doi = "10.1016/j.ppnp.2018.01.006",
-    journal = "Prog. Part. Nucl. Phys.",
-    volume = "100",
-    pages = "1--68",
-    year = "2018"
-}
-@article{Rafelski:2017hce,
-    author = "Rafelski, Johann and Formanek, Martin and Steinmetz, Andrew",
-    title = "{Relativistic Dynamics of Point Magnetic Moment}",
-    eprint = "1712.01825",
-    archivePrefix = "arXiv",
-    primaryClass = "physics.class-ph",
-    doi = "10.1140/epjc/s10052-017-5493-2",
-    journal = "Eur. Phys. J. C",
-    volume = "78",
-    number = "1",
-    pages = "6",
-    year = "2018"
-}
-@article{Formanek:2021mcp,
-    author = "Formanek, Martin and Steinmetz, Andrew and Rafelski, Johann",
-    title = "{Motion of classical charged particles with magnetic moment in external plane-wave electromagnetic fields}",
-    eprint = "2103.02594",
-    archivePrefix = "arXiv",
-    primaryClass = "physics.class-ph",
-    doi = "10.1103/PhysRevA.103.052218",
-    journal = "Phys. Rev. A",
-    volume = "103",
-    number = "5",
-    pages = "052218",
-    year = "2021"
-}
-@article{Formanek:2020zwc,
-    author = "Formanek, Martin and Steinmetz, Andrew and Rafelski, Johann",
-    title = "{Radiation reaction friction: Resistive material medium}",
-    eprint = "2004.09634",
-    archivePrefix = "arXiv",
-    primaryClass = "hep-ph",
-    doi = "10.1103/PhysRevD.102.056015",
-    journal = "Phys. Rev. D",
-    volume = "102",
-    number = "5",
-    pages = "056015",
-    year = "2020"
-}
\ No newline at end of file