Merge branch 'master' of https://git.overleaf.com/5c58622e98873812604…

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main.tex

@@ -119,11 +119,11 @@ \subsection*{Summary}
 %Astrophysical probes provide the only constraints on the minimum and maximum mass scale of dark matter, and 
 %Astrophysical observations will likely continue to guide other experimental efforts.
 %the experimental particle physics program for years to come.
-The impact of the LSST dark matter program will be enhanced by access to massively multiplexed spectroscopy on medium- to large-aperture telescopes ($\roughly 8–10$-meter class), and giant segmented mirror telescopes ($\roughly 30$-m class) with relatively smaller fields of view, together with high-resolution optical and radio imaging.
+The impact of the LSST dark matter program will be enhanced by access to massively multiplexed spectroscopy on medium- to large-aperture telescopes ($\roughly 8$--$10$-meter class), and giant segmented mirror telescopes ($\roughly 30$-m class) with relatively smaller fields of view, together with high-resolution optical and radio imaging.
 
 This whitepaper is a summary of Drlica-Wagner et al. (2019) \citep{drlica-wagner_2019_lsst_dark_matter}.
 
-\begin{table}[h]
+\begin{table}[ht]
 \footnotesize
 \begin{center}
 \begin{tabular}{l c c c}
@@ -202,8 +202,8 @@ \subsection*{Dark Matter Probes}
 
 
 \noindent {\bf Anomalous Energy Loss:}
-Observations of stars provide a mechanism to probe temperatures, particle densities, and time scales that are inaccessible to laboratory experiments. Since conventional astrophysics allows us to quantitatively model the evolution of stars, the detailed study of stellar populations can provide a powerful technique to probe new physics. In particular, if new light particles exist and are coupled to Standard Model fields, their emission would provide an additional channel for energy loss. 
-LSST will greatly improve our understanding of stellar evolution by providing unprecedented photometry, astrometry, and temporal sampling for a large sample of faint stars. In particular, measurements of the white dwarf luminosity function, giant branch styles, and core-collapse supernovae.
+Observations of stars provide a mechanism to probe temperatures, particle densities, and time scales that are inaccessible to laboratory experiments. Since conventional astrophysics allows us to quantitatively model the evolution of stars, detailed study of stellar populations can provide a powerful technique to probe new physics. In particular, if new light particles exist and are coupled to Standard Model fields, their emission would provide an additional channel for stellar energy loss. 
+LSST will greatly improve our understanding of stellar evolution by providing unprecedented photometry, astrometry, and temporal sampling for a large sample of faint stars. In particular, measurements of the white dwarf luminosity function, giant branch stars, and core-collapse supernovae will provide sensitivity to the axion-electron coupling.
 
 \noindent {\bf Large-Scale Structure:} LSST will produce the largest and most detailed map of the distribution of matter and the growth of cosmic structure over the past 10 Gyr.
 The large-scale clustering of matter and luminous tracers in the late-time universe is sensitive to the total amount of dark matter, the fraction of dark matter in light relics that behave as radiation at early times, and fundamental couplings between dark matter and dark energy.
@@ -259,13 +259,16 @@ \subsection*{Complementarity}
 
 \noindent {\bf High-Resolution Imaging:} High-resolution imaging at the milliarcsecond-scale from space and with ground-based adaptive optics will benefit strong lensing, microlensing, and galaxy cluster studies with LSST.
 
-\noindent {\bf Indirect Detection:} By precisely mapping the distribution of dark matter on Galactic and extragalactic scales, LSST will enable more sensitive searches for energetic particles created by dark matter annihilation and/or decay, e.g., using gamma-ray or neutrino telescopes \citep{Charles:2016,Albert:2017}.
+\noindent {\bf Indirect Detection:} By precisely mapping the distribution of dark matter on Galactic and extragalactic scales, LSST will enable more sensitive searches for energetic particles created by dark matter annihilation and/or decay, e.g., using gamma-ray or neutrino telescopes \citep{Charles:2016,Albert:2017,1404.5503}.
+LSST will also provide sensitivity to axion-like particles via monitoring extreme events in the transient sky \citep{2017PhRvL.118a1103M}.
+
 %Leading constraints on the dark matter annihilation cross section come from gamma-ray analysis of Milky Way satellite galaxies.
 %originating from the dark sector.
-% KB: What is meant by "extreme events"
+% KB: What is meant by "extreme events". Maybe a separate sentence?
 %and tracking extreme events 
 
-\noindent {\bf Direct Detection:}  LSST will complement direct detection experiments by improving measurements of the local phase-space density of dark matter.
+
+\noindent {\bf Direct Detection:} LSST will complement direct detection experiments by improving measurements of the local phase-space density of dark matter using precision astrometry of Milky Way stars.
 Large-scale structure measurements with LSST can probe dark matter masses and cross sections outside the range accessible to direct detection experiments.
 
 \subsection*{Outlook: Discovery Potential}