Update on Overleaf.

complementarity/complementarity.tex

@@ -31,7 +31,7 @@ \subsection{Milky Way Dwarfs \Contact{Josh}}
 
 Spectroscopy of individual stars in the faint Milky Way satellites that will be identified with LSST will require deep observations with multiplexed spectrographs on large telescopes.  Measurements of the stellar velocity dispersions of these systems can be obtained either with 8-10~m-class telescopes or with the next generation of 25-30~m telescopes.  As illustrated in Fig.~\ref{fig:specfollowup_distance}, spectroscopy of a nearly complete sample of satellites can be pushed $\sim2$~mag fainter in luminosity and a factor of $\sim2$ farther in distance with plausible investments of observing time on a GSMT than with existing facilities.
 
-In additional to inferring the minimum dark matter halo mass, kinematics from stellar spectroscopy can also reveal the density profile of the dwarf galaxies at the lowest luminosities, in which the baryonic effects are minimum and therefore dark matter physics can be separated from the astrophysics of galaxy formation (cite). A direct measurement of the density profile in these dwarf galaxies will allow us to distinguish between collisionless CDM  which predicts a cusp NFW profile, and SIDM which predicts a core profile (cite). Moreover, the stellar kinematics will also reveal the integral of the dark matter density profile in the dwarf galaxy (or J-factor), which is an essential input for the constraints on the dark matter self-annihilation cross section for the indirect dark matter search in X-ray and gamma-ray experiments \citep[e.g.][]{1108.3546}.
+In additional to inferring the minimum dark matter halo mass, kinematics from stellar spectroscopy can also reveal the density profile of the dwarf galaxies at the lowest luminosities, in which the baryonic effects are minimum and therefore dark matter physics can be separated from the astrophysics of galaxy formation \citep{governato2012,read2017}. \AHGP{Problem: Justin read shows that density profile measurement requires about a thousand stars.  It's (relatively) easy to get a central density, hard to do a profile.} A direct measurement of the density profile in these dwarf galaxies will allow us to distinguish between collisionless CDM  which predicts a cusp NFW profile, and SIDM which predicts a core profile \citep{Rocha:2012jg,2012MNRAS.423.3740V}. Moreover, the stellar kinematics will also reveal the integral of the dark matter density profile in the dwarf galaxy (or J-factor), which is an essential input for the constraints on the dark matter self-annihilation cross section for the indirect dark matter search in X-ray and gamma-ray experiments \citep[e.g.][]{1108.3546}.
 
 
 \begin{comment}
@@ -71,7 +71,7 @@ \subsection{Galaxy Clusters \Contact{Will}}
 \Contributors{Will, ...}
 As noted in \S\ref{sec:merging_clusters} one of largest systematics associated with merging galaxy cluster constraints of SIDM is modeling the merger. The more complex the merger the more severe the systematics.
 The best means of constraining merging galaxy cluster substructure is with spectroscopic measurement of as many galaxy cluster member galaxies as possible \cite[see e.g.,][]{2018arXiv180610619G}.
-As noted in \cite{2016arXiv161001661N}, perhaps the best spectroscopic follow-up facilities are large telescopes with slitmask-like multi-object spectrometers, or fiber-based multiplex spectrometers with low ($\mathcal{O}(arcsec)$) fiber collision regions, due to the density of cluster members.
+As noted in \cite{2016arXiv161001661N}, perhaps the best spectroscopic follow-up facilities are large telescopes with slitmask-like multi-object spectrometers, or fiber-based multiplex spectrometers with low ($\mathcal{O}(\hbox{arcsec})$) fiber collision regions, due to the density of cluster members.
 
 \begin{comment}
 \subsection{Lyman-$\alpha$ Forest \Contact{Francis-Yan}}
@@ -92,7 +92,7 @@ \subsection{Astrometric Microlensing of Compact Dark Matter \Contact{Will}}
 \label{sec:astrometric_microlens}
 Related to photometric microlensing (\S\ref{sec:microlensing}), astrometric microlensing relies on the fact that the two images generated during a compact object lensing event will be of differing brightness, and the brightness ratio of these two images will vary throughout the duration of the lensing event.
 The two images will be of most similar brightness when the projected lens-source separation is at its minimum.
-By precisely measuring the astrometry of these blended images as a function of time and combining with the LSST photometric microlensing measurement one can break the lens mass-distance degeneracy and precisely measure the mass and location of individual black holes \cite{2015ApJ...814L..11Y}.
+By precisely measuring the astrometry of these blended images as a function of time and combining with the LSST photometric microlensing measurement one can break the lens mass-distance degeneracy and precisely measure the mass and location of individual black holes \citep{2015ApJ...814L..11Y}.
 
 % Strong-microlensing
 \subsection{Strong-Microlensing of Compact Dark Matter \Contributors{Will, ...}}
@@ -156,7 +156,7 @@ \subsection{Baryon Scattering \Contact{Vera}}
 
 Current null results from targeted laboratory searches motivate broad scans of parameter space that is inaccessible to underground experiments. Cosmological and astrophysical observables provide such a complementary search strategy. In particular, they are sensitive to scattering of sub-GeV particles with baryons at any point in cosmic history. Furthermore, there is no upper boundary on the interaction cross section they can probe. Finally, they are not subject to the uncertainty on local astrophysical properties of dark matter particles (their phase-space distribution), which affects the inferred limits on the particle properties of dark matter. 
 
-If dark matter particles scatter with baryons, they transfer momentum between the two cosmological fluids, affecting density fluctuations and suppressing power at small scales; the power suppression can be captured by a variety of observables. The current limits come from the CMB \citep{Gluscevic:2017ywp}, cosmic-ray \citep{Cappiello:2018hsu}, and Lyman-$\alpha$ forest measurements \cite{Xu:2018efh}. For illustration, Figure \ref{fig:dd} compares currently excluded regions of dark matter parameter space, from analyses of Planck data, and from null results of various direct-detection searches.\footnote{We caution the reader that this is not a comprehensive list of current upper limits, but only serves to illustrate complementarity of cosmological and direct detection probes.} LSST will deliver state-of-the-art measurements of observables that trace matter fluctuations on a range of smaller scales, extending the sensitivity of astrophysical and cosmological searches far beyond the reach of Planck.
+If dark matter particles scatter with baryons, they transfer momentum between the two cosmological fluids, affecting density fluctuations and suppressing power at small scales; the power suppression can be captured by a variety of observables. The current limits come from the CMB \citep{Gluscevic:2017ywp}, cosmic-ray \citep{Cappiello:2018hsu}, and Lyman-$\alpha$ forest measurements \citep{Xu:2018efh}. For illustration, Figure \ref{fig:dd} compares currently excluded regions of dark matter parameter space, from analyses of Planck data, and from null results of various direct-detection searches.\footnote{We caution the reader that this is not a comprehensive list of current upper limits, but only serves to illustrate complementarity of cosmological and direct detection probes.} LSST will deliver state-of-the-art measurements of observables that trace matter fluctuations on a range of smaller scales, extending the sensitivity of astrophysical and cosmological searches far beyond the reach of Planck.
 
 \subsection{Local Dark Matter Velocity Distribution \Contact{Lina}}
 \Contributors{Lina N.}

endorsers.tex

@@ -105,7 +105,7 @@
 \affil{$^{11}$ Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, 02138}
 \affil{$^{12}$ Department of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON, M5S 3H4, Canada}
 \affil{$^{13}$ Department of Physics and Astronomy, Rutgers University}
-\affil{$^{14}$ Center for Astrophysics | Harvard & Smithsonian}
+\affil{$^{14}$ Center for Astrophysics | Harvard \& Smithsonian}
 \affil{$^{15}$ NASA Goddard Space Flight Center}
 \affil{$^{16}$ Department of Astronomy and Astrophysics, University of Chicago, IL 60637, USA}
 \affil{$^{17}$ Kavli Institute of Cosmological Physics, University of Chicago, IL 60637, USA}

main.bib

@@ -6449,6 +6449,20 @@ @article{Buote:2002wd
 	Year = {2002},
 	Bdsk-Url-1 = {http://dx.doi.org/10.1086/342158}}
 
+@ARTICLE{goldstein2018,
+   author = {{Goldstein}, D.~A. and {Nugent}, P.~E. and {Goobar}, A.},
+    title = "{Rates and Properties of Strongly Gravitationally Lensed Supernovae and their Host Galaxies in Time-Domain Imaging Surveys}",
+  journal = {arXiv e-prints},
+archivePrefix = "arXiv",
+   eprint = {1809.10147},
+ keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
+     year = 2018,
+    month = sep,
+   adsurl = {http://adsabs.harvard.edu/abs/2018arXiv180910147G},
+  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
+}
+
+
 
 @article{Kahlhoefer:2015vua,
 	Archiveprefix = {arXiv},
@@ -7276,6 +7290,24 @@ @article{Oguri:2010
  year = {2010}
 }
 
+@ARTICLE{read2017,
+   author = {{Read}, J.~I. and {Steger}, P.},
+    title = "{How to break the density-anisotropy degeneracy in spherical stellar systems}",
+  journal = {\mnras},
+archivePrefix = "arXiv",
+   eprint = {1701.04833},
+ keywords = {methods: miscellaneous, proper motions, globular clusters: general, galaxies: clusters: general, galaxies: haloes, dark matter},
+     year = 2017,
+    month = nov,
+   volume = 471,
+    pages = {4541-4558},
+      doi = {10.1093/mnras/stx1798},
+   adsurl = {http://adsabs.harvard.edu/abs/2017MNRAS.471.4541R},
+  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
+}
+
+
+
 @ARTICLE{read2018,
    author = {{Read}, J.~I. and {Walker}, M.~G. and {Steger}, P.},
     title = "{Dark matter heats up in dwarf galaxies}",

models/particles.tex

@@ -152,7 +152,7 @@ \subsection{Baryon-Scattering Dark Matter (BSDM) \Contact{Vera}}
 
 \begin{figure}
 \centering
-\includegraphics[width=0.6\columnwidth]{figures/dmbaryon_pk2.png}.png}
+\includegraphics[width=0.6\columnwidth]{figures/dmbaryon_pk2.png}
 \caption{Linear matter power spectrum at $z=0$. We show the residuals between the CDM case and the case where there is velocity-independent spin-independent scattering between dark matter and protons. The dark matter particle mass is set to 1 MeV, and all other cosmological parameters are set to their best-fit Planck 2015 values \citep{Ade:2015xua}. Different residual curves display cutoffs at different angular scales, controlled by the magnitude of the interaction cross section. The highest cross section shown corresponds to the current 95\% confidence-level upper limit inferred from analyses of CMB data \citep{Gluscevic:2017ywp,Boddy:2018kfv}.
 \ADW{I think we need a better version of this figure.}
 }