From ccbf3c54cbb43cbaaf79bfb9c60e4beb1f39e0ef Mon Sep 17 00:00:00 2001 From: kbechtol Date: Mon, 4 Mar 2019 09:09:02 +0000 Subject: [PATCH] Update on Overleaf. --- main.bib | 6 +++++ main.tex | 79 ++++++++++++++++++++++++++++++++++++-------------------- 2 files changed, 57 insertions(+), 28 deletions(-) diff --git a/main.bib b/main.bib index 65b2de2..452d182 100644 --- a/main.bib +++ b/main.bib @@ -12548,3 +12548,9 @@ @ARTICLE{drlica-wagner_2019_lsst_dark_matter adsnote = {Provided by the SAO/NASA Astrophysics Data System} } +@article{Gluscevic:prep, + author = {{Gluscevic}, V. and {Nadler}, E.~O. and {Boddy}, K.~K.}, + year = {in prep}, + journal = {~} +} + diff --git a/main.tex b/main.tex index ca516bd..5e18660 100644 --- a/main.tex +++ b/main.tex @@ -74,7 +74,7 @@ %Future observations with the Large Synoptic Survey Telescope (LSST) will provide necessary guidance for the experimental dark matter program. In the coming decade, astrophysical observations will guide other experimental efforts, while simultaneously probing unique regions of dark matter parameter space. This white paper summarizes astrophysical observations that can constrain the fundamental physics of dark matter in the era of LSST. -We discuss how astrophysical observations will inform our understanding of the fundamental properties of dark matter, such as particle mass, self-interaction strength, non-gravitational interactions with the Standard Model, and compact object abundances. Additionally, we discuss experiments and facilities that will complement LSST to strengthen our understanding of the fundamental characteristics of dark matter. +We describe how astrophysical observations will inform our understanding of the fundamental properties of dark matter, such as particle mass, self-interaction strength, non-gravitational interactions with the Standard Model, and compact object abundances. Additionally, we highlight theoretical work and experimental/observational facilities that will complement LSST to strengthen our understanding of the fundamental characteristics of dark matter. %More information on the LSST dark matter effort can be found at \href{https://lsstdarkmatter.github.io/}{https://lsstdarkmatter.github.io/}. \pagebreak @@ -123,12 +123,14 @@ %By leveraging a soon to-exist-facility, a small program with LSST will provide critical information about the fundamental nature of dark matter over the next decade at a low cost. %The study of dark matter with LSST presents a small experimental program that is guaranteed to provide critical information about the fundamental nature of dark matter over the next decade. %LSST will rapidly produce high-impact science on the nature of fundamental dark matter by exploiting a soon-to-exist facility. -Astrophysical dark matter studies will explore parameter space beyond the current sensitivity of the high-energy physics program and will complement to other experimental searches. +Astrophysical dark matter studies will explore parameter space beyond the current sensitivity of the high-energy physics program and will complement other experimental searches. This has been recognized in Astro 2010 \citep{Astro2010}, during the Snowmass Cosmic Frontier planning process \citep[][]{1310.8642, 1310.5662, 1305.1605}, in the P5 Report \citep[]{P5Report}, and in a series of recent Cosmic Visions reports \citep[][]{1604.07626,1802.07216}, including the ``New Ideas in Dark Matter 2017:\ Community Report'' \citep{Battaglieri:2017aum}. %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. -In the 2020s, 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. +In the 2020s, the impact of the LSST dark matter program will be enhanced by access to wide-field massively multiplexed spectroscopy on medium- to large-aperture telescopes ($\roughly 8$--$10$-meter class), deep spectroscopy on giant segmented mirror telescopes ($\roughly 30$-m class), together with high-resolution optical and radio imaging. +%with relatively smaller fields of view +Further theoretical work is also needed to interpret those observations in terms of particle models, to combine results from multiple observational methods, and to develop novel probes of dark matter. This whitepaper is a summary of Drlica-Wagner et al. (2019) \citep{drlica-wagner_2019_lsst_dark_matter}. @@ -141,7 +143,7 @@ \hline \hline Warm Dark Matter & Halo Mass & Particle Mass & $m \sim 18 \keV$ \\ -Self-Interacting Dark Matter & Halo Profile & Cross Section & $\sigmam \sim 0.1\text{--}10\cm^2/\g$ \\ +Self-Interacting Dark Matter & Halo Profile & Cross Section & $\sigmam \sim 0.1\text{--}1\cm^2/\g$ \\ Baryon-Scattering Dark Matter & Halo Mass & Cross Section & $\sigma \sim 10^{-30} \cm^2$ \\ Axion-Like Particles & Energy Loss & Coupling Strength & $g_{\phi e} \sim 10^{-13} $ \\ Fuzzy Dark Matter & Halo Mass & Particle Mass & $m \sim 10^{-20} \eV$ \\ @@ -152,7 +154,7 @@ \end{tabular} \end{center} \vspace{-1em} -\caption{\label{tab:models} Probes of fundamental dark matter physics in the LSST era organized by dark matter model and associated observables. Sensitivity forecasts appear in the rightmost column.} +\caption{\label{tab:models} Probes of fundamental dark matter physics in the LSST era, organized by dark matter model and associated observables. Sensitivity forecasts appear in the rightmost column.} %Probes of fundamental dark matter physics with LSST. The four columns indicate classes of dark matter models, primary observational probe, corresponding dark matter parameters, and the estimated senstivity of LSST.} %Sensitivity forecasts of Probes of fundamental dark matter physics in the LSST era. @@ -162,12 +164,14 @@ \vspace{-1em} \subsection*{Dark Matter Models} \vspace{-0.5em} -Astrophysical observations use gravity to directly probe dark matter. +%Astrophysical observations use gravity to directly probe dark matter. +Astrophysical observations probe the physics of dark matter through its +impact on structure formation throughout cosmic history. On large scales, current observational data are well described by a simple model of stable, non-relativistic, collisionless, cold dark matter (CDM). However, many viable theoretical models of dark matter predict deviations from CDM that are testable with current and future observations. -Fundamental properties of dark matter---e.g., particle mass, self-interaction cross section, coupling to the Standard Model, and time-evolution---can imprint themselves on the macroscopic distribution of dark matter in a detectable manner. LSST will be sensitive to several distinct classes of dark matter models, including particle dark matter, field dark matter, and compact objects (\tabref{models}). +Fundamental properties of dark matter---e.g., particle mass, self-interaction cross section, coupling to the Standard Model, and time evolution---can imprint themselves on the macroscopic distribution of dark matter in a detectable manner. With supporting theoretical efforts and follow-up observations, LSST will be sensitive to several distinct classes of dark matter models, including particle dark matter, field dark matter, and compact objects (\tabref{models}). -\noindent \textbf{Particle Dark Matter:} LSST, in combination with other observations, will be able to probe microscopic characteristics of particle dark matter such as self-interaction cross section, particle mass, baryon-scattering cross section, self-annihilation rate, and decay rate. These measurements will complement and guide experimental efforts to probe particle dark matter. +\noindent \textbf{Particle Dark Matter:} LSST, in combination with other observations, will be able to probe microscopic characteristics of particle dark matter such as self-interaction cross section, particle mass, baryon-scattering cross section, self-annihilation rate, and decay rate. These measurements will complement and guide collider, direct, and indirect detection efforts to study particle dark matter. %Minimum halo mass, halo profiles, compact object abundance, anomalous energy loss mechanisms, and large-scale structure. @@ -196,12 +200,12 @@ By identifying additional stellar streams and increasing the density contrast of known streams against the smooth Milky Way halo, LSST will shift analysis from individual gaps into the regime of subhalo population statistics and (in)consistency with cold dark matter predictions. Importantly, LSST will allow studies of streams farther from the center of the Galaxy for which confounding baryonic effects are lessened. %LSST will mitigate both of these issues by examining streams farther from the center of the Galaxy where these effects are lessened. -Meanwhile, strong gravitational lensing can be used to measure the abundance and masses of subhalos in massive galaxies and small isolated halos along the line-of-sight at cosmological distances, independent of their baryon content. +Meanwhile, strong gravitational lensing can be used to measure the abundance and masses of subhalos in massive galaxies and small isolated halos along the line of sight at cosmological distances, independent of their baryon content. LSST will increase the number of lensed systems from the current sample of hundreds to an expected sample of thousands of lensed quasars \citep{O+M10} and tens of thousands of lensed galaxies \citep{Collett2015}. %Through analysis of flux ratio anomalies, gravitational imaging, and measuring the power spectrum of \noindent {\bf Halo Profiles:} -Measurements of the radial density profiles and shapes of dark matter halos are sensitive to the microphysics governing non-gravitational dark matter self-interactions, which could produce flat density cores \citep{Spergel:1999mh} and more spherical halo shapes \citep{Peter:2013} +Measurements of the radial density profiles and shapes of dark matter halos are sensitive to the microphysics governing non-gravitational dark matter self-interactions, which could produce flat density cores \citep{Spergel:1999mh} and more spherical halo shapes \citep{Peter:2013}. %Dwarf galaxies, galaxy clusters, merging clusters. Through galaxy-galaxy weak lensing, LSST will be able to distinguish cored versus cuspy NFW density profiles for a sample of low-redshift dwarf galaxies with masses $M_\text{halo} = 3\times10^9\,h^{-1}\Msun$. Studies of the density profiles of massive galaxy clusters, as well as systems of merging galaxy clusters, will constrain the scattering cross section at the level $\sigmam \sim 0.1-1 \cmg$. @@ -222,14 +226,14 @@ \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. Measurements of large-scale structure with LSST will enhance constraints on massive neutrinos and other light relics from the early universe that could compose a fraction of the dark matter. -Additionally, LSST will use SN and $3\times2$pt galaxy clustering to measure dark energy in independent patches across the sky, allowing for spatial cross correlation between dark matter and dark energy \citep{0902.2590}. +Additionally, LSST will use supernovae and $3\times2$pt galaxy clustering and weak lensing to measure dark energy in independent patches across the sky, allowing for spatial cross correlation between dark matter and dark energy \citep{0902.2590}. \begin{figure}[t] \centering \includegraphics[width=0.53\columnwidth]{figures/SIDM_WDM_figw_coll.pdf} \includegraphics[width=0.46\columnwidth]{figures/WDM_SIDM_discovery_test.pdf} \caption{\emph{Left}: Projected joint sensitivity to WDM particle mass and SIDM cross section from LSST observations of dark matter substructure. -\emph{Right}: Example of a measurement of particle properties for a dark matter model with a self-interaction cross section and matter power spectrum cut-off just beyond current constraints ($\sigmam = 2 \cmg$ and $\mWDM = 6\keV$, indicated by the red star).} +\emph{Right}: Example of a measurement of particle properties for a dark matter model with a self-interaction cross section and matter power spectrum cut-off just beyond current constraints ($\sigmam = 2 \cmg$ and $\mWDM = 6\keV$, indicated by the red star) \citep{drlica-wagner_2019_lsst_dark_matter}.} \end{figure} %\begin{figure}[t] @@ -265,13 +269,17 @@ \vspace{-1em} \subsection*{Complementarity} \vspace{-0.5em} %While LSST is the discovery engine, many other complementary observations are required to realize the astrophysical dark matter program. -LSST discoveries will enable complementary studies of dark matter with spectroscopy, high-resolution imaging, indirect detection experiments, and direct detection experiments. -While LSST can substantially improve our understanding of dark matter in isolation, the combination of experiments is essential to provide a holistic picture of dark matter physics. +LSST will enable complementary studies of dark matter with spectroscopy, high-resolution imaging, indirect detection experiments, and direct detection experiments. +While LSST can substantially improve our understanding of dark matter in isolation, the combination of experiments is essential to confirm future discoveries and provide a holistic picture of dark matter physics. +%the combination of experiments is essential to provide a holistic picture of dark matter physics. + + \noindent {\bf Spectroscopy:} -Wide field-of-view, massively multiplexed spectroscopy on 8--10-meter-class telescopes and smaller field-of-view deep spectroscopy with 30-meter-class telescopes will complement studies of minimum halo mass and halo profiles. +Wide field-of-view, massively multiplexed spectroscopy on 8--10-meter-class telescopes as well as deep spectroscopy with 30-meter-class telescopes will complement studies of minimum halo mass and halo profiles. +% smaller field-of-view -\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 High-Resolution Imaging:} High-resolution follow-up imaging at the milliarcsecond-scale from space and with ground-based adaptive optics are needed to maximize 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:2017,1404.5503}. LSST will also provide sensitivity to axion-like particles via monitoring extreme events in the transient sky \citep{2017PhRvL.118a1103M}. @@ -283,7 +291,7 @@ \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. +For dark matter-baryon scattering, large-scale structure measurements with LSST can probe dark matter masses and cross sections outside the range accessible to direct detection experiments. %\vspace{-1em} \subsection*{Outlook: Discovery Potential} \vspace{-0.5em} @@ -302,7 +310,7 @@ %The projected LSST Milky Way (MW) microlensing and paralensing constraints are from a Monte Carlo analysis where lenses were injected into light curves based on LSST OpSim cadence simulations %% (see \url{https://github.com/lsstdarkmatter/dark-matter-paper/issues/8} for details). %The paralensing constraint comes from assuming that only the secondary microlensing parallax signal is used for discovery, and not the primary heliocentric microlensing signal. - \emph{Right}: Constraints on dark matter-baryon scattering through a velocity-independent, spin-independent contact interaction with protons from existing constraints (blue and gray) and projections for LSST observations of Milky Way satellite galaxies (gold). + \emph{Right}: Constraints on dark matter-baryon scattering through a velocity-independent, spin-independent contact interaction with protons from existing constraints (blue and gray) and projections for LSST observations of Milky Way satellite galaxies (gold) \citep{drlica-wagner_2019_lsst_dark_matter,Gluscevic:prep}. %Existing constraints are shown in blue and gray. %Existing constraints (shown in blue) include measurements of the CMB power spectrum \citep[CMB;][]{Gluscevic:2017ywp} and constraints from the X-ray Quantum Calorimeter experiment \citep[XQC;][]{0704.0794}. Direct detection constraints include results from CRESST-III \citep{1711.07692}, the CRESST 2017 surface run \citep{1707.06749}, and XENON1T \citep{1705.06655}, as interpreted by \citet[][]{1802.04764}. %\citep{2018PhRvD..97l3013K}. %Additional constraints that include the effects of cosmic-ray heating of dark matter are shown in gray \citep[][]{1810.10543}. @@ -312,21 +320,35 @@ \vspace{-1em} \subsection*{Recommendations for Astro 2020} \vspace{-0.5em} -LSST is scheduled to begin a decade of science operation in 2022; however, science with LSST is currently unfunded. -We therefore make the following recommendations to facilitate the dark matter science goals outlined here: +LSST is scheduled to begin a decade of science operation in 2022; however, dark matter research with LSST is not yet funded. +Recognizing new opportunities created by LSST to constrain a range of dark matter models, we make the following recommendations to facilitate this science case: +%to facilitate the dark matter science goals outlined here: %and in Drlica-Wagner et al. (2019)\citep{drlica-wagner_2019_lsst_dark_matter}: -\setlist{nolistsep} -\begin{itemize}[noitemsep] +%\setlist{nolistsep} +%\begin{itemize}[noitemsep] +\begin{itemize} - \item (Funding agencies should) Support individual PIs and collaborative teams to analyze LSST data for dark matter science. %, leveraging the statistical power of LSST, and developing new techniques in image analysis, time-domain analysis, object classification, etc. + % (Funding agencies should) + \item Support individual PIs and collaborative teams to analyze LSST data for dark matter science. %, leveraging the statistical power of LSST, and developing new techniques in image analysis, time-domain analysis, object classification, etc. %, to enhance sensitivity - \item (Funding agencies should) Support associated theoretical research to better understand the galaxy-halo connection, investigate novel signatures of dark matter microphysics, study confounding baryonic effects, etc. + %(Funding agencies should) + \item Support associated theoretical research to better understand the galaxy-halo connection, examine confounding baryonic effects, perform joint analyses of cosmological probes, investigate novel signatures of dark matter microphysics, and strengthen ties with the particle physics community. + %This work will likely involve dedicated numerical simulation activities. - \item (Funding agencies should) Support other complementary facilities to investigate dark matter, including spectroscopic follow-up, high-resolution imaging, joint-analysis of cosmological datasets, numerical simulations, etc. + % (Funding agencies should) + \item Support complementary observational facilities to investigate dark matter, including spectroscopic follow-up and high-resolution imaging, as well as multiwavelength analyses. + %, as well as theoretical activities including joint-analysis of cosmological datasets and numerical simulations. + %, as well as coordination of these efforts. % assemble into a cohesive community - \item (Scientists) The astrophysical dark matter community should congeal around a common language, and build stronger connections with particle physics efforts. + % The dark matter community should strive to present results in a manner that encourages... + %\item (Scientists) The astrophysical dark matter community should converge around a common language, and build stronger connections with particle physics efforts. + + %\item (Scientists) + % Recognizing opportunities to enhance sensitivity and mitigate systematic uncertainty through the use fo joint probes, + %The astrophysical dark matter community should strive to present results in ways that facilitate comparison between multiple probes and between theory and experiment. + %The astrophysics and particle physics dark matter community should strive to present results in ways that facilitate comparison between multiple astrophysical probes and between theory and experiment. %\item (Scientists) The LSST dark matter science community should maintain/expand opportunities for collaboration. (This could mean finding a home within an existing Science Collaboration, forming a new collaboration, and/or establish strong connections between science collaborations. A key point is consistency between probes.) @@ -334,8 +356,9 @@ \end{itemize} -\noindent The multi-faceted LSST data will allow novel probes of dark matter physics that have yet to be considered. -New ideas are especially important as the absence of evidence for the most popular dark matter candidates continues to grow. +\noindent We anticipate that the multi-faceted LSST data will allow further probes of dark matter physics that have yet to be considered. +New ideas are especially important as searches for the most popular dark matter candidates gain in sensitivity while lacking a positive detection. +%the absence of evidence for the most popular dark matter candidates continues to grow. As the particle physics community seeks to diversify the experimental effort to search for dark matter, it is important to remember that astrophysical observations provide robust, empirical measurement of fundamental dark matter properties. In the coming decade, astrophysical observations will guide other experimental efforts, while simultaneously probing unique regions of dark matter parameter space.