bib

exec-sum.tex

@@ -21,7 +21,7 @@
 The study of dark matter with LSST presents a small experimental program with a short timescale and low cost 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 fundamental dark matter physics by exploiting an existing US facility. 
 The study of dark matter with LSST explores dark matter parameter space beyond the high-energy physics program's current sensitivity, while being highly complementary to other experimental searches. % BRN text.
-This has been recognized during the Snowmass Cosmic Frontier planning process \citep[\eg,][]{1305.1605, 1310.8642, 1310.5662} and in a series of more recent Cosmic Visions reports \citep[\eg,][]{1604.07626,1802.07216}, including the ``New Ideas in Dark Matter 2017:\ Community Report'' \citep{1707.04591}.
+This has been recognized during the Snowmass Cosmic Frontier planning process \citep[\eg,][]{1305.1605, 1310.8642, 1310.5662} and in a series of more recent Cosmic Visions reports \citep[\eg,][]{1604.07626,1802.07216}, including the ``New Ideas in Dark Matter 2017:\ Community Report'' \citep{Battaglieri:2017aum}.
 It is worth remembering that astrophysical probes provide the only constraints on the minimum and maximum mass-scale of dark matter, and it is likely that astrophysical observations will continue to guide the  experimental particle physics program for years to come.
 
 \clearpage

models/machos.tex

@@ -13,7 +13,7 @@ \section{Compact Objects \Contact{Simeon}}
 Compact object dark matter is fundamentally different from particle models; black holes cannot be formed in an accelerator and can only be detected through their gravitational force. Current constraints suggest that primordial black holes do not make up all of the dark matter. However, primordial black holes are one possible source of the merging $30 M_\odot$ black holes recently detected by LIGO \citep{Bird:2016,Clesse:2016}. This possibility has rekindled interest in these objects, both as a source of dark matter and in their own right.
 
 Limits on the abundance and mass range of primordial black holes are wholly observational. The black hole mass is set by the mass enclosed within the horizon at the time of black hole collapse and thus ranges between $10^{15}$ g ($10^{-18} M_\odot$), below which the black hole would evaporate, to $10^{42}$ g  ($10^9 M_\odot$), above which structure formation, big bang nucleosynthesis and the formation of the microwave background would be severely affected \citep{Sasaki:2018}. 
-For $\sim $ stellar mass black holes, the gold standard technique for detecting compact objects is microlensing. Current microlensing constraints set limits on the black hole abundance at the level of $10\%$ for black holes $0.01 - 10 M_\odot$, see however \citep{Calcino:2018}. LSST will revolutionize the astrometric microlensing technique,  constraining the abundance of primordial black holes to a level of $10^{-4}$ of the dark matter over a wide range of masses (see Section \secref{compact_objects}).
+For $\sim $ stellar mass black holes, the gold standard technique for detecting compact objects is microlensing. Current microlensing constraints set limits on the black hole abundance at the level of $10\%$ for black holes $0.01 - 10 M_\odot$, see however \citep{2018MNRAS.479.2889C}. LSST will revolutionize the astrometric microlensing technique,  constraining the abundance of primordial black holes to a level of $10^{-4}$ of the dark matter over a wide range of masses (see Section \secref{compact_objects}).
 
 As primordial black holes form directly from the primordial density fluctuations, measuring their abundance is a direct constraint on the amplitude of density fluctuations \citep{Clesse:2015}. Although these constraints are several orders of magnitude weaker than, for example, those from the microwave background, they probe small scales between $k = 10^{7} - 10^{19}$ $h$/Mpc, much smaller than those measured by other current and future probes \citep{Bringmann:2012}. Because these scales are highly non-linear in the late-time universe, there is no other possible constraint; the information present at early times has been washed away by gravitational evolution. Primordial black holes are thus a probe of primordial density fluctuations in a range that is inaccessible to other techniques\citep{Bellido:2017}.
 
@@ -22,7 +22,7 @@ \section{Compact Objects \Contact{Simeon}}
 
 %For example, the long lever of scales means that the constraints on simple scale-invariant inflation models expressed in terms of a scalar index, $n_s$ and a running, $\alpha_s$ can be competitive for some models. 
 
-Furthermore, it may be possible for LSST to constrain the existence of ultra-compact mini-halos using correlated microlensing signals \citep{erickcek2011,li2012}. These objects arise from initial overdensities not large enough to collapse to a primordial black hole. These overdensities still collapse at high redshift to form low-mass halos. As these objects form early and have few mergers \citep{Bringmann:2011ut,Delos:2018}, they have a high concentration and a steeper internal density profile than the standard Navarro-Frenk-White shape, making them easier to detect via lensing and harder to disrupt than standard subhalos.
+Furthermore, it may be possible for LSST to constrain the existence of ultra-compact mini-halos using correlated microlensing signals \citep{erickcek2011,li2012}. These objects arise from initial overdensities not large enough to collapse to a primordial black hole. These overdensities still collapse at high redshift to form low-mass halos. As these objects form early and have few mergers \citep{Bringmann:2012t,Delos:2018}, they have a high concentration and a steeper internal density profile than the standard Navarro-Frenk-White shape, making them easier to detect via lensing and harder to disrupt than standard subhalos.
 
 Current constraints on these objects are highly model-dependent; they come from assuming a WIMP dark matter annihilation cross-section and counting gamma-ray photons. LSST would place wholly new constraints on the existence of small halos from micro-lensing, and thus constrain the physics of the inflaton on scales of $k = 10 - 10^7 $ h/Mpc for the first time in a model-independent way.