text:
\section{Introduction}

In an expanding cosmology, a particle's trajectory depends not only on its initial velocity, but also on the dynamical evolution of nearby structure.  The meaning of ``unbound'' in this case is both nontrivial and physically interesting.  Traditionally, this word describes particles which can escape to arbitrarily large distances from their initial host dark matter halo.  We investigate the basic demographics of unbound dark matter by tracing particle trajectories in cosmological simulations.  In addition, we also investigate traditional unbound particle classification techniques based on kinetic energies.

While intellectual curiosity motivated this work, there are many practical implications.  For example, we find that the fractional abundance of high-energy dark matter particles depends strongly on halo environment; e.g., the distance to the nearest larger halo.  This suggests that the velocity distribution of dark matter depends on halo environment, which is important for dark matter direct detection experiments \citep{XENON100,CRESST,DAMA,COGENT,CDMS,Mao12,Lisanti11,PS1,PS2,PS3,PS4,PS5,PS6,PS7}.  We therefore test the expected effect from Andromeda on the Milky Way's dark matter velocity distribution directly.

Dark matter particle trajectories also have an effect on the baryon fraction in halos.  When a high-energy dark matter particle leaves the virial radius, the virial mass of the halo is lowered.  The hot halo gas will expand adiabatically in the reduced potential, nominally leaving the hot gas fraction unchanged.  However, the centrally-concentrated stars will not be able to expand, meaning that the overall baryon fraction will increase.  This effect will result in a redshift- and halo-mass-dependent baryon fraction.  Of course, the true picture is made more complicated by a number of effects, including angular momentum exchange, gas cooling, and galaxy feedback.  Nonetheless, it is possible to make a straightforward estimate of its magnitude. In the future, constraining this effect may be important for surveys which aim to place precision constraints on cosmology (e.g., BOSS, DES, BigBOSS, Pan-STARRS, eRosita, Herschel, Planck, JWST, and LSST; \cite{BOSS,DES,BigBOSS,Pan-STARRS,eROSITA,Herschel,Planck,JWST,LSST}).  In order to fully realize their statistical power, these surveys depend on precision calibrations of the halo mass function to 1\% or better accuracy \cite{Wu10,Cunha10}.

Observations of intergalactic supernovae \citep{Sharon10,Sand11,Barbary12} relate to unbound particles, especially observations of supernovae traveling at high speeds \citep{GalYam03} and hostless gamma-ray bursts (GRBs) \cite{Fong13}.  Such escaping objects might either come from the intracluster stellar population \citep{Monaco06,Barbary12}, from merging events \citep{Murante07,Teyssier09}, or from hypervelocity stars ejected from the central galaxy \citep{Napiwotzki11}.  Since stars are effectively collisionless and so evolve dynamically like dark matter particles, one can place upper limits on the fraction of supernova and GRB progenitors ejected through merger events.

In \S \ref{s:methods}, we discuss the dark matter simulations we employ as well as the halo finder and conventions used for calculating kinetic and potential energies.  We discuss unique qualitative features of unbound particles in \S \ref{s:energy} and derive kinetic escape thresholds; we also test how well kinetic escape thresholds can classify unbound particles in full cosmological simulations.  We present the main results for the population of unbound particles in \S \ref{s:results} and discuss how these results impact the science considerations above in \S \ref{s:discussion}.  Finally, we summarize our conclusions in \S \ref{s:conclusions}.  We use simulations with multiple cosmologies in this work, but our primary results assume a flat, $\Lambda$CDM cosmology with main parameters $\Omega_b = 0.04$, $\Omega_M = 0.27$, $\Omega_\Lambda = 0.73$, and $h = 0.7$.  All halo masses at $a\le1$ are defined using the virial overdensity criterion \cite{mvir_conv}.

\section{Methods and Conventions}

\label{s:methods}

\subsection{Simulation}

The primary simulation used is a large (1 Gpc $h^{-1}$ on a side) collisionless dark matter volume run from early redshifts ($a=0.02$) to the far future ($a=100$) using \textsc{gadget}-2 \citep{Springel05}.  This simulation traces $1024^3$ particles, with a particle mass resolution of $10^{11}M_{\odot}$ and a spline force softening of $30$ kpc $h^{-1}$.  This makes it ideal for particle studies from group-scale halos ($10^{13.6}M_{\odot}$, 400 particles) to massive clusters ($10^{15}M_{\odot}$, 10000 particles).  The initial conditions were generated from a flat, $\Lambda$CDM cosmology ($\Omega_M = 0.27$, $\Omega_\Lambda = 0.73$, $h = 0.7$, $\sigma_8 = 0.79$, and $n_s = 0.95$), which is similar to the WMAP7 best-fit cosmology \citep{wmap7}.  From this simulation, 300 snapshots were saved from $a=0.075$ to $a=100$, spaced at uniform logarithmic intervals in scale factor.

We also make use of the \textit{Consuelo} simulation from the Large Suite of Dark Matter Simulations (McBride et al., in preparation).\footnote{LasDamas Project, {\tt http://lss.phy.vanderbilt.edu/lasdamas/}} Consuelo covers a large volume (420 $h^{-1}$ Mpc on a side) with $\sim$2.7 billion particles ($1400^3$), corresponding to a particle mass resolution of $2.7 \times 10^9$ $M_{\odot}$.  Its large size and resolution make it ideal for more detailed particle studies from Milky Way-sized halos ($10^{12}M_{\odot}$, 400 particles) to the largest clusters ($10^{15}M_{\odot}$, 400,000 particles).  This simulation was also performed using \textsc{gadget}-2, with a spline force softening of 8 $h^{-1}$ kpc.  The assumed simulation conditions were a flat, $\Lambda$CDM cosmology ($\Omega_M = 0.25$, $\Omega_\Lambda = 0.75$, $h = 0.7$, $\sigma_8 = 0.8$, and $n_s = 1.0$); 100 snapshots were saved from $a=0.075$ to $a=1.0$, also spaced at uniform logarithmic intervals in scale factor.

In a few cases where resolution tests are necessary, we make use of the \textit{Esmeralda} simulation, also from the LasDamas Project.  This simulation was run with identical parameters and software as the Consuelo simulation, with the exception of its box size (640 $h^{-1}$ Mpc, particle count ($1250^3$), mass resolution ($1.33 \times 10^{10}$ $M_{\odot}$, and spline force softening (15 h$^{-1}$ kpc).  For one test, we also make use of the \textit{Bolshoi} simulation \cite{Bolshoi}, which has much higher resolution ($2048^3$ particles, each $1.9 \times 10^8 M_{\odot}$, with force resolution of 1 $h^{-1}$ kpc) but a much smaller volume of 250 $(h^{-1}$ Mpc$)^3$.  Bolshoi was run with the \textsc{art} code \cite{kravtsov_etal:97}, and it assumed a flat, $\Lambda$CDM cosmology similar to our main simulation ($\Omega_M = 0.27$, $\Omega_\Lambda = 0.73$, $h = 0.7$, $\sigma_8 = 0.82$, and $n_s = 0.96$).

\subsection{Halo Finding and Properties}

\label{s:halo_finding}

Halo finding was performed using the \textsc{rockstar} algorithm, which is a phase-space temporal (7D) halo finder designed for high consistency and accuracy of halo properties \citep{Rockstar,BehrooziTree}.  The \textsc{rockstar} halo finder locates peaks in the particle phase-space density distribution using a locally adaptive phase-space metric.  A seed halo is placed at the location of each peak, and particles are assigned to the closest seed halo in phase space (see \cite{Rockstar} for full details).  Particle potentials are computed using a tree method (see \S\ref{s:grav_pot}); contrary to the default setting, we do not remove positive-energy particles for the analysis in this paper.  For cases where host/satellite halo relationships are ambiguous (such as in major mergers), \textsc{rockstar} uses the host/satellite relationship at the previous snapshot if available.

In this analysis, we consider host halos only (i.e., halos whose centers are not within the radius of more massive halos).  This is because satellite halos (i.e., non-host halos) are almost always \textit{defined} as a collection of self-bound particles within a larger halo---meaning that unbound particles are automatically excluded.  Moreover, there are many reasonable choices of satellite halo boundaries \cite{Onions12}, which makes essential quantities like gravitational potentials depend strongly on the halo finder used.

We also restrict our analysis in general to halos with more than 400 particles, which have been shown to have robustly measurable properties when compared to higher-resolution resimulations \citep{Trenti10}.  We have performed resolution tests with the Esmeralda simulation to verify that gravitational potential calculations for 400-particle halos result in identical energy distributions as for the equivalent 2000-particle halos in Consuelo.  Halo virial masses and virial radii are defined according to the spherical overdensity criterion of \cite{mvir_conv}; if a halo includes satellite halos within its virial radius, those are considered to contribute towards its virial mass.

\subsection{Kinetic and Potential Energy Calculation}

\label{s:grav_pot}

Calculating particle kinetic energies is straightforward ($\frac{1}{2}v^2$ per unit mass), where  $v$ is the physical velocity of the particle relative to the halo bulk velocity. The calculation of potential energies in expanding cosmologies poses normalization issues---the usual practice of setting the potential to zero at infinity is not well-defined.  The traditional method \cite{Rockstar,Klypin99,Springel01,Knollmann09,ASOHF10} is to ignore these issues and compute particle potentials in a Newtonian metric.  In this case, the potential $\phi$ of a point mass $M$ (i.e., the Green's function) is
\begin{equation}
\label{e:pot}
\phi(r) = -\frac{GM}{r}
\end{equation}
We discuss appropriate corrections for an expanding cosmology in later sections, but these are straightforwardly related to the Newtonian potential.
For calculating Newtonian gravitational potentials, we use a modified Barnes-Hut algorithm \citep{BarnesHut86}, as detailed in \cite{Rockstar}.

\section{Unbound Particles in an Expanding Universe}

In this section, we first derive basic energy thresholds for unbound particles in an expanding universe and discuss basic qualitative features of their behavior (\S\ref{s:analytic}; see also Appendices \ref{s:boundedness} and \ref{s:num_sim} for more complete approaches).  We next present our operational definition of unbound particles in cosmological simulations in \S\ref{s:definition}.  Finally, we test how well kinetic energies can predict whether particles will become unbound in cosmological simulations in \S \ref{s:full_sims}.

\label{s:energy}

\subsection{Energy Thresholds and Qualitative Features}

\label{s:analytic}

\begin{figure}
\begin{center}
\vspace{-5ex}
\plotgrace{graphs/qH2}
\vspace{-5ex}
\end{center}
\caption{The evolution of the cosmological acceleration term $-qH^2$ with scale factor, relative to the Hubble parameter today ($H_0^2$).  Negative values imply that the Hubble flow decelerates escaping particles; escape to infinity is impossible while this is the case (see Eq.\ \eqref{e:a}).  Positive values of $-qH^2$ imply that the Hubble flow accelerates escaping particles.  The transition between these states occurs at $a=0.55$ for a flat cosmology with $\Omega_M = 0.25$ and $H_0 = 70$ km s$^{-1}$ Mpc$^{-1}$. In the far future, $-qH^2$ asymptotes to $\Omega_\Lambda H_0^2$.}
\label{f:qH2}
\end{figure}

If one considers a point mass in an expanding cosmology, the effective acceleration $\vec{a}_t$ experienced by a nonrelativistic test particle will be \citep{Nandra11}:
\begin{equation}
\label{e:a}
\vec{a}_t = \left(-\frac{GM}{r^2} -qH^2r\right)\hat{r}
\end{equation}
where $M$ is the value of the point mass, $H$ is the Hubble expansion rate ($\dot{a}a^{-1}$), and $q$ is the deceleration parameter ($-\dot{H}H^{-2} - 1 = -\ddot{a}a^{-1}H^{-2}$).  Both $q$ and $H$ evolve with time; the evolution of the product $-qH^2$ for our chosen cosmology is shown in figure \ref{f:qH2}.

At early times ($a<0.55$), $-qH^2$ is negative, and it is impossible for the test particle to escape to infinity.  This is because the deceleration rate increases linearly with distance: the farther the test particle gets, the stronger the deceleration it experiences.  However, at later times ($a>0.55$), $-qH^2$ becomes positive, and it becomes easier and easier for the test particle to escape.

The time-evolution of the force term in Eq. \eqref{e:a} means that energy is not conserved until the far future, when $-qH^2$ asymptotes to $\Omega_\Lambda H_0^2$ (see figure \ref{f:qH2} and \cite{Loeb11}).  The amount of kinetic energy loss (or gain) of the test particle until that time depends on its orbit.  Because a test particle launched at $a<0.55$ can orbit the point mass several times before escaping at $a>0.55$, \textit{there is not always a single energy threshold} for escape: certain orbit trajectories will have better resonance with the Hubble force term and experience larger kinetic energy changes than others.  However, for every location and initial direction of travel for the test particle, there is always a maximum kinetic energy threshold above which the particle is guaranteed to be unbound.

At very late times, the expansion of the universe becomes exponential (constant $H$), implying $q\to-1$.  Therefore, the product $-qH^2$ approaches a final value of $\Omega_\Lambda H_0^2$ (see also \cite{Loeb11}), as may be seen from the evolution of $H$ in a flat universe ($H^2(a) = H_0^2(\Omega_M a^{-3} + \Omega_\Lambda)$).  In this late-time case, it is possible to solve for the motion of the test particle analytically.\footnote{As may be seen in figure \ref{f:qH2}, this is a good approximation even at the present day; $qH^2=-0.63H_0^2$ at $z=0$ and changes only by $\sim 10\%$ in the next 3 Gyr.}  There is an equivalence radius where the ``push'' of the Hubble flow balances the pull of gravity:\footnote{If $M$ corresponds to the mass of a dark matter halo, $r_e = R_h \sqrt[3]{\frac{\Delta_h}{-2q}}$, where $R_h$ is the halo radius, and $\Delta_h$ is the overdensity which is used to define $R_h$.  Thus, the equivalence radius is typically 3-5 times the virial radius for $a\ge1$.}
\begin{equation}
\label{e:r_e}
r_e = \sqrt[3]{\frac{GM}{-qH^2}},
\end{equation}
If the particle can travel beyond this equivalence radius, it will escape; otherwise, it will remain bound.  The minimal velocity threshold for escape on a radial path is easy to find:\footnote{Due to Gauss's law, this formula works for any spherical matter distribution contained within $r_0$.}
\begin{equation}
\label{e:b_limit}
v_0^2 > \frac{2GM}{r_0} + qH^2 \left[r_0^2 - 3 r_e^2\right]
\end{equation}
where $r_0$ and $v_0$ are the test particle's initial radius and speed.  When $-qH^2 > 0$ at late times, the velocity required to escape is less than in the Newtonian case ($\sqrt{\frac{2GM}{r_0}}$).  Deriving the escape threshold for non-radial paths is substantially messier as it involves a quartic equation (see Appendix \ref{s:boundedness}).  However, it is a fact that \textit{escape along a tangential trajectory requires more energy than escape along a radial trajectory}.  Nonzero initial angular momentum (i.e., at least a partially tangential trajectory) means that the angular momentum at the equivalence radius will also be nonzero.  Thus, it is impossible to convert all the initial kinetic energy into potential energy as in the radial case, requiring slightly more energy to cross the escape threshold radius $r_e$.

\subsection{Defining ``Unbound'' Particles in Cosmological Simulations}

\label{s:definition}

The ability to trace particles into the far future provides a simple way to classify which particles are ``bound'' or ``unbound.''  At late times, the exponential expansion of the universe means that halos become widely separated \cite{Busha03}.  They also become more spherical, meaning that the gravity---Hubble flow equivalence radius $r_e$ (Eq.\ \eqref{e:r_e}) is an excellent approximation to halo boundaries.\footnote{As may be readily verified, using $r_e$ as the halo radius at late times is identical to defining halos using a spherical overdensity criterion of $2\Omega_\Lambda$ times the critical density.}

At a given redshift $z$, every halo in the simulation we use can be associated with a descendant halo at late times ($a=100$ in our case), defined as the halo which shares the largest number of particles.  Then, particles in a halo at redshift $z$ can then be checked against the descendant halo.  If a particle is within $r_e$ of the descendant at $a=100$, it is considered bound; otherwise, it is considered unbound.

The main remaining source of ambiguity is halo mergers: if a smaller halo will eventually merge into a larger one, it is unclear how to classify its particles.  Many high-energy particles from the smaller halo will be captured by the larger halo even though, in isolation, they would have readily escaped from the smaller halo.  It is somewhat unappealing to call these high-energy particles ``bound,'' even though they will never escape to infinity.  An instantaneous measure of boundedness, such as total kinetic and potential energy, would provide a way around this issue; however, as we discuss in the next section, the use of total energies introduces more problems than it solves.  For this reason, we provide in later sections separate estimates of unbound particle fractions for halos which are the most-massive progenitors of their descendants at $a=100$.

\subsection{Kinetic and Potential Energies as an Unbound Classification Technique}
\label{s:full_sims}

\begin{figure}
\begin{center}
\vspace{-5ex}
\plotgrace{graphs/ub_hist_raw}\plotgrace{graphs/ub_hist}\\[-3ex]
\plotgrace{graphs/cons_esmer_raw}\plotgrace{graphs/cons_esmer_norm}
\vspace{-5ex}
\end{center}
\caption{\textbf{Top-left panel}: the kinetic energy plus potential energy ($KE+PE$) distribution at $z=0$ of all particles in $M_\mathrm{vir} > 10^{15}M_{\odot}$ halos which become unbound by $a=100$.  No energy threshold is capable of reliably distinguishing bound from unbound particles.  \textbf{Top-right panel}: same, except normalized by the potential energy of a particle at the halo virial radius.  \textbf{Bottom panels}: the $KE+PE$ distribution at $z=1$ for particles with $KE>|PE|$ and particles with $KE<|PE|$ at $z=0$.  As above, the left panel shows the direct $KE+PE$, and the right panel shows $KE+PE$ normalized to the potential energy of a particle at the virial radius at $z=1$.  $M_p$ represents the particle mass, which is $10^{11}M_{\odot}$ in the simulation in the top panel, $1.33\times 10^{10}M_{\odot}$ for the \textit{Esmeralda} simulation, and $2.7\times 10^{9}M_{\odot}$ for the \textit{Consuelo} simulation.  See text for details.  }
\label{f:energy_thresh}
\end{figure}

Particle motion in cosmological halos is more complex than for the point-mass models described in \S \ref{s:analytic}.  Some additional effects include particles scattering off of substructure, tidal disruption of substructure, halo mass accretion, nonspherical halo mass profiles, and halo mergers.  These phenomena all result in dark matter particles exchanging energy with the environment in nontrivial ways.  Therefore, because particle kinetic energies have been used almost exclusively in the literature (our previous papers included) to classify bound and unbound structure \cite{Rockstar,Knollmann09,ASOHF10,Klypin99,Genel09,Wang11}, it is important to test the validity of this technique.

Since we can directly classify boundedness by tracing particle trajectories, it is straightforward to plot the energy distribution of unbound particles at $z=0$.  We do so for $M_\mathrm{vir}>10^{15}M_{\odot}$ halos in our main simulation (which are resolved with $>$10,000 particles) at $z=0$.  While these halos are almost always the largest collapsed structures in their nearby environment, we exclude the few which merge into even larger halos from this test.

As the top panels of figure \ref{f:energy_thresh} show, we find that \textit{no} energy threshold at $z=0$ is able to accurately predict which particles will have escaped the halo by $a=100$.  \textit{No matter} what a particle's kinetic energy is at $z=0$, it is more likely to be bound than unbound.  We have also tested increasing the radius for particles included in the potential energy calculation to $2R_\mathrm{vir}$ and $3R_\mathrm{vir}$; the identical conclusion applies.

Because we only have a single simulation run to $a=100$, it is very difficult to perform a direct resolution test of this conclusion.  Instead, we perform a simpler test, which is to check how well particle total energies ($PE+KE$) at $z=1$ correspond to those at $z=0$ for both the \textit{Esmeralda} and \textit{Consuelo} simulations.  In both simulations, we categorize particles depending on whether they have $KE>|PE|$ or $KE<|PE|$ at $z=0$.  Then, we plot the distributions of $KE+PE$ for both sets of particles at $z=1$.  To avoid small particle-number effects, we exclude halos below $10^{13}M_{\odot}$ (780 and 3700 particles for Esmeralda and Consuelo, respectively).  As before, we only consider halos at $z=1$ which are the most-massive progenitors of halos at $z=0$, so as to exclude cases where a smaller halo merges into a larger one.  Finally, we exclude halos which lose mass between $z=1$ and $z=0$, as these are most likely experiencing tidal forces from a nearby larger halo which could influence particle trajectories.

As shown in the bottom panels of figure \ref{f:energy_thresh}, particle total energies are very much not conserved between $z=1$ and $z=0$.  This makes the previous conclusion even stronger: particle energies at $a=0.5$ are in general a poor predictor of particle energies at $a=1$, let alone at $a=100$.  That said, \textit{highly-bound} particles at $z=1$ and $z=0$ do seem much more likely to remain bound at later times, meaning that highly-bound particles such as stars are unlikely to escape entirely from halos in mergers (see also \S \ref{s:hostless} and \S \ref{s:baryons}).

Having done many tests over shorter time intervals (not shown), we remark that the decoherence of kinetic energies over time is a generic feature of dark matter particles.  However, this is not necessarily the case for high-velocity objects such as hypervelocity stars.  We derive how the standard kinetic energy threshold for escape changes when properly accounting for the Hubble expansion as well as halo mass accretion in Appendix \ref{s:num_sim}.  In these cases, when the kinetic energy source is not large-scale gravitational forces, then the effect of interactions with substructure is expected to be small (see Appendix \ref{s:substructure}).

\begin{figure}[tp]
\plotminigrace{graphs/unbound_hist}
\plotminigrace{graphs/unbound_dist}
\caption{The \textbf{left panel} shows the probability distribution of unbound mass fractions in halos at $z=0$, derived from tracing particle trajectories to $a=100$.  This averages 2-6\% for the halos in question, with significant mass dependence.  The \textit{dotted} lines show the probability distribution for the halos at $z=0$ which are the most-massive progenitors (MMPs) of halos at $a=100$.  The \textbf{right panel} shows the conditional density distribution of the unbound particle fraction as a function of radius in massive ($10^{14.5}M_{\odot} < M_\mathrm{vir} < 10^{15}M_{\odot}$) halos at $z=0$.  The \textit{red dashed line} shows the limit of one particle per radial bin; effectively, the individual halo sensitivity limit.  Because the unbound fraction as a whole passes below this limit at small radii, the median unbound fraction (\textit{blue dot-dashed line}) rapidly drops to zero from the floor effect.  On the other hand, the average unbound fraction (\textit{green double dot-dashed line}) follows the trend established at higher radii down to a small fraction of the virial radius.
}
\label{f:p_dist}
\end{figure}

\begin{figure}[tp]
\vspace{-15ex}
\plotgrace{graphs/unbound_mr}\plotgrace{graphs/unbound_zs}\\[-4ex]
\plotgrace{graphs/unbound_mmp}\plotgrace{graphs/unbound_mm}\\[-4ex]
\caption{\textbf{Top-left panel}: The average unbound fraction as a function of mass and radius; smaller halos have more unbound particles.  For this and other panels, limited resolution prevents calculating unbound fractions within 50 h$^{-1}$ kpc of halo centers.  \textbf{Top-right panel}: The unbound fraction as a function of radius and redshift for $10^{14}-10^{14.5}M_{\odot}$ halos.  The unbound fraction drops off precipitously at higher redshifts.  \textbf{Bottom-left panel}: The unbound fraction for all halos as compared to halos which are the most-massive progenitors of halos at $a=100$.  Most-massive progenitors have fewer unbound particles than average; at higher masses, more halos are most-massive progenitors, so this effect is less apparent. \textbf{Bottom-right panel}: The unbound fraction for all halos as compared to halos undergoing major mergers.  Halos in major mergers have surprisingly few extra unbound particles, on average.  Error bars for all panels are calculated using jackknife statistics.}
\label{f:radial}
\end{figure}

\section{Properties of Unbound Particles}

\label{s:results}

As discussed in the previous section, total kinetic and potential energy is a poor classifier of unbound dark matter particles.  Instead, we turn to a simulation run through the far future ($a=100$) and trace particle and halo trajectories.  We present statistics of the fraction of unbound particles in halos in \S \ref{s:radial}, as well as the variation with respect to radius, redshift, and halo mass.  We also discuss variations in the unbound fraction with environment in \S \ref{s:env_dep}.

\subsection{Fractional Occurrence of Unbound Dark Matter Particles in Halos}

\label{s:radial}

Individual host halos can have a wide variety of unbound particle fractions at $z=0$, as shown in the left panel of figure \ref{f:p_dist}.  On average, about 2-6\% of particles will escape to infinity over the mass range considered ($10^{13.6}M_{\odot} < M_\mathrm{vir} < 10^{15} M_{\odot}$), with significant mass dependence.  There is also a strong dependence on whether a halo is a most-massive progenitor (MMP) of the descendant halo at $a=100$ or not.  On average, a non-MMP has an unbound fraction 2-3x larger than an MMP halo of similar mass.  Indeed, we note that some halos in the top panels of Fig.\ \ref{f:p_dist} can have very high unbound fractions, approaching 100\%.  These halos end up being shredded into many pieces at $a\gg 1$.  Two out of the $\sim$76,000 halos in the mass range $10^{13.6}M_{\odot} < M_\mathrm{vir} < 10^{14} M_{\odot}$ ended up being shredded into more than 5 pieces, each no larger than 20\% of the original mass.

The right panel in figure \ref{f:p_dist} shows the spread in unbound fractions as a function of radius for massive halos ($10^{14}M_{\odot} < M_\mathrm{vir} < 10^{14.5} M_{\odot}$) at $z=0$.  The significant scatter seen in figure \ref{f:p_dist} remains at all radii.  However, at small radii ($<0.2R_\mathrm{vir}$), the average unbound fraction is so low that most halos will have less than a single unbound particle per radial bin.  As a consequence, the median unbound fraction across halos significantly underestimates the overall trend at small radii.  For that reason, we express radial unbound fractions in terms of the average across all halos, which better follows the trend of unbound fractions established at larger radii.

The average radial profile of the unbound fraction (i.e., the ratio of unbound to total particles in radial bins) is shown in figure \ref{f:radial}.  In all cases, the unbound fraction increases roughly linearly with radius.  For an NFW \cite{NFW97} halo density profile, this would imply that the physical density of unbound particles peaks at the halo center.

The top-left panel in figure \ref{f:radial} shows how the radial dependence of the average unbound fraction depends on halo mass.  As in the top panel of figure \ref{f:p_dist}, smaller halos have larger unbound fractions across all radii.  For smaller halos in this panel, the radial dependence is truncated at 50 h$^{-1}$ kpc, as the gravitational accuracy of the simulation degrades rapidly below that radius.

The top-right in figure \ref{f:radial} shows the redshift dependence of the radial unbound fraction, which has substantial evolution from $z=0$ to higher redshifts.  This trend is preserved across all the mass ranges we consider, and matches the qualitative expectation that the deceleration of the universe at early times makes it much harder for particles to escape (see Appendix \ref{s:num_sim}).

The bottom-left panel in figure \ref{f:radial} shows how the unbound fraction changes if only most-massive progenitor halos are selected.  As expected from figure \ref{f:p_dist}, MMP halos have lower unbound fractions at all radii, as compared to average halos of the same mass.  However, this difference is less pronounced for more massive halos, as the overall fraction of halos which are MMPs increases with halo mass.

The bottom-right panel in figure \ref{f:radial} shows how the unbound fraction changes if only halos undergoing major mergers are selected.  Specifically, a halo is considered to be undergoing a major merger if it contains a satellite halo with $v_\mathrm{max,sat} > 0.6v_\mathrm{max,host}$, where $v_\mathrm{max}$ is the maximum circular velocity, corresponding approximately to an infalling mass ratio of 0.3:1.  This panel shows that, for massive halos, the presence of a major merger has very little impact on the unbound fraction.  However, for less-massive halos (e.g., $10^{13.5}M_{\odot} < M_\mathrm{vir} < 10^{14.0}M_{\odot}$), a major merger can increase the unbound fraction somewhat more (by 5--20\% overall).  At first glance, it may appear surprising that halos undergoing major mergers do not have substantially more unbound particles.  However, the mass in an incoming major merger gets added to that of the main host halo.  Hence, while the incoming particles may have been unbound relative to the potential of the original merging halo, they are mostly bound relative to the \textit{combined} gravitational potential of the incoming and original particles within the virial radius.  This effect is explicitly shown in \S \ref{s:env_dep}.

To summarize the most important trends, the unbound fraction is a strong function of radius.  The unbound fraction on galaxy scales (within $0.05 R_\mathrm{vir}$) is below 1\%, whereas it can reach 10\% or more at the halo radius.  Major mergers, lower halo masses, and lower redshifts all correlate with increased unbound fractions, but these effects are comparatively subdominant.

\begin{figure}
\plotgrace{graphs/unbound_f_with_r_13.5}\plotgrace{graphs/unbound_f_with_rvir_13.5}\\[-5ex]
\begin{centering}
\plotgrace{graphs/ke_13.5}\\[-4ex]
\end{centering}
\caption{\textbf{Top-left panel}: The conditional probability distribution of the unbound fraction in $10^{13.6}-10^{14}M_{\odot}$ halos as a function of the distance to the nearest larger halo at $z=0$.  \textbf{Top-right panel}: Same as top-left panel, except now in units of the larger halo's virial radius.  This shows that the unbound fraction for smaller halos climbs steeply within 3-4$R_\mathrm{vir}$ of a larger halo.   \textbf{Bottom panel}: For comparison, the fraction of particles in halos with kinetic energies larger than the magnitude of their potential energies ($KE>|PE|$).}
\label{f:env}
\end{figure}

\subsection{Environmental Dependence}

\label{s:env_dep}

There are several ways of quantifying the local environment; one common method is to use the distance to the nearest larger halo.  As shown in the top-left panel of figure \ref{f:env}, the unbound fraction for $10^{13.6}-10^{14}M_{\odot}$ halos has a clear maximum when a larger halo is 5 Mpc away.  In units of the larger halo's virial radius, this occurs between 3 and 4 $R_\mathrm{vir}$ (top-right panel of figure \ref{f:env}).  This maximum persists for more massive halos as well (not shown).

This feature has a straightforward explanation.  When larger halos are much more than $3-4R_\mathrm{vir}$ away, the Hubble flow is stronger than the influence of gravity (see Eq.\ \eqref{e:r_e}); this will accelerate away the larger halos before they have the chance to interact strongly.  When a larger halo is around $3-4R_\mathrm{vir}$ away, the smaller halo is just barely within the region which will eventually collapse onto the larger halo; hence, particles in the smaller halo can more easily escape.  Finally, when there is a larger halo very nearby to the smaller halo, then most of the particles in the smaller halo will remain bound to the larger halo's gravitational potential.

This last point reinforces the main issue with our adopted definition for unbound particles.  Smaller halos merging into larger ones will have most of their particles considered as ``bound'' even if, in isolation, they would have escaped from the smaller halo.   The bottom panel of figure \ref{f:env} shows this clearly---the fraction of high-energy ($KE>|PE|$) particles in halos increases dramatically when a larger halo is nearby.  That said, the source of many of these high-energy particles is the larger halo itself, meaning that their association with the smaller halo is just as much an issue with the spherical overdensity definition of a halo as it is with the definition of unbound particles.

\section{Discussion and Implications}

\label{s:discussion}

The most important radius for the individual trajectory of dark matter particles is the equivalence radius (Eq.\ \eqref{e:r_e}), beyond which the Hubble flow will accelerate the particle away from the gravitational pull of the halo.  At early times ($a<0.55$), the deceleration of the universe makes it impossible for particles to completely escape from halos.  However, at late times, the acceleration of the universe brings the equivalence radius from infinity down to roughly 4.5 times the virial radius.  This leads to the creation of ``islands'' at late times ($a\gg 1$), whereby particles (and, indeed, other halos) which are not within the equivalence radius are expanded away at rates that gravity cannot overcome (see also \cite{Busha05,Loeb11}).

Perhaps surprisingly, we have shown that total kinetic and potential energy is a poor predictor of whether particles will become unbound in cosmological simulations (\S \ref{s:full_sims}).  Instead, the only robust way of determining which particles are unbound is to test whether they leave the equivalence radius in the far future.  We have shown that the fraction of unbound particles defined this way  is a strong function of distance to the halo center as well as redshift (\S \ref{s:radial}).  The fraction of unbound particles also depends somewhat on the distance to the nearest larger halo, although the fraction of high kinetic-energy particles has a much stronger environmental dependence (\S \ref{s:env_dep}).

We note that the total kinetic and potential energy should not fare any better as a predictor for boundedness in satellite halos.  Over the long term, this is clear because most satellites will dissipate into their hosts---i.e., none of the particles will remain bound to each other.  Even over the short term, the total kinetic and potential energy ignores the tidal force from the host halo, which can be significant compared to the gravitational force from the satellite halo.  That said, removing particles with positive total kinetic and potential energy from satellite halos does represent a convenient cut in phase space for \textit{categorizing} particle membership.  Many other possible cuts exist \citep[e.g.,][]{Rockstar,Maciejewski09,Elahi11}.

In the remainder of this section, we discuss several implications of the previous results on unbound particles.  The dependence of particle kinetic energies on halo environment suggests a possible implication for direct dark matter detection experiments, which we test in \S \ref{s:dm_detect}.  The radial dependence of the unbound particle fraction is interesting in connection to the kinetic energy source for hypervelocity supernovae and GRBs, which we discuss in \S \ref{s:hostless}.  Finally, the possibility of escaping dark matter particles raising the baryon fraction in halos is discussed in \S \ref{s:baryons}.

\subsection{The Effect of Environment on Dark Matter Detection}

\label{s:dm_detect}

\begin{figure}
\begin{centering}
\plotgrace{graphs/vdf}
\caption{The velocity distribution function (VDF) for Milky Way-sized halos at the Earth radius as a function of environment.  Lines in the plot show the VDF for halos binned by the distance to the nearest larger halo, in units of the larger halo's virial radius.  (This serves as a proxy for the tidal force).  Very little difference is seen except for halos currently merging with a larger halo.  Andromeda ($\sim3R_\mathrm{vir}$ away) therefore has minimal effect on the VDF near the Earth radius.}
\end{centering}
\label{f:vdf}
\end{figure}

For the Milky Way, the nearest larger halo would be associated with M31 (Andromeda), which is approximately three virial radii away \cite{Ribas05}.  Assuming an NFW profile, the approximate one-sigma mass range of the Milky Way is $5.4\times 10^{11}M_{\odot} < M_\mathrm{vir} < 1.4 \times 10^{12}M_{\odot}$ \cite{Smith07,Busha11,Xue08}, the galactocentric distance is $\sim$8 kpc \cite{Honma12}, and the circular velocity at the Earth's radius is $\sim$238 km/s \cite{Honma12}.  Selecting halos in the one-sigma mass range from the Bolshoi simulation, we calculate the velocity distribution (after correcting for the motion of the Earth) 7-9 kpc from the halo center, and bin results by the distance to the nearest larger halo.  The results are shown in figure \ref{f:vdf}.  While there is a significant increase in the high-energy velocity distribution at 8kpc for Milky Way-sized halos about to cross the virial radius of a larger halo, this effect is gone when the larger halo is $\ge 2R_\mathrm{vir}$ away.  As such, the presence of M31 should not impact dark matter detection experiments.

\subsection{Hostless Supernovae and GRBs}
\label{s:hostless}
\begin{figure*}
\begin{centering}
\plotgrace{graphs/nmax150}
\caption{The conditional probability distribution of particles within 0.05 $R_\mathrm{vir}$ of halo centers at $z=1$ which escape the halo radius by $z=0$, from the \textit{Consuelo} simulation.  This fraction is so small that many halos do not have \textit{any} particles in that radius which leave the halo; these are not shown on the density plot, but they influence the overall averages.  The fact that the average fraction is so small suggests that large-scale gravitational forces which affect halo mass accretion and mergers are unable to significantly accelerate much material out of halo centers.  For example, if more than 1\% of supernovae are undergoing hypervelocity escape, then the source of the kinetic energy will most likely be from the supernova progenitors, rather than from the halo potential well.}
\end{centering}
\label{f:statistics}
\end{figure*}

Stars are expected to form within a small radius of the center of halos \cite{Kravtsov13}, typically within 1.5-5\% of $R_\mathrm{vir}$.  To obtain a constraint on how many stars are expected to leave due to merging events, we can tag dark matter particles in halos within $0.05R_\mathrm{vir}$ at a given redshift and track how many leave their halos at later times.  Clearly, this will result in an upper bound on the escape fraction, since stars are in general much more bound than the nearby dark matter.

Nonetheless, this upper bound is an interesting one.  We trace particles in the Consuelo simulation between $z\sim1$ and $z=0$ to see which of them actually remain in the halo with which they were associated at $z=1$.  For every progenitor halo at $z=1$, we can find the descendant halo at $z=0$ which receives the largest fraction of the progenitor's particles.  The progenitor particles which do not end up in the descendant may then be assumed to have escaped sometime between $z=1$ and $z=0$.

For particles which were initially within $0.05R_\mathrm{vir}$, figure \ref{f:statistics} shows that 0.5\% or less can escape the halo's descendant completely by $z=0$.  In terms of hostless supernovae and GRBs, this would imply that it is extremely difficult for central dark matter particles to acquire enough energy to leave their hosts.  Thus, depending on the host halo mass, the fraction of stars (i.e., supernovae and GRB progenitors) which receive enough of a kick in halo-halo mergers to leave the halo is minimal.  Confirmed hostless high-energy events above this fraction must therefore be due to progenitor-linked energy sources, rather than long-range gravitational sources.

\subsection{The Effect of Unbound Particles on the Baryon Fraction}

\label{s:baryons}

\begin{figure}
\begin{center}
\vspace{-5ex}
\plotlargegrace{graphs/baryon}
\vspace{-5ex}
\end{center}
\caption{In satellite mergers, high-energy incoming dark matter particles will tend to escape halos, whereas the more tightly-bound stellar material will tend to remain.  This will enhance the baryon fraction over the cosmic average; this figure shows the relative increase in the baryon fraction as a function of halo mass and redshift due to this effect.  For small halos, baryonic feedback effects (such as supernovae and stellar winds) overwhelm the importance of this effect and decrease the baryon fraction below the cosmic average.  For large halos, the effect is too small to impact current cosmological surveys.  Errors shown are jackknife uncertainties in the average across halos at a given mass and redshift.}
\label{f:baryon_f}
\end{figure}

As mentioned in the introduction, high-energy dark matter particles can freely pass through dark matter halos, whereas more tightly-bound stars will tend to remain inside the halo (see \S\ref{s:full_sims}).  This effect is one of many which will influence the baryon fraction, including galaxy outflows, shocks, and angular momentum exchange.  Indeed, galaxy outflows have a much stronger impact than any other mechanism for lower-mass halos ($M_h<10^{13}M_{\odot}$), as the energy transfer in feedback effects can be comparable to the binding energy of the baryons.  However, in high-mass clusters ($M_h>10^{14}M_{\odot}$), the binding energy is large enough that it is very difficult for baryons to escape the halo once they are accreted.

To estimate the effects due to the different binding energies of dark matter and stars, we evaluate a toy model on all particles in the Consuelo simulation.  We assume that dark matter particles entering a halo for the first time will be accompanied by baryons according to the cosmic fraction $f_b$ (0.16, for the Consuelo cosmology).  Some fraction $f_\ast$ of the baryons will then be converted into stars; in this analysis, we use the results of \cite{Behroozi12}, which observationally constrain $f_\ast$ as a function of halo mass from $z=0$ to $z=8$.  When a dark matter particle leaves, the hot gas will undergo adiabatic expansion in the reduced potential well, expelling a fractional mass $f_b (1-f_\ast)$ of baryons.\footnote{This fraction is valid for adiabatic simulations, in which the gas fraction is roughly independent of radius \cite{Kravtsov05}.  However, this is not necessarily the case in simulations with radiative cooling; so we leave a more detailed analysis for future work.}  Any stars formed will remain in the halo, resulting in a net increase in the baryon fraction.

This model serves to put a lower limit on the baryon fraction increase from this effect.  The presence of cold gas will result in even more baryons staying behind when dark matter particles leave.  However, cold gas is limited to the same lower-mass halos which are strongly influenced by galaxy outflows---a much larger uncertainty than the effect examined here.

Predictions for the relative increase in the baryon fraction as a function of halo mass and redshift are shown in figure \ref{f:baryon_f}.  There is a strong trend towards larger increases in the baryon fraction for smaller halos, which is mainly due to the much stellar mass fraction in such halos \cite{Behroozi12}.  The relative change in the baryon fraction also increases at later redshifts; this is likely related to the smaller fraction of unbound particles at high redshifts (figure \ref{f:radial}) as well as the increasing ease of escape at later times due to the acceleration of the universe (figure \ref{f:sims}).

Overall, at $z=0$, the relative increase in the baryon fraction is between 0.5-4\%.  For very massive halos, the effect is completely negligible, as the average stellar mass to dark matter mass (including satellites and intracluster light) is less than 1\%.  Consequently, it is unlikely that this effect will influence precision calibrations of the dark matter halo mass function.  For smaller halos, the effect seems to balance the effect of angular momentum exchange, which would otherwise reduce the baryon fraction by $\sim$3\% \cite{Kravtsov05}; yet, as mentioned above, galactic outflows are likely to be significantly more important for these halos.

\section{Conclusions}

\label{s:conclusions}

We have studied the properties of unbound dark matter particles, defined as particles which can travel arbitrarily far from their halo in the far future.  Our main findings are as follows:
\begin{enumerate}
\item On average, at $z=0$, 2--6\% of particles in halos are unbound (i.e., can escape to infinity; \S \ref{s:radial}).
\item The fraction of unbound particles in halos is a very strong function of redshift, and approximately a linear function of distance from the halo center (\S \ref{s:radial}).
\item Total kinetic and potential energies cannot be used to predict which particles will become unbound.  Moreover, total kinetic and potential energies are strongly non-conserved at the single-particle level in simulations.  The level of non-conservation is independent of simulation resolution (\S \ref{s:full_sims}).
\item The presence of Andromeda does not impact the velocity distribution of dark matter in the Milky Way at the galactocentric radius (\S \ref{s:dm_detect}).
\item Halo mergers cannot be used to explain a hostless supernovae or gamma ray burst fraction which exceeds the order of 1\% (\S \ref{s:hostless}).
\item The baryon fraction in massive ($10^{14}$--$10^{15}M_{\odot}$) halos is negligibly boosted ($0.5-1\%$) on account of dark matter particles which leave after entering the halo (\S \ref{s:baryons}).
\end{enumerate}

\acknowledgments

We are especially indebted to Matthew R.\ Becker for supplying the main simulation used in this work, as well as to Douglas Rudd and the University of Chicago Research Computing Center for support in running it.  We also very much appreciate the many improvements to this paper made at the suggestion of our referee, Andrey Kravtsov.  We thank Michael Busha, who ran the Consuelo and Esmeralda simulations used here, on the Orange cluster at SLAC; these were run as a part of the LasDamas collaboration simulations.  We also appreciate Joel Primack and Anatoly Klypin for providing access to the Bolshoi simulation.  Finally, we would like to thank Dusan Keres and Tom Abel for useful discussions on baryon fractions in hydrodynamical simulations, as well as Paul Schechter for other helpful comments.  This work received support from Stanford University and the U.S. Department of Energy under contract number DE-AC02-76SF00515.

redpajama_set_name: RedPajamaArXiv


text:
ISO food standards developers find right recipe for leadership award
An ISO technical committee that has developed nearly 780 International Standards for the food industry has been recognized through an award for superior performance, presented at the 34th ISO General Assembly, held in New Delhi, India, 21-23 September 2011.
For 2011, The Lawrence D. Eicher Leadership Award for excellence in creative and innovative standards development goes to ISO technical committee ISO/TC34, Food products.
From left: ISO/TC 34 Chair, Mr. François Falconnet; ISO President, Dr. Boris Aleshin, and ISO Vice-President (technical management), Mr. Jacob Holmblad.
Apple to Tie Exec Bonuses to Climate, Social Goals
The initiative was reportedly announced in response to a shareholder proposal to cut executive pay.
NAM Calls on Armed Thugs to Cease Violence at Capitol
"This is not the vision of America that manufacturers believe in and work so hard to defend."

redpajama_set_name: RedPajamaCommonCrawl


text:
Coroner's Court
Facebook photographs foil couple who staged car crash
David Ward and Lynsey Ivory pretended to be strangers and submitted injury claims
Wed, Nov 25, 2015, 17:18
A couple who staged a car crash while pretending to be strangers were discovered when the insurance company saw that they appeared in each other's Facebook profile pictures, a court has heard.
David Ward (30) was the front seat passenger in an Opel Corsa which rear-ended the Volkswagen Passat Lynsey Ivory (27) was driving.
Ward and Ivory of The Beeches, Clonshaugh, Priorswood, Dublin pleaded guilty at Dublin Circuit Criminal Court to attempting to dishonestly by deception cause a loss to FBD Insurance on dates between July 22nd, 2013 and January 1st, 2014.
Both claimed to be suffering injury from the collision but denied to gardaí, who arrived to investigate the crash, that they knew each other. They were transferred to hospital in the same ambulance during which they continued to pretend to be strangers.
Both Ward and Ivory later submitted a personal injury claim to FBD Insurance in which they again denied knowing the occupants of the other vehicle. They both made voluntary statements to gardaí outlining what had happened and stating that the people in the other car were strangers.
Garda Neill Plunkett told Martina Baxter BL prosecuting, that a claims handler with FBD examined both Ward's and Ivory's Facebook accounts, having received their claims and noted that they appeared in each other's profile pictures.
Gardaí were contacted and when officers arrived at Ivory's home to arrest her for questioning Ward answered the door.
The court heard that if the couple's claim had been successful they could each have been awarded up to €15,000. The pair will be sentenced on Thursday.
Ward has seven previous convictions for offences including criminal damage and theft, while Ivory has no convictions. The couple have two children and have since married.
Garda Plunkett told Judge Martin Nolan that he had been suspicious of the couple's claims that they were strangers from his first investigation of the collision on Corballis Road, Donabate on July 22nd, 2013.
He said Ivory told him she had been rear-ended and the driver of the car Ward was travelling in admitted that he had been speeding around a bend on the road and hadn't seen the Passat until it was too late.
Garda Plunkett said the damage caused to both vehicles was inconsistent with the account he was given and the air bags had not been deployed in either vehicle as would be expected.
He said Ivory was still sitting in the driver's seat when he arrived on the scene and she was complaining of neck and back pain. Her passenger, who later transpired to be the wife of the man who was driving the car Ward was in, said she was uninjured.
Ward, who was the front seat passenger of the second vehicle, confirmed his friend's account of how the crash had occurred. He was removed from the Corsa on a spinal board and was complaining of back pain.
Sinn Féin may change stance on Special Criminal Court abolition
Too many promises risks making voters nervous
Dublin south west election contest a 'challenge', says Zappone
Sinn Féin may change stance on Special Criminal Court abolition 19:57
5 Who was murdered teenager Keane Mulready-Woods?


The Gimli Film Festival will literally have something for even the toughest of film critics when it screens more than 59 Manitoba-made films.
Filmmaker Guy Maddin is one of the big names attending this year's festival, whose film "Archangel" will be screened on July 26.
"The film community in Manitoba is extremely supportive and consistently produces captivating and dynamic cinema that we can't wait to share with our film fans," says GFF director Leona Johnson.
Other Manitoba filmmakers in attendance include director Andy Blicq for his film "A Song for John Ramsay," and Cam Patterson, director of "Aboard the Namao," a documentary on the state of Lake Winnipeg. John Barnard, director of "Bachman," Shelagh Carter, director of "Before Anything You Say," Katharina Stieffenhofer, director of "From Seed to Seed," and Dave Barber, co-director of "Tales from the Winnipeg Film Group" will also be in attendance.
The Gimli Film Festival is presenting two distinct awards this year to celebrate Manitoba film excellence. The first award for Best Manitoban Director is presented by the Directors Guild of Manitoba and will be announced at the awards reception on July 28.
Awards for Best Actor and Best Actress in a Manitoba Short Film will be presented by ACTRA Manitoba during the Manitoba Short Films in Competition program alongside Manitoba Film & Music's Audience Choice award for best Manitoba Short Film.
Film fans can purchase their passes and tickets online at GimliFilm.com, through the GFF app or at the box office.
ChrisD.ca is a proud media sponsor of this year's Gimli Film Festival, which runs July 25-29.


text:
import { asyncEnumerate } from './index'
export default asyncEnumerate

redpajama_set_name: RedPajamaGithub


MBohemian Rhapsody Big and splashy, sentimental and not completely true, this is the biopic that Freddie Mercury deserved, an absorbing story about an outsider who was either going to be a weirdo or an artist, and so he became a very flamboyant artist. The soundtrack is full of Queen songs, and even if you're not a big Queen fan, you'll find they sound better in the movie than they do on the radio. Rated PG-13. 135 minutes.
NCan You Ever Forgive Me? Melissa McCarthy is terrific in this real-life story of the writer Lee Israel who, after the collapse of her literary career, found a lucrative second career as the forger of letters by historical people. Directed by Marielle Heller, it's a film of wit and atmosphere and about the most twisted rags-to-riches story you could ever hope to see. Rated R. 106 minutes.
NGreen Book Viggo Mortensen and Mahershala Ali are ideally paired as an Italian American driver and an African American pianist on a concert tour through the Deep South in 1962. Mortensen completely transforms and has been nominated for an Oscar. Rated PG-13. 130 minutes.


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text:
Trump Expands Sanctions on Iran
Via Economic Policy Journal
Sanctions, the step-by-step escalation of intervention, is a favorite policy of the warmongers. … … Sanctions are simply the coward's and the babbler's halfway house to war.–Murray Rothbard
The Trump administration, via the Treasury Department, has slapped another round of sanctions on Iran.
The Treasury's Office of Foreign Assets Control has announced that it took action against eight senior Iranian regime officials as well as the largest steel, aluminum, copper, and iron manufacturers in Iran, who collectively generate billions of dollars annually.
The Treasury's action includes the designations of Ali Shamkhani, the Secretary of Iran's Supreme National Security Council; Mohammad Reza Ashtiani, the Deputy Chief of Staff of Iranian armed forces; and Gholamreza Soleimani, the head of the Basij militia of the Islamic Revolutionary Guards Corps (IRGC).
In addition, Treasury designated 17 Iranian metals producers and mining companies; a network of three China- and Seychelles-based entities; and a vessel involved in the purchase, sale, and transfer of Iranian metals products, as well as in the provision of critical metals production components to Iranian metal producers.
Concurrently with today's designations, the President signed a new Executive Order that targets additional sources of revenue used by the Iranian regime to fund and support its nuclear program, missile development, terrorism and terrorist proxy networks, and malign regional influence.
Specifically, this E.O. authorizes the Secretary of the Treasury, in consultation with the Secretary of State, to impose sanctions against persons operating in or transacting with additional sectors of the Iranian economy, including construction, mining, manufacturing, and textiles.
READ ALSO Hong Kong's tycoons come under scrutiny amid protests
"The United States is targeting senior Iranian officials for their involvement and complicity in Tuesday's ballistic missile strikes," said Secretary Steven T. Mnuchin. "We are also designating Iran's largest metals manufacturers, and imposing sanctions on new sectors of the Iranian economy including construction, manufacturing, and mining. These sanctions will continue until the regime stops the funding of global terrorism and commits to never having nuclear weapons."


text:
November Residency Alert: LAPD at The Bootleg
Robben Barquist
COLLiDE is proud to present LA-based pop-psych troubadour Los Angeles Police Department (AKA Ryan Pollie), who has taken up a residency at the Bootleg Theater for the month of November.
Pollie recently released his second eponymous album under the LAPD moniker (that's right, both albums are titled LAPD, try to keep up) in April of this year. The new album is a big leap forward for Pollie, both in terms of the development of his songwriting chops, as well as his more nuanced approach to the album's production. And yet, it seems many things have stayed constant since the debut album's release in 2014: the whimsical, almost childlike visual aesthetic, the introspective bedroom ballad vibe of the songs, and of course, the cold, even violent, nature of the band/album names that seem eternally at odds with Pollie's gentle musicianship.
Tonight is the first performance of Ryan Pollie's month long residency and we couldn't be more excited to be bringing the sounds of LAPD to the city he draws so much inspiration from. The stellar lineup is filled out by Shannon Lay, Dante Elephante, 93 Bulls, and DJ Chris Cohen, so you know it's going to be a rad time. The event is totally FREE so we hope to see you guys there!
Where: Bootleg Theater – Bar Stage – 2220 Beverly Blvd, Los Angeles CA 90057
When: Monday November 6, 2017
Time: Doors open at 8:30 P.M.
photo by: Cara Robbins
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LISTEN: GRIFF CLAWSON PONDERS FLEETING LOVE ON "2lovely"
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hannah hausman
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COLLiDE presents month-long Talk Time residency at The Satellite
In a relatively short time since launching the band, Talk...


text:
Home » News » India » India and Russia to Ink Number of Pacts During PM Modi-Putin Summit on Monday
India and Russia to Ink Number of Pacts During PM Modi-Putin Summit on Monday
File photo of PM Narendra Modi and Vladimir Putin. (Photo: Reuters)
The two sides are also expected to focus on the situation in Afghanistan and threat of terrorism including from groups like Lashkar-e-Taiba and Jaish-e-Mohammed.
PTI New Delhi
India and Russia are expected to ink a raft of pacts to further boost cooperation in key areas of defence, trade and investment, energy and technology at the summit talks between Prime Minister Narendra Modi and President Vladimir Putin on Monday, government sources said. In the summit as well as in the inaugural '2+2' defence and foreign ministerial talks, the two sides are also expected to focus on the situation in Afghanistan and the rising threat of terrorism including from groups like Lashkar-e-Taiba and Jaish-e-Mohammed.
It is learnt that the joint statement to be issued after the summit is likely to reflect India's concerns over cross-border terrorism and the security implications arising out of the Afghan crisis. While Putin will arrive in Delhi on Monday, Russian Foreign Minister Sergey Lavrov and Defence Minister Sergey Shoygu are reaching on Sunday night. According to the Ministry of External Affairs (MEA), PM Modi and President Putin will begin the summit talks at 5:30 pm and the Russian leader will emplane from Delhi at 9:30 pm.
Ahead of the summit, India has cleared the long-pending AK 203 Kalashnikov rifles deal worth nearly Rs 5,000 crore for production of over five lakh AK-203 assault rifles at Korwa in Amethi by an Indo-Russian joint venture. The two sides are also likely to wrap up the final phase of negotiations for a logistics support agreement, which is likely to be signed either during the two-plus-two talks or at the summit.
In reflection of their time-tested defence ties, India and Russia are also set to renew for the next decade a framework for military-technical cooperation at the summit besides announcing a joint commission on technology and science. The two sides may also firm up a number of defence procurement proposals besides deliberating on the long-pending project for joint production of 200 twin-engine Kamov-226T light helicopters for Indian armed forces.
Ukraine Says Has 'Evidence' Russia Was Behind Cyberattack
Navies of India and Russia Conduct Passing Exercise in Arabian Sea
According to sources, India is likely to apprise the Russian side about its position on the eastern Ladakh border row as well as its concerns over various regional developments. The sources said President Putin's decision to visit India notwithstanding the current COVID-19 situation in Russia reflected the importance he attaches to the relationship with India.
"December 6 will be a full Russia Day," said a source referring to back-to-back important meetings. The day will begin with Defence Minister Rajnath Singh's talks with his Russian counterpart Shoygu under the framework of the India-Russia Inter-Governmental Commission on Military-Technical Cooperation. Separately, External Affairs Minister S Jaishankar will hold talks with his Russian counterpart Lavrov. Then the foreign and defence ministers of the two sides will hold the '2+2' dialogue at 11:30 pm.
Prime Minister Modi and President Putin will hold a one-on-meeting before the 21st India-Russia summit. A dinner will also be hosted for the Russian leader. The pacts to be signed will cover a wide range of areas including trade, energy, culture, defence and technology, the sources said.
Besides government-to-government agreements, a number of other pacts are also set to be firmed up on the sidelines of the summit, the sources said. "Despite global geo-political changes, our relations with Russia have been very steady," said another source.
On cooperation in areas of defence, the sources said the two sides are set to focus on co-production and co-development of military equipment and platforms. Referring to investment ties, they said the target of USD 30 billion has already been met in 2018 and now the focus is on raising it to USD 50 billion by 2025. They said efforts would be to diversify trade ties which has till now been dominated by cooperation in the energy sector. "We are looking at new drivers of growth," the source said.
The sources said India is also keen on boosting trade relations with the Russian Far East and 11 governors from the region have been invited for the upcoming Vibrant Gujarat conclave. The last India-Russia Annual Summit was held in September 2019 during the visit of Modi to Vladivostok. The annual summit could not take place last year due to the COVID-19 pandemic.
first published:December 04, 2021, 19:20 IST
Russia Staging Provocations, Sending Operatives to Cook Up Pretext to Invade Ukraine, Says US
EU Warns Russia of 'Robust' Response as Ukraine Crisis Deepens
Havana Syndrome: New Cases Reported In Europe, US Yet To Find Answers
US Believes Russia Undecided On Invading Ukraine, Remains Ready For All Possibilities
Russia Sees Sharp Rise in Covid-19 Cases Amid New Surge Fears


Lunit, an artificial intelligence (AI)-powered image analysis software company, is demonstrating for the first time its new, advanced cloud-based AI solution for real-time analysis. The first commercially available AI module of Lunit INSIGHT is a chest x-ray solution.
The chest x-ray AI module detects major chest abnormalities, lung nodule/mass, consolidation and pneumotherax. The company states that it has a 97% standalone accuracy in nodule detection and a 99% accuracy for consolidation and pneumothorax. A spokesperson for the Seoul, South Korea-based company said that clinical studies have shown Lunit INSIGHT to significantly increase the diagnostic performance of its users up to 20% for both radiologists and non-radiology physicians.
Users can upload medical images online at the Lunit INSIGHT web page. AI analysis results appear in several seconds. These results include the level of abnormality and the visualization of the AI attention map.
RSNA 2017: Lunit's INSIGHT cloud-based AI software makes debut. Appl Radiol.


text:
True Sound Façade
Athens Animfest 2021 Official Screening, Saturday 27/03/2021 01:00 - 03:00
Directed by: Laura N-Tamara
Screenplay: Laura N-Tamara
Animation: Laura N-Tamara
Technique: Live action, 2D digital
Music: Narae Chung
Production/School: The Smalls
Dialogue language: no dialogues
"True Sound Facade" is a poetic dance and animation film in which a dancer realises their digital self feels truer than their real world self. It plays with the japanese notions of 'honne', the 'true sound', one's innermost feelings, and 'tatemae', the façade one puts on to live in society. It stars Kino McHugh, dancing with and against a colourful animated environment born out of her movements. By combining live-action and animation, the film becomes a celebration of how our inner and outer lives merge with each other in the act of artistic creation. The film was commissioned by the Barbican museum in London, for their "Inside out" short film series.


Bangabandhu Sheikh Mujib Medical University (BSMMU) today observed World AIDS Day with great hope and optimism for a successful prevention of the Human immunodeficiency virus infection and acquired immune deficiency syndrome (HIV/AIDS) across the country.
BSMMU arranged a rally and provided AIDS-related information with T-shirt, cap, Leaflet, poster, said a press release.
The rally was inaugurated by BSMMU Vice-Chancellor Prof Dr. Kanak Kanti Barua while Pro-Vice-Chancellor (Research and Development), Pro-Vice-Chancellor (Administration), Pro-Vice-Chancellor (Academic), Treasurer, Proctor, Register, Director- Hospital, Prof. Saleha Begum Chowdhury were present, among others.
The rally started at 8:30 am from Bot-tola of BSMMU and passed important blocks and circles and ended to Between C and D Block of BSMMU.
BSMMU VC said BSMMU is the pioneer to start public facility-based HIV service in Bangladesh.
He also mentioned the major achievements regarding HIV service in BSMMU.


text:
Henri Lepage, född 1941, är en fransk nyliberal ekonom. Han har skrivit boken Demain le Capitalisme (I morgon kapitalism, ).

Betydelse i Sverige
I morgon kapitalism gavs ut på svenska av Ratio 1980. Översättningen av "le nouveau libéralisme" till nyliberalism anses ha påverkat termens användning i Sverige. Boken anses även viktig för nyliberalismens tidiga spridning i Sverige.

Referenser

Externa länkar
Henri Lepages blogg

Franska nationalekonomer
Franska författare
Franskspråkiga författare
Nyliberaler
Födda 1941
Män
Levande personer

redpajama_set_name: RedPajamaWikipedia


Axia Corporate Property is pleased to present Units 1 & 2, 69 Collingwood Street, Osborne Park for Lease.
The offering comprises two adjoining units with Unit 1 having a lettable area of 804sqm* and Unit 2 having 392sqm*.
The units can be leased individually or combined to form a total lettable area of 1,196sqm*.
The property is conveniently located within the heart of the Osborne Park commercial/industrial precinct with excellent accessibility to major arterial thoroughfares such as Mitchell Freeway, Scarborough Beach Road, Hutton Street and numerous others.
Astute occupiers seeking to secure very cost effective and conveniently located office/warehouse accommodation in arguably one of western Australia's premier commercial/industrial precincts, need look no further than Units 1 & 2, 69 Collingwood Street, Osborne Park.


text:
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text:
Национальная кинопремия — название нескольких кинематографических премий разных стран:

 Национальная кинопремия (Бангладеш),  — присуждается с 1975 года под эгидой правительства Бангладеш.
 ,  — присуждается с 2007 года.
 Национальная кинопремия (Индия), , , позднее National Film Awards) — присуждается с 1954 года под эгидой правительства Индии.

 Национальная кинопремия (Пакистан)

См. также
Кинопремии с собственным именем, но с этим или схожим словосочетанием в полном названии:

 Национальнальная кинематографическая премия «Ника» — премия России, стран СНГ и Балтии, присуждается с 1988 года.
 Национальная кинопремия «Ак Илбирс» — премия Киргизии, присуждается с 2012 года.


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Sunbrella Elements in Canvas Palm (5421-0000) adds a unique character to any room. Offered by the yard. Warranty: 5 years. Width: 54 in. Weight: 8 oz.


text:
Ronald Florijn (* 21. April 1961 in Leiden) ist ein ehemaliger niederländischer Ruderer. Er gewann bei drei Olympiateilnahmen zwei Goldmedaillen.

Sportliche Karriere
Florijn belegte 1977 im Doppelvierer den vierten Platz beim Match des Seniors, einem Vorläuferwettbewerb der U23-Weltmeisterschaften. 1978 gewann er zusammen mit Victor Scheffers im Doppelzweier die Bronzemedaille bei den Junioren-Weltmeisterschaften. 1979 belegte er im Einer den siebten Platz.

1982, 1983 und 1987 war der 1,91 m große Ronald Florijn niederländischer Meister im Einer. 1983 startete Florijn auch bei den Weltmeisterschaften in Duisburg im Einer und belegte den neunten Platz. 1986 in Nottingham erreichte der niederländische Doppelvierer mit Hermanus van den Eerenbeemt, Ronald Florijn, Henk-Jan Zwolle und Nico Rienks das A-Finale und belegte den fünften Platz. Im Jahr darauf saß nur noch Florijn im Boot. In der Besetzung Hans Keldermann, Ronald Florijn, Robbert Bakker und Jürgen Nelis belegte der niederländische Doppelvierer den sechsten Platz bei den Weltmeisterschaften 1987 in Kopenhagen.

1988 ruderte Ronald Florijn zusammen mit Nico Rienks im Doppelzweier. Bei den Olympischen Spielen in Seoul gewannen die beiden ihren Vorlauf vor dem Boot aus der Bundesrepublik Deutschland. Im Halbfinale belegten sie den zweiten Platz hinter dem Boot aus der DDR aber vor den Schweizern. Im Finale erwiesen sich die Schweizer Beat Schwerzmann und Ueli Bodenmann als die härtesten Gegner. Florijn und Rienks gewannen die Goldmedaille mit 46 Hundertstelsekunden Vorsprung vor den Schweizern, dahinter erhielt das Boot aus der Sowjetunion die Bronzemedaille vor den beiden deutschen Booten.

Bei den Weltmeisterschaften 1989 in Bled siegten im Doppelzweier die Norweger Rolf Thorsen und Lars Bjønness vor Florijn und Rienks. Im Jahr darauf belegten die beiden Niederländer den achten Platz bei den Weltmeisterschaften in Tasmanien. 1991 trat Rienks mit Henk-Jan Zwolle im Doppelzweier an und gewann den Titel bei den Weltmeisterschaften in Wien. Dort startete Florijn im Doppelvierer mit Rutger Arisz, Koos Maasdijk und Hans Keldermann. Die Crew erkämpfte die Bronzemedaille hinter den Booten aus der Sowjetunion und aus Italien. Bei den Olympischen Spielen 1992 in Barcelona belegten Arisz, Maasdijk, Florijn und Keldermann den fünften Platz mit anderthalb Sekunden Rückstand auf die drittplatzierten Italiener.

Im nacholympischen Jahr 1993 wechselte Ronald Florijn in den niederländischen Achter. Bei den Weltmeisterschaften im tschechischen Račice u Štětí belegte das niederländische Großboot den fünften Platz hinter den Booten aus Deutschland, Rumänien, den Vereinigten Staaten und Australien. 1994 in Indianapolis erhielt der US-Achter die Goldmedaille vor den Niederländern mit Kai Compagner, Nico Rienks, Niels van der Zwan, Jaap Krijtenburg, George van Iwaarden, Niels van Steenis, Henk-Jan Zwolle, Ronald Florijn und Steuermann Jeroen Duyster. Im Jahr darauf siegte bei den Weltmeisterschaften 1995 in Tampere der Deutschland-Achter vor den Niederländern, die mit einer Ausnahme mit der Crew des Vorjahres angetreten waren, lediglich Michiel Bartman war für George van Iwaarden ins Boot gerückt.

1996 gewann der niederländische Achter bei den Regatten in Köln, Duisburg und Luzern. Bei den Olympischen Spielen 1996 in Atlanta trat der niederländische Achter in der Besetzung Henk-Jan Zwolle, Diederik Simon, Michiel Bartman, Koos Maasdijk, Niels van der Zwan, Niels van Steenis, Ronald Florijn, Nico Rienks und Jeroen Duyster an. Die Niederländer gewannen ihren Vorlauf vor den Booten aus Kanada und aus Australien. Im Finale siegten sie mit fast zwei Sekunden Vorsprung auf den Deutschland-Achter, dahinter gewannen die Russen Bronze.

Ronald Florijn ruderte für die Amsterdamsche Studenten Roeivereeniging NEREUS. Seine Tochter ist die Ruderin Karolien Florijn.

Weblinks

 Ruderweltmeisterschaften im Achter auf sport-komplett.de

Fußnoten

Ruderer (Niederlande)
Olympiasieger (Rudern)
Niederländischer Meister (Rudern)
Olympiateilnehmer (Niederlande)
Teilnehmer der Olympischen Sommerspiele 1988
Teilnehmer der Olympischen Sommerspiele 1992
Teilnehmer der Olympischen Sommerspiele 1996
Träger des Ordens von Oranien-Nassau (Ritter)
Niederländer
Geboren 1961
Mann


text:
<?php
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	 *
	 * @return string
	 */
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		return Craft::t('Add a tag');
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	// Private Methods
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	/**
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	 *
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	{
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		if ($tagGroupId)
		{
			return craft()->tags->getTagGroupById($tagGroupId);
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	/**
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	 *
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			if (strncmp($source, 'taggroup:', 9) == 0)
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		return $this->_tagGroupId;
	}
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Currently, 216 people are on our waiting list.
216 people in dire need of home repair.
Unfortunately, that list grows daily! Many seniors live on tight budgets. They have to make the difficult choice between fixing their aging homes or paying medical bills. And when their homes are desperately in need of home repair, their options are few and far between. Aging in place becomes harder and harder to achieve.
A Brush With Kindness volunteers helped repaint and repair the home of Patricia Lucas, an 81-year-old Airforce Veteran.
With the help of volunteers, Habitat Tucson combats the crisis every day through our critical home repair projects. Our largest population in need of assistance is seniors. Most are in need of roof repair and air conditioning (in the summer), and furnace or water heaters (in the winter). Habitat Tucson also recieves many requests for windows and plumbing.
Every day our team works to help those in need in our community. Our projects range from roof resheathing to plumbing repairs to installing new doors that can safely lock. One day our construction crew and volunteers help to repaint a chipping exterior, and the next move on to creating new accessible showers for disabled homeowners.
We couldn't do it without our amazing volunteers.
Still, our waiting list grows.
The more hands on deck, the more we can do to make sure the homes in our community are safe, strong, and stable.
We can't do it alone. You can give families a chance to build a better life. Support those in need of critical home repairs.


text:
FIP 63: Human Capital Series 3/3 – Creating Company Culture and the Role of Self-Confidence with Ayla Schlosser
April 17, 2018 /1 Comment/in Podcast /by Andy Narracott
http://media.blubrry.com/the_finding_impact/p/traffic.libsyn.com/findingimpact/FIP063.mp3
Today we hear from Ayla Schlosser, co-founder of Resonate, whose mission is to unlock the leadership potential of women and girls in East Africa. Through storytelling, confidence-building workshops and leadership training, Resonate is aiming to close the confidence gap that impedes opportunity and potential in women. Resonate takes this missed opportunity and turns it into action. As of February 2018, Resonate has worked with over 3000 participants across East Africa and partnered with forty different organizations, including a few big names like Kate Spade, Imbuto Foundation (the flagship organization of Rwanda's first lady Jeannette Kagame), and the Segal Family Foundation
On this episode you'll learn:
How Ayla came to create Resonate. Ayla found that there was a huge emphasis on building skills and education for women, but the internal transformation needed to build confidence and put these skills to use was often overlooked.
Ayla was the problem that she was trying to solve. A big part of her growth came from understanding the difference between standing up for an idea vs. yourself.
What about men? Ayla confirms that women struggle disproportionately. This is due to societal roles, history, and a number of institutionalized and systematic inequalities in other spaces.
Ayla tells us stories about women VPs and Founders that she has met at conferences who have struggled with confidence and the feeling "not enough-ness."
Too much cake? Ayla and her team celebrate their achievements and successes a lot. They have a slack channel dedicated to acknowledging the good work of their team!
Resonate worked backwards into their culture and have been very careful with every hire. A couple years in, they realized that they had a strong culture, but had never codified it. They found times when they felt most proud and uncovered their core values.
Ayla and her team acknowledge that there will be times in the future where they may need to call out times where they didn't embody their desired culture.
They like to check in on their team on a personal level too. "What are you going to do to take care of yourself this week?" Then be accountable and follow-up! Show that you care about your colleagues beyond the work space. It builds trust.
Have you invested in your onboarding process? Resonate has made this a priority. They encourage their staff to, "keep learning and welcome challenges." New hires are given an on-boarding project. It is meant to be 1-2 weeks long and gives them a quick iteration of project cycle and feedback process.
Be like the Hummingbird! Ayla shares one of her favourite stories and how it has inspired a recognition award within Resonate.
Ayla talks about the important of transformations within your own team. Their current Director of Operations began as their administrator and is now working with Execs and Phds in the US.
When employees say "I can't do that or I don't have the skills"; there is a temptation to bring in the experts. Ayla tells us how she has fought this off. That's when people get better. When they are given the opportunity to do something that is slightly out of their depth.
Create a network of mentors and advisors – surround yourself with people who know what they are doing.
Grow your people at the same rate as you are growing your organization and you will be way better off. Invest in everyone!
Ayla tells us about an example of her training having an impact at one of the Kate Spade operations in Rwanda.. Employees were given the confidence to speak up and see their own worth. Ayla considered this a huge step forward.
In start ups, we are always sprinting and moving on to the next thing. Pause to acknowledge. Pay attention to how your employees want to be acknowledged. Some like cake and some would be so embarrassed by that. Knowing the difference will build trust and a rapport.
Feedback can have an inherently negative feeling to it. Positive feedback is super important too. Ayla narrows it down to three different types of feedback – goal oriented, appreciative, and constructive.
Lastly, Ayla reminds us that even experts are always doing some things for the first time. If you don't know something, chances are you can still do it anyway.
Links to Resources:
How startup leaders can use storytelling to motivate their teams – Village Capital
The Little Hummingbird by Michael Nicoll Yahgulanaas
Connect with Ayla:
Ayla on Linkedin
What was your favourite lesson from this episode? Let me know on Twitter by clicking here!
Tags: human capital
https://findingimpact.com/wp-content/uploads/2018/04/CROP-edit.jpg 619 635 Andy Narracott https://findingimpact.com/wp-content/uploads/2017/01/findingimpactlogo250px.png Andy Narracott2018-04-17 19:00:242018-08-09 19:31:28FIP 63: Human Capital Series 3/3 – Creating Company Culture and the Role of Self-Confidence with Ayla Schlosser
FIP 017: Teaching the Skills to Make a Difference with Roshan Paul
FIP 004: Micro-promotion: an effective way to train and retain a low-skilled workforce, with Michael Kuntz
FIP 32: Designing an Organisation that People Love to Work For with Jim Taylor
FIP 61: Human Capital Series 1/3 – Building Strong Teams Through Trial and Error with Anastasia Uglova
FIP 23: Local Talent and Learning to be a CEO, with Xavier Helgesen
FIP 62: Human Capital Series 2/3 – Recruiting and Retaining High Performers at more Mature Organizations with Sarah Perrott
FIP 024: Finding Your Calling, with Jonathan Golden
FIP 007: Developing Middle Management in Africa with Rebecca Harrison
FIP 85: Audience Stories – Emily Woods from Sanivation – Finding Impact says:
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Shrek the Third (2007)
Norbit (2007)
Shrek 2 (2004)
Meet Dave (2008)
Shrek Forever After (2010)
Shrek: The Whole Story (2010)
Tower Heist (2011)
Wall•E (2008)
The Rocker (2008)
Rescue Dawn (2007)
Sunshine (2007)
Sahara (2005)
National Security (2003)
Sunshine Cleaning (2009)
Diary of a Wimpy Kid (2010)
Diary of a Wimpy Kid: Rodrick Rules (2011)
Diary of a Wimpy Kid: Dog Days (2012)
Dallas Buyers Club (2013)
War for the Planet of the Apes (2017)
Year of the Dog (2007)
The Ant Bully (2006)
Miss Congeniality 2: Armed and Fabulous (2005)
Legally Blonde 2: Red, White & Blonde (2003)
The Boondocks—The Complete Second Season (2008)
If Beale Street Could Talk (2018)
Weeds: Season Five (2009)
Just Go with It (2011)
Are We Done Yet? (2007)
Rebound (2005)
Are We There Yet? (2005)
Paul Blart: Mall Cop (2009)
Middle School: The Worst Years of My Life (2016)
This Film On
Peter Canavese 2003-05-05 16:15:39 -0700
90 min. distributer. Director: Steve Carr. Cast: Eddie Murphy, Jeff Garlin, Steve Zahn, Regina King, Kevin Nealon.
Anyone familiar with Chris Columbus's pre-Harry Potter output will recognize Daddy Day Care as a Columbus film: alternately tinkly and sweeping John Williams score, sunny visuals, upper-middle-class characters, well-scrubbed homes, and cute kids. Except Daddy Day Care is scored by David Newman and directed by Steve Carr (Dr. Dolittle 2).
Whatever. It's still the cinematic opiate of the masses. Too hackneyed for adults to truly enjoy and, as ever, a trifle questionable even for the kids in its ability to hold attention between fart jokes, Daddy Day Care cuts a good preview and stars Eddie Murphy, so it's juuuust fine by Hollywood. Crank up the Jackson Five!
Eddie Murphy plays Charlie Hinton, a hapless health-food pusher clogged in the bowels of a junk food conglomerate. Along with his humorously overweight buddy Phil (Jeff Garlin), Charlie gets downsized. Remarkably, this experienced professional utterly fails to hook any employment bites, so he finds himself stewing at home with his young son (Khamani Griffin). While at the park one day, Charlie has a brainstorm: by God, he should open a PG-rated comedy--I mean, a day care center in his home!
Charlie and Phil are the sort of dingbats who think passing out a mission statement to the rugrats is a great idea. Charlie's wife (Regina King) raises an eyebrow, as does the increasingly skeptical Phil, but Marvin (Steve Zahn), the to-the-day-care-born Trekkie who joins Charlie and Phil, knows better: Daddy Day Care is destiny!
Murphy is, unsurprisingly, above this material, so it's a back-handed pleasure seeing him elevate it with easy-going, funny line readings, probable ad libs ("I ain't gonna front. Those little crumb-snatchers got under my skin"), and at least one credible dramatic beat. Garlin has his moments, though he seems ill at ease with an uncharacteristically large part, while Zahn typically aces his typecast slacker role. Garlin and Zahn execute multiple pratfalls with aplomb, but the familiarly inorganic plot machinations blunt the film's attempts at scoring the big laughs.
Screenwriter Geoff Rodkey sets up and knocks down the requisite plot reversals, conflicts, and character types, including the interference of the tightly-coiled Miss Harridan (Anjelica Huston). Huston reprises her tightly-coiled dominatrix-under-wraps persona from The Witches as the headmistress of Chapman Academy, a pre-school which offers SAT prep.
Indeed, Daddy Day Care flirts with horror more than once, first in an "upper class panic" scene which has the Hintons recoil at the white trash alternatives to Chapman, then in a projectile poop scene appropriating Bernard Herrmann's Psycho strings yet once more (might as well put poor Bernie's casket on a mechanized spit).
Such pop music and pop culture references are half the fun of this half-fun (and, it must be said, cute) movie. One of the tykes identifies as the Flash and refuses to doff his beloved costume. Another speaks primarily in Klingon, which immediately endears him to Zahn's fanboy. Jonathan Katz turns up to do his next-generation Newhart routine as the man from Child Services, whose Star Trek puppet show for the kids ventures humorously into adult themes.
The film also includes an appearance by the band Cheap Trick, which is appropriate as it's a rather cheap trick to rip off Mr. Mom (a la Columbus's Tootsie rip off Mrs. Doubtfire). For the record, I'd take Columbus's marginally better cookie-cutter comedies over Daddy Day Care's blunt-edged scissors any day.
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