text:
\section{Introduction}
\label{sec:intro}

Arguably the defining prediction of the canonical Cold Dark Matter (CDM) model
of cosmological structure formation is that dark matter haloes should contain an
abundance of low-mass substructure haloes
\citep[hereafter subhalos; e.g.][]{klypin.etal.1999b,moore.etal.1999,reed.etal.2005,springel.etal.2008,ishiyama.etal.2013},
remnants of the merging hierarchy through which their hosts assembled. Cosmological
$N$-body simulations have revealed that the number density of these subhalos increases
with decreasing subhalo mass scale \citep[e.g.][]{reed.etal.2005}, approximately as
$n_{\rm sub} \propto M_{\rm sub}^{-\alpha}$, with $\alpha \simeq 1.9$
\citep[e.g.][]{gao.etal.2004,diemand.etal.2007,springel.etal.2008,garrison-kimmel.etal.2014},
and this applies equally in the dark matter host halos of massive
galaxy clusters of $10^{15} {\rm M}_{\odot}$ down to the hosts of galaxies like the
Milky Way ($\sim 10^{12} {\rm M}_{\odot}$) and dwarfs
\citep[e.g.][]{angulo.etal.2009,xie.gao.2015,rodriguez-puebla.etal.2016}.

Alternatives to the CDM model, such as Warm Dark Matter (WDM), suppress the abundance
of low-mass dark matter halos, and consequently the abundance of subhalos,
\citep[e.g.][]{smith.markovic.2011,schneider.2013,benson.2013,pacucci.2013}, but
distinguishing between these alternatives and CDM in a robust fashion has proven
challenging \citep[e.g.][]{knebe.etal.2008}. The mass scale at which differences
between plausible dark matter models is most
likely to be evident -- at or below the scale of the satellites of the Milky Way
\citep[e.g.][]{anderhalden.etal.2013,schneider.etal.2014} -- is also the mass scale
at or below which galaxy formation is inefficient and apparently stochastic
\citep[e.g.][]{boylan-kolchin.etal.2011,power.2014,garrison-kimmel.etal.2016}. The latest generation of
cosmological hydrodynamical galaxy formation simulations in the CDM model can produce
satellite populations that are broadly consistent with observations
(e.g. \citealt{brooks.zolotov.2014}, \citealt{sawala.etal.2016a}, \citealt{sawala.etal.2016b},
\citealt{dutton.etal.2016}, \citealt{wetzel.etal.2016}, \citealt{zhu.etal.2016}).
However, it is noteworthy that the internal properties of galaxies and their satellites in plausible
alternatives, such as WDM or Self-Interacting Dark Matter (SIDM), can also provide similarly good
consistency with observations
(e.g. \citealt{zavala.etal.2013}, \citealt{herpich.etal.2014},
\citealt{colin.etal.2015}, \citealt{elbert.etal.2015}, \citealt{fry.etal.2015},
\citealt{governato.etal.2015}).

These results suggest that, provided a galaxy can form, the properties of the galaxy that
we observe are likely to be shaped by the physics of galaxy formation rather than the physics
of dark matter \citep[e.g.][]{herpich.etal.2014}. Arguably this is not so surprising, when one
considers the relative dominance of baryonic material for the central gravitational potential in all but
the most dark matter dominated galaxies, and the relatively short timescales (e.g. crossing times,
cooling times) in these regions. What about the outskirts of galaxies, where timescales are long
and the influence of dark matter dominates that of baryons? Could these regions offer a test of
the underlying dark matter model?

\medskip

Deep observations of the Milky Way and external galaxies reveal that
they are embedded in diffuse, extended stellar structures of shells, streams, and
halos \citep[][]{freeman.bland-hawthorn.2002,helmi.2008}. These structures are strikingly evident
around our nearest massive galactic neighbour, M31 -- see, for example, results from
the {\small PAndAS} \citep[e.g.][]{mcconnachie.etal.2009,mackey.etal.2010} and {\small SPLASH} surveys
\citep[e.g.][]{gilbert.etal.2012} -- and they are also apparent in deep imaging of more distant galaxies
\citep[e.g.][]{martinez-delgado.etal.2010,radburn-smith.etal.2011,monachesi.etal.2013,trujillo.etal.2013,crnojevic.etal.2015}.
Stellar halos are predicted to arise naturally
in hierarchical galaxy formation models, built up, at least partially, by the merger
and accretion events that drive galaxy assemly \citep[e.g.][]{searle.zinn,helmi.white.1999,bullock.johnston.2005,abadi.etal.2006,johnston.etal.2008,zolotov.etal.2009,cooper.etal.2010,font.etal.2011,scannapieco.etal.2011,mccarthy.etal.2012,cooper.etal.2013}; partially, because cosmological galaxy formation simulations have
demonstrated that such halos likely have a dual origin, comprising of a component that
formed in-situ \citep[cf.][]{abadi.etal.2006,zolotov.etal.2009,font.etal.2011}, in
addition to the accreted component that formed via tidal disruption of satellite galaxies
\citep[e.g.][]{bullock.johnston.2005} and star clusters \citep[e.g.][]{boley.etal.2009}.
The in-situ component is believed to originate in dynamical heating of the stellar disc
at early times \citep[cf.][]{mccarthy.etal.2012}, and so it dominates at smaller
galacto-centric radius; in contrast, the outer halo is dominated by the accreted
component (e.g. \citealt{zolotov.etal.2009}, \citealt{scannapieco.etal.2011},
\citealt{amorisco.2015}, \citealt{rodriguez-gomez.etal.2016}).

In this paper, we investigate how the underlying dark matter model might influence this accreted
component by exploring the spatial and kinematic
structure of stellar halos of simulated galaxies, to which we refer hereafter as extended
stellar components (ESCs), and focus on those that form in
cosmological galaxy formation simulations in CDM and WDM models. We reason that there
should be an imprint on properties of the accreted component; because this component
is built up through mergers and accretions of lower mass satellite galaxies, it
follows that a dark matter model that suppresses the abundance of low-mass subhalos, and
consequently low-mass satellite galaxies, is likely to result in less massive -- and
lower luminosity -- ESCs at large galacto-centric radii, or equally, more
centrally concentrated ESCs in WDM models compared to the CDM counterpart.

We do not expect the dynamics of subhalos to differ significantly between CDM and WDM
models \citep[e.g.][]{knebe.etal.2008}. The orbital distribution will be preferentially
radial \citep{benson.2005}, while the orbits of lower mass subhalos and their satellites
will
require many pericentric passages to decay \citep{tormen.etal.1998}; this implies that
tidally stripped stars from a low-mass satellite can be spread over large galacto-centric
distances, and the greater the number of low-mass satellite undergoing such tidal
stripping, the greater the radial extent of the resulting ESC. We make the reasonable
assumption that the physical processes that govern galaxy formation (e.g. cooling, star
formation, feedback) should not depend on the underlying dark matter, consistent with
previous studies \citep[e.g.][]{herpich.etal.2014,governato.etal.2015}. This means that
differences in the properties of the accreted component of the ESC should
reflect differences in the abundance of satellites, which depends on the subhalo
abundance. These differences could be accessible to future surveys that target the
diffuse, low surface brightness environs of galaxies, extending the work of deep imaging
studies such as {\small PAndAS} \citep[cf.][]{mcconnachie.etal.2009} and {\small SPLASH}
\citep[e.g.][]{gilbert.etal.2012} and the the ``Dragonfly Telephoto Array''
\citep[cf.][]{dragonfly}, and so potentially represents an observational test of dark matter.

\medskip

In the remainder of this paper, we present our exploration of this idea, using
cosmological zoom simulations of a set of six Milky Way mass system
($M_{200} \simeq 2 \times 10^12 h^{-1} {\rm M}_{\odot}$). In all six cases, we
follow their formation and evolution in a fiducial CDM model, and for one system
we carry out a further set of simulations in three WDM models, with equivalent
particle masses of $m_{\rm WDM}$=0.5, 1 and 2 ${\rm keV}/c^2$; we motivate these choices
below. All simulations assume
the same prescriptions for cooling, star formation and supernova feedback, and we carry
out a set of simulations to assess the sensitivity of our predictions to the assumed
galaxy formation parameters. Details of the simulations are presented in
\S\ref{sec:sims}. Results of our analysis are given in \S\ref{sec:results}; here we
quantify the $z$=0 spatial and kinematic structure of the ESC; verify that
these results are reasonable in the context of the mass assembly histories of the
galaxies and the orbital structure of the ESC; and estimate whether or not the
differences could provide a useful test of dark matter, allowing for the system-to-system
variation we might expect within the CDM model. Finally, in \S\ref{sec:summary},
we summarise our results.

\section{Simulations}
\label{sec:sims}

\paragraph*{Parent Simulation} The parent $\Lambda$CDM $N$-body simulation is a
$256^3$ particle $L_{\rm box}=50 h^{-1} \rm Mpc$ cube. Following \citet{komatsu.etal.2011},
we assume total matter, baryon, and dark energy density parameters of $\Omega_{\rm m}=0.275$,
$\Omega_{\rm b}=0.0458$, and $\Omega_{\Lambda}=0.725$, and dimensionless Hubble parameter of
$h=0.702$, and we compute the CDM power spectrum using {\texttt{CAMB}} \citep[cf.][]{lewis.etal.2000},
with a power spectrum normalisation of $\sigma_8=0.816$ and primordial spectral index
$n_{\rm s}=0.968$. This results in a particle mass of $m_p \simeq 5.6 \times 10^8 h^{-1} \rm M_{\odot}$.
The simulation is run with {\small GADGET2} \citep{springel.2005} with a constant comoving
gravitational softening $\epsilon=5 h^{-1} \rm kpc$, and candidate haloes for resumulation
are identified in the friends-of-friends (FOF) group catalogue at $z$=0, where we use a
linking length of $b$=0.2$\bar{d}$. Note that we post-process each FOF group to compute its centre of
density $\vec{r}_{\rm cen}$
\citep[using the iterative ``shrinking spheres'' method; cf.][]{power.etal.2003} and obtain
virial masses, which we define as
\begin{equation}
  M_{200} = \frac{4\pi}{3}\times 200 \times \rho_{crit,0} R_{200}^3;
\end{equation}
here $\rho_{\rm crit,0}=2.7755\times10^{11}{\rm M}_{\odot}h^{2}{\rm Mpc}^{-3}$ is the critical density
of the Universe at $z$=0. We select Milky Way mass haloes as those having virial masses of
$M_{200} \sim 2\times 10^{12} h^{-1} \rm M_{\odot}$, which ensures that they are resolved at $z$=0 with
$\sim 3,500$ particles; this is sufficient to define accurately the Lagrangian region at high
redshifts from which the halo collapses.

\begin{table*}
\begin{center}
  \caption{\textbf{Galaxy Properties at $z$=0.} For each of the galaxies that form in our runs with fiducial galaxy formation parameters, we give (1) the virial mass, ${M}_{200}$, as defined in the text; (2,3) $f_{\rm g}$ and $f_{\rm s}$, the fraction of ${\rm M}_{200}$ in gas and stars, respectively; (3,4,5) $N_{\rm d}$, $N_{\rm g}$, $N_{\rm s}$, the number of dark matter, gas, and star particles within ${\rm R}_{200}$; and (6,7,8) $\sigma_{\rm 3D}^{\rm d}$, $\sigma_{\rm 3D}^{\rm g}$, and $\sigma_{\rm 3D}^{\rm s}$, the 3D velocity dispersions of all the dark matter, gas, and star particles within ${\rm R}_{200}$.}
\vspace*{0.3 cm}

\begin{tabular}{lcccccccccc}\hline
  & $M_{200}$   & $f_{\rm g}$& $f_{\rm s}$ & $N_{\rm d}$& $N_{\rm g}$& $N_{\rm s}$ & $\sigma_{\rm 3D}^{\rm d}$ & $\sigma_{\rm 3D}^{\rm g}$ & $\sigma_{\rm 3D}^{\rm s}$\\
  & [$h^{-1} {\rm M}_{\odot}$] &&&&&[km/s]&[km/s]&[km/s]\\
  \hline
MW01 & $2.95 \times 10^{12}$&  0.095 & 0.077 & 518,571 & 298,102 & 242,495 & 303 & 149 & 410\\
MW02  &                      &        &       &         &         &         &
&    &    \\
\hline
WDM0.5 & $2.19 \times 10^{12}$&  0.099 & 0.083 & 374,586 & 227,325 & 190,160 & 293 & 122 & 329\\
WDM1 & $2.28 \times 10^{12} $ &  0.098 & 0.079 & 392,963 & 233,625 & 190,266 & 302 & 156 & 327 \\
WDM2 & $2.203 \times 10^{12}$ &  0.095 & 0.077 & 380,905 & 217,819 & 176,575 & 298 & 137 & 324 \\
CDM & $2.26 \times 10^{12}$   &  0.086 & 0.096 & 385,618 & 204,528 & 227,176 & 319 & 134 & 369 \\
\hline
MW03 & $2.24 \times 10^{12} $ &  0.115 & 0.079 & 392,963 & 233,625 & 190,266 & 302 & 156 & 327 \\

MW04 & $2.45 \times 10^{12}$ &  0.097 & 0.08 & 370,748 & 217,678 & 179,171 & 296 & 147 & 383 \\

MW05 & $2.33 \times 10^{12}$ &  0.108 & 0.077 & 383,492 & 253,462 & 167,170 & 298 & 127 & 368 \\

MW06 & $2.54 \times 10^{12}$ &  0.119 & 0.048 & 392,423 & 279,630 & 111,835 & 265 & 151 & 292 \\

\hline
\end{tabular}
\label{tab:assembly_histories}
\end{center}
\end{table*}

\bigskip

\paragraph*{Galaxy Resimulations} We resimulate a suite of 6 Milky Way mass halos (MW01-MW06; see
Table~\ref{tab:assembly_histories} for details) with both dark matter and gas. They were chosen to
reside in low-density (void) regions, identified using the {\small V-web} algorithm of
\citet{hoffman.etal.2012}, which is a kinematic classification of the cosmic web based
on diagonalisation of the local velocity shear tensor. Our approach to generating initial
conditions is presented in detail in \citet{power.etal.2014}, but we summarise the key
steps as follows.

\begin{enumerate}
\item We select all particles within radius $5 R_{200}$ at $z$=0 centred on
  $\vec{r}_{\rm cen}$ of the halo of interest within the parent simulation, and use
  these to define the Lagrangian volume encompassing the desired high resolution region in the
  resimulation initial conditions at $z=\infty$.
\item We populate this high resolution region with both dark matter and gas
  particles whose relative mass densities are set by the baryon and dark matter density
  pararmeters $\Omega_{\rm b}=0.0458$ and $\Omega_{\rm DM}=0.2292$, and whose number densities are
  set by the desired maximum mass resolution of the resimulation. This high resolution region is
  then embedded within regions of coarser mass resolution consisting of collisionless tidal
  particles, where the average particle mass increases with increasing distance from the
  centre of the high resolution patch.
\item We choose a starting redshift $z_{\rm start}$, in this case $z_{\rm start}=99$, and
  impose the appropriate set of density perturbations on the composite particle
  distribution.

  The first set are applied to all particles and are the original perturbations
  used in the parent simulation, with minimum and maximum wavenumbers, $k_{\rm min}=2\pi/L_{\rm box}$ and
  $k_{\rm max}=\pi\,N_{\rm parent}/L_{\rm box}$; here $L_{\rm box}$ is the length of the parent cube
  and $N_{\rm parent}$ is the number of particles on a side within this cube.

  The second set are applied to the particles in the high resolution region and are a new set of
  perturbations that were not present in the initial conditions; note that we sample from
  the appropiate baryon and dark matter power spectra for the gas and dark matter particles separately.
  Here the minimum and maximum wavenumbers are $k_{\rm min}=2\pi/L_{\rm hires}$ and
  $k_{\rm max}=\pi\,N_{\rm hires}/L_{\rm hires}$, where $L_{\rm hires}$ is the length of the cube
  encompassing the high resolution patch and $N_{\rm hires}$ is the number of particles
  on a side within this cube.

\item Finally, we use the Zel'dovich approximation to generate particles'
  initial displacements and velocities \citep[cf.][]{zeldovich.1970,efstathiou.etal.1985}.
\end{enumerate}
\medskip
In the case of MW02, we run a series of simulations in which we vary galaxy formation
parameters and numerical resolution (see below), and, crucially for this study, the
underlying dark matter model.
Following \citet{bode.etal.2001}, we obtain the initial power spectra
for our WDM models by filtering the CDM power spectrum with an additional transfer
function of the form
\begin{equation}
  \label{eq:transfer}
  T^{\rm WDM}(k) = \left(\frac{P^{\rm WDM}(k)}{P^{\rm CDM}(k)}\right)^{1/2}=\left[1+(\alpha\,k)^{2\nu}\right]^{-5/\nu}
\end{equation}
where $\alpha$ is a function of the WDM particle mass \citep[see equation A9 of][]{bode.etal.2001}, $k$ is the wave-number and $\nu$=1.2 is a numerical constant. We do
not include an additional velocity to mimic the effects of free-streaming in the
early Universe. Arguably this omission is likely to be unimportant for the
WDM particle masses we consider \citep[e.g.][]{colin.etal.2008,angulo.etal.2013}, but
we note also that modelling this effect correctly in a $N$-body simulation is
difficult -- it can lead to an unphysical excess of small-scale power in the initial
conditions if the simulation is started too early (see Figure 1 of
\citealt{colin.etal.2008} for a nice illustration of this problem) -- so for
clarity we ignore this effect \citep[see also discussion in][]{power.2013}.

In running our suite of resimulations, we use a version of {\small GADGET3} that has been
extended to model various galaxy formation processes, which we describe briefly in the following
subsection. Our version of {\small GADGET3} solves the equations of hydrodynamics using
SPHS, a form of SPH that includes a higher order dissipation switch
\citep[SPHS; cf.][]{read.hayfield.2012,hobbs.etal.2013,power.etal.2014,sembolini.etal.2016}
with a Wendland $C^4$ kernel with 200 neighbours \citep[cf.][]{dehnen.aly.2012}.
Gravitational force softenings are set using the \citet{power.etal.2003} criterion,
$\epsilon_{\rm opt}=4\,R_{200}/\sqrt{N_{200}}$, where $N_{200}$ is the number of particles
within $R_{200}$ (cf. Table~\ref{tab:assembly_histories}).

\bigskip
\paragraph*{Galaxy Formation Prescription}
We follow the prescriptions for cooling, star formation, and supernova feedback
set out in \citet{hobbs.etal.2013}, which we now describe briefly.
Gas cools radiatively at temperatures above $10^4$ following \citet{katz.etal.1996},
assuming primordial abundances, and between $10^4$ and a floor of
$T_{\rm floor}$=$10^2$K following the prescription of \citet{mashchenko.etal.2008}.
These simulations do not include chemical evolution, which will influence cooling
rates as the abundance of heavier elements increases, especially in higher density
regions, but we are interested principally in relative differences and adopt the
same cooling rates in all of the resimulations.

Gas is prevented from cooling to the point at which the Jeans mass for gravitational
collapse becomes unresolved. We quantify mass resolution as
$M_{\rm res} = N_{\rm res}\,m_{\rm gas}$, where $m_{\rm gas}$ is the mass of a gas
particle and $N_{\rm res}$ is the number of gas particles that correspond to a single
resolution element; this is set to $N_{\rm res}=128$, which is reasonable for our
choice of smoothing kernel \citep[for further discussion, see][]{hobbs.etal.2013}.
This ensures that the Jeans mass is always resolved within our simulations, and we
write the Jeans density as
\begin{equation}
  \label{eq:jeans_density}
  \rho_J=\left(\frac{\pi\,k\,T}{\mu\,m_p\,G}\right)^3M_{\rm res}^{-2}
\end{equation}
where $k$ is Boltzmann's constant, $G$ is the Gravitational constant, $T$ is gas
temperature, $m_p$ is the proton mass, and $M_{\rm res}$ is the mass resolution, as
defined above. This manifests as a polytropic equation of state $P=A(s)\rho^{4/3}$,
where $s$ is the entropy; gas is prevented from collapsing to densities higher than
given by Eq~\ref{eq:jeans_density}, and any gas that lies on the polytrope forms
stars above a fixed density threshold with an efficiency of $\eta$=0.1, in accord
with observations of giant molecular clouds\citep[e.g.][]{lada.lada.2003}. The
star formation rate follows the \citet{schmidt.1959}
and \cite{kennicutt.1998} relation, $\rho_{\rm SFR}\propto \rho_{\rm gas}^{3/2}$, which
we implement by employing the dynamical time as the relevant star formation
timescale, i.e.
\begin{equation}
  \label{eq:dsfdt}
  \frac{d\rho_{\ast}}{dt}=\eta\frac{\rho_{\rm gas}}{t_{\rm dyn}}.
\end{equation}
We include feedback from supernovae (SNe) by injecting thermal energy from active
star particles into nearby gas particles. Finite resolution implies that each star
particle represents a single stellar population, which we assume to have a
\citet{salpeter.1955} initial mass function, and they become active once the age of
the star particle exceeds the mean main sequence age of stars more massive than 8
$\rm M_{\odot}$ and less massive than the maximum value of 100 $\rm M_{\odot}$. At
that point energy equivalent to $N_{\rm SNe}$ times the individual supernova energy
of $E_{\rm SN}=10^{51}$ ergs is injected as a delta function in time into a mass of
$M_{\rm res}$ gas particles, thereby ensuring that both star formation and feedback
is resolved.

\section{Results}
\label{sec:results}

\begin{figure*}
  \centerline{
    \plottwo{f1a.pdf}{f1b.pdf}
  }
  \centerline{
    \plottwo{f1c.pdf}{f1d.pdf}
  }
  \caption{{\bf Projected density of stellar material within 50 $h^{-1}$ kpc
      radius of galaxy at $z$=0.} The CDM case is shown in the top left;
    the WDM $m_{\rm WDM}$=2, 1, and 0.5 keV/$c^2$ cases are shown in the top right, bottom
    left and right respectively. In each case, we have rotated the galaxy
    coordinates such that it is viewed edge on in the frame of the principal
    axes; see text for further details on how this has been calculated.}
  \label{fig:projected_density_z0}
\end{figure*}

\paragraph*{Visual Impression} In Figure~\ref{fig:projected_density_z0}, we show
how the projected density of
stellar material within a 50 $h^{-1}$ kpc radius, centred on the galaxy, varies
between the fiducial CDM run and its WDM counterparts. In each case, we have
rotated the system such that the central galaxy is viewed edge-on in the
frame of its principal axes, which we do by diagonalising the reduced
moment of inertia tensor computed for star particles within spherical shells,
\begin{equation}
  \label{eq:inertia_tensor}
  I_{ij} = \sum \frac{\Delta x_i \Delta x_j}{r^2}.
\end{equation}
Here we compute offsets in the three spatial components $\Delta x^i$ with respect
to the centre of density of the mass distribution, projected onto the unit
sphere, and then diagonalise to obtain eigenvalues, which provide a measure
of the shape of the stellar mass distribution within the shell, and
eigenvectors, which provide us with the necessary rotation matrix to convert
coordinates into the principal axes. When rotating the system, we use the
rotation matrix derived from the innermost shell of particles.

This Figure reveals a number of points worthy of note. First, the stellar
distribution within the galaxies takes the form of a disc, with a radial
scale length that is broadly the same in each of the runs; visually, the
CDM disc appears slightly more compact than the corresponding WDM discs.
Second, the projected density of extra-disc stellar material is greatest at
small galacto-centric radii, and it is flattened in the direction perpendicular
to the disc. Third, and most significantly for this study, we observe that the
spatial extent of extra-disc material is similar in the CDM and WDM
$m_{\rm WDM}$=2 keV/$c^2$ runs,
but the density appears to decline more rapidly in the WDM $m_{\rm WDM}$=0.5 and 1
keV$/c^2$ runs.

\medskip

\paragraph*{Mass Distribution}
The flattening evident in Figure~\ref{fig:projected_density_z0} is quantified
in Figure~\ref{fig:minor_axes_z0}, where we show how the minor-to-major axis
ratio $c/a$ varies with radius. The behaviour of $c/a$ measured for the different
components is broadly similar across the different dark matter models --
the dark matter $c/a$ varies little with radius ($\sim 0.8-0.9$),
whereas $c/a$ for both the gas and stars is small at small radii
($\sim 0.2-0.4$ at $R \mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$<$}}} 0.05-0.1 R_{200}$) before rising
rapidly between $\sim 0.1-0.2 R_{200}$ to $c/a \sim 0.7$ for the stellar
component and $c/a \sim 0.8-0.9$ for the gas component. This is consistent
with our visual impression in Figure~\ref{fig:projected_density_z0}, at least
for the stellar component.

\begin{figure}
  \centerline{\plotone{f2.pdf}}
  \caption{{\bf Radial variation of minor-to-major axis (c/a) ratio at $z$=0.}
    We have computed a simple measure of the flattening of the mass
    distribution, as quantified by $c/a$, as a function of radius (see text
    for details). Different curves correspond to stellar, gas, and dark matter
    components (green, blue and red curves) in the fiducial CDM run
    (dotted-dashed curves) and WDM $m_{\rm WDM}$=2, 1, and 0.5 keV/$c^2$ curves
    (dotted, dashed, and solid curves).}
  \label{fig:minor_axes_z0}
\end{figure}

\medskip

In Figure~\ref{fig:density_profile_z0}, we focus on the spherically averaged
mass density profiles at $z$=0 for the stars, gas, and dark matter
(green, blue, and red curves) in the CDM and WDM $m_{\rm WDM}$=2, 1, and
0.5 keV/$c^2$ keV runs
(dotted-dashed, dotted, dashed, and solid curves) respectively. Profiles
are constructed by defining the centre of density $\vec{r}_{\rm cen}$ of the
composite system using the shrinking spheres method \citep[cf.][]{power.etal.2003},
sorting particles by radius, and assigning them to 25 spherical
logarithmic bins equally spaced between $R_{\rm min}=0.01 R_{200}$ and
$R_{200}$.

Interestingly, differences in the dark matter and gas mass profiles are small
between dark matter models, especially at radii $R/R_{200}\mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$>$}}} 0.1$. At smaller
radii, the spherically averaged gas density differs by a factor of a
few in density over a factor of a few in radius within $R/R_{200}\sim 0.1$,
but these differences occur in the peripheries of the galaxy disc. However, there
are striking differences in the spherically averaged stellar mass density;
outside of the region within which the galaxy disc reside, between
$R/R_{200}\sim 0.1$ and $R/R_{200}\sim 0.5$, we find that the spherically
averaged stellar density is approximately an order of magnitude smaller in
the WDM $m_{\rm WDM}$=1 and 0.5 keV$/c^2$ runs than in the CDM and WDM 2 keV$/c^2$ runs.

As we demonstrate in Appendix Figure~\ref{fig:density_profile_cdm_z0}, we
expect these differences in the
spherically averaged mass profiles of the ESC to be relatively insensitive to our
choice of galaxy parameters parameters -- the properties of the central galaxy
show a much greater dependence on what we assume for the threshold for star formation
($n_{\rm thresh}$) or strength of supernova feedback ($\epsilon_{\rm feed}$). On the
other hand, we expect our results to be sensitive to mass resolution -- as we resolve
lower mass systems and gas can reach higher densities, where star formation occurs and
how it is affected by, for example, feedback, will affect when stars form and the rate
at which satellites disrupt; this is evident as we go to higher resolution. As we show
in Figure \ref{fig:density_profile_cdm_z0}), this is apparent especially within the central
regions where the galaxy resides at $z\simeq 3$ (the latest time at which we we have data
available currently), although the properties of the ESC are reasonably consistent between
resolutions. However, we focus on relative
differences in this study, and we are confident that the runs we use are adequate for
this purpose.

\begin{figure}

  \centerline{\plotone{f3.pdf}}
  \caption{{\bf Spherically Averaged Mass Profiles at $z$=0.} Here we show
    spherically averaged stellar, gas, and dark matter mass profiles (green,
    blue and red curves) in the fiducial CDM run (dotted-dashed curves) and
  WDM 2, 1 and 0.5 keV curves (dotted, dashed, and solid curves).}
  \label{fig:density_profile_z0}
\end{figure}

\medskip

To what extent are these differences at $z$=0 evident at earlier times?
In Figure~\ref{fig:assembly_history_mvir}, we track the growth of the total
virial mass, which we define as $M_{200}$ at all redshifts, as well as the gas
and stellar masses within $R_{200}$ at each redshift. At late times, the
masses in the different components are similar across the models, but as we
go to earlier times ($z\mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$>$}}} 4$), differences between the models become
apparent. The rate at which both the total mass (upper curves) and gas
mass (middle curves) grows is similar in the CDM, WDM 2 and 1 keV models,
but there is a substantial lag in the 0.5 keV model; the rate at which the
stellar mass grows shows greater variation between the models and is evident
down as late as $z \sim 1$.

We explore the growth the stellar mass in more detail in
Figure~\ref{fig:assembly_stellar_mass}, where we separate stellar mass within
$R_{200}$ into contributions from $R/R_{200}<0.1$, which contain the central
galaxy (upper curves), and $0.1 \leq R/R_{200} \leq 0.8$ (lower curves). This
reveals that, at late times especially, the amount of stellar mass associated
with the central galaxy is consistent between the different dark matter runs;
the differences that we see in Figure~\ref{fig:assembly_history_mvir} are
driven by differences in the outer stellar component surrounding the galaxy.
The contribution from the outer stellar component in the CDM model is
$\sim 2 \times 10^9 h^{-1} \rm M_{\odot}$ at $z$=0 and has remained at this level
since $z \simeq 4$; the contributions in the WDM 1 and 0.5 keV models are
approximately 1/2 and 1/4 of this at $z$=0, but these were larger in the
past, by roughly a factor of 2 at $z\simeq 4$.

\begin{figure}
  \centering
  \plotone{f4.pdf}
  \caption{{\bf Growth of Virial Mass with Redshift.} Here we show how
    the virial mass $M_{200}$, including stellar, gas, and dark matter mass
    (black curves), and the stellar and gas masses (green and blue curves
    resectively) within $R_{200}$ have been assembled as a function of
    redshift, in the fiducial CDM model (dotted-dashed curves) and in the
    WDM 2, 1 and 0.5 keV models (dotted, dashed, and solid curves
    respectively).}
  \label{fig:assembly_history_mvir}
\end{figure}

\begin{figure}
  \centering
  \plotone{f5.pdf}
  \caption{{\bf Growth of Stellar Mass in Halo with Redshift.} Here we
    show how the stellar mass in the halo between $0.1 \leq R/R_{200} \leq 0.8$,
    in the fiducial CDM model (dotted-dashed curves) and in the
    WDM 2, 1 and 0.5 keV models (dotted, dashed, and solid curves).}
  \label{fig:assembly_stellar_mass}
\end{figure}

\medskip
\paragraph*{Kinematics and Orbits}
Figures~\ref{fig:density_profile_z0} and~\ref{fig:assembly_stellar_mass}
confirm our visual impression that the density of stellar material outside of the
galaxy disc drops off more rapidly in the WDM 1 and 0.5 keV runs when compared to
the CDM and WDM 2 keV runs. In
Figure~\ref{fig:velocity_anisotropy_z0} we investigate whether or not this
reflects differences in the kinematics of the stellar material, because the
nature of the orbits that a population of stars follow will be imprinted on the mass
density profile. We quantify this by considering the ratio of the tangential
and radial velocity dispersions, $\sigma_{\rm tan}$ and $\sigma_{\rm rad}$,
which allow us to estimate the velocity anisotropy as a function of radius.
$\sigma_{\rm tan}/\sigma_{\rm rad}\sim 1$ indicates that orbits are approximately
isotropic; $\sigma_{\rm tan}/\sigma_{\rm rad} < 1$ indicates that orbits are
preferentially radial; while $\sigma_{\rm tan}/\sigma_{\rm rad} > 1$ indicates
preferentially tangential orbits.

Figure~\ref{fig:velocity_anisotropy_z0} reveals that the velocity anistropy
of the dark matter is similar in each of the runs, isotropic at small radii
and becoming mildly radial at larger radii. The velocity anisotropy of the
gas shows that it is preferentially tangential (unsurprisingly) within
$R_{200}$. Between $R/R_{200} \sim 0.3$ and $R/R_{200} \sim 1$, it is mildly
tangential and declining with increasing radius, and the behaviour is broadly
similar between the runs. Within $R/R_{200} \sim 0.3$, the behaviour differs
sharply and with no obvious trend with underlying dark matter model; the
anisotropy peaks with $\sigma_{\rm tan}/\sigma_{\rm rad} \sim 3-4$ between
$R/R_{200} \sim 0.02-0.1$. The stellar material follows preferentially
tangetial orbits within $R/R_{200}\sim 0.1$, as we would expect from the
degree of flattening evident in Figure~\ref{fig:projected_density_z0}, but
becomes markedly radial between $R/R_{200}\sim 0.1$ and $R/R_{200}\sim 1$.
There are differences within $R/R_{200}\sim 0.1$ between the CDM run and the
WDM runs; the anistropy profile peaks and starts to roll over at a smaller
radius ($R/R_{200}\sim 0.02$) in the CDM run than in the WDM runs
($R/R_{200}\sim 0.04$), which reflects the slightly smaller radial scale
length we have observed already. At the larger radii of most interest when
considering the ESC, however, we find no appreciable differences.

\medskip

\begin{figure}
  \centering

  \plotone{f6.pdf}
  \caption{{\bf An Estimate of the Velocity Anisotropy at $z$=0.} Here we
    estimate the relative importance of radial to tangential motions by
    showing the ratio of the spherically averaged stellar, gas, and dark
    matter tangential and radial velocity dispersions (green, blue, and
    red curves) in the fiducial CDM (dotted-dashed curves) and WDM 2, 1, and
    0.5 keV (dotted, dashed, and solid curves) runs.}
  \label{fig:velocity_anisotropy_z0}
\end{figure}

Could differences in the spatial structure of the ESC reflect differences
in the kinds of orbits traced out by the progenitors of the material that composes
in the ESC? We check this explicitly in Figure~\ref{fig:orbital_eccentricities},
where we probe the orbits of
the stellar material that lie within the radial range $0.1 \mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$<$}}} R/R_{200} \leq 1$
at $z$=0. Here we characterise the orbit by $R_{\rm min}$, the minimum peri-centric
distance from the centre of the galaxy, estimated from the minimum turning point of
the curve tracking star particle radius versus time\footnote{Note that this is
  distinct from pericentre of first infall; this minimum decreases gradually with
  the number of orbits.}; star particles that are on their initial infall onto the
system lie on the diagonal of $R_{\rm min}$ versus $R_0$, where
$R_0$ is the present day radius. In this Figure, we smooth the distribution
of $R_{\rm min}$ and $R_0$ using a 2D binned kernel density estimate. Our expectation
is that satellite galaxies will follow preferentially radial orbits that bring
them close to the centre of the potential, and this is borne out by this plot --
the majority of the stellar material has values of $R_{\rm min}$ within a narrow
range between $\sim 10$ and $\sim 20 h^{-1} {\rm kpc}$. Few of the star particles
that constitute the ESC are infalling for the first time, and satellites that have
yet to disrupt are apparent as dense knots in the distribution. The key point here
is that there is no systematic difference between the distributions in the
four models; orbits are preferentially radial (cf. \citealt{benson.2005},
\citealt{abadi.etal.2006}, \citealt{khochfar.burkert.2006}, \citealt{font.etal.2011},
\citealt{wetzel.2011}, \citealt{rashkov.etal.2013}, \citealt{jiang.etal.2015}) and there is no
compelling reason why the distribution should differ between
CDM and plausible WDM models, as is borne out by numerical simulations
\citep[e.g.][]{knebe.etal.2008} -- material funnels from the cosmic web and into
the potential of the halo, which does not differ substantially between models.

\begin{figure*}
  \centerline{
    \plottwo{f7a.pdf}{f7b.pdf}
  }
  \centerline{
    \plottwo{f7c.pdf}{f7d.pdf}
  }
  \caption{{\bf Orbital eccentricities of the extended stellar component} Here
    we have tracked
    the orbits of individual star particles and estimated the eccentricity $e$ as the
    ratio of $r_{\rm min}$ to $r_{\rm max}$, where where both are computed following
    initial pericentric passage. The CDM case is shown in the top left; the WDM 2 keV,
    1 keV and 0.5 keV cases are shown in the top right, bottom left and right
    respectively.}
  \label{fig:orbital_eccentricities}
\end{figure*}

\paragraph*{A Potential Test of Dark Matter?} The results presented so far suggest
that the low surface brightness surroundings of galaxies could contain the observable
imprint of dark matter. Could, because the differences between the fiducial CDM model
and WDM are really
only evident in the runs with the more extreme candidates
(i.e. $m_{\rm WDM}<$2 keV/$c^2$). However, for the same reasons that we argued
that there should be differences betweenn the CDM model and dark matter models
in which the abundance of substructure is suppressed, we can also argue that
there should be natural halo-to-halo variation within the CDM model, reflecting
variations in assembly histories.

In Figure~\ref{fig:density_profile_variation_z0}, we show spherically averaged density
profiles for six runs in the CDM model (including the run already presented), all with
virial masses of $M_{200} \simeq 2 \times 10^{12} h^{-1} {\rm M}_{\odot}$ at $z$=0
(cf. Table~\ref{tab:assembly_histories}), and all selected to lie in low-density
environments. This Figure highlights the difficulty of using the ESC as a test
of dark matter -- the system-to-system variation in the properties of the ESC are as
large as we see in the model-to-model variation when we vary the underlying dark matter
model. However, it does suggest that the ESC can be used to extend the
concept of galactic archaeology to systems beyond the Milky Way and Andromeda, as is
being done in nearby galaxies \citep[e.g.][]{martinez-delgado.etal.2010,radburn-smith.etal.2011,dragonfly}
and groups \citep[e.g. the PISCeS survey][]{crnojevic.etal.2015}, and will become possible for
statistical samples of galaxies within the Local Volume with, for example, {\small LSST} \citep[cf.][]{lsst}.
Combining metallicity, kinematics, and spatial structure, it should be possible to
trace the assembly history of galaxies.

\begin{figure}
  \plotone{f8.pdf}
  \caption{{\bf Galaxy-to-galaxy variation in the CDM model.} Here we show
    how much variation between different galaxies we might expect by plotting
    spherically averaged stellar, gas, and dark matter mass profiles (green,
    blue and red curves) for the CDM run already analysed and a further five
    galaxies, all selected to form in low-density regions with
    $M_{200}\simeq 2 \times 10^{12} h^{-1} {\rm M}_{\odot}$ at $z$=0.}
  \label{fig:density_profile_variation_z0}
\end{figure}

\section{Summary}
\label{sec:summary}
We have used a set of cosmological zoom galaxy formation simulations of
Milky Way mass galaxies, with $M_{200} \simeq 2 \times 10^{12} h^{-1}
{\rm M}_{\odot}$ at $z$=0, to explore whether or not the spatial and kinematic
properties of the diffuse, extended stellar components (ESCs), in which galaxies
are embedded, might depend on the underlying dark matter model. In our simulations
of a single system in which we vary the underlying dark matter model, this ESC extends
from approximately $15 h^{-1} {\rm kpc}$, the outskirts of the
galaxy disc, to $R_{200} \simeq 200 h^{-1} {\rm kpc}$, and the stellar remnants of
disrupting satellite galaxies make a signficant contribution to its mass. For our
dark matter models, we considered fiducial Cold Dark Matter (CDM) and Warm Dark
Matter (WDM) alternatives with particle masses of $m_{\rm WDM}$=0.5, 1, and 2
keV/$c^2$; as we discussed in \S\ref{sec:sims}, although models with
$m_{\rm WDM}<2 {\rm keV}/c^2$ are not favoured by current observational limits,
we are interested in establishing whether or not dark matter models that alter
the abundance of substructure could leave an imprint on observable properties of
galaxies. Because the orbital properties of subhalos in CDM and WDM models are
similar, the suppression of low-mass subhalos in WDM models means that the average
subhalo mass is more massive than in the corresponding CDM model, which implies
shorter merging timescales on average. The tail of low-mass subhalos with long
merging timescales in the CDM model means that satellites disrupting in the tidal
field of the galaxy lose mass over an extended radial range, tracking their orbit.
In other words, the nature of
dark matter should be evident in the structure of the ESC, which should be more
centrally concentrated in WDM models with lower particle masses (i.e. warmer dark matter).

Our results confirm our expectation that properties of the ESC do vary with
the underlying dark matter model, but that differences are most readily
apparent only in the more exteme WDM models that we consider, with $m_{\rm WDM}<2 {\rm keV}/c^2$.
The average stellar density between $15 h^{-1} {\rm kpc} \mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$<$}}} R \mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$<$}}} 150 h^{-1}
{\rm kpc}$ in the $m_{\rm WDM}$=0.5 and 1 keV/$c^2$ runs is a factor of $\sim 10$
smaller than in the $m_{\rm WDM}$=2 keV/$c^2$ and CDM runs. This difference is
imprinted early in the history of the galaxy at least back to $z \simeq 4$ -- and
persists to the present day. Interestingly, the properties of the central galaxy, a
thin rotationally supported disc, are in good agreement between the different models,
consistent with the conclusions of previous studies \citep[e.g.][]{herpich.etal.2014}.
Otherwise, the degree of flattening as measured by the axis
ratio $c/a$; the kinematics as measured by the ratio of radial to tangential velocity
dispersions, $\sigma_{\rm tan}/\sigma_{\rm rad}$; and the orbits of stars, as estimated
from the distribution of pericentric distance $r_{\rm min}$ to present day position
$r_0$, are all indistinguishable between models. Similarly, the properties of the
dark matter halo and gas are also in very good agreement between models.

Using properties of the ESC to place observational limits on plausible dark matter models
that suppress the abundance of low-mass subhalos, and consequently satellites, is likely
to be challenging, however. Analysing the results of a further five zoom simulations
of Milky Way mass galaxies, all selected to lie within a similar low-density environment,
we find sufficient system-to-system variation in the properties of the spherically averaged
stellar density profile beyond the central stellar component -- all flattened and rotationally
supported -- to make observational measurements using spatial structure alone that distinguish
between even the more extreme WDM models (i.e. $m_{\rm WDM}<2 {\rm keV}/c^2$) and CDM
unconvincing.

Note that we have focussed essentially on the unresolved ESC -- simply considering the
spatial and kinematic distribution of stellar material in galactic outskirts, because these should be
accessible to deep imaging surveys, possibly stacking large numbers of galaxies by central galaxy
stellar mass or halo mass bins. It is worth noting that there may be potential to look at the
resolved ESC and to combine spatial, kinematic and metallicity substructure information to test
dark matter; this will require the kind of statistical sample of Local Volume galaxies that will be
accessible with LSST \citep{lsst}. Even if this remains a challenging test of dark matter, there is
good reason to expect that we can use properties of the ESC to explore the mass assembly histories
of galaxies, tracing merger and accretion events using material in the outer halo, and placing limits
of the growth of galaxies in the context of their larger scale environment. We will explore this
idea in forthcoming work.

\section*{Acknowledgments}
\noindent The authors thank the referee for their careful reading of the paper.
CP acknowledges support of Australian Research Council (ARC) Future
Fellowship FT130100041 and Discovery Project DP130100117. ASGR acknowledges
support of a University of Western Australia Research Fellowship. Both CP and
ASGR acknowledge support of an ARC Discovery Project DP140100198. CP thanks
Alexander Hobbs and Justin Read for making this version of {\small GADGET-SPHS}
available. The research presented in this paper is undertaken as part of
the Survey Simulation Pipeline (SSimPL; {\texttt{http://ssimpl.org/}). This
work was supported by resources provided by the Pawsey Supercomputing
Centre with funding from the Australian Government and the Government of
Western Australia.

redpajama_set_name: RedPajamaArXiv


text:
<?php
/**
 * Created by PhpStorm.
 * User: erico.oliveira
 * Date: 22/02/16
 * Time: 13:26
 */

namespace CoderOrders\V1\Rest\Clients;

use Zend\Db\ResultSet\HydratingResultSet;
use Zend\Db\TableGateway\TableGateway;
use Zend\ServiceManager\FactoryInterface;
use Zend\ServiceManager\ServiceLocatorInterface;

class ClientsRepositoryFactory implements FactoryInterface {

    /**
     * Create service
     *
     * @param ServiceLocatorInterface $serviceLocator
     * @return mixed
     */
    public function createService(ServiceLocatorInterface $serviceLocator)
    {
        $dbAdapter = $serviceLocator->get('DbAdapter');
        $clientsMapper = new ClientsMapper();
        $hydratory = new HydratingResultSet($clientsMapper, new ClientsEntity());

        $tableGateway =  new TableGateway('clients', $dbAdapter, null , $hydratory);

        $clientsRepository =  new ClientsRepository($tableGateway);

        return $clientsRepository;
    }
}

redpajama_set_name: RedPajamaGithub


Our 2019 degustation dates are finalised! Featuring 4 dates to choose from in 2019 at Botticell Ristorante! Menus will be posted in the weeks prior to the event, but reserve your table today! $100 per person includes 6 courses including 3 Entrees, 2 Mains and a Dessert with wines!
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text:
New 'Harry Potter' e-books are coming this summer
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The series features four short books based on Hogwarts classes. The first book, "Harry Potter: A Journey Through Charms and Defence Against the Dark Arts" publishes June 27 with "Harry Potter: A Journey Through Potions and Herbology," "Harry Potter: A Journey Through Divination and Astronomy," and "Harry Potter: A Journey Through Care of Magical Creatures" following soon after.
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redpajama_set_name: RedPajamaCommonCrawl


text:
/ How BYU Adopted Instagram Stories to Address Sexual Assault on Campus
By: Jon McBride
How BYU Adopted Instagram Stories to Address Sexual Assault on Campus
Using Instagram Stories, Jon McBride and the team at Brigham Young University were able to directly help students who were in crisis or knew someone who was.
Marketing & Branding / March 19, 2019
Last February, I experienced one of the most personally-rewarding days of my career as Media Relations and Social Media Manager at Brigham Young University. Surrounded by a team of colleagues, students, survivors, and subject matter experts, I witnessed the power of social media to leave a positive and lasting impact. Together, we launched an Instagram campaign to better equip our students with the resources they need to handle the epidemic of sexual assault on college campuses. The response our Instagram Story garnered from students is one I'll never forget.
One year and many more Instagram stories later, let's dive into what made this such an important and impactful project.
Rather than merely reacting to the news surround sexual assault issues on our campus, we wondered if there was a way to discuss sexual assault in a more proactive, positive, and helpful way.
How did we tackle such a complex, serious topic using a platform usually reserved for beautiful imagery and photos of food? It took strategic planning, teamwork, and courage. In episode 30 of the Hashtag Higher Ed podcast, I recount this journey in more detail. Here, I've distilled it into four main components:
The Mission: Why we launched the campaign
The Strategy: How we polished and presented the idea
The Process: What the campaign looked like and how we created it
The Outcome: How students responded to the campaign
Part One: The Mission and Vision Behind BYU's Instagram Story Addressing Sexual Assault on Campus
For years, sexual assault has plagued college campuses across the country. And in the #MeToo era, there is increased pressure on colleges and universities to better protect students from sexual violence and support survivors. From a communications perspective, this has left many schools struggling to determine the best course of action. What is an appropriate way to participate in this important conversation while respecting the privacy of the survivors?
Rather than merely reacting to the news surround sexual assault issues on our campus, we wondered if there was a way to discuss sexual assault in a more proactive, positive, and helpful way. We decided to focus on the resources available on campus for survivors of sexual assault and what to do if someone you know is assaulted and needs help. Based on data from our campus climate survey—which said that two out of three students who are assaulted turn first to a friend or roommate before family, Title IX, or on-campus resources—we knew it was important for this campaign to speak to every single BYU student and not just survivors of sexual assault.
Part Two: How We Chose Instagram and Earned Institutional Buy-In
From the moment we had the idea for this campaign, we knew it was critical to connect with students where they already are. Based on conversations with students and recent survey data, we knew most students were using Instagram and that Story consumption was on the cusp of overtaking Feed consumption on the platform. This data gave us the confidence we needed to investigate the platform further as a way to converse with students about such an important topic.
By showing, rather than telling, others about our idea, we were able to effectively demonstrate the strategic impact of this campaign in its final form.
Once we had the initial go-ahead from our boss to explore this idea in more detail, we immediately got to work creating the campaign. Because of how important this topic was to address, we thought it was necessary to go all in from the very beginning in order to give it the best possible chance to succeed. Rather than take a half-baked idea to our high-level administrators, we wanted to show them the finished product and give them as many reasons as possible to say yes.
The good news is that this bold approach worked. After two months of storyboarding, script writing, filming, and editing, we presented the idea to the administration and received the go-ahead. By showing, rather than telling, others about our idea, we were able to effectively demonstrate the strategic impact of this campaign in its final form.
Part Three: Building the Campaign
As we began to craft the script for the Instagram Story, we knew peer-to-peer communication would be at the center of our messaging. We felt it was important to feature real students in the campaign who could walk their peers through how to handle such a sensitive situation. When selecting students for the Story, we wanted to pick people who came across as authentic. These were not theater kids, bubbly cheerleaders, or social media influencers. They were real students who were genuinely interested in the topic and wanted to lend their voices to a meaningful cause on campus.
Before the students agreed to take part in the Story, we had a transparent conversation with them about what the process would look like and the responsibility that comes with being the face of this topic on campus. Since we were talking about sexual assault, we asked students to consider whether someone could potentially level a complaint against them after the Story went live. Ultimately, we wanted to make sure the students felt comfortable and that they'd be able to strike the right tone with our audience.
When selecting students for the Story, we wanted to pick people who came across as authentic. They were real students who were genuinely interested in the topic and wanted to lend their voices to a meaningful cause on campus.
Another thing we took into consideration when planning the Story was the types of direct messages we would get from students the day it went live. We knew students would have questions and that these questions could potentially be nuanced and tricky for us to handle as social media managers. To prepare, we planned to have a room full of experts, including a nursing professor, our Title IX Director, and our survivor advocate on hand that day to answer direct messages from students.
From the start, we knew this wasn't going to be your average Instagram story. Because of the nature of the discussion, we wanted the production quality to be top notch in order to signal to students that this was something different—something worth paying greater attention to. To improve the quality of this particular story, we used high-quality visuals that were carefully shot by our department videographer and then incorporated text overlays.
Since the story went live at 9 a.m., we wanted to be conscious of students who might be commuting or in class and scrolling through Instagram with the sound off. Aside from having students and subject matter experts talking on screen, we also broke up the story with text overlays and images of the resources they would need. This way, they could easily screenshot the addresses and phone numbers they'd need to get help. Finding the right mix of student advocates, trained professionals, and text-based resources was an important part of telling this story. We wanted students watching to feel comfortable asking for help and to know exactly how to go about it.
This was far from a lighthearted, funny, flashy Instagram Story that was going to go viral on its own. Instagram Stories also don't have a built-in Share or Retweet button to help these spread, either. We knew we needed to focus on promotion to get this important topic in front of as many students as possible. We promoted it on our official university accounts on Twitter and Facebook and notified our social media committee on campus, which is made up of anyone who runs a social account related to BYU.
The campaign generated a response beyond what we had imagined: 24,000+ unique views and more than 100 direct messages from students.
Then, we notified our street team who have influence in a number of different areas on campus. We provided these influencers with assets from the campaign, including the first part of the Instagram Story with a filter over it and a text overlay showing people how to get to the Story. However, we made it clear that they didn't have to use the exact example we provided. Finally, we asked them to like, comment, and share the Story to amplify its message.
Lastly, we leveraged the experts in the Story to share it and to even help pitch this to the media for us. Rather than going directly to the media, one of our nursing professors from the video volunteered to send an email to some of her press contacts. The media was interested in covering the project, so we created an embargoed version of the Instagram Story that we could send to them before it went live. This brought high-profile press coverage to campus the day the campaign went live.
Part Four: The Impact of an Instagram Story
The campaign generated a response beyond what we had imagined: 24,000+ unique views and more than 100 direct messages from students. This Story garnered more eyeballs and higher engagement than our typical, fun Instagram stories do, which is a testament to our promotion strategy as well as to our audience, who really did want to consume this content.
The DMs were remarkable to see. Some came from students who were personally in crisis. We were able to immediately connect them to our experts in that room, and through our Instagram account, they were setting up appointments with those students to come in and get the help they needed. There were many other nuanced questions that began vitally-important conversations. It was absolutely remarkable to step back throughout the day and realize that such incredibly-meaningful conversations were being facilitated through Instagram. Walking out of the office at the end of the day, it was the most rewarding experience I've experienced professionally.
For years, the higher ed social media community has been talking about moving beyond just entertaining audiences with things like memes and cat videos. Pure entertainment has been the focus on social media for so long, but we felt it was time to start using our platform for good and to truly make an impact. With this campaign, we were able to use Instagram to directly help students who were in crisis or knew someone who was. This was an eye-opening, powerful experience that was rewarding far beyond the paycheck.
Check out Bringham Young University on Instagram to see the full Story addressing sexual assault on campus.
Jon McBride
Media Relations and Social Media Manager
A hockey-playing Canadian by birth who still says "sorey," Jon McBride transplanted to Utah in 2001 and hasn't found a reason to leave. Jon is one of the few digital marketers who can say he's been working in social media for 10+ years. He started Weber State's social accounts in 2008, shortly after Facebook Pages were launched. Jon is now a media relations and social media manager at BYU where he brings a media relations approach to spreading the digital reach of the university. Jon writes feature stories, pitches to media, oversees social strategy campus-wide and manages an amazing student street team. Jon's most unique professional accomplishment was landing a pitch to Beyoncé's publicist and getting a post out to her 63 million Facebook followers. His recent focus has been tackling tough topics such as sexual assault, consent, hate speech and mental health through institutional Instagram stories.


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Updates »In The News
Check out all the great work MassBike is doing across the commonwealth. We keep our supporters updated on our MassBike Updates page, but here you will find what other people are saying about MassBike.
This page is updated periodically with news articles that feature MassBike's work across Massachusetts.
"Worcester E-Bike Users Have Traveled Halfway Around Earth" (Patch - 1/24/23)
"Getting Boston on board with e-bikes" (Commonwealth Magazine - 1/11/23)
"Cars need to stay 4 feet away while passing bikes, pedestrians, new Mass. law says" (MassLive - 1/3/23)
"Pedestrians, cyclists gain protections with new law meant to reduce traffic deaths" (Boston Globe - 1/3/23)
"MassBike shares why bicycling in Massachusetts is tops in the nation" (WWLP - 1/24/23)
"Road safety bill again headed to Baker" (Newburyport News - 12/31/22)
"Prospective Buyers Await Details of Mass. E-Bike Rebate Program" (Streetsblog MASS - 12/15/22)
"How To Bike through a Boston Winter" (Streetsblog MASS - 12/5/22)
"Baker gets bill to protect 'vulnerable' road users" (WWLP - 09/14/22)
"A bill sent to Gov. Charlie Baker would protect 'vulnerable road users' like cyclists and pedestrians" (The Berkshire Eagle - 09/13/22)
"New Worcester E-Bike Users Take Group Tour Of City" (Worcester Patch - 08/22/2022)
"Politics and the City: E-Bikes 'take the lane' on Worcester Streets in Pilot Project" (Worcester Telegram & Gazette - 08/21/2022)
"Orange Line shutdown: Some tips to safely bike around shuttle bus routes" (Boston Herald -08/20/2022)
"Last-Minute Legislation Legalizes (Some) E-Bikes, Axes Low-Income Fares, and Throws More Cash At EVs" (Streetsblog MASS - 08/01/2022)
"Massachusetts Bicycle Coalition starting Worcester e-bike program" (Spectrum News1 - 06/10/2022)
"Cyclists honor Black female biking pioneer of the late 1800s" (Boston Globe - 05/05/2022)
"MassBike giving away 100 free electric bikes to Worcester residents, workers; Here's how you can get one" (MassLive - 05/26/2022)
"Green Program Offering Free E-Bikes To Worcester Residents" (thisweekinworcester.com - 05/24/2022)
"What is an e-bike? Advocates in Mass. want to update definition, legal framework in hope they help reduce greenhouse gas emissions" (MassLive - 05/11/2022)
"Massachusetts Ranked #1 in 2022 Bicycle Friendly State Report Card" (MassDOT Blog - 04/19/2022)
"Worcester MassBike Program Provides Free E-Bikes to Low Income Residents" (WBZ NewsRadio 1030 - 04/05/2022)
"How Massachusetts is getting electric vehicles, e-bikes to low-income populations" (Worcester Telegram & Gazette - 03/31/2022)
"Mass. Clean Energy Center Awards $3 Million to New E-Bike Subsidy Programs" (Streetsblog MASS - 03/09/2022)
"Push to strengthen Massachusetts' hands-free driving law hits Beacon Hill" (WCVB 5 - 03/09/2022)
"E-Bikes For Worcester Residents: Grant Funds Test Program" (Patch - 03/08/2022)
The Horse Race - Episode 218: E-Bicycle Built for Who? (6/23/2022 - Featuring MassBike ED, Galen Mook)
"MassBike Gives & Sheds Light on Bicycling Safety" (WBZ NewsRadio 1030 - 12/7/2021)
"Road-safety advocates push Massachusetts lawmakers to pass road safety bills as fatalities pile up" (Boston Herald - 11/21/2021)
"This Sunday, think about ways to reduce traffic fatalities" (Commonwealth Magazine - 11/19/2021)
"MassBike Hands Out Free Lights for the Long Nights" (Streetsblog MASS - 11/8/2021)
"E-bikes are here – the question is where should by be?" (The Boston Globe - 10/31/2021)
"As e-bikes soar in popularity, a proposed Massachusetts law would clarify how and where they can be used" (The Berkshire Eagle - 10/21/2021)
"MassDOT chooses design for $1.7B Allston Pike project" (ConstructionDive - 10/5/2021)
"MassDOT Picks "At-Grade" Option for Allston/I-90 Project" (Streetsblog MASS - 9/29/2021)
"September is Bike Month in Massachusetts" (22 News WWLP - 9/21/2021)
"Cape Cod Celebrating Bike Month with Several Events" (Patch - 9/20/2021)
"Five steps toward a better bike strategy" (Commonwealth Magazine - 9/18/2021)
"MassBike Celebrates Bay State Bike Month In September" (massitsallhere.com - 9/10/2021)
"The West End Museum Celebrates Bay State Bike Month on Sept. 18" (Beacon Hill Times - 9/8/2021)
"New Berkshire County Campaign Celebrates Bike Safety" (WUPE.com - 8/31/2021)
"Berkshire Bike Path Council Kicks Off Berkshire Streets for All" (iBerkshires.com - 8/31/2021)
"Group to launch bike safety campaign with ride down Pittsfield's North Street" (The Berkshire Eagle - 8/30/2021)
"Getting tuned up: Bike Repair clinic at Florence Heights gets cyclists back on the road" (Daily Hampshire Gazette 8/22/2021)
"MassBike giving away free bike lights to cyclists" (22 News WWLP - 4/9/2021)
"Meet Peter Cheung, MassBike's 'Advocate of the Year'" (Streetsblog MASS - 12/17/2020)
"New Ghost Bike, and finished Bike Lanes, Honor BU student Killed in 2021 Crash" (BU Today - 12/2/2020)
"Ghost bike honors cyclist's memory, impact on Commonwealth Avenue" (Boston Globe - 11/21/2020)
"'Ghost bike' memorial in Boston dedicated to victim of deadly 2012 crash" (WCVB 5 - 11/21/2020)
"Bicycle light giveaway in Turners Falls encourages road safety" (Greenfield Recorder - 11/6/2020)
"As I See It: Biking for health in the face of pandemic" (Newburyport News - 10/13/2020)
"Local bicyclist honored with Minuteman Bikeway memorial" (yourArlington.com - 9/9/2020)
"Bicyclist dies after crash involving tractor-trailer in Harvard Square" (Boston Globe - 8/18/2020)
"'Bike boom' clearing out bicycle shops in Boston" (Boston Herald - 8/2/2020)
"Meet the Pedal People, Northampton's Bike-Powered Cargo Haulers" (Streesblog MASS - 7/6/2020)
"Hamilton-Wenham Public Library announces upcoming programs" (Wicked Local - 6/9/2020)
"Charlie Proctor Memorial Fund" (Scuttlebut Sailing News - 5/13/2020)
"Biking in the Valley: Even with COVID-19, bicycling is the way to go for many" (Daily Hampshire Gazette - 4/6/2020)
"Bike Shops Deemed 'Essential' As Bike Transport Surges" (Streetsblog MASS - 4/24/2020)
"Westfield Breaks Ground on Columbia Greenway Extension" (Streetsblog MASS - 1/30/2020)
"Should low speed electric bikes be allowed on multi-use paths in Mass.?" (Boston Globe - 12/19/2019)
"Street Safety Advocates Hold 'Day of Remembrance' Vigil This Sunday" (Streetsblog MASS - 11/15/2020)
"E-bikes get green light on National Seashore trails" (Cape Cod Times - 9/30/2019)
"Biking In Boston: What To Know Before You Get Rolling" (WBUR - 5/30/2019)
"Junior high schoolers giddy up at bike rodeo" (Sippican Week Today - 5/2/2019)
"Bike Activists, Armed with Video of Fatal 2015 Back Bay Crash, Say Police Got It Wrong" (Boston Magazine - 1/24/2018)
"Cyclists Want Truck Driver Charged After Fatal 2015 Crash" (CBS Boston - 1/23/2018)
"Group blames truck driver for fatal 2015 bike crash; police say prosecution's not warranted" (Boston Globe - 1/23/2018)
Jes Slavin published this page in Updates 2020-12-28 16:09:58 -0500


This work is a self-study examining my positioning as a Grade 10 Essentials math teacher during one school semester. Using a framework that draws on Bandura's (1995) notion of self-efficacy, Dweck's (2000) ideas of growth mindset, and Costa and Kallick's (2008) and Cuoco, Goldenberg, and Mark's (1996) work on habits of mind and mathematical habits of mind, I sought to position myself and my teaching in a way that would increase my students' sense of confidence and capability in mathematics. I used narrative inquiry (Clandinin and Connelly, 2000) and autobiographical narrative (Bullough & Pinnegar, 2001) as interpretive frames to re-tell the story of the semester. What I came to understand is that I need to operate with a positioning that is dynamic, open-minded, and rooted in the notions of care (Noddings, 2013) and expectation if I hope to nurture students who are not only confident and capable, but who also accept the key role they must play in growing as effective and responsible learners. Despite being rooted in a particular time and place, and with particular students, this story seeks to acknowledge the realities teachers face in an honest and hopeful manner.


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Angel: Long Night's Journey by Brett Matthews and Joss Whedon: C-
February 15, 2010 by Michelle Smith 2 Comments
An enemy from Angel's past has come to L.A., and enlisted three powerful supernatural creatures to break Angel's spirit before killing him. In one catastrophic night, Angel has to figure out who's after him, and then bring him down, in a climactic battle above the glittering Los Angeles skyline.
Wow, this is really lousy. It's written at least partly by Joss, but it's so lackluster that it'd pass for something written by Keith R. A. DeCandido.
The basic plot is thus: a boobalicious snake lady (Joss seems to like these, since one appears in the Buffy season 8 comics), a fiery stone guy, and a knight with a glowy sword all attack Angel and are eventually bested. A symbol on the knight's chest (Joss seems to like this idea, too, since it also figures into the season 8 comics) clues him in to the fact that his foe is a Chinese vampire he once met.
Turns out the Chinese vamp is upset because he was supposed to be the champion vamp with a soul but instead Angel has that role. This plot is pretty irksome, because it all of a sudden introduces notions like that when Angel was cursed, he was just a test subject for the real deal, and that perhaps the soul he received isn't even his. It's annoying and vague and I'm happy all of these ideas were dropped along with Dark Horse's publication of Angel comics after this miniseries.
The art is competent enough except that nobody looks like they should. I conducted a test by obscuring all but one panel, which featured Cordelia and Wesley, and asking my Whedon-loving coworker, "Who are these people?" She stared at it for a full minute and could not hazard a guess, even though she'd surmised the answer was probably Whedon-related. Cordelia comes off the worst, looking either trampy or middle-aged, and sometimes both at once. Still, it's so nice to see her appear in a comic at all that I have revised the grade slightly upward from the D this dreck truly deserves.
Filed Under: Comics, Media Tie-In, Supernatural, Whedon Tagged With: Angel, Dark Horse
The Angel art has really been a problem altogether. I haven't read this one, but you know my opinion on the art in the official S6 comics. Blah.
Of the two, I think I actually prefer the S6 art. At least the characters look right some of the time.


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The Speed of Now World Tour 2022
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Keith Urban has spent the better part of his life harnessing a deep-seated passion for music. This, when combined with his authenticity, talent and driving musical inquisitiveness, helps to understand why he is one of the most successful and well-respected artists in the world. He's won four GRAMMY© Awards, thirteen CMAs, fifteen ACMs, three AMAs, two People's Choice Awards and celebrated nine consecutive gold, platinum or multi-platinum albums.
On August 19, Urban began a new musical chapter. He released "Wild Hearts," an autobiographical, fist-pumping, arena-ready Urban track that is as authentic as it is infectious – quintessential Urban. It comes on the heels of "One Too Many" (his duet with P!nk), the last from The Speed of Now Part 1, which marked his fourth in an historic streak of simultaneous #1 album debuts in the United States, Canada and Australia. He also collaborated with Yamaha for the release of the URBAN Guitar and lessons app. The rest of the year has seen Urban featured on two songs from Taylor Swift's album Fearless (Taylor's Version) including "That's When" and "We Were Happy," a part of the performance of the John Lennon's "Imagine," for the opening ceremonies of the Olympics, as well as his return as host for the 56th Annual Academy of Country Music Awards with Mickey Guyton.
But while plans for a 2020 U.S. Tour were put on hold due to COVID, the wait is now over. The stage is set for what will be Urban's biggest tour in nearly four years, "The Speed of Now World Tour 2022," which will play to fans in six countries, including in the U.S., U.K., Germany, Netherlands, Australia and Canada, on three continents. Urban's concerts have become legendary - as unpredictable as they are explosive. An explosive experience of emotion, musical texture, energy and showmanship, Urban's concerts connect to and touch every soul whether in an arena of 15,000 or outdoors in front of 50,000 "Speed" produced the top 5 songs "God Whispered Your Name," and "We Were," as well as "One Too Many" that not only gave Urban his 43rd Top 10 single in the U.S. and his 27th #1 in Canada. The song also reached #1 on the Australian Artist singles chart, spent 44 weeks in the Top 50 on the UK Airplay Chart and garnered over 100 million Spotify streams in just 10 months.
Urban's musical virtuosity and fluidity has made him the musician's musician. He's collaborated with a diverse group of artists that include, among others; Billy Gibbons, Buddy Guy, Carrie Underwood, Chris Stapleton, Eric Church, John Mayer, Julia Michaels, Justin Timberlake, Dzeko, Miranda Lambert, Nile Rodgers, Post Malone, Taylor Swift, The Rolling Stones and Vince Gill.
He's long supported numerous charities. His "All For The Hall" benefit concerts for the Country Music Hall of Fame and Museum© have raised over $4.2 million. He is the first Ambassador of the CMA Foundation, an advisory board member at the St. Jude's Children's Hospital and is a longtime supporter of The Mr. Holland's Opus Fund and The Grammy Foundation.
Presented by Walmart AMP in partnership with Live Nation.


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Scuba Forum - Scuba Diving Forums and Discussion Board > Forums by Diving Categories > Marine Life > Lake Divers - News in the Fight Against Al-Quaqqa!
View Full Version : Lake Divers - News in the Fight Against Al-Quaqqa!
At least those concerned with invasive mussels. Here's an article about stocking with sunfish to fight quaqqa and other mussel infestation.
Unfortunately, it's from our local print newspaper, and doesn't cite any references.
Very interesting article. Lake Champlain had a big problem with zebra muscles.
Thank goodness they are "waiting to see" how it goes elsewhere before acting on this idea. Some people would have just gone ahead with it.


What do you enjoy about serving in Virginia's House of Delegates?
The best part of my job is being able to meet people and to learn about their interests and concerns. I am constantly exposed to new information and new networks of people which helps me connect the dots to assist others.
I wished I knew Virginia and American history better. As an immigrant who came to America at age 14, I didn't have the opportunity to learn sooner, so I've been trying hard to catch up as an adult on what I missed through formal education.
Leadership generally means to act and to not ignore a problem when you see it, and to offer solutions in place of criticism. In public service, leadership means understanding the roles and limitations of government in order to best utilize the tools and resources of government to improve people's lives and society at large.
For others who wish to follow in your footsteps, what skill sets are beneficial in serving as an elected official?
Being open-minded and willing to meet everyone and listen to every viewpoint, even if I disagree. I also recognize my own limitations and know that I don't know a lot so I need to collaborate with others who are knowledgeable.
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Picked up my first track bike yesterday. Planning to race quite a bit this year at the local Velodrome, which appears to be a good one. The bike is a 2019 Throne Track Lord (I guess I can't post a pic until I have had 10 posts). This is basically the third iteration of this bike. People had some complaints about the first two, but this one seems really solid for the price. Nice and stiff, carbon seatpost, carbon fork, and relatively lightweight. I am more than satisfied so far.
Right now, I am viewing this as my starter bike. If I like racing a bunch, I plan to upgrade to some aero carbon wheels soon (probably HEDs or Yoeleos) and then possibly get a nicer frameset (probably a Look 875 Madison, Dolan DF4, Fuji Track Elite, or Argon 18 Electron C) next season. Looking forward to getting into the track scene big time though.
I am definitely open to any ideas or recommendations anyone has at this point.
Last edited by rashadabd; 12-09-18 at 07:59 PM.
Right now, I am viewing this as my starter bike. If I like racing a bunch, I plan to upgrade to some aero carbon wheels soon (probably HEDs or Yoeleos) and then possibly get a nicer frameset (probably a Look 875 Madison, Dolan DF4, Fuji Track Elite, or Argon 18 Electron C) next season. Looking forward to getting it the track scene big time though.
Nothing like a new bike to get the excitement going. Tell us, where is your local track? Check out there program and take there introductory courses or mandatory certification class. Track cycling is a great venue for competition and community. Have fun!
Thanks man! Couldn't agree more. It's Boulder Valley Velodrome. I am really looking forward to this spring and plan on signing up for the certification course sometime between now and then. Thank you for the info!
You lucky dog! Beautiful facility. I was in the area this summer and stopped by to visit. There was a training session on, and I met the father of a junior rider. We spoke for awhile, good guy. The director of the track is a former National team rider from my generation. You will be in a great place to learn.
Hi. Welcome to the forum and to the sport!
This thread is a few years old, but the info therein is still valid. Most questions you have (and many you haven't thought of, yet) are covered there.
Thank you for the confirmation. They certainly seem top notch from everything I have seen and heard. We also have the Olympic training center track about an hour and a half away as well. I might check them out at some point as well. I agree though, being a cyclist in Colorado definitely has some benefits.
Thanks Carleton! I will try to check this stuff out while I have some time off over the next few weeks.


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Having recently got a Macbook Pro, I installed Xcode and tried to port zenlang over to it. The lemon parser was a piece of cake, but re2c... not so much. This is using XCode 4.3 on OSX 10.7.
Having downloaded and extracted the source tarball, I tried running ./configure and got the error "C++ compiler cannot create executables".
The config.log file showed that the test file created by ./configure wasn't getting linked, it could not find crt1.10.6.
Now configure goes through successfully, but make doesn't. It is unable to find the standard include files, so I had to re-run configure with the include paths, again, discovered using find.
Note that we are also adding the include directory for the C++ header files (iostream, iomanip, etc) as well.
Now make should run successfully and create the re2c binary.