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

\begin{figure*}
\gridline{
\fig{shifts.pdf}{0.375\textwidth}{(a)}
\fig{Figure_6.pdf}{0.675\textwidth}{(b)}
}
\caption{
Effect of an LMC-induced shift in the COM positions and velocities on the observed MW dwarfs.
Panel (a) shows the shifts in the center-of-mass position $\Delta r_i$\ and velocity $\Delta v_i$\ for simulation particles in spherical shells of distance $r$\ around their host galaxy center, in three Cartesian coordinates $i \in \{x, y, z\}$, with $x$ measured along the Galactic Center-Sun direction, $y$ in the direction of Galactic rotation at the Sun, and $z$ towards the North Galactic Pole. The results reported by \citetalias{GC21} are shown (solid lines) and compared to our final simulation snapshot (dashed lines). Panel (b) shows the positions and velocities (as vectors) of the MW satellites. They are color-coded by the observed alignment angle $\theta_\mathrm{VPOS}^\mathrm{obs}$\ of their orbital pole directions with the VPOS normal (red is co-orbiting). Smaller, fainter symbols indicate the position after applying the \citetalias{GC21} shifts from panel (a) in reverse. The $y-z$\ plane is displayed, in which the majority of the shift takes place and which aligns well with the VPOS. The position and orientation of the edge-on MW is indicated in green.
\label{fig:shifts}}
\end{figure*}

The phase-space correlation of satellite galaxies around their hosts is currently one of the most pressing challenges for our understanding of galaxy formation \citep{2017ARA&A..55..343B, 2018MPLA...3330004P}. In short, a large fraction of dwarf satellite galaxies of the Milky Way and M31 are distributed within flattened and kinematically coherent structures that are at odds with the expected phase-space distribution of their associated dark matter sub-halos \citep{2005A&A...431..517K, 2013Natur.493...62I}. In the Milky Way, this structure is called the Vast Polar Structure (VPOS, \citealt{2012MNRAS.423.1109P}): it is perpendicular to the galactic disc, has a root-mean-square thickness of only $\sim$25 kpc for a 10 times larger spatial extension, and its normal vector is aligned with the orbital poles of 50\% to 75\% of the galaxies spatially located in it \citep{2021ApJ...916....8L}.

Similar planar structures have been found outside of the Local Group \citep[e.g.][]{2018Sci...359..534M, 2021A&A...645L...5M, 2021ApJ...917L..18P, 2021A&A...652A..48M, 2021arXiv210810189H}, and are calling for an explanation. Many theoretical scenarios for the formation of these satellite-plane structures have been proposed over the years \citep[for a review, see][]{2018MPLA...3330004P}, but thus far all have failed to clearly reproduce the extreme phase-space distributions observed around real galaxies. Recently, a new possible explanation for the VPOS around the Milky Way has been put forward by \citet{GC21} (hereafter \citetalias{GC21}). It partly relies on the old observation by \citet{1976MNRAS.174..695L} and \citet{1976RGOB..182..241K} that the Large Magellanic Cloud (LMC) and the Magellanic Stream, align with and orbit along the VPOS.

In recent years, an array of evidence has accumulated for a more massive LMC than initially thought \citep{2013ApJ...764..161K, 2016MNRAS.456L..54P, 2019A&A...623A.129F, 2020MNRAS.495.2554E, 2021NatAs...5..251P}, with a total mass at infall of at least $1.5 \times 10^{11} \, {\rm M}_\odot$. Such a massive LMC should necessarily cause a shift in the orbital barycenter of the Milky Way–LMC system compared to the center of the Milky Way disk, which could influence the kinematics of satellite galaxies.

\citetalias{GC21} demonstrated with a numerical simulation of a massive LMC-analog interacting with a MW-like host that the resulting reflex motion and offset in overall center-of-mass conspire to induce an overdensity of orbital poles in the dark matter particles that constitute the dark halo of the MW model. The direction of this overdensity aligns with the orbital pole of their LMC analog. As the orbital pole of the observed LMC is well aligned with the observed VPOS and its associated overdensity of satellite galaxy orbital poles, \citetalias{GC21} suggest that this LMC-induced effect might help explain the presence of the VPOS.

We here go beyond the original study and test whether this proposed mechanism can have a sufficient effect on the inferred orbital poles of the {\it observed} MW satellite system.

\section{Effect on Milky Way Satellites} \label{sec:MWsats}

\begin{figure}
\gridline{
\fig{Figure_2.pdf}{0.4\textwidth}{(a)}
}
\gridline{
\fig{Figure_4.pdf}{0.4\textwidth}{(b)}
}
\gridline{
\fig{Figure_3.pdf}{0.4\textwidth}{(c)}
}
\caption{
Panels (a) to (c) show the relative effect that the COM shifts have (see Fig. \ref{fig:shifts}) on the position and velocity, angular momentum, and direction of orbital pole, respectively. Here and throughout the following figures the MW dwarfs are color-coded as in panel (b) of Fig.~\ref{fig:shifts}.
\label{fig:shifts2}}
\end{figure}

\citetalias{GC21} argue that the orbital pole enhancement in their simulation can be reproduced by shifting the positions and velocities of simulation particles in the initial conditions. Effectively, this means that for different radial shells, different reference centers-of-mass (COM) are adopted, mimicking the perturbation to the MW dark matter halo by the infall of a massive LMC. They have demonstrated that this approach accounts for both the degree and direction of the orbital pole overdensity of dark matter particles in their simulation, making a convincing argument for the validity of their model.

We adopt this model but invert the approach to estimate to what degree the infall of the LMC can be responsible for the observed clustering of satellite orbital poles. If adding shifts to an isotropic initial distribution reproduces the LMC's influence, then subtracting those shifts from the observed MW dwarf galaxies, which are exposed to the LMC influence, should substantially reduce the observed orbital pole overdensity if its main cause is the gravitational influence of the LMC.

In Fig. \ref{fig:shifts} we reproduce the COM shifts (as obtained from figures 4 and 6 in \citetalias{GC21}). We subtract the respective distance-dependent values from the Cartesian positions and velocities of the observed MW satellites, for which we adopt the dataset by \citet{2021arXiv210608819B} who provide proper motions based on Gaia EDR3. Here and in the following we focus on satellites in the Galactocentric distance range of 50 to 250\,kpc, which results in a sample of 31 dwarfs. For more nearby objects no effect due to the LMC is expected according to \citetalias{GC21}, while more distant objects have only weakly constrained orbital poles due to the large proper motion uncertainties.

Panel b of Fig. \ref{fig:shifts} plots the most-likely positions and velocities of the MW satellites. Also shown are the shifted positions and velocities. For most dwarfs the shifts are minor. The overall orbital directions do not appear to be substantially altered; especially the objects co-orbiting closely along the VPOS (red) keep their preferred orbital sense (clockwise).

This impression is confirmed by Fig. \ref{fig:shifts2}, which shows the relative change in position $\mathbf{r}$ and velocity $\mathbf{v}$, the relative change in the norm of the specific angular momentum $h$, and the difference $\Delta \theta_\mathrm{pole}$\ in the direction of the resulting orbital pole (direction of the angular momentum) before and after applying the shifts  of each dwarf galaxy, respectively. The positions shift by no more than 10\% of the Galactocentric distance of each dwarf, most velocities change by no more than 20\%, though for some the velocity change can reach up to 50\% of their full 3D velocity. Note, however, that a complete reversal of the velocity requires a change of 200\%. The specific angular momenta change by no more than 30\%. Most importantly, the direction of the orbital poles of the majority of MW dwarfs changes by no more than $\sim 5^\circ$. Only 7 of the 31 considered dwarfs display $\Delta \theta_\mathrm{pole} > 10^\circ$. Of these, only one is strongly co-orbiting and one strongly counter-orbiting relative to the VPOS. The mean (median) change on orbital pole direction for the MW dwarfs is $3^\circ (6^\circ)$.

\begin{figure*}
\gridline{
\fig{orbital_poles_v2.png}{0.99\textwidth}{(a) Observed orbital poles}
}
\gridline{
\fig{orbital_poles_GC21_v2.png}{0.99\textwidth}{(b) Orbital poles after correcting for LMC effect}
}
\caption{Directions of orbital poles for the observed MW satellites calculated relative to the MW center (upper panel a), and after shifting the dwarf galaxy positions and velocities as in Fig. \ref{fig:shifts} to correct for the effect of the LMC (lower panel b). The most-likely orbital poles are shown as open circles, and the orbital poles from 5000 Monte-Carlo realizations drawing from the measurement uncertainties as dots. The colors follow those in Fig. \ref{fig:shifts}, with strongly co-orbiting dwarfs in red and counter-orbiting ones in green. If the LMC's influence were the main reason for the observed overdensity of orbital poles towards the VPOS normal vector (green cross), then the lower panels should show a much reduced overdensity. They do not. Most orbital pole directions are barely affected by the shifts.
\label{fig:Poles}}
\end{figure*}

The impact on the distribution of orbital poles is illustrated in Fig. \ref{fig:Poles}.
To account for measurement uncertainties in distances, velocities, and proper motions, we draw 5000 realizations for each dwarf.
The distributions without and with shifts are virtually indistinguishable. In both cases a clear overdensity of orbital poles close to the center of the figures is apparent.
Overall, the number of MW dwarfs with most likely orbital poles within $36.87^\circ$\ (10\% of the area of the sphere around the VPOS normal direction, see e.g. \citealt{2018A&A...619A.103F, 2021ApJ...916....8L}) is 12 for the observed orbital poles out of the 31 dwarfs (ignoring two counter-orbiting dwarfs)\footnote{Note that many of the others remain consistent with aligning with the VPOS within their considerable proper motion uncertainties; their orbital poles are only very weakly constrained.}. This corresponds to an orbital pole enhancement in the 10\% VPOS region of almost 300\% over the expected isotropic share of 3.1 orbital poles out of 31 dwarfs. After applying the shifts, 11 orbital poles remain within the VPOS region, and the median alignment angle $\theta_\mathrm{VPOS}$\ with the VPOS changes from $59^\circ$ to $61^\circ$.

We note that this is only a first-order estimate of the influence of the LMC. More accurate results require full orbit modelling under the influence of the time-varying potential sourced by the MW and LMC. Recently, \citet{2021arXiv211000018C} have presented such a work. They report that re-winding the satellite orbits under the influence of a massive LMC, and then forward-integrating them again without an LMC until present time, results in no significant change in the orbital pole distribution and preserves its strong non-uniformity. We are thus confident that the LMC's impact on the orbital pole clustering observed for the MW satellites is indeed very minor.

This begs the question as to why the model of \citetalias{GC21} appears to be insufficient to account for the observed orbital pole clustering. Our hypothesis is that the reason lies in different orbital properties between typical DM particles in a halo, on which their work is based, and the dwarf galaxies of the Milky Way. \citetalias{GC21} used a slightly radially biased setup for their dark matter halo particle velocities. If an orbit is strongly radial, then a minor shift in position or velocity of the reference point for angular momentum calculations has much greater impact on the orbital pole direction than if the orbit were more circular. While dark matter particles can be on highly radial orbits, the observed MW dwarf galaxies have been found to follow more tangentially biased orbits \citep{ 2017MNRAS.468L..41C,2019MNRAS.486.2679R,2021arXiv210911557H}.
This is not entirely unexpected in a $\Lambda$CDM framework. \citet{2004MNRAS.352..535D} report for galaxy cluster mass simulations that dark matter particles in the inner regions of halos are on slightly more radial orbits than subhalos, and that subhalos typically have higher velocities than dark matter particles.
The presence of a baryonic central galaxy seems to further strengthen this difference, because the additional potential in the inner region of a halo results in stronger tidal forces that even more efficiently destroy subhalos on radial orbits. Using the hydrodynamical FIRE simulations, \citet{2017MNRAS.471.1709G} showed that this leads to more tangentially biased subhalo velocities when compared to dark-matter-only simulations. They also showed that the surviving subhalos in the hydrodynamical runs have considerably higher tangential velocities within 100\,kpc than those in dark-matter-only runs, which implies higher angular momenta.
This effect has been confirmed by \citet{2019MNRAS.487.4409K} for the PhatELVIS simulations which contain an analytically grown MW-like disk potential, and by \citet{2019MNRAS.486.2679R} who find that satellites in the Auriga simulations are on more tangentially biased orbits, probably because the Auriga halos contain rather massive baryonic disks that destroy subhalos on radial orbits.

\section{Our Simulation} \label{sec:Sim}

To test our hypothesis, we run our own simulation of a MW-LMC-like interaction. The $N$-body simulation is run with \textsc{Gyrfalcon} \citep{2000ApJ...536L..39D}, and we use \textsc{Agama} \citep{2019MNRAS.482.1525V} to generate initial conditions. For the MW, we use the Model 1 of \citet{2008gady.book.....B} as given in \textsc{Agama}, which includes a stellar bulge, a thin disk, a thick disk, and a DM halo. We make two changes: (i) we use the same halo mass of $1.2\times10^{12}$ M$_\odot$ as \citetalias{GC21}, and (ii) in order to have a spherical halo, we remove the z-axis flattening coefficient of its potential. We generate $2\times10^5$ particles for the stars and $8\times10^5$ for the dark matter halo. For the LMC, we generate $10^5$ particles based on the spheroid potential of \textsc{Agama} for a total mass of $1.8\times10^{11}$ M$_\odot$, following the fiducial model of \citetalias{GC21}.
The initial conditions of our simulated MW halo model deliberately adopt isotropic orbits, in order to facilitate our aim to examine the effect of the infall of the LMC model on the halo particles as a function of their specific angular momenta.

Initially we place the LMC at $(x, y, z) = (12, 215, 130)$\,kpc and $(v_x, v_y, v_z) = (12, 13, -77)\,\mathrm{km\,s}^{-1}$ in the MW-centred reference frame, a slight alteration of the initial conditions of \citetalias{GC21}. We run the simulation for 2 Gyr. For each snapshot, we use the {\it snapcenter} function of \textsc{Nemo} \citep{1995ASPC...77..398T} to obtain the positions and velocities of the COM of the MW based on its stars, then we shift the positions and velocities of all particles by these values in order to make the MW the center of phase space.
In this reference frame, the coordinates of the COM of the LMC after 2 Gyr are $(x, y, z) = (-1.87, -31.42, -17.07)$\,kpc and $(v_x, v_y, v_z) = (-48.61, -207.98, 150.63)\,\mathrm{km\,s}^{-1}$.
For comparison, the present day values retained by \citet{2021MNRAS.501.2279V} are $(x, y, z) = (-0.6, -41.3, -27.1)$\,kpc and $(v_x, v_y, v_z) = (-63.9, -213.8, 206.6)\,\mathrm{km\,s}^{-1}$.

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

\begin{figure*}
\gridline{
\fig{Figure_11.pdf}{0.5\textwidth}{(a): Initial angular momentum}
\fig{Figure_12_lowh.pdf}{0.5\textwidth}{(b): Low initial angular momentum}
}
\gridline{
\fig{Figure_12_intermediateh.pdf}{0.5\textwidth}{(c): Intermediate initial angular momentum}
\fig{Figure_12_highh.pdf}{0.5\textwidth}{(d): High initial angular momentum}
}
\caption{Specific angular momenta of MW dwarfs (symbols) and dark matter particles in our simulation (density maps, with logarithmic scale). Panel (a) shows the initial specific angular momentum $h_\mathrm{ini}$\ (and the one inferred after shifting the observed MW dwarf positions and velocities), while panels (b) to (d) show the angular momentum $h$\ of the same set of particles in the final simulation snapshot (and the angular momenta of the MW satellites relative to today's MW center), split into low, intermediate, and high initial angular momentum bins (as indicated by the green lines in panel a). Particles are selected from the distance range of 50 to 250\,kpc in the final snapshot. The observed MW dwarfs best agree with the simulation particles in the high angular momentum bin.
\label{fig:AngMom}}
\end{figure*}

We follow the evolution of individual DM particles in the simulation from the initial to final snapshot, selecting all particles at a distance of 50 to 250\,kpc from the MW analog center in the final snapshot. We divide them in three bins of low ($h_\mathrm{ini} < 5 \times 10^3\,\mathrm{kpc\,km\,s}^{-1}$, $N = 49,884$), intermediate ($5 \times 10^3\,\leq h_\mathrm{ini} < 10^4\,\mathrm{kpc\,km\,s}^{-1}$, $N = 109,905$) and high ($10^4\,\mathrm{kpc\,km\,s}^{-1} \leq h_\mathrm{ini}$, $N = 232,533$) initial specific angular momenta. While the two bins with lower angular momentum constitute only 41\% of all particles in the considered distance range, we will show in the following that they contribute the bulk to the orbital pole overdensity around the VPOS direction.

Fig. \ref{fig:AngMom} plots the specific angular momenta of the observed MW dwarfs against their Galactocentric distance. It compares to particles in our simulation, selected to reside in the considered distance range {\it at the end of the simulation}.
The LMC affects the angular momenta of the particles, spreading them beyond their initial bin boundaries, though overall they preserve their ranking in specific angular momentum (note the density scale is logarithmic).
The observed MW dwarfs agree best with the final particle distribution of the high-angular-momentum bin. As expected, the MW dwarfs have relatively high specific angular momenta compared to dark matter particles in a MW-like halo.
To more quantitatively judge this visual impression, we calculate the likelihood ratios of the high angular momentum bin to the low and the intermediate angular momentum bins, respectively.

\begin{figure*}
\gridline{
\fig{Figure_15_allh.pdf}{0.5\textwidth}{(a) all particles in distance range}
\fig{Figure_15_lowh.pdf}{0.5\textwidth}{(b) low initial angular momentum}
}
\gridline{
\fig{Figure_15_intermediateh.pdf}{0.5\textwidth}{(c) intermediate initial angular momentum}
\fig{Figure_15_highh.pdf}{0.5\textwidth}{(d) high initial angular momentum}
}
\caption{All-sky maps in Galactic Coordinates of the orbital pole enhancement for dark matter particles in our simulation. Panel (a) contains all particles within a distance range of 50 to 250\,kpc, while the other panels only show subsets based on the particles' initial specific angular momenta. The green cross marks the VPOS normal vector direction, and the green circle indicates the 10\% area on the sphere where the relative VPOS enhancement is measured. While panel (a) confirms the overall findings of \citetalias{GC21} that an LMC-like infall enhances the density of orbital poles towards the VPOS normal, low angular momentum particles (panel b) are most affected and show a pronounced overdensity, while high angular momentum particles (panel d) -- which are comparable to the observed MW dwarfs -- show only a very slight overdensity.
\label{fig:LMCeffectObs}}
\end{figure*}

The likelihoods are estimated using the maps of angular momenta and distances in Fig. \ref{fig:AngMom} as follows: for each observed satellite, we identify the Galactocentric distance $d$\ bin (of 10\,kpc width) it falls in. We then calculate the weighted contribution of this observed satellite's angular momentum to each of the angular momentum bins (of 2500\,kpc\,km\,s$^{-1}$\ width) at this $d$. This is done by adopting the most-likely measured value of $h$\ for this satellite and assuming a normal distribution with a width as given by the uncertainties on $h$ (see error bars in Fig. \ref{fig:AngMom}). Since $h$\ can only be positive we cut off these distributions at $h = 0$\ and re-normalize them accordingly. To avoid being dominated by a few high-$h$\ outliers, we also do not consider satellites or particles with $h > 5 \times 10^4\,\mathrm{kpc\,km\,s}^{-1}$. The likelihood for one individual satellite is then the weighted contribution of simulation particles in these bins, normalized to the total number of simulation particles in the considered set (i.e. either low, intermediate, or high $h_\mathrm{ini}$). Finally, the individual likelihoods of all observed satellites are multiplied to obtain the overall likelihood. We find that the likelihood ratio of high-to-low $h_\mathrm{ini}$\ is $1.3 \times 10^{22}$, while that of high-to-intermediate $h_\mathrm{ini}$\ is $4.1 \times 10^{8}$. This strongly confirms the impression that the set of observed Milky Way satellite galaxies match best with the high initial angular momentum bin.

\subsection{Orbital Pole Enhancement}

\begin{figure*}[ht!]
\gridline{
\fig{Figure_10.pdf}{0.5\textwidth}{(a)}
\fig{Figure_9.pdf}{0.5\textwidth}{(b)}
}
\caption{ The change in orbital pole direction of particles in the simulation depends on the specific angular momentum they had initially.
Panel (a) shows that particles with smaller initial specific angular momentum $h_\mathrm{ini}$\ show larger changes in the direction of their orbital poles as measured by the angle $\Delta \theta_\mathrm{pole}$\ between their orbital pole in the initial and final simulation snapshot. Also shown are the observed MW dwarfs.
Panel (b) shows the distribution of $\Delta \theta_\mathrm{pole}$\ for three specific angular momentum bins. Low angular momentum particles (red dotted line) are affected most, while high angular momentum particles (blue solid line) show the least change in their orbital pole directions.
 \label{fig:polechange}}
\end{figure*}

The enhancement of the density of orbital pole directions for the particles in our simulation are plotted in Fig. \ref{fig:LMCeffectObs}. We follow the method of \citetalias{GC21}, and calculate for each bin in the Healpix map how many orbital poles in the particle sample contribute to it, subtract the expected number for an isotropic distribution, and divide by the latter. Despite the lower resolution of the maps due to our smaller particle numbers, we clearly confirm the results of \citetalias{GC21}. The infall of an LMC-like object onto a MW-like host results in an enhancement of orbital poles of dark matter particles in the general direction of the VPOS.

We also calculate how many more orbital poles than in an isotropic distribution contribute to the VPOS region. We assume the VPOS normal points to Galactic coordinates $(l, b)_\mathrm{VPOS} = (169.3^\circ, -2.8^\circ)$\ to be consistent with previous works \citep[e.g.][]{2018A&A...619A.103F, 2021ApJ...916....8L,GC21}. Also following these previous works, we consider a region of $36.87^\circ$\ around this direction, which corresponds to 10\% of the area on the sphere. The excess of the number of particle orbital poles in this area in the final simulation snapshot over the corresponding number using the same set of particles in the initial setup, divided by the latter, is the relative VPOS enhancement. Within the adopted distance range of 50 to 250\,kpc, we find an overall VPOS enhancement of 9\%. This means that there are 1.09 times the number of orbital poles within the VPOS region than expected from isotropy. As the region constitutes 10\% of the sphere, for 31 dwarf galaxies 3 should typically be found in the region if they are isotropically distributed. The LMC effect would then suggest an enhancement of about one quarter of an additional orbital pole. This is hardly sufficient to account for the observed clustering of 12 (or more within their uncertainties) out of 31 orbital poles aligned with the VPOS.

In the other panels of Fig. \ref{fig:LMCeffectObs} we separate the dark matter particles by their initial angular momentum. The resulting maps of orbital pole enhancement strongly confirm our suspicion that mainly particles with small angular momenta are affected by the LMC's influence. The low angular momentum bin shows the strongest VPOS enhancement of 35\%. The pole density distribution also displays a slight s-shape that further confirms the results reported by \citetalias{GC21}. Particles with intermediate specific angular momenta still display some enhancement in the orbital pole density, but to a much reduced degree (VPOS enhancement of 9\%). Once only high angular momentum particles are considered, the map mainly consists of noise, with no substantial enhancement of orbital poles towards the VPOS direction (VPOS enhancement of 3\%).

\subsection{Change in Orbital Pole Directions}

We now investigate how the orbital poles change between the initial and the final simulation snapshot to assess how much the LMC-like infall has affected the orbital direction of each individual particle.
Panel (a) of Fig. \ref{fig:polechange} plots the angle between the initial and the final direction of orbital poles, $\Delta \theta_\mathrm{pole}$. The vast majority of simulation particles (note the logarithmic color scale) overlap with the region covered by the observed MW dwarfs. There is a clear tendency for particles with higher initial specific angular momentum to have smaller changes in their orbital pole direction.
Panel (b) of Fig. \ref{fig:polechange} confirms this. Low angular momentum particles display an extended tail to high $\Delta \theta_\mathrm{pole}$, some reaching as high as $\Delta \theta_\mathrm{pole} = 170^\circ$\ and thus almost flip their orbital direction. Their mean (median) change in orbital pole direction is $43.9^\circ (29.2^\circ)$. The particles with intermediate angular momentum show smaller changes of $19.7^\circ (12.8^\circ)$. The vast majority of particles with high initial angular momentum, however, change their orbital pole direction by less than $20^\circ$, and correspondingly their mean (median) $\Delta \theta_\mathrm{pole}$\ are only $12.5^\circ (9.4^\circ)$.

\subsection{Change in Alignment with VPOS}

\begin{figure*}[ht!]
\gridline{
\fig{Figure_13.pdf}{0.5\textwidth}{(a)}
\fig{Figure_14.pdf}{0.5\textwidth}{(b)}
}
\caption{ The enhancement in the alignment of orbital poles with the VPOS normal direction of particles in the simulation depends on the specific angular momentum they had initially.
Panel (a) plots the Cosines of the angle between the VPOS normal vector and the particle orbital poles as measured in the initial ($\theta_\mathrm{VPOS}^\mathrm{ini}$) and final ($\theta_\mathrm{VPOS}^\mathrm{obs}$) simulation snapshot. The corresponding angles for the observed (and shifted) MW dwarf positions and velocities are also shown as colored symbols.
Panel (b) compares histograms of $\theta_\mathrm{VPOS}^\mathrm{obs}$\ for three different bins in specific angular momentum for the particles in the simulation, with the alignment of orbital poles of the observed set of MW dwarfs. Only the low angular momentum (red dotted line) particles show some enhancement towards the VPOS normal (at $\cos(\theta_\mathrm{VPOS}^\mathrm{obs}) = 1$). The high angular momentum particles (blue solid line) follow a flat distribution as expected for isotropically distributed orbital poles.  The observed MW dwarfs have specific angular momenta that are comparable to the high angular momentum bin, but they display a very pronounced overdensity of orbital poles close to the VPOS normal, which is more than an order of magnitude higher than even the enhancement shown by the low angular momentum particles.
 \label{fig:VPOSangle}}
\end{figure*}

Changing the direction of the orbital poles does not necessarily imply an enhancement of poles towards the VPOS. To quantify this, we measure the angle $\theta_\mathrm{VPOS}$\ between each particle's orbital pole and the normal vector to the VPOS. We again do this for both the initial snapshot which should be comparable to the ``corrected'' positions after shifting the observed MW dwarf positions and velocities ($\theta_\mathrm{VPOS}^\mathrm{ini}$), and the final one which is comparable to the observed situation ($\theta_\mathrm{VPOS}^\mathrm{obs}$). Panel (a) of Fig. \ref{fig:VPOSangle} compares these two quantities\footnote{The Cosines are plotted as they ensure that isotropically distributed directions result in a flat distribution.}. If the clustering of observed MW orbital poles close to the VPOS were substantially affected by the LMC infall, $\theta_\mathrm{VPOS}^\mathrm{ini}$\ should show a much wider distribution than $\theta_\mathrm{VPOS}^\mathrm{obs}$, and in particular the dwarfs with closely aligned poles (red) should scatter appreciably towards lower $\cos(\theta_\mathrm{VPOS}^\mathrm{ini})$. Yet, the distributions largely follow the diagonal in the figure, suggesting that the overall changes are small.

The situation is even clearer when looking at histograms of $\theta_\mathrm{VPOS}^\mathrm{obs}$\ (panel (b) in Fig. \ref{fig:VPOSangle}).
An isotropic distribution of directions on the sphere, such as the DM particle orbital poles in our initial simulation snapshot, gives a flat histrogram with probability density 0.5. Clearly, the simulation particles in the final snapshot mostly follow this distribution, in particular for the high angular momentum bin. While an isotropic distribution should have a mean (median) alignment angle of $90^\circ$, the low, intermediate, and high specific angular momentum bins show only mildly smaller angles, namely $85.8^\circ (84.6^\circ)$, $88.0^\circ (87.2^\circ)$, and $89.4^\circ (89.1^\circ)$ respectively. The corresponding values for the observed MW dwarfs are $63.0^\circ (58.5^\circ)$. Only the low angular momentum bin shows some clear excess towards $\cos(\theta_\mathrm{VPOS}^\mathrm{obs}) = 1$, i.e. around the VPOS direction. However, this excess is neither comparable in strength to the distribution of observed dwarf galaxy orbital poles, nor do the observed MW satellites have such low specific angular momenta.

\subsection{Dependency on Distance from Host}

\begin{figure}[ht!]
\plotone{VPOSenhancement_radius_withGC2.pdf}
\caption{ The enhancement of orbital pole density of dark matter particles in the simulation over that expected for isotropy in the 10\% region around the VPOS normal vector. The enhancement is measured as a function of distance from the host center $d$, in radial shells of 50\,kpc width. While low angular momentum particles can show very pronounced enhancements at larger distances, the higher-angular momentum particles, which are more comparable to the observed MW satellites, show a substantially lower enhancement and also dominate the sample of particles at larger distances. Also plotted are the VPOS enhancements as reported in \citetalias{GC21} and extracted from their figure 15. \label{fig:VPOSenhancement}}
\end{figure}

These results are not strongly dependent on the exact radial range considered. Fig. \ref{fig:VPOSenhancement} plots the VPOS enhancement as a function of radius, split into the three angular momentum bins. The high initial angular momentum particles always show the least VPOS enhancement. In particular, they show no more than a 10\% enhancement within 200\,kpc from the host, the distance range covered by most MW satellites with reliably measured orbital poles. We also note that our overall VPOS enhancement is very comparable to that reported by \citetalias{GC21} for their fiducial model  (see their Fig. 15)\footnote{The slight excess of their data points over ours in the inner distance bins can be attributed their isolated MW analog already resulting in a 10\% enhancement over a perfectly isotropic distribution.}, upon which we modelled our initial conditions. This confirms that our results are indeed comparable with their study.

\section{Conclusions} \label{sec:conclusions}

\citetalias{GC21} have demonstrated that the infall of a massive, LMC-like galaxy onto a MW-like host results in an enhancement of orbital poles of dark matter particles in the direction of the orbital plane of the interaction. For the MW, this direction aligns with the VPOS. This in turn lead \citetalias{GC21} to propose that the infall of a massive LMC could have changed the orbital pole directions of the observed MW satellite galaxies, and that this could help explain the observed clustering or satellite orbital poles towards the VPOS normal.

We confirm the overall results of \citetalias{GC21} with our own simulation of a LMC-MW like interaction. However, our results strongly disagree with their suggestion that this can help explain the origin of the VPOS. We find that accounting for the radius-dependent shifts in position and velocity of the MW halo center-of-mass induced by the LMC infall does not remove nor appreciably weaken the clustering of orbital poles towards the VPOS normal. This is likely due to the small relative COM shifts on the positions and velocities of the MW satellites. While the orbital pole direction of objects on more radial orbits (low angular momenta) can be substantially changed by even a small perturbation to their position or velocity, objects on less radial orbits (higher angular momenta) are much less affected by the same shifts. The observed MW satellites, as well as dark matter sub-halos in hydrodynamical cosmological simulations, have less radial orbits and higher tangential velocities (and thus higher specific angular momenta) than many dark matter halo particles or subhalos in dark-matter-only simulations \citep{2004MNRAS.352..535D, 2017MNRAS.468L..41C, 2017MNRAS.471.1709G, 2020ApJ...894...10L}. We hypothesize that the observed MW satellites have too high angular momenta to be sufficiently affected by the LMC infall to explain their strong clustering of orbital poles.

Our numerical simulation of an LMC-MW like interaction confirms this. Within the distance range of 50 to 250\, kpc, which is most relevant for the observed MW satellites, the simulation predicts an orbital pole enhancement of 9\% in the VPOS direction. In the same area of sky, 12 out of 31 MW satellite orbital poles are found, corresponding to an enhancement of 300\% over the expected isotropic share of three orbital poles. The observed signal is thus substantially larger than the one predicted to be induced by the LMC. This discrepancy increases further to two orders of magnitude (3\% vs. 300\%) if only particles with angular momenta as high as those of the MW satellites are considered. Particles that initially had very low angular momenta show the strongest enhancement in orbital pole density towards the VPOS normal. However, these angular momenta are inconsistent with the observed dwarf galaxies, as based on Gaia EDR3 proper motions \citep{2021arXiv210608819B}. Restricting the analysis to particles of comparably high angular momenta, the orbital pole enhancement all but vanishes. The LMC-like infall is therefore unable to induce a pronounced enhancement of orbital poles in the VPOS direction for simulation particles with angular momenta comparable to those inferred for the observed MW dwarfs.

In summary, the LMC-induced overdensity of orbital poles is (i) only present for particles with low specific angular momenta, while the effect becomes fully negligible towards the higher specific angular momenta of the observed MW satellites, and (ii) is still too small an effect to account for the strong degree of orbital pole clustering among the observed MW satellites even if assuming the impact on them were as strong as on particles with low specific angular momenta. The LMC's infall onto the MW therefore does not suffice by a large margin to explain the observed VPOS.

If the LMC cannot explain the VPOS, its orbital alignment with the VPOS despite its very recent infall nevertheless remains a puzzling coincidence \citep{Pawlowski2013}. While alternative approaches have proposed some potential explanatory mechanisms \citep{1976MNRAS.174..695L, 2010ApJ...725L..24Y, 2018A&A...614A..59B}, at least within a classical $\Lambda$CDM framework this alignment appears to be nothing but a chance event.

\section*{Data Availability}

The initial conditions and final snapshot of the simulation described in Section~\ref{sec:Sim} can be obtained at the following address: \href{https://seafile.unistra.fr/d/f0ff2f519f4e42b792a0/}{https://seafile.unistra.fr/d/f0ff2f519f4e42b792a0/}.

\begin{acknowledgments}
MSP and ST acknowledge funding of a Leibniz-Junior Research Group (project number J94/2020) via the Leibniz Competition, MSP also thanks the Klaus Tschira Stiftung and German Scholars Organization for support via a KT Boost Fund. MSP and BF acknowledge support from the Partenariat Hubert Curien (PHC) for PROCOPE project 44677UE and the Deutscher Akademischer Austauschdienst for PPP grant 57512596 funded by the Bundesministerium fur Bildung und Forschung. PAO, BF and RI acknowledge funding from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation programme (grant agreement No. 834148) and from the Agence Nationale de la Recherche (ANR projects ANR-18-CE31-0006 and ANR-19-CE31-0017).
This research has made use of NASA's Astrophysics Data System.
\end{acknowledgments}

\subsubsection*{#1}}

\pagestyle{headings}
\markright{Reference sheet: \texttt{natbib}}

\usepackage{shortvrb}
\MakeShortVerb{\|}

\begin{document}
\thispagestyle{plain}

\newcommand{\textsc{Bib}\TeX}{\textsc{Bib}\TeX}
\newcommand{\texttt{#1}\def\filedate{#2}\def\fileversion{#3}}}{\texttt{#1}\def\filedate{#2}\def\fileversion{#3}}}
\begin{center}{\bfseries\Large
    Reference sheet for \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}\ usage}\\
    \large(Describing version \fileversion\ from \filedate)
\end{center}

\begin{quote}\slshape
For a more detailed description of the \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}\ package, \LaTeX\ the
source file \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}\texttt{.dtx}.
\end{quote}
\head{Overview}
The \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}\ package is a reimplementation of the \LaTeX\ |\cite| command,
to work with both author--year and numerical citations. It is compatible with
the standard bibliographic style files, such as \texttt{plain.bst}, as well as
with those for \texttt{harvard}, \texttt{apalike}, \texttt{chicago},
\texttt{astron}, \texttt{authordate}, and of course \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}.

\head{Loading}
Load with |\usepackage[|\emph{options}|]{|\texttt{#1}\def\filedate{#2}\def\fileversion{#3}}|}|. See list of
\emph{options} at the end.

\head{Replacement bibliography styles}
I provide three new \texttt{.bst} files to replace the standard \LaTeX\
numerical ones:
\begin{quote}\ttfamily
 plainnat.bst \qquad abbrvnat.bst \qquad unsrtnat.bst
\end{quote}
\head{Basic commands}
The \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}\ package has two basic citation commands, |\citet| and
|\citep| for \emph{textual} and \emph{parenthetical} citations, respectively.
There also exist the starred versions |\citet*| and |\citep*| that print
the full author list, and not just the abbreviated one.
All of these may take one or two optional arguments to add some text before
and after the citation.
\begin{quote}
\begin{tabular}{l@{\quad$\Rightarrow$\quad}l}
  |\citet{jon90}| & Jones et al. (1990)\\
  |\citet[chap.~2]{jon90}| & Jones et al. (1990, chap.~2)\\[0.5ex]
  |\citep{jon90}| & (Jones et al., 1990)\\
  |\citep[chap.~2]{jon90}| & (Jones et al., 1990, chap.~2)\\
  |\citep[see][]{jon90}| & (see Jones et al., 1990)\\
  |\citep[see][chap.~2]{jon90}| & (see Jones et al., 1990, chap.~2)\\[0.5ex]
  |\citet*{jon90}| & Jones, Baker, and Williams (1990)\\
  |\citep*{jon90}| & (Jones, Baker, and Williams, 1990)
\end{tabular}
\end{quote}
\head{Multiple citations}
Multiple citations may be made by including more than one
citation key in the |\cite| command argument.
\begin{quote}
\begin{tabular}{l@{\quad$\Rightarrow$\quad}l}
  |\citet{jon90,jam91}| & Jones et al. (1990); James et al. (1991)\\
  |\citep{jon90,jam91}| & (Jones et al., 1990; James et al. 1991)\\
  |\citep{jon90,jon91}| & (Jones et al., 1990, 1991)\\
  |\citep{jon90a,jon90b}| & (Jones et al., 1990a,b)
\end{tabular}
\end{quote}

\head{Numerical mode}
These examples are for author--year citation mode. In numerical mode, the
results are different.
\begin{quote}
\begin{tabular}{l@{\quad$\Rightarrow$\quad}l}
  |\citet{jon90}| & Jones et al. [21]\\
  |\citet[chap.~2]{jon90}| & Jones et al. [21, chap.~2]\\[0.5ex]
  |\citep{jon90}| & [21]\\
  |\citep[chap.~2]{jon90}| & [21, chap.~2]\\
  |\citep[see][]{jon90}| & [see 21]\\
  |\citep[see][chap.~2]{jon90}| & [see 21, chap.~2]\\[0.5ex]
  |\citep{jon90a,jon90b}| & [21, 32]
\end{tabular}
\end{quote}
\head{Suppressed parentheses}
As an alternative form of citation, |\citealt| is the same as |\citet| but
\emph{without parentheses}. Similarly, |\citealp| is |\citep| without
parentheses. Multiple references, notes, and the starred variants
also exist.
\begin{quote}
\begin{tabular}{l@{\quad$\Rightarrow$\quad}l}
  |\citealt{jon90}| & Jones et al.\ 1990\\
  |\citealt*{jon90}| & Jones, Baker, and Williams 1990\\
  |\citealp{jon90}| & Jones et al., 1990\\
  |\citealp*{jon90}| & Jones, Baker, and Williams, 1990\\
  |\citealp{jon90,jam91}| & Jones et al., 1990; James et al., 1991\\
  |\citealp[pg.~32]{jon90}| & Jones et al., 1990, pg.~32\\
  |\citetext{priv.\ comm.}| & (priv.\ comm.)
\end{tabular}
\end{quote}
The |\citetext| command
allows arbitrary text to be placed in the current citation parentheses.
This may be used in combination with |\citealp|.
\head{Partial citations}
In author--year schemes, it is sometimes desirable to be able to refer to
the authors without the year, or vice versa. This is provided with the
extra commands
\begin{quote}
\begin{tabular}{l@{\quad$\Rightarrow$\quad}l}
  |\citeauthor{jon90}| & Jones et al.\\
  |\citeauthor*{jon90}| & Jones, Baker, and Williams\\
  |\citeyear{jon90}|   & 1990\\
  |\citeyearpar{jon90}| & (1990)
\end{tabular}
\end{quote}
\head{Forcing upper cased names}
If the first author's name contains a \textsl{von} part, such as ``della
Robbia'', then |\citet{dRob98}| produces ``della Robbia (1998)'', even at the
beginning of a sentence. One can force the first letter to be in upper case
with the command |\Citet| instead. Other upper case commands also exist.
\begin{quote}
\begin{tabular}{rl@{\quad$\Rightarrow$\quad}l}
  when & |\citet{dRob98}| & della Robbia (1998) \\
  then & |\Citet{dRob98}| & Della Robbia (1998) \\
     &   |\Citep{dRob98}| & (Della Robbia, 1998) \\
     &   |\Citealt{dRob98}| & Della Robbia 1998 \\
     &   |\Citealp{dRob98}| & Della Robbia, 1998 \\
     &   |\Citeauthor{dRob98}| & Della Robbia
\end{tabular}
\end{quote}
These commands also exist in starred versions for full author names.

\head{Citation aliasing}
Sometimes one wants to refer to a reference with a special designation,
rather than by the authors, i.e. as Paper~I, Paper~II. Such aliases can be
defined and used, textual and/or parenthetical with:
\begin{quote}
\begin{tabular}{lcl}
  |\defcitealias{jon90}{Paper~I}|\\
  |\citetalias{jon90}| & $\Rightarrow$ & Paper~I\\
  |\citepalias{jon90}| & $\Rightarrow$ & (Paper~I)
\end{tabular}
\end{quote}
These citation commands function much like |\citet| and |\citep|: they may
take multiple keys in the argument, may contain notes, and are marked as
hyperlinks.
\head{Selecting citation style and punctuation}
Use the command |\bibpunct| with one optional and 6 mandatory arguments:
\begin{enumerate}
\item the opening bracket symbol, default = (
\item the closing bracket symbol, default = )
\item the punctuation between multiple citations, default = ;
\item the letter `n' for numerical style, or `s' for numerical superscript
      style, any other letter for
      author--year, default = author--year;
\item the punctuation that comes between the author names and the year
\item the punctuation that comes between years or numbers when common author
      lists are suppressed (default = ,);
\end{enumerate}

The optional argument is the character preceding a post-note, default is a
comma plus space. In redefining this character, one must include a space if
one is wanted.

Example~1, |\bibpunct{[}{]}{,}{a}{}{;}| changes the output of
\begin{quote}
  |\citep{jon90,jon91,jam92}|
\end{quote}
into [Jones et al. 1990; 1991, James et al. 1992].

Example~2, |\bibpunct[; ]{(}{)}{,}{a}{}{;}| changes the output of
\begin{quote}
  |\citep[and references therein]{jon90}|
\end{quote}
into (Jones et al. 1990; and references therein).

\head{Other formatting options}
Redefine |\bibsection| to the desired sectioning command for introducing
the list of references. This is normally |\section*| or |\chapter*|.

Define |\bibpreamble| to be any text that is to be printed after the heading but
before the actual list of references.

Define |\bibfont| to be a font declaration, e.g.\ |\small| to apply to
the list of references.

Define |\citenumfont| to be a font declaration or command like |\itshape|
or |\textit|.

Redefine |\bibnumfmt| as a command with an argument to format the numbers in
the list of references. The default definition is |[#1]|.

The indentation after the first line of each reference is given by
|\bibhang|; change this with the |\setlength| command.

The vertical spacing between references is set by |\bibsep|; change this with
the |\setlength| command.

\head{Automatic indexing of citations}
If one wishes to have the citations entered in the \texttt{.idx} indexing
file, it is only necessary to issue |\citeindextrue| at any point in the
document. All following |\cite| commands, of all variations, then insert
the corresponding entry to that file. With |\citeindexfalse|, these
entries will no longer be made.

\head{Use with \texttt{chapterbib} package}

The \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}\ package is compatible with the \texttt{chapterbib} package
which makes it possible to have several bibliographies in one document.

The package makes use of the |\include| command, and each |\include|d file
has its own bibliography.

The order in which the \texttt{chapterbib} and \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}\ packages are loaded
is unimportant.

The \texttt{chapterbib} package provides an option \texttt{sectionbib}
that puts the bibliography in a |\section*| instead of |\chapter*|,
something that makes sense if there is a bibliography in each chapter.
This option will not work when \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}\ is also loaded; instead, add
the option to \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}.

Every |\include|d file must contain its own
|\bibliography| command where the bibliography is to appear. The database
files listed as arguments to this command can be different in each file,
of course. However, what is not so obvious, is that each file must also
contain a |\bibliographystyle| command, \emph{preferably with the same
style  argument}.
\head{Sorting and compressing citations}
Do not use the \texttt{cite} package with \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}; rather use one of the
options \texttt{sort} or \texttt{sort\&compress}.

These also work with author--year citations, making multiple citations appear
in their order in the reference list.

\head{Long author list on first citation}
Use option \texttt{longnamesfirst} to have first citation automatically give
the full list of authors.

Suppress this for certain citations with |\shortcites{|\emph{key-list}|}|,
given before the first citation.

\head{Local configuration}
Any local recoding or definitions can be put in \texttt{#1}\def\filedate{#2}\def\fileversion{#3}}\texttt{.cfg} which
is read in after the main package file.

\head{Options that can be added to \texttt{\char`\\ usepackage}}
\begin{description}
\item[\ttfamily round] (default) for round parentheses;
\item[\ttfamily square] for square brackets;
\item[\ttfamily curly] for curly braces;
\item[\ttfamily angle] for angle brackets;
\item[\ttfamily colon] (default) to separate multiple citations with
     colons;
\item[\ttfamily comma] to use commas as separaters;
\item[\ttfamily authoryear] (default) for author--year citations;
\item[\ttfamily numbers] for numerical citations;
\item[\ttfamily super] for superscripted numerical citations, as in
     \textsl{Nature};
\item[\ttfamily sort] orders multiple citations into the sequence in
     which they appear in the list of references;
\item[\ttfamily sort\&compress] as \texttt{sort} but in addition multiple
     numerical citations are compressed if possible (as 3--6, 15);
\item[\ttfamily longnamesfirst] makes the first citation of any reference
     the equivalent of the starred variant (full author list) and subsequent
     citations normal (abbreviated list);
\item[\ttfamily sectionbib] redefines |\thebibliography| to issue
     |\section*| instead of |\chapter*|; valid only for classes with a
     |\chapter| command; to be used with the \texttt{chapterbib} package;
\item[\ttfamily nonamebreak] keeps all the authors' names in a citation on
     one line; causes overfull hboxes but helps with some \texttt{hyperref}
     problems.
\end{description}
\end{document}

redpajama_set_name: RedPajamaArXiv


text:
Loggers take two, push win streak to four
La Verne (14-6) 1 0 0 1 2 0 0 4 10 4
Puget Sound (4-11) 1 0 0 6 0 0 X 7 7 2
Puget Sound (4-11) 3 0 0 0 2 4 0 9 10 3
Denison (3-4) 0 0 1 1 0 0 2 4 7 1
2B: Mackenzie Dutton
3B: Rachel Ogata
HR: Mackenzie Dutton; Alexis Schiff
2B: Erica Gott; Kayla Andrus 2; Haley Gray; Jaci Young
HR: Kayla Andrus
2B: Laura Bagan
3B: Katie Nichols
TUCSON, Arizona – The Loggers continued their winning ways when they took two games in Arizona on Thursday. Puget Sound defeated Denison, 9-4, before taking down La Verne, 7-4, in the afternoon.
Kayla Andrus led the Loggers (5-11), going 4-for-7 on the day, with six RBI. The senior hit a home run, two doubles, and had a sacrifice fly. She also earned a victory in the circle. Erica Gott recorded three runs batted in during the two games. Kristi Nagamine and Jessica Gott had two RBI, while Amber Popovich and Jaci Young each had a run batted in.
Puget Sound 9, Denison 4
The Loggers jumped on the board early, with Kayla Andrus launching a three-run home run in the first inning after Kristi Nagamine and Amber Popovich reached base.
Denison scored one run in the bottom of the third inning, and cut the Loggers lead to 3-2 in the fourth inning.
Puget Sound responded in the fifth inning, scoring two runs to go up, 5-2. Andrus recorded her fourth RBI in the inning.
The Loggers broke the game open in the sixth inning, scoring four runs to give the team a seven run cushion at 9-2. Jaci Young hit an RBI single, while Erica Gott hit a 3-RBI double.
In the Big Red's last chance of game, Denison scored two runs, but the Logger defense shut them down to earn the victory.
Jaci Young (2-7) started the game in the circle for the Loggers. She allowed two runs (one earned) in 4.0 innings to earn the win. She struck out three batters. Erica Gott earned the three-inning save. She allowed two runs (one earned), while striking out one.
Puget Sound 7, La Verne 4
La Verne got on the board first in the second game of the day for the Loggers. Mackenzie Dutton hit an RBI single to give the Leopards a 1-0 lead, however, Puget Sound responded in the bottom half of the inning, tying the game 1-1.
The Leopards again took a one run lead, this time 2-1 in the fourth inning. Once again, the Loggers responded in their own half of the inning. In the bottom of the fourth, Puget Sound scored six runs on four hits. Kristi Nagamine and Jessica Gott each recorded 2 RBI in the inning, while Amber Popovich also had a run batted in. The Loggers also took advantage of two La Verne errors in the frame.
La Verne led off the fifth inning with two solo home runs, but the Puget Sound defense held firm to extend the team's winning streak to four games.
Kayla Andrus (1-1) earned the win after throwing 4.0 innings. She allowed just two runs and struck out one. Jaci Young threw the final three innings.
The Loggers will wrap up their Arizona trip on Friday, March 18. The team will take on Wis.-Eau Claire at 11 a.m., before playing Carleton at 1:30 p.m.
Follow the Loggers on Instagram | @PSloggers
Follow the Loggers on Twitter | @PSloggers
Like the Loggers on Facebook | Facebook.com/PSloggers

redpajama_set_name: RedPajamaCommonCrawl


text:
using System;

using Duality;
using Duality.Editor;

namespace Duality.Plugins.Steering
{
	/// <summary>
	/// Implementation of <see cref="IAgentCharacteristics"/> which offers parameters
	/// which are intuitve for end users. The purpose of this implementation is to
	/// hide implementation details as much as possible. If you need more control you can
	/// either use <see cref="AdvancedAgentCharacteristics"/> or use a custom implementation.
	/// </summary>
	public class DefaultAgentCharacteristics : IAgentCharacteristics
	{
		private float aggressiveness = 0.5f;

		[DontSerialize] private AdvancedAgentCharacteristics baseImpl = new AdvancedAgentCharacteristics();
		[DontSerialize] private bool updateBaseImplParams = true;

		public float MaxSpeed
		{
			get { return this.baseImpl.MaxSpeed; }
		}
		public float PreferredSpeed
		{
			get { return this.baseImpl.PreferredSpeed; }
			set { this.baseImpl.PreferredSpeed = value; }
		}
		[EditorHintRange(0.0f, 1.0f)]
		public float Aggressiveness
		{
			get { return this.aggressiveness; }
			set
			{
				this.aggressiveness = value;
				this.updateBaseImplParams = true;
			}
		}

		public float CalculateVelocityCost(Agent agent, Vector2 sampleVelocity, float toiPenality)
		{
			if (this.updateBaseImplParams)
			{
				// [aggressiveness]
				// interpretation: aggressive agents are likely to ignore other agents more => avoid them only if absolutly necessary
				// implementation:
				// we use a function which is
				// - zero if aggressiveness == 0
				// - one if aggressiveness == 0.5
				// - infinity if aggressiveness == 1 [to prevent numerical problem we don't actually use infinity but just a high value]
				// ... and use it as toi exponent. This will lead to a toi-cost-function which is very steep close to one
				// => the agent will avoid other agents in the last moment
				// => if aggressiveness is 0 the opposit happens - the agent avoids other agents very early
				this.baseImpl.ToiExponent = AdvancedAgentCharacteristics.DEFAULT_TOI_EXPONENT * (1f / (1f - MathF.Lerp(0.01f, 0.99f, this.aggressiveness)) - 1f);

				this.updateBaseImplParams = false;
			}
			return this.baseImpl.CalculateVelocityCost(agent, sampleVelocity, toiPenality);
		}

		public override string ToString()
		{
			return string.Format("Default Characteristics");
		}
	}
}

redpajama_set_name: RedPajamaGithub


This summer, I had the amazing opportunity to intern for New Profit as part of "The LinkedIn Volunteer Marketplace Intern Program". LinkedIn teamed up with New Profit and similar organizations to arm nonprofits with a new platform, the LinkedIn Volunteer Marketplace (LVM). With the LVM, nonprofits can fulfill their high-quality volunteer needs by discovering the millions of LinkedIn professional members who have expressed interest in volunteering, and these members can find volunteer opportunities that nonprofits are seeking to fill. I worked with several New Profit portfolio organizations to leverage the LVM to attract skilled volunteers. To provide you with a lens on some of this work, I will focus here on how I worked with Citizen Schools, which greatly benefited from what New Profit and LinkedIn had to offer.
I was excited to introduce the platform to Citizen Schools, whose program relies on skilled volunteers to achieve their mission. After all, this was an opportunity that nonprofits seeking high quality volunteers couldn't miss; posting opportunities on the LVM is absolutely free for New Profit organizations through September of this year. Before doing so, I made sure to collect thorough information on Citizen Schools' mission, program model, and volunteer needs. With help from the New Profit team, I learned that Citizen Schools partners with public middle schools in low-income communities to provide an expanded learning day, where volunteers (also known as "Citizen Teachers") fill afternoons with a variety of educational experiences— from science to architecture to business to law—all intended to develop critical thinking and leadership skills.
Eager to learn more about Citizen School's existing process for recruiting their volunteers, I met with Carolyn Roscoe, the Director of Civic Engagement at Citizen Schools. Citizen Schools currently recruits its volunteers through various pipelines, including corporate partners, universities, civic organizations, and individuals. More than 55% of all volunteers each year are recruited from corporate partners, 35% are from university and civic organization partners, and only 10% are recruited via Facebook, Twitter, Idealist, and VolunteerMatch. While these recruitment channels provide a steady flow of volunteers for the organization, Carolyn was very transparent about the organization's ongoing need to effectively recruit diverse, skilled-based volunteers. In fact, she specifically mentioned that Citizen Schools' Massachusetts office was hungry for skilled professionals to volunteer for their program now more than ever; the organization is currently seeking a number of "Citizen Teacher" volunteers before mid-September for the 2014 fall semester.
Confident that Citizen Schools would benefit from using the LVM, I presented the platform to Carolyn and David Blinn, the National Teaching Fellow who manages Citizen School's online presence. With the customized tools and guides I created, I showed them how the LVM provides more flexibility and viability than Citizen Schools' existing recruitment channels through its ability to target individual volunteers with specific and diverse skill sets. Carolyn and David were so enthusiastic about the free posting platform and its unique skills-targeting feature that within two weeks of my first meeting with them, Citizen Schools had already posted several high quality volunteer opportunities that attracted many professionals with the specific skill-sets Citizen Schools was looking for. Fascinated with the results, Citizen Schools expressed a strong interest in working with New Profit to continue to use the LVM in the longer term. New Profit's communications team is already in touch with LinkedIn and is thrilled to continue with this work.
My experience working with New Profit as part of the "LinkedIn Volunteer Marketplace Intern Program" has been invaluable. Not only did I learn a tremendous amount about New Profit's organizations and all that LinkedIn has to offer, but I also made a significant impact in connecting talent to opportunity, in setting the stage for long-term partnerships, and in modernizing organizations' volunteer recruitment processes to help them achieve their mission.
Citizen Schools is a past New Profit portfolio organization. To learn more about Citizen Schools please click here.


text:
Q: Export-Csv -Append isn't actually appending second set of items I am trying to take two CSV files of users and append one to the other. I start by importing the CSVs and selecting only the columns I want from each, then moving those edited CSVs to temp CSV files (Temp1.csv and Temp2.csv). I then take the two temp CSV files and remove the first line (the header) using Select-Object -Skip 1 and set those to two new temp CSVs (Temp3.csv and Temp4.csv). Next, I import Temp3.csv as a variable, then immediately export that CSV as my final file. Finally, I import Temp4.csv as a variable, then export it to the same file name that I saved Temp3, but with the -Append and -Force flags. However, Temp4 is not appended to Temp3 as I would expect. I feel I'm missing something obvious, and this almost definitely not the best method for writing this script. Everything works up till that last part, though. Any help would be appreciated.
I followed Example 6 of the Export-CSV PowerShell doc here: https://learn.microsoft.com/en-us/powershell/module/microsoft.powershell.utility/export-csv?view=powershell-6
I've also tried combinations of Set-Content and Get-Content with combinations of Import-CSV and Export-CSV. Below are my most recent version and associated outputs:

# Get today's date to add to the end of the user upload file
$importDate = Get-Date -Format "yyyy.MM.dd"

# Import the record, but only select the employee's email address, preferred first name, and last name
# and place those three columns' worth of data in the temp csv file
Import-Csv -Path "EmployeeList.csv" |
Select-Object "Email","FName","LName" |
Where-Object {$_."Email" -ne ""} |
Export-Csv -Path "Temp1.csv" -NoTypeInformation

# Import the record, but only select the employee's email address, preferred first name, and last name
# and place those three columns' worth of data in the temp csv file
Import-Csv -Path "ContractorList.csv" |
Select-Object "Email","FName","LName" |
Where-Object {$_.Email -like "*@company.com"} |
Export-Csv -Path "Temp2.csv" -NoTypeInformation

# Remove column headings
$tempCSVone = (Get-Content -Path "Temp1.csv")
$tempCSVone | Select-Object -Skip 1 | Set-Content -Path "Temp3.csv"

# Remove column heading
$tempCSVtwo = (Get-Content -Path "Temp2.csv")
$tempCSVtwo | Select-Object -Skip 1 | Set-Content -Path "Temp4.csv"

# Export to final csv
$tempCSVthree = (Import-Csv -Path "Temp3.csv")
$tempCSVthree | Export-Csv -Path "TempFinal_$importDate.csv"-NoTypeInformation

# Append to TempFInal
$tempCSVfour = (Import-Csv -Path "Temp4.csv")
$tempCSVfour | Export-CSv -Path "TempFinal_$importDate.csv" -Append -Force -NoTypeInformation

Results in CSV files:

Temp1.csv
Email   FName   LName
a@company.com   A   AAA
b@company.com   B   BBB
c@company.com   C   CCC

Temp2.csv
Email   FName   LName
d@company.com   D   DDD
e@company.com   E   EEE
f@company.com   F   FFF

Temp3.csv
a@company.com   A   AAA
b@company.com   B   BBB
c@company.com   C   CCC

Temp4.csv
d@company.com   D   DDD
e@company.com   E   EEE
f@company.com   F   FFF

Expected result in TempFinal.csv:
a@company.com   A   AAA
b@company.com   B   BBB
c@company.com   C   CCC
d@company.com   D   DDD
e@company.com   E   EEE
f@company.com   F   FFF

Actual result in TempFinal.csv:
a@company.com   A   AAA
b@company.com   B   BBB
c@company.com   C   CCC

A: You are overcomplicating things, after having files

*

*imported, same properties and order

*simply -Append the 2nd to the same file:

## Q:\Test\2019\09\12\SO_57910524.ps1
Import-Csv -Path "EmployeeList.csv" |
  Select-Object Email,FName,LName |
    Where-Object Email -ne "" |
      Export-Csv -Path "Temp1.csv" -NoTypeInformation

Import-Csv -Path "ContractorList.csv" |
  Select-Object Email,FName,LName |
    Where-Object Email -like "*@company.com" |
      Export-Csv -Path "Temp1.csv" -NoTypeInformation -Append

> Get-Content .\Temp1.csv
"Email","FName","LName"
"a@company.com","A","AAA"
"b@company.com","B","BBB"
"c@company.com","C","CCC"
"d@company.com","D","DDD"
"e@company.com","E","EEE"
"f@company.com","F","FFF"

redpajama_set_name: RedPajamaStackExchange


Normally, the investigative processes along understanding, describing, predicting and controlling could also be wanted to respond the priority on psychological and emotional disturbances. Amazingly with these products, you wouldn't have to panic. Virtually all the merchandise on this line have a pH stability much like faucet water. There is no such thing as a chlorine bleach or ammonia found in the merchandise either. Just final weekend I cleaned our youngsters's bathroom (scary!) with a few of these cleaners, and it was a shock that I may nonetheless breathe whereas wiping up the messes. The glass cleaner was the most effective I've ever used. I did not have to scrub at the cussed, dried spots on the mirror, they simply wiped off on the first move. It even made a squeaky clear sound as I used to be wiping it down.
State insurance regulators say the proposal harks back to the times when insurance coverage companies, even household names like Aetna and Blue Cross, offered policies so skimpy they might hardly be referred to as coverage in any respect. Derided as junk insurance coverage," the plans had very low premiums however typically came with five-determine deductibles. Many didn't pay for medical care that is now deemed important.
Will we get well? Sure. For violence, like Achilles' lance, can heal the wounds that it has inflicted. At this time, we are certain hand and foot, humiliated and sick with fear; we can't fall lower. Happily this is not but sufficient for the colonialist aristocracy; it cannot complete its delaying mission in Algeria until it has first finished colonizing the French. On daily basis we retreat in front of the battle, however you may be sure that we is not going to avoid it; the killers want it; they're going to go for us and hit out blindly to left and proper.
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This is because personal insurance coverage bureaucracy and paperwork devour one-third (31 p.c) of every health care greenback. Streamlining fee although a single nonprofit payer would save more than $350 billion per yr, enough to provide complete, excessive-high quality protection for all Individuals. Beneath is a summary of a petition that was created by Mike Adams – the Health Ranger, editor of , which outlines the requirements of health care which is purposeful and managed by the people, not the corporations and authorities.


text:
McCall man runs 20 miles to heroically rescue missing hiker
"There was a little marshy lake, so she had water but no food for four plus days," Jeremy Humphrey said. "So, it was time. It was getting serious."
Author: Gretchen Parsons
Published: 5:31 PM MDT July 20, 2020
Updated: 6:19 PM MDT July 20, 2020
BOISE, Idaho — A McCall man made a brave and daring rescue in the Valley County wilderness.
Jeremy Humphrey is an avid ultra-marathon runner and can move quickly in rough terrain so he put his skills to the test to rescue a hiker who hadn't been seen in nearly a week.
Valley County Search and Rescue says 43-year-old Laura set out to go hiking July 3 and hadn't been seen since.
Her car was found at Peril Lake Trail Head in Valley County.
Humphrey said he was familiar with the area and felt called to help.
"I just felt like a spark," Humphrey said. "I knew I had to get out of bed, throw some stuff in the pack and run. My father passed in the mountains. My entire life is intertwined in mountains."
Humphrey believed he could provide a fresh pair of eyes and legs to the search.
"I thought I had something to offer because I can move quickly in weird, bad terrain," Humphrey said. "It was looking like it was going to be a 40-mile day if I did it right. I got to that Brush Lake area and walked around and didn't see anything."
Humphrey said he climbed to a higher peak, called out to Laura and she answered.
"She was just settled into this little depression in the topography," Humphrey said. "If you weren't above, you would never see it."
When Humphrey got to the woman, he said she was in rough shape.
"There was a little marshy lake, so she had water but no food for four plus days," Humphrey said. "So, it was time. It was getting serious."
Humphrey gave Laura some food and immediately called for help.
"I was very thankful I had three or four bars on the cell and had plenty of battery left," Humphrey said.
A helicopter picked the woman up and carried her to safety.
Despite suffering a sunburn and exhaustion, Humphrey says the woman is okay.
Humphrey says the two plan to get dinner soon and talk about what happened.
"It felt good to do something not selfish," Humphrey said. "Something for somebody else and to use multiple skills that I have honed over my entire lifetime to put me in that position to do something."
Gretchen Parsons is an anchor, reporter and producer at KTVB since 2016. You can follow her on Instagram @gretchenparsonsKTVB or @gretchenKTVB on Twitter.
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Watch more 'Local News'


text:
THE KING AND I SAN ANTONIO
Musicals /
The King and I /
The King and I San Antonio Tickets
About The King and I San AntonioSell tickets
One of Rodgers and Hammerstein's best-loved works, The King and I tells the story of fiery British schoolteacher Anna and her tempestuous relationship with the spoiled and dictatorial King of Siam. This new production has been skillfully refreshed for the 21st century.
Combining sumptuous costumes, opulent staging and a score that features such classics as "Shall We Dance," "Getting To Know You" and "I Whistle a Happy Tune," The King and I is thoroughly enchanting from start to finish. From the moment the curtain rises to reveal the ship Chow Phya slowly docking in Bangkok, the audience is caught in crossfire of East and West, old and new - all played out with classy Broadway production values and a splash of humor.
The production is appearing at the Majestic Theater, San Antonio as part of a national tour. The King and I San Antonio tickets will surely sell out quickly, so book your seat while you can.
The King and I San Antonio storyline
It is 1860's Bangkok and the King of Siam has invited the newly widowed Anna to teach English to his wives and 77 children. He's patriarchal and prone to temper tantrums; she stubbornly insists on being treated as an equal. This clash of personalities and cultures is at the heart of the show.
At first, Anna is horrified by the traditions that the King holds dear, viewing his wives and concubines as little more than pampered slaves. Her convictions are shaken, however, by the King's first wife, Lady Thiang, who is fiercely loyal to the King. Being deeply in love with her husband, Thiang resists Anna's lessons on emancipation (clumsily delivered through a reading of "Uncle Tom's Cabin") and brings the audience to tears with her heart-wrenching delivery of "Something Wonderful," surely one of the show's most moving songs. Get the hankies ready.
By contrast, the King's junior wife Tuptim, a "gift" from the King of Burma, takes Anna's lessons very much to heart. She joins her secret lover Lun Tha and the young couple resolve to run away together.
Over time, a cautious romance flowers between Anna and the King. With both keeping a strong grip on their respective traditions and values, they slowly teach each other about respect, love and understanding that somehow manages to transcend the greatest of cultural differences.
The King and I San Antonio history and accolades
The King and I premiered on Broadway in 1951, scooping Tony Awards for Best Musical, Best Scenic Design, Best Costume Design, Best Actress (for Gertrude Lawrence) and Best Featured Actor (for Yul Brynner). Subsequent revivals have all earned Tony gongs. The current production won four Tony awards including Best Revival of a Musical in 2015.
Similar to The King and I San Antonio
If you're a fan of lavish, over the top musicals, be sure to check out The Phantom of the Opera as part of its North American Tour. Closer to home, the Majestic Theater is also staging the award-winning The Bodyguard, based on the smash-hit film of the same name.


The Levellers were a crucial component of a radically democratic movement during the civil wars in seventeenth-century England. This was to be democratic at a time when the very idea of democracy conjured up nothing good; with its suggestion of anarchy and the 'levelling' of distinctions in rank and of property, even the holding of women in common. This collection of thirteen fully annotated Leveller writings, including their famous Agreements of the People, is important as a contribution not only to the understanding of the English civil wars, but also of democratic theory. The editor's introduction sets the Leveller ideas in their context and, together with a chronology, short biographies of the leading figures and a guide to further reading, will be of interest to students of the English civil wars, the history of political thought and the history of democratic ideas.


text:
Lebanon Photos
Habeeb.com | Arabic Bible | Arabic Bible IBS | Links | Cedar of Lebanon | Lebanon Main Pg | English Letter | French Letter | Spanish Letter | Farsi Letter | Arabic Letter | Lebanese Recipes
Lebanon Photos - Chouf Region & Cedars
This page contains photos of the Chouf region in Mount Lebanon
See bottom of page for many links to hundreds of photos and information about Lebanon. See also the index for a listing of photo topics
The Chouf region, with Mount Lebanon covered with cedars and snow
Entrance to the Cedar preserve in Chouf
Youn cedar trees in the Chouf preserve
Cedars of Lebanon trees, Chouf
Beautiful cedar trees, Chouf
Entrance of the Chouf cedar preserve
Foot path inside the preserve
Chouf mountain
View down from the top of the Chouf mountain
Cedar in the snow, Chouf
Cedar cones
Road in the chouf region
Moussa Castle, Chouf, Lebanon
Chouf pine trees
Chouf, Mount Lebanon
Chouf Pine trees are in the foreground.
The cedar trees are on the top of the mountain amid the snow
More Chouf photos
God's country - the Chouf
I love the view of the Chouf mountain with cedars on top
It is as if they are reaching to the heavens
The dark spot amid the snow are cedar trees
Hope these photos made you drool. Do you miss the peaceful Lebanon we grew up in, way back when... 1960-1974
Thank you for the opportunity to share Lebanon's beauty with the world. Please browse the Lebanon Photo pages below
Thank you to everyone who contributed photos in the past three years. Click on the links below to see more photos:
Index of Lebanon Photos: Click here for index
More Lebanon Photo Pages: 1 | 2 | 3 | 4 | 5 | 6 | 7 | 8 | 9 | 10 | 11 | 12 | 13 | 14 | 15 | 16 | 17 | 18 | 19 | 20 | 21 | 22 | 23 | 24 | 25 | 26 | 27 | 28 | 29 | 30 | 31 | 32 | 33 | 34 | 35 | 36 | 37 | 38 | 39 | 40 | 41 | 42 | 43 | 44 | 45 | 46 | 47 | 48 | 49 | 50 | 51 | 52 | 53 | 54 | 55 | 56 | 57 | 58 | 59 | 60 | 61 | 62 | 63 | 64 | 65 | 66 | 67 | 68 | 69 | 70 | 71 | 72 | 73 | 74 | 75 | 76 | 77 | 78 | 79 | 80 | 81 | 82 | 83 | 84 | 85 | 86 |
Cedar of Lebanon Photos: | Main Page | Page 1 | Page 2 | Old Cedars | Cedar Info | The Cedar as a Cultural Asset |
Map of Lebanon - Click here for excellent Lebanon maps with extreme detail
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text:
Aniak Slough
Bethel (CA)
Tributary to
Kuskokwim River
16 mi (25.75 km)
49 ft (14.94 m)
Aniak Slough in Detail.
anabranch of Kuskokwim River, heads at Aniak and flows W Yukon-Kuskokwim Delta; 16 miles long.
Local name; reported in 1942 by U.S. Geological Survey (USGS).
Russian Mission (1947), Russian Mission (1947), Russian Mission (1950), Russian Mission C-2 (1952), Russian Mission C-2 (1952), Russian Mission (1980), Russian Mission (1980), Russian Mission (1980),
Places Near Aniak Slough
Aniak,
Aniak Slough,
Swift Creek,


Turmeric has many health benefits such as prevent cancer, protect the digestive tract, slow the aging process, alleviate pain, eliminate depression, reduce inflammation, ease menstrual difficulties, protect cognitive abilities and it has ability to heal wounds. This herb is closely related to other members of the ginger family. It is a perennial herb which is native to India. The scientific name of turmeric is Curcuma longa. Turmeric itself is derived from the rhizome of the plant which is dried before the useful powdered form can be acquired. This herb needs a rather specific temperature and environment to thrive. This is a reason why it is not widely cultivated throughout the world but it is exported all around the globe due to its desirability. Many people have seen turmeric but they have not recognized it. If you have ever enjoyed Indian food, then you have almost certainly consumed it. Turmeric is not considered to be an allergic subsstance but it can have some side effects on the body such as diarrhea, dizziness and nausea, particularly when turmeric is consumed in large quantities. There are some cases in which when turmeric was consumed in excessive amounts in a medicinal capacity, then it has caused heart irregularities. Talk with medical professional before you add turmeric in your diet.
Depression: Curcumin is a versatile substance. There are some studies in which is shown that curcumin has a similar effect as Prozac on patients suffering from stress, anxiety, mood swings and depression. This is making it a powerful alternative to pharmaceutical routes which often have addictive or dangerous side effects.
Cognitive abilities: In the traditional medicine, this home remedy was often relied to boost memory retention, increase concentration and boost cognitive abilities. Many of the mentioned traditional benefits have ended up being legitimated by research and this herb is still considered as brain boosting herb. It can increase general cognitive ability. Also it can protect the neural pathways from long – term oxidative stress and the build – up of plaque. It is a powerful antioxidant herb. This means that it can stimulate neural activity and prevent cognitive degradations, which often comes in the form of dementia and Alzheimer's disease. There are many studies in which is shown that curcumin is very effective treatment in clearing out amyloid plaque which is the major indication of Alzheimer's disease progression.
Heart health: Vitamin B6 and curcumin are turmeric components which can boost your cardiovascular health. Vitamin B6 can inhibit the production of homocysteine. This is a negative bodily byproduct that seriously is damaging cell walls. These weakened walks can cause many complications in the heart, particularly when exacerbated by plaque build – up or high blood pressure. Curcumin can directly balance your cholesterol levels because it is eliminating low – density cholesterol from the blood vessels and arteries. The previous mentioned property can help you in the prevention of atherosclerosis, so when turmeric is combined with stronger blood vessels, then it is representing a comprehensive solution for different range of heart issues.
Detoxification of the body: Turmeric and its active organic components can improve your liver function and they can reduce the levels of toxicity in your body. By ensuring that toxins are removed efficiently and stimulating the lymphatic system, the antioxidant activities of turmeric are an ideal solution for toxicity or liver ailments.
Cancer treatment and prevention: Turmeric is one of the best natural cures for the treatment or prevention of cancer. Curcumin is a powerful antioxidant agent which is linked to reduction in colon cancer cells and also this component is a direct inhibitor for a protein which is essential for tumor growth. This is a reason why turmeric should be added in every diet as a preventive measure. Also it slows metastasis of cancerous growth. The most studies are done about the effects of turmeric for colon cancer prevention but there should be done a lot more studies in the feature about this topic.


Since 1955, Standard Change-Makers, Inc. has been setting the "standard" in bill, coin & card acceptance and change, token and ticket dispense for self-service, coin-operated entities, including the laundry, carwash, amusement and vending sectors. Maintaining a reputation for building the most secure, reliable and dependable products in the industry, we have grown with the industries we serve by being on the forefront of technology for bill validation, electronic dispense and modular "plug & play" components. Further, client feedback is the cornerstone of our innovation – you talk, we listen.
As such, we launched several technologies over the past year that resolved several key problematic customer pain-points. What follows is a recap of the innovations that made 2018 both a rewarding and remarkable year for all of us here at Standard.
Technology has definitely changed since the release of our System 500, 500-E, System 600-FST, and 600-EF bill validator products in the 1980's. With thousands of these systems still in operation, keeping pace with advances in technology has been challenging for these clients. Our new SC-Conversion Kit was developed to replace those aging bill acceptors, allowing customers to upgrade equipment without forfeiting reliable coin hopper operation or removing permanently placed cabinets. Best of all, the SC-Conversion Kit includes our Remote Notification Feature that owners can program to receive daily audit reports and text or email alerts when a problem occurs.
To increase the capabilities of the original Expanded Function (EF) Module feature used in our Modular Series change machines, we created the second generation, dubbed the EF+ Module. The EF+ not only features advanced technology with more onboard memory and a faster processor, it also has an Ethernet port that enables the Remote Notification Feature. Using an Ethernet cable hardwired directly to the location's network router, this feature empowers alerts and reporting to up to five email addresses or mobile phone numbers. Furthermore, the new EF+ Module enables a new level of programmability. When a hopper or bill dispenser is replenished, owners can program the "Dispenser Low Level" Alert to send a text alert when a specific level is reached. Likewise, you can also program a "Bill Stacker Full" alert when the bill validator's stacker box is almost full. These capabilities help ensure that your machine continues operating and gives you advance notice that it's time to collect and replenish.
Standard has integrated MEI (Mars) Bill Recycling technology into our products. This advanced replenishing technology takes bill validating to the next level by accepting notes for payment, then storing those same notes (up to 30 bills) in internal barrels which are then returned as change to consumers when they use larger denominations. Machines equipped with Recyclers can provide more convenience for patrons and free attendants from spending time on making bill change for customers, to focus on more important daily duties.
Say hello to EMV-compliance and goodbye to fraud risk! Standard's new Alternative Credit Card Acceptance Interface Kits allow customers to convert existing Credit Card-to-Token machines to EMV-compatible solutions.
The Nayax VPOS™ Card Reader and AMIT™ Cellular/IP device. Standard has also successfully integrated the USA Technologies ePort™ Card Reader and G-10 device. Both solutions support both traditional magnetic stripe credit and debit cards along with the newer NFC technology found in contactless cards and mobile wallets.
We are also working on interfacing with the CrytoPay™ reader.
IMPORTANT NOTE: Please be advised that these solutions may requires software upgrades (EF Module and/or Hopper Boards); and Card Reader Mounting Brackets will be necessary. You will be required to order the MDB-only Card Readers & Modem device kits directly from Nayax or USA Technologies in order to sign up for processing under your own merchant account using their approved and certified processor.
Bill dispensing has always required a different approach. Our Glory single note bill dispenser, aka MiniMech, ups the ante from our previous models, the UniNote Bill Dispenser and Fujitsu F50 Bill Dispenser, offering the best of both and more. Featuring patented Double Bill Detection (DBT) technology that prevents the inadvertent dispense of multiple bills and a self-adjustment sensor that auto-adjusts tension for optimum alignment, the MiniMech bill dispenser dispenses bills horizontally using fewer belts and gears than other models, helping to lower the probability of required maintenance. Easy to load, the MiniMech has a 1,000-note capacity, providing the ultimate in low-maintenance bill dispensing. Already installed in our BX Rear Load machines, the system has been in the field for over a year now, garnering rave reviews for being reliable and easy to maintain.
Standard Change-Makers has several initiatives planned for 2019.
MiniMech bill dispensers will be installed in our Front Load BX1010-G systems.
MultiMech, our Glory dual-note bill dispenser, will be released in our Front Load and Rear Load models. Our BX1020-G and BX1020RL-G models will boast a 3,000 bills capacity!
Glory bill dispensers will be incorporated into our BCX (Bill-and-Coin Exchangers) Series machines.
A new EMV-ready chip card reader and Datacap Modem device with an intuitive touch screen interface will be introduced into our Credit Card-to-Token series, providing more package selections for both credit card acceptance and cash acceptance.
Both the iU285 Card Reader, offering chip card, mag-stripe, near-field "Tap 'n' Go" or mobile phone pay card acceptance, and the Datacap Systems IPTran LT™ hi-speed, internet-based processing device that allows the choice of multiple EMV-ready processor networks (i.e. First Data, Paymentech, Global, Vantiv-Worldpay, etc.) will be incorporated into our systems.
Throughout our more than 60 years in business, Standard Change-Makers has maintained its commitment to secure construction, reliability, accuracy and long product life. Further, our customer service support leads the industry, providing rapid response and remedy for both new systems and machines that have been in the field for decades. We have many milestones ahead of us in 2019, and are sure that in each endeavor, we will mimic the successes we achieved in 2018 to bring you the latest in reliable, secure currency changers.


You will receive a confirmation e-mail that contains your submission as well as the next step in receiving your free virtual training and consultation with BedBug Central. If you happen to notice any of the information provided was misspelled or in error, please contact us through our contact form link at the top of our site so that we can quickly remedy it. Thank you again and we look forward to serving you.