Camp David is the site for the long sought after Mideast peace talks. The President and his family are at Camp David when it is attacked by terrorists hell-bent on sabotaging the peace process.
The terrorists want to kidnap Laura Davidson, the President's daughter, to hold the peace process hostage. Lt. Alan Lambrow and Laura barely escape the attack and are on the run. They are ruthlessly pursued by terrorists with orders to capture Laura, or failing that, to kill her. Alan and Laura can't phone in because they discover that the phone lines to the White House are tapped. They are out of money and out of places to hide. In addition to the terrorists hunting them, the FBI thinks the Lt. might be one of the kidnappers.
An extraordinarily fast-moving adventure, the story's unexpected ending will leave you breathless.


I also found a "white" Yoplait with the word "matok" (sweet) included, but wasn't paying full attention to all the words on the package. So this morning, when I opened one, thinking it was slightly sweetened plain yogurt, I noticed that it was rather airy. I began to scrutinize the back of the package and noticed that the fat content was 4.6%, so the reason that it was only 90 calories was because at least half of the container was air. So really, it was like eating airy whipped cream. For breakfast. Later when I was rhapsodizing about it to Taxman, he looked at the container and noted, with his mad Hebrew skillz, that I had missed the word "mousse." Oh, yeah, that would pretty much describe it. Somehow I have a feeling the 1.5% peach I knock back tomorrow will not feel quite as special.
And now I think I am done talking about yogurt, because I can pretty much guarantee that I will not be making my own. At this point, I don't know that I will ever cook again. Our oven was delivered Friday, but apparently in this fine country the person who delivers your appliances and the person who installs them? Not the same.
full disclosure: the feeding and laundry-ing was all in hopes of getting such a great shout-out on your blog. so yay! it worked!
I still don't know how to use my oven and I've owned it for 12 years. I cook everything between 3 and 4 using turbo unless i'm baking and then I just use the top and bottom elements.
I love that Yoplait mousse.. I has one everyday in July!


text:
Hydrophoria trivittata är en tvåvingeart som först beskrevs av Zetterstedt 1860.  Hydrophoria trivittata ingår i släktet Hydrophoria och familjen blomsterflugor.

Artens utbredningsområde är Sverige. Inga underarter finns listade i Catalogue of Life.

Källor

Blomsterflugor
trivittata

redpajama_set_name: RedPajamaWikipedia


transmission of information and clinical follow-up.
Comprehensive treatments intended to ensure the proper health and hygiene of your feet.
the prescription of orthotics for your feet.
(Order of Podiatrists of Quebec) and also hold licences in radiology.
Specialized intervention methods for the treatment of the most complex foot issues.
Members of the Podiart Team have the necessary skills and training to operate and grow in a medical environment adapted to different methods and techniques related to podiatric surgery.
Various surgical interventions may be required for the treatment of local conditions while more complex orthopaedic issues are treated with surgery under anesthesia.
Located at the podiatry clinic in Montreal, our operating room offers all the versatility required to perform our surgeries, from minor interventions for the treatment of local wounds to surgeries under anaesthesia for more complex orthopaedic issues.
Various deviations affecting the bone and joint structure of the foot.
Surgical interventions are performed on the foot. They may involve ablation, reconstruction or excision procedures related to tendons, ligaments, muscles or bone structures.


text:
+22 All Photos
Horseshoe Bay Sanctuary - Cherry Blossom
West Vancouver, Horseshoe Bay WV
Address: 6693 Nelson Avenue, West Vancouver, BC, Canada
Postal Code: V7W 2B2
Number of Floor: 3
Number of Unit: 5
Developer: Westbank Corp.
Strata Plan: EPS7278
Building Name: Horseshoe Bay Sanctuary - Cherry Blossom
Concierge Gym
Horseshoe Bay Sanctuary is built on West Vancouver's most beautiful parcel of waterfront land. Designed by architect Paul Merrick and completed in 2022 by Westbank, it provides panoramic views of Horseshoe Bay as well as the alpine peaks along Howe Sound. The multi-coloured buildings were inspired by Portofino in Italy given the unique bay location of this project. Each of the buildings feature on-site heating and cooling as provided by a geothermal ocean loop, which allows for the reduction of greenhouse gas emissions of up to 70%. Residents can access luxurious amenities which include the Boathouse that features a Chris Craft Corsair 25 with a dedicated captain and rentable paddleboards and kayaks, as well as a 24-hour concierge and state-of-the-art gym. Each lobby hosts local artwork and offers restricted floor access with the elevators.
The local Horseshoe Bay Village has easy access to North Vancouver by Taylor Way, both Squamish and Whistler by way of the Sea to Sky highway and is steps from the ferries for a quick getaway to Vancouver Island.
Horseshoe Bay Sanctuary's Cherry Blossom buildings have 3 levels used for 10 townhouses.

redpajama_set_name: RedPajamaCommonCrawl


text:
HeadhunterPOV
Neal Click is an executive recruiter specializing in the placement of transportation, logistics and supply chain management professionals. Neal spent over 25 years in management and executive positions in the transportation industry. His blog addresses current issues relating to the job market and our economy. He is also inclined to comment from time to time on politics, society, culture and religion.
Stop Limiting My Potential
What Was, What Is and What Will Be
Protect This House and Other Lies We Tell Ourselves
Neal Click
From BBC news-
"A ban on adverts featuring "harmful gender stereotypes" or those which are likely to cause "serious or widespread offence" has come into force.
The ban covers scenarios such as a man with his feet up while a woman cleans, or a woman failing to park a car.
The UK's advertising watchdog introduced the ban because it found some portrayals could play a part in "limiting people's potential".
"Our evidence shows how harmful gender stereotypes in ads can contribute to inequality in society, with costs for all of us. Put simply, we found that some portrayals in ads can, over time, play a part in limiting people's potential," says Guy Parker, chief executive of the ASA (Advertising Standards Authority)."
At the risk of being stereotyped as an older, white, conservative male this seems to me to be just one more crazy attempt by progressives to brute force the round peg of equality into the square hole of reality.
People are different, genders are different. Why people are who they are is complicated and we still don't fully understand it. But the scientific evidence for real differences between the sexes is undeniable. Gender matters. And there is substantial evidence that other factors matter, they matter a lot. Personality type matters. Where you grow up matters? Race matters. Money matters. Health matters. Education matters. Your decisions and the decisions of others matter. The weather matters. IQ matters. Physical appearance matters. Age matters. Like it or not, fair or not…differences matter.
To be clear, I am all for equal opportunity for everyone. But equal outcomes are not possible. Over the past 100 years most of the modern, industrialized world has made tremendous progress toward creating equal opportunity for all. Yet, we still see unequal outcomes among people of different genders, races, places of origin, etc.
Some of this will take time to work through. Ever since we started walking upright, discovered fire and began telling our stories on cave walls, human civilization hasn't been all that big on equal opportunity. Rulers and subjects have been the norm. The fortunate few selected by the gods to run things. On the timeline of human history we are still new at this equal opportunity idea. We are very much a work in process. And, going forward things will get incrementally better for more people. But not for all and never the same for all. This is a hard pill to swallow for social scientists. So they spend their time and someone else's grant money doing studies that show where and how society does these awful things to perpetuate inequality.
As I grow older, I resent the assumptions that many people have about aging and ability. I am still in good shape, the mind is sharp and I'm not all that different than I was 20 years ago. But, the reality is that I am different. My hearing isn't as good as it used to be. I'm not as strong and don't recover from a hard workout or heavy physical labor the way I used to. I tend to be more forgetful. I have to pee more frequently. I watch Blue Bloods and most of the music I listen to is from the last century. So I fit a lot of older adult stereotypes.
But I don't want to watch catheter commercials. I don't need a reverse mortgage. I'm not moving to an "active senior" community. I don't much like seeing older people portrayed in movies and television as incompetent, sad and helpless.
All of this stereotyping could be limiting my potential. But, it's not. If anything, it motivates me to keep going as well as I can for as long as I can. While I am not the man I used to be, in many ways that's a good thing. I'm kinder and gentler and don't take life as seriously. I have gained the perspective that comes with age. That is a difference and an advantage that I gladly embrace.
My potential is limited by many things. Now, most of all, by time. I don't need a well-meaning social scientist to ban advertisements that I don't like or want to watch. But, if they could come up with a Time Machine that actually worked, I'd take a spin.
"It would be interesting to find out what goes on in that moment when someone looks at you and draws all sorts of conclusions."
― Malcolm Gladwell
Posted by Neal Click at 8:22 AM No comments:
If you want to know how someone is likely to vote ask them how they feel about the Past, the Present and the Future. If they are honest with their answers, you can predict with a fair degree of accuracy how they are likely to vote. There will always be special circumstances that override attitudes toward past, present and future. Race and gender perhaps being the most likely to override all other voter attitudes, opinions and interests.
But for the most part, how people vote depends on how they feel about the Past, the Present and the Future. Those who think the Past was better will pretty much tend toward voting conservatively; including those within a left-leaning party such as the Democrats. Those Democrats who like the "old Democratic Party" will tend toward someone more conservative or as they prefer to call in, centrist. (Joe Biden's current status is a prime example). But clearly, most of the "past was better" crowd is going to vote Republican, even if it means voting for Trump again.
Those with a positive view about the Present are definitely more inclined to vote for the incumbent. But then it gets interesting. When it comes to those having a negative view of the Present, they tend to fall into two camps. One camp thinks The Present would be better IF it were more like the Past. The other has a Future vision of a new and improved way of life that will be much better than the Present. Those unhappy with the Present and looking for a return to the Past will tend toward conservatism and vote Republican. (This was a key factor in Trump's win). The other unhappy camp is all about fixing those things that are broken and have been broken for a long-time and are likely to get worse if we don't change and become more "progressive".
And then lastly, how one feels about the Future will tend to impact ones vote. In 2008, even people who thought America was or had been a great place for them and their families, were scared and confused. The Future did not look all that great and a lot people went with Hope and Change because they didn't know what else to do. So even people who pretty much wanted their good old familiar, reliable country back voted for a guy who had a much more progressive agenda which, under normal circumstances, would have made them very uncomfortable.
The problem Republicans are facing in 2020 is that a growing number of voters under the age of 35 have not lived in an America that made them long for the good old days. And a good number of them aren't doing all that great in the here and now either. These folks will be inclined to vote Democrat (or not at all.) Some might even go for a far-left third party candidate if such an option were available. Most all of the "identity" politics crowd will vote Democrat because the Democrats have done a great job of appealing to that audience. They started doing it in 60's, eventually forming the Rainbow coalition and other groups of progressive activists. It probably cost them a lot of elections over the past 40 years, but now it's ready to bear fruit. Older white, males who pretty much loved the America they grew up in, are a dying breed…literally.
Increasingly we are now told that the Past was only great for certain people. The Present works great for The One Percent, but everyone else is worse off and losing ground. The Future looks like melting ice caps and rising sea levels, a bad moon rising. All of this resonates with millions of people in this country. So does the narrative shape the people or do the people shape the narrative? Or is it a bit of both? And "What Will Be" ultimately comes down to one question….who actually shows up and votes.
When you are right you cannot be too radical; when you are wrong, you cannot be too conservative.
-Martin Luther King, Jr.
"The truth will set you free, but not until it is finished with you"- David Foster Wallace
Three years ago, Art Briles was removed from his position as head football coach of the Baylor University Bears. From a lawsuit filed on behalf of 17 women, it is alleged that over a period of five years 19 of Briles' players committed sexual and/or physical assaults. The victims claim that Briles and his staff knew about most, if not all, of these attacks and did nothing. Took no action to report these complaints to the police or the university authorities and, for the most part, worked to protect the players and the program.
This whole terrible event is now back on the front page because Art Briles just got hired to coach a football team here in Texas. A nice Sunday drive to the southeast of where I live is the hometown of Don Meredith, Mount Vernon. Dandy Don the almost great and much beloved QB of the early days Dallas Cowboys; and the good ol' boy star of Monday Night Football back when Monday Night Football was a thing. The fine folks of Mount Vernon and Franklin County, Texas are now the talk of the football world. A handful of their fellow citizens decided that Art Briles would be the right man to lead their Mount Vernon Tigers to football glory. They spoke to several of his references, most notably Grant Teaff, Baylor coaching legend and former head of the American Football Coaches Association. Grant Teaff is a devout Christian and a man of impeccable character. If he endorses someone, it's like gold in the state of Texas. And he gave Briles his golden thumbs up.
Much has been written about the Baylor/Briles mess. Regardless of who knew what, when did they know and what did they do or not do about it; the big question is WHY? Why do people and institutions allow bad things, or even alleged bad things, to go on without being addressed and resolved, one way or the other?
What is behind the bad judgment and poor decision-making that goes on to create outcomes like the Baylor mess, or the Penn State/Paterno/Sandusky thing, or going to war over non-existent WMDs, or Watergate, or the Catholic Church sex abuse scandal…or, or, or….?
The core issue is one of morality. Either their moral compass is broken or they simply rationalize their decision to fit the situation. In most cases, including the ones mentioned above, people made decisions which they thought were "right". So how does one see "right" in something that is so "wrong". Or at least wrong when viewed objectively in the clear light that tends to shine after the damage has been done.
When ones first priority is "Protecting This House", or position, or company, or reputation, or fortune…or anything we place great value upon…we simply lie to ourselves and then to others. We cast doubt on the "wrong" that has been done or will be done. Maybe it's not that bad or it didn't happen at all or nothing will happen. Maybe what we are doing is for the greater good and what has happened or will happen to innocent people is just collateral damage. Or maybe they aren't all that innocent in the first place. Maybe we are doing what we really believe to be the right thing, but we take the easy way out and make up stories that sound better (if they actually turn out to be true…WMDs were there…yes they really were…no matter what the facts are.)
In the end, the truth and doing the right thing may get you nailed to a cross. But the truth and the doing the wrong thing leaves you hanging up there….or seeking redemption too late in a place like Mount Vernon.
Posted by Neal Click at 2:52 PM No comments:


We are happy to welcome you in our shops located in the Old Quebec's Quartier petit Champlain and in Sainte-Marie.
Please refer to the Quartier Petit Champlain website for our opening hours.
Business hours are extended during Summer.


text:
\section{Introduction}

In the current paradigm of structure formation, the virialized dark
matter halos are considered to be the building blocks of the mass
distribution in the universe. The structure and number distribution of
dark matter halos, as well as their formation histories and clustering
(bias) properties, are the main ingredients of halo models.  Among
these properties, theoretical halo bias models have been derived
either analytically using the (extended) Press-Schechter formalism
\citep[e.g.][]{Press1974, Bardeen1986, Mo1996, Sheth1999, Sheth2001},
or formulated empirically from numerical simulations
\citep[e.g.][]{Jing1998, Seljak2004, Tinker2005, Pillepich2010,
  Tinker2010}.  So far, at a given redshift, the halo bias appears to
have a first order dependance only on halo mass with more massive
halos tending to be more strongly clustered.  This mass dependence has
played crucial roles both in cosmological probes using the clustering
measurements of clusters or groups \citep[e.g.][]{Bahcall2003,
  Yang2005}, and in galaxy formation studies such as understanding the
correlation functions of dark matter and galaxies via so called halo
models \citep[e.g.][]{Cooray2002}, halo occupation models
\citep[e.g.][]{Jing1998b, Berlind2002}, and conditional luminosity
functions \citep[e.g.][]{Yang2003, Bosch2003, Yang2012}.

Apart from the mass dependence, many studies in recent years have
tried to reveal additional dependences, among which the most notable
is the {\it halo assembly bias} \citep[e.g.][] {Sheth2004, Gao2005,
  Gao2007}. The assembly bias was first observed among halos of
similar masses in simulations where halos that formed earlier are more
strongly clustered than those that formed later \citep{Gao2005}.
Different studies shed light on additional second or third order
dependencies on spin, shape, substructures and halo trajectory
\citep[e.g.][] {Wechsler2006, Gao2007, Li2008, Dalal2008, Wang2011,
  More2016, Mao2017}.  In observations, \citet{Yang2006} was the first
claiming detection of an age dependence in the halo bias from
clustering measurements of galaxy groups in the 2dFGRS
\citep{Colless2001}. Additional confirmed findings were made from
various observations \citep[e.g.][]{Blanton2007, Swanson2008,
  Wang2008, Wang2013, Deason2013, Lacerna2014, Miyatake2016}.
However, null detection was also reported \citep[e.g.][]{Lin2016,
  Zu2017}. By means of galaxy bias models or halo occupation
distribution and conditional luminosity function models, the
clustering properties of galaxies have been extensively used in
cosmological probes and galaxy formation constraints. The impact of
the assembly bias is thus an important issue that one needs to take
into account. For this reason the degree of assembly bias that is
transferred to galaxies and its impact on cosmology and galaxy
formation have been extensively discussed \citep[e.g.][] {Croton2007,
  Reed2007, Zu2008, Jung2014, Zentner2014, Hearin2015, Tonnesen2015,
  Hearin2016}.  So far, these studies have shown that the impact of
assembly bias on galaxy clustering properties is quite trivial.

In addition to the halo structures, numerical simulations and large
galaxy redshift surveys have also shown striking structures: clusters,
filaments, sheets, and voids. These diversity of structures are best
referred as the cosmic web. From a dynamical point of view, dark
matter flows out of the voids, accretes onto the sheets, collapses
into filaments and finally accumulates in clusters. In this picture,
the assembly histories of halos as well as the galaxies formed in them
are expected to be affected by the large scale environment. There are
different approaches in literature to quantify the cosmic web
environments, among which the most straightforward one is using
Hessian matrix.  \citet{Hahn2007a, Hahn2007b} have quantified the
cosmic web environments using the Hessian matrix of the potential
field where, according to the number of positive eigenvalues, a region
was classified as belonging either to a cluster, a filament, a sheet, or
a void environment. The only free parameter in this analysis is the
smoothing length of the density field. Similar probes were carried out
by \citet{Aragon2007a, Aragon2007b}, who computed the Hessian matrix
based on the density field constructed with a Delaunay triangulation
field estimator \citep[see also][ and references therein]{Zhang2009}.

Over the past decade, numerical simulations have revealed that the
properties of halos have dependences on the large scale environments
in which they reside \citep{Sheth2004, Hahn2007b, Jung2014,
  Fisher2016, Borzy2017, Lee2017, Paranjape2017}.  \citet{Sheth2004}
showed that halos in dense environment form slightly earlier than
halos of the same mass in less dense environment. \citet{Hahn2007b}
claimed that low mass halos in the four different environments have
significantly different assembly histories. Particularly, low mass
halos at fixed mass tend to be older in clusters and younger in voids.
Using the Millennium simulation, \citet{Fisher2016} show that at fixed
halo mass, the clustering properties of halos dependent on the cosmic
web environments significantly.  \citet{Borzy2017} investigated the
origin of halo assembly bias, using 7 zoom-in simulations of
{$\mathcal{O}\left( 10^{11}\>h^{-1}\rm M_\odot\right)$} halos. They concluded that
halo assembly bias originates from quenching halo growth by tidal
interaction during the formation of nonlinear structures in the cosmic
web.

Several observational studies also endeavored to investigate the
dependence of either galaxy or halo properties within different large
scale environments. Using galaxy groups that are associated with dark
matter halos, \citet{Wang2009} proposed a sophisticated and robust way
to reconstruct the density field of Universe. Based on the matter
density field constructed from galaxy groups, \citet{Zhang2009}
classified the groups/galaxies in the SDSS observation into different
cosmic web environments and probed the alignment signals of
galaxies. In addition to the cosmic web classification,
\citet{Wang2012} used the galaxy groups in the SDSS observation to
reconstruct the mass density, tidal and velocity fields in the local
Universe. Thus obtained mass density field was used to perform the
constrained simulation of the local universe in \citet{Wang2016},
where they found that the red fraction of galaxies in four different
cosmic web environments do show very different behaviors.  Apart from
the SDSS observation, using the GAMA survey \citep{Driver2011},
\citet{Eard2015} computed the tidal tensor from a smoothed galaxy
density field and classified galaxies into different cosmic web
environments. They showed that there is no significant influence of
the cosmic web on galaxy luminosity functions. Using the same sets of
data, a recent study by \citet{Tojeiro2016} indicates that low mass
halos in clusters are older than halos of similar mass in
voids. However, the trend is reversed for high mass halos, with halos
in clusters being younger than halos in voids. Their work provides the
first direct observational evidence for halo assembly bias in
connection with strong tidal interactions.  Note however, since
galaxies are biased tracers of dark matter, caution should be
exercised when interpreting these observational results where the
cosmic web environments are classified according to the smoothed
galaxy density field.

In this study, with the help of a large N-body simulation, we set out
to measure the halo clustering properties in different cosmic web
environments. Here we mainly focus on the large scale behaviors of the
clustering measures, i.e., the biases of the halos.  The purpose of
this work are two folded: (1) to see if the halo biases have
significant cosmic web environmental dependence, which might be useful
for cosmological probes \citep[e.g.][]{Hamaus2014, Dai2015,
  Hamaus2016}, and (2) to see if the age dependent halo assembly bias
can be explained in terms of the cosmic web environmental dependence
\citep[e.g.][]{Borzy2017}.

This paper is organized as follows.  Section \ref{sec_data} gives a
detailed description of the data and method we used in this study.  In
Section~\ref{sec_clustering}, we investigate the clustering properties
of dark matter halos in different comic web environments.  In
Section~\ref{sec_age}, we explore the age dependence of the halo
biases in those environments. We summarize our results in
Section~\ref{sec_conclusion}.  Throughout the paper we adopt a
$\Lambda$CDM cosmology with parameters that are consistent with the
fifth-year data release of the WMAP mission \citep[][hereafter WMAP5
cosmology]{Dunkley2009}; $\Omega_{\rm m} = 0.258$,
$\Omega_{\Lambda} = 0.742$,$\Omega_{\rm b} = 0.044$,
$h=H_0/(100 \>{\rm km}\,{\rm s}^{-1}\,{\rm Mpc}^{-1}) = 0.719$, $n=0.963$ and $\sigma_8 = 0.796$.

\begin{figure*}
\center
\vspace{0.5cm}
\includegraphics[height=10.0cm,width=10.5cm,angle=0]{f1.eps}
\caption{Projected distribution of halos within a $2\>h^{-1}{\rm {Mpc}}$ thick
  slice. For clarity, only randomly selected 20\% halos with masses
  larger than $10^{10} \>h^{-1}\rm M_\odot$ are shown and color coded in red, cyan,
  green and blue colors accordingly to their cosmic web environments:
  clusters, filaments, sheets and voids, respectively. }
\label{fig:slice}
\end{figure*}

\section{Data and method}
\label{sec_data}

\subsection{Halos in the ELUCID simulation}
\label{sec:simulation}

In this study we use dark matter halos extracted from the ELUCID
(Exploring the Local Universe with re-Constructed Initial Density
field) simulation.  This simulation which evolves the distribution of
$3072^{3}$ dark matter particles in a periodic box of $500 \>h^{-1}{\rm {Mpc}}$ on a
side was carried out in the Center for High Performance Computing,
Shanghai Jiao Tong University. The simulation was run with {\tt
  L-GADGET}, a memory optimized version of {\tt GADGET2}
\citep{Springel2005b}. The cosmological parameters adopted by this
simulation are consistent with WMAP5 results with a mass per particle
of $3.0875\times10^{8}\>h^{-1}\rm M_\odot$.

Even though this is not relevant to this particular study, the ELUCID
simulation is a reconstruction of the mass density field extracted
from the galaxy \citep[e.g.][]{Blanton2005} and group
\citep[e.g.][]{Yang2007} distribution in the north galactic pole
region of the SDSS Data Release 7 \citep{Abazajian2009}. This density
field has been used to constrain the initial conditions using a
Hamiltonian Markov Chain Monte Carlo method with particle mesh
dynamics \citep[ELUCID I:][]{Wang2014}. The genesis of the ELUCID
simulation in particular and its basic properties such as the output
power spectrum and halo mass functions are described in detail in
\citet[][ELUCID III]{Wang2016}.

Dark matter halos have been identified in the ELUCID simulation with
the friends-of-friends algorithm. We have used a linking length
of $0.2$ times the mean particle separation. Only halos containing at
least $20$ particles are used for our study.  The dark matter halo
mass function of this simulation at redshift $z=0$ is in very good
agreement with the theoretical predictions of \citet{Sheth2001} and
\citet{Tinker2008}.

\subsection{Separating halos into different cosmic web types}
\label{sec:cosmicweb}

\begin{figure}
\center
\vspace{0.5cm}
\includegraphics[height=7.3cm,width=7.5cm,angle=0]{f2.eps}
\caption{Mass distribution of halos.  Red, cyan, green and blue
  lines indicate the mass distributions for halos in cluster,
  filament, sheet and void environments, respectively.}
\label{fig:mass}
\end{figure}

\begin{figure*}
\center
\vspace{0.5cm}
\includegraphics[height=10.0cm,width=10.0cm,angle=0]{f3.eps}
\caption{Formation redshift of halos within different cosmic web
  environments. Each panel correspond to a specific halo mass bin.
  Red, cyan, green and blue lines indicate the formation redshift
  distributions for halos in cluster, filament, sheet and void
  environments, respectively. }
\label{fig:age}
\end{figure*}

In order to probe the clustering properties of halos within different
cosmic web environments, we first classify the dark
matter halos' environment using the method by \citet{Zhang2009}. This method is
based on the Hessian matrix of the smoothed density field. This matrix
is defined as
\begin{equation}
  H_{i,j} = \frac {\partial^2 \rho_s} {\partial x_i \partial x_j},
\end{equation}
where the Hessian matrix indices $i$ and $j$ and the corresponding
coordinates $x_i$ and $x_j$ can take values from the cartesian
coordinates along the box axis $x$, $y$ and $z$. The smoothed density
field $\rho_s$ is calculated using a Gaussian filter with a smoothing
scale $R_s=2.1 \>h^{-1}{\rm {Mpc}}$ \citep{ Hahn2007a, Zhang2009}. The 3 eigenvalues
$\lambda_{[1,2,3]}$ of the Hessian matrix $H_{i,j}$ are then
calculated at the position of each halo. We adopt the convention where
$\lambda_1\leq\lambda_2\leq\lambda_3$. The number of negative
eigenvalues of $H_{i,j}$ can be used to classify the environment in
which the halo resides as follows
\citep[see][]{Zhang2009}:
\begin{description}
\item[cluster] a point where all three eigenvalues are negative,\\
  $\lambda_1\leq\lambda_2\leq\lambda_3<0$;
\item[filament] a point with 2 negative eigenvalues,\\
  $\lambda_1\leq\lambda_2<0<\lambda_3$;
\item[sheet] a point with only 1 negative eigenvalue,\\
  $\lambda_1<0<\lambda_2\leq \lambda_3 $;
\item[void] a point with no negative eigenvalues,\\
  $0<\lambda_1\leq\lambda_2\leq\lambda_3$.
\end{description}
Of the $48,129,323$ halos at redshift $z=0$ in the ELUCID simulation,
$9,529,790$ $(19.8\%)$ are located in clusters,
$27,439,946$ $(57.0\%)$ are located in filaments,
$10,649,415$ $(22.1\%)$ are located in sheets and
$510,172$ $(1.1\%)$ are located in voids.
Fig.~\ref{fig:slice} shows the projected distribution of dark matter
halos in the ELUCID simulation in a $500\>h^{-1}{\rm {Mpc}} \times 500\>h^{-1}{\rm {Mpc}}$ slice
of thickness $2\>h^{-1}{\rm {Mpc}}$. Halos in clusters, filaments, sheets, and voids
are indicated with red, cyan, green and blue colors, respectively.

We show in Fig. \ref{fig:mass} the mass distributions of halos in
different cosmic web environments. Halos are the least numerous in the
voids and are more numerous in the filaments than in the sheets.
In the clusters, the number of halos obeys a
different trend. At low mass ($M_{\rm h}<10^{11.5} \>h^{-1}\rm M_\odot$) end, this
number lies between those obtained for voids and sheets  and
at intermediate mass range ($10^{11.5}<M_{\rm h}<10^{12.5} \>h^{-1}\rm M_\odot$)
between those of sheet and filament numbers. As higher and higher
masses are explored, halos in clusters increasingly dominate the whole
population.

The formation of dark matter halos is a complex physical process which
can be characterized through a timescale: the halo formation time.
Among the various existing definition found in the literature, we use
the most common one which corresponds to the time at which the halo's
main branch assembled half of its present (redshift $z=0$) mass
$M_{\rm h}$.  Fig.~\ref{fig:age} shows the distribution of halos as a
function of their formation redshift. The different cosmic web
environments are distinguished and denoted by different colors. Each
panel corresponds to a different halo mass range as indicated. The age
distribution of halos are quite similar in the filaments, sheets and
voids. The halos in clusters however, show broader age distributions,
especially for low mass ones.  Nevertheless, the peak formation
redshifts of halos in all four cosmic web environments are similar,
which gradually change from $z\sim 1$ in low mass halos to $z\sim 0.5$
in massive halos.  In addition, we find that low mass halos
($M_{\rm h}<10^{11.0} \>h^{-1}\rm M_\odot$) in clusters (red) are slightly older
than halos of the same mass that reside in voids (blue).

\subsection{Cross correlation and auto correlation functions}
\label{sec:2PCF}

With all the halos being classified as part of different cosmic web
environments, we proceed to probe their clustering properties. The
first quantity we measure is the cross correlation function (CCF)
between halos and dark matter particles,
\begin{equation
\xi_{\rm CCF} (r) = \frac{P_{\rm HD}(r)}{P_{\rm HR}(r)} -1\,,
\end{equation}
where $P_{\rm HD}(r)$ and $P_{\rm HR}(r)$ are the number of halo-dark
matter and halo-random pairs, respectively.  For our investigations,
the number of random points has been set to be the same as the number
of dark matter particles within the simulation box. Those points follow
a uniform distribution within the simulation volume.

In order to ensure self-consistency of the CCFs, we also measure the auto
correlation function (ACF) of dark matter halos,
\begin{equation
\xi_{\rm ACF} (r) = \frac{N_{\rm R}^2 P_{\rm HH}(r)}{N_{\rm H}^2P_{\rm
    RR}(r)} -1\,,
\end{equation}
where $P_{\rm HH}(r)$ and $P_{\rm RR}(r)$ are the number of halo-halo
and random-random pairs, $N_{\rm H}$ and $N_{\rm R}$ are the number of
halos and random points, respectively.

\section{The clustering properties of halos in different cosmic web
  environments}
\label{sec_clustering}

\begin{figure*}
\center
\vspace{0.5cm}
\includegraphics[height=10.0cm,width=10.0cm,angle=0] {f4.eps}
\caption{Cross correlation functions between halos and dark matter
  particles. The different panels correspond to the same mass ranges
  as in Fig. \ref{fig:age}. Results are shown with open squares and
  error bars. For reference, the solid lines indicate the dark matter
  auto correlation in the ELUCID simulation and the dotted lines the
  same auto correlation multiplied by the bias factor of the halos in
  consideration. }
\label{fig:CCF1}
\end{figure*}

\begin{figure*}
\center
\vspace{0.5cm}
\includegraphics[height=10.0cm,width=10.0cm,angle=0]{f5.eps}
\caption{Same as Fig. \ref{fig:CCF1}, but for halos in different
  cosmic web environments. In each panel, the open squares, open
  circles, stars and dots are results for halos in different cosmic web
  environments: clusters, filaments, sheets and voids, respectively. For
  comparison, results for the overall population are represented using
  a solid line. }
\label{fig:CCF2}
\end{figure*}

\subsection{Halo cross correlations}
\label{sec:ccf}

We first measure the CCFs between halos and dark matter particles in
the ELUCID simulation. We use the subsamples introduced in Fig
\ref{fig:age}, namely 9 mass ranges ($\Delta\log M_h =0.5$):
$10.0\le \log M_h <10.5$, $10.5\le \log M_h <11.0$, ...
$14.0\le \log M_h$.  The open squares shown in Fig. \ref{fig:CCF1} are
the CCFs measured from halos within these mass bins. The error bars
are obtained from 200 bootstrap re-samplings of the dark matter halos.
There are two features in these CCFs:
\begin{enumerate}
\item more massive halos have overall stronger CCFs;
\item the 1-halo and 2-halo terms in the CCFs can be clearly separated
  by a change in the slope.
\end{enumerate}

For comparison, we also measured the auto correlation function (ACF)
of dark matter particles in the ELUCID simulation. It is shown in each
panel of Fig. \ref{fig:CCF1} as a solid line. Quite interestingly,
the CCF of halos with mass $\la 10^{13.5}\>h^{-1}\rm M_\odot$ is much smaller than
the ACF at the 1-halo and 2-halo transition scales.  This is caused by
the lack of 1-halo pairs in the CCF. On larger scales, $r\ga 3\>h^{-1}{\rm {Mpc}}$,
the shape of CCF is quite consistent with the ACF.  Since massive
halos are more strongly clustered (biased) than low mass ones, to take
this bias into account in the ACF we use the theoretical predictions
obtained by \citet{Tinker2010}. The dotted line in each panel is the
ACF of dark matter particles multiplied by the median bias factor for
the halos in consideration. In general, we find that the biased ACFs
on large scales are in nice agreement with the CCFs.

Once we measured the CCFs of halos in different mass bins, we proceed
to measure the CCFs of subsamples of halos in different cosmic web
environments. We show in Fig \ref{fig:CCF2} the CCFs measured
separately from the four halo subsamples corresponding to their large
scale environments, namely: clusters (red open squares), filaments
(cyan open circles), sheets (green filled pentagons) and voids (blue
filled circles).  The CCFs of these subsamples show quite different
behaviors compared to the overall halo sample.  This is a clear
indication that a significant cosmic web environment dependence
exists, both on intermediate and large scales.  More precisely, this
figure reveals the following features:
\begin{enumerate}
\item On very small scales, where the CCFs are dominated by the 1-halo
  term, the CCFs of halos in different cosmic web
  environments follows the expected asymptotic trends. This behavior
  may not appear clearly for halos  $\la 10^{11.0}\>h^{-1}\rm M_\odot$ as the scale
  is limited to values $\ga 0.15\>h^{-1}{\rm {Mpc}}$. Still it is quite distinct
  in more massive halos.
\item At intermediate scales between the 1-halo term region and
  $\sim 3\>h^{-1}{\rm {Mpc}}$, some interesting variations are revealed especially
  for relatively low mass $\la 10^{12.5}\>h^{-1}\rm M_\odot$ halos. Halos in
  cluster, filament, sheet and void environments sequentially show
  suppressed CCFs. This feature is again quite expected, as the cosmic
  web environments themselves are defined according to the density
  field on such scales.
\item On large scales at $\ga 8\>h^{-1}{\rm {Mpc}}$, however, an interesting and
  unexpected feature is found in the CCFs. The halos in cluster,
  filament, sheet and void environments sequentially show {\it
    enhanced} CCFs.  At any fixed mass, halos in the void region have
  the highest bias.
\end{enumerate}

\begin{figure*}
\center
\vspace{0.5cm}
\includegraphics[height=10.0cm,width=10.0cm,angle=0]{f6.eps}
\caption{Same as Fig, \ref{fig:CCF1}, but for the halo auto
  correlation functions. }
\label{fig:ACF1}
\end{figure*}

\begin{figure*}
\center
\vspace{0.5cm}
\includegraphics[height=10.0cm,width=10.0cm,angle=0]{f7.eps}
\caption{Same as Fig, \ref{fig:CCF2}, but for the halo auto
  correlation functions. }
\label{fig:ACF2}
\end{figure*}

\begin{deluxetable*}{ccccccc}
  \tabletypesize{\scriptsize}
  \tablecaption{The biases of halos in different cosmic web environments.}
  \tablewidth{0pt}
  \tablehead{  (1) & (2) & (3) & (4) & (5) & (6) & (7) \\
  ID & $\log M_h$ & All & Cluster & Filament & Sheet & Void }

\startdata
  1 & 10.20  &   0.799 $\pm$  0.063  &   0.897 $\pm$  0.054  &   0.753 $\pm$  0.127  &   0.829 $\pm$  0.081  &   1.171 $\pm$  0.041 \\
  2 & 10.70  &   0.822 $\pm$  0.084  &   0.633 $\pm$  0.049  &   0.691 $\pm$  0.060  &   0.867 $\pm$  0.046  &   1.456 $\pm$  0.097 \\
  3 & 11.20  &   0.672 $\pm$  0.049  &   0.438 $\pm$  0.054  &   0.802 $\pm$  0.123  &   1.194 $\pm$  0.082  &   2.165 $\pm$  0.057 \\
  4 & 11.70  &   0.785 $\pm$  0.070  &   0.272 $\pm$  0.090  &   0.836 $\pm$  0.090  &   1.624 $\pm$  0.058  &   3.116 $\pm$  0.274 \\
  5 & 12.20  &   0.845 $\pm$  0.036  &   0.159 $\pm$  0.092  &   1.077 $\pm$  0.098  &   2.387 $\pm$  0.056  &   4.451 $\pm$  0.801 \\
  6 & 12.70  &   1.112 $\pm$  0.048  &   0.369 $\pm$  0.043  &   1.663 $\pm$  0.115  &   3.487 $\pm$  0.171  & -- \\
  7 & 13.20  &   1.248 $\pm$  0.075  &   0.896 $\pm$  0.066  &   2.459 $\pm$  0.156  &   4.692 $\pm$  0.703  & -- \\
  8 & 13.70  &   1.695 $\pm$  0.056  &   1.502 $\pm$  0.051  &   3.645 $\pm$  0.121  & --  & -- \\
  9 & 14.20  &   2.711 $\pm$  0.098  &   2.716 $\pm$  0.106  & --  & --  & -- \\
 \cline{1-7}\\
10 & 10.20  &   0.697 $\pm$  0.050  &   0.902 $\pm$  0.020  &   0.701 $\pm$  0.032  &   0.751 $\pm$  0.025  &   1.080 $\pm$  0.054 \\
 11 & 10.70  &   0.703 $\pm$  0.055  &   0.646 $\pm$  0.039  &   0.727 $\pm$  0.040  &   0.935 $\pm$  0.031  &   1.515 $\pm$  0.022 \\
 12 & 11.20  &   0.770 $\pm$  0.069  &   0.432 $\pm$  0.018  &   0.726 $\pm$  0.043  &   1.144 $\pm$  0.034  &   2.057 $\pm$  0.209 \\
 13 & 11.70  &   0.765 $\pm$  0.016  &   0.291 $\pm$  0.052  &   0.875 $\pm$  0.022  &   1.595 $\pm$  0.084  &   3.514 $\pm$  0.387 \\
 14 & 12.20  &   0.831 $\pm$  0.045  &   0.324 $\pm$  0.044  &   1.104 $\pm$  0.038  &   2.316 $\pm$  0.200  & -- \\
 15 & 12.70  &   1.035 $\pm$  0.039  &   0.522 $\pm$  0.049  &   1.642 $\pm$  0.076  &   3.416 $\pm$  0.367  & -- \\
 16 & 13.20  &   1.286 $\pm$  0.052  &   0.953 $\pm$  0.066  &   2.448 $\pm$  0.080  & --  & -- \\
 17 & 13.70  &   1.621 $\pm$  0.090  &   1.465 $\pm$  0.087  &   3.647 $\pm$  0.764  & --  & -- \\
 18 & 14.20  &   2.618 $\pm$  0.126  &   2.633 $\pm$  0.105  & --  & --   & --
\enddata

\tablecomments{Column (1): ID. Results listed in rows 1-9 are obtained
  from CCFs, 10-18 are obtained from ACFs.  Column (2): logarithm of
  the halo mass. Column (3): average biases of halos of overall
  population. Columns (4)-(7): average biases of halos in the cluster,
  filament, sheet and void environments, respectively. } \label{tab:bias}
\end{deluxetable*}

\subsection{Halo auto correlations}
\label{sec:acf}

The clustering strengths of large scale CCFs in different cosmic web
environments obviously contradict our naive expectation that halos in
voids should be less clustered. To test the robustness of
these findings, we proceed to calculate the halo ACFs.

Similar to the CCFs, we first measure the ACFs of halos that are
separated into nine samples in different mass ranges:
$10.0\le \log M_h <10.5$, $10.5\le \log M_h <11.0$, ...
$14.0\le \log M_h$. The open squares shown in Fig. \ref{fig:ACF1} are
the ACFs we measured from these halos. The error bars are once again
obtained from 200 bootstrap re-samplings of the dark matter halos. We
also show, for comparison, the ACF of dark matter particles as solid
line, and the biased ACF as dotted one. The later is obtained by
multiplying the unbiased ACF by the square of the median bias factor
of those halos in consideration.  Similarly to the CCFs, we find that
the ACFs of halos are quite consistent with the biased ACFs of dark
matter particles on large scales.  The small scale ACFs cut off is
especially apparent for massive halos. These are caused by the
halo-halo exclusion effect as modeled in \citet{Wang2004}.  Overall,
the ACFs in different mass bins behave as expected.

Next, we proceed to measure the ACFs for halos in different cosmic web
environments. Shown in each panel of Fig. \ref{fig:ACF2} are the ACFs
for halos in different cosmic web environments: clusters, filaments,
sheets and voids.  These ACFs show quite different behaviors compared
to the overall sample. This further indicates that a significant
cosmic web environment dependence exists. On small to intermediate
scales, the clustering properties of ACFs are different from CCFs,
especially for the halos in the voids where they show
overall stronger clusterings.  Nevertheless, the clustering behaviors
on these scales are not the main focus of this probe.  The most
exciting feature is that, on scales $\ga 15\>h^{-1}{\rm {Mpc}}$, the halos show the
same cosmic web environment dependence as the CCFs, where strongest
clustering strength is revealed in the ACFs of void halos.

The cosmic web dependence of the clustering strengths found here is
opposite to that obtained by \citet{Fisher2016}, who claimed that halo
bias monotonically increases with cosmic web environments from voids
to clusters.  Although it is unclear to us what is the main cause of
such a discrepancy, one possibility is that they used the velocity
shear tensor to classify halos into different cosmic web types.
Nevertheless, in a very recent study using a Fourier analysis method,
\citet{Paranjape2017} found the same trends of halo biases as ours:
the halos in filaments have significantly larger biases than those in
clusters.  Coming back to the strongest clustering strength of void
halos, one intuitive explanation is that the clustering of void halos
might be composed of the void-void correlation weighted by the void
occupation numbers.

\begin{figure*}
\center
\vspace{0.5cm}
\includegraphics[height=10.0cm,width=10.0cm,angle=0]{f8.eps}
\caption{Halo biases as a function of halo mass. Each panel refers to
  a different cosmic web environment. Halo biases calculated using the
  CCFs and ACFs of the overall population are shown with open circles
  and squares, respectively. The ones obtained from CCFs and ACFs of
  halo subsamples are displayed as solid circles and squares,
  respectively. For comparison, the model prediction of
  \citet{Tinker2010} is indicated by the solid line. }
\label{fig:bias1}
\end{figure*}

\begin{figure*}
\center
\vspace{0.5cm}
\includegraphics[height=10.0cm,width=10.0cm,angle=0]{f9.eps}
\caption{Cross correlation functions between halos in the clusters
   and the dark matter particles.  In each panel, the open
  squares and solid dots focuses on the 20\% oldest and 20\% youngest
  halos, respectively. For comparison, we also show using a solid line
  the results for overall population. }
\label{fig:ageCCF1}
\end{figure*}

\subsection{Cosmic web dependent  halo bias}

In order to quantify the overall clustering strengths of halos within
different cosmic web environments, we measure the average biases of
halos. These average biases are measured using the ratios between the
halo CCFs and the dark matter particles' ACFs within radii
$15<r<45\>h^{-1}{\rm {Mpc}}$ as shown in Fig. \ref{fig:CCF1}.  In all panels of
Fig. \ref{fig:bias1} and displayed with open circles are the average
biases thus measured for overall population as a function of halo
mass. The error bars indicate the variances of the CCF ratios (biases)
at different radii. Once again we use the halo ACFs to confirm those
measurements, and display as open squares the average square root
ratios between the ACFs of halos and dark matter particles within
radii $15<r<45\>h^{-1}{\rm {Mpc}}$. This second measurements of the average biases
obtained agree very well with those obtained from the CCFs.  For
completeness, we have added to the figure a solid line representing
theoretical model prediction by \citet{Tinker2010}. The average biases
of halos measured from the ELUCID simulation show an overall very nice
agreement with the model.

In addition to the generic features relevant to the overall population
we have just mentioned, each panel is used to distinguish a specific
cosmic web environment for which the halo bias measurements are
repeated. Environmental bias measurement made using the CCF are shown
as red filled circles.  While the ones made using the ACF are shown as
filled squares.  The average biases of halos in the clusters
(upper-left panel of Fig. \ref{fig:bias1}) agree with the overall
population on both massive and low mass end, but are significantly
suppressed for intermediate mass halos. The average biases of halos
with mass $\sim 10^{12.0}\>h^{-1}\rm M_\odot$ is almost by a factor of 3 lower than
the overall population.  Compared to those in clusters, halos in
filaments (upper-right panel) show significantly enhanced biases,
especially at the massive end with mass $\ga 10^{12.5}\>h^{-1}\rm M_\odot$.  Shown
in the lower-left and lower-right panels of Fig. \ref{fig:bias1} are
the average biases of halos in the sheets and the voids, respectively.
Again we see a clear trend that halos in the sheets and voids are ever
increasingly enhanced.  Overall, the clustering strength of halos
increases significantly from the clusters to the voids, with stronger
impact in more massive halos.  For instance, Milky Way sized halos
(mass $\sim 10^{12.0}\>h^{-1}\rm M_\odot$) in the voids have bias $\ga 3$, which is
even larger than the overall clustering strength of cluster sized
halos.

Finally, for reference, the related biases of halos in different
cosmic web environments are listed in Table \ref{tab:bias}.  Such a
strong cosmic web dependent halo bias may play important roles in
cosmological and galaxy formation probes. For instance,
\citet{Hamaus2014} proposed a method of using galaxy-void cross
correlation to constrain cosmologies, the very different clustering
behaviors of void halos found here must be properly taken into account
in such kind of studies.  On the other hand, as pointed out in ELUCID
III, the fractions of red galaxies as functions of the $r$-band
absolute magnitude depend very strongly on the cosmic web
environments. It would be very interesting to see if galaxies in
different cosmic web environments have different galaxy-halo
connections. For this purpose, the very different halo biases in
different cosmic web environments have to be taken into account in
establishing the galaxy-halo connections using the HOD or CLF models.

\begin{figure*}
\center
\vspace{0.5cm}
\includegraphics[height=10.0cm,width=10.0cm,angle=0]{f10.eps}
\caption{Similar to Fig. \ref{fig:ageCCF1}, but for halos in the
  filaments. }
\label{fig:ageCCF2}
\end{figure*}

\begin{figure*}
\center
\vspace{0.5cm}
\includegraphics[height=10.0cm,width=10.0cm,angle=0]{f11.eps}
\caption{Similar to Fig. \ref{fig:ageCCF1}, but  for halos in the
  sheets. }
\label{fig:ageCCF3}
\end{figure*}

\begin{figure*}
\center
\vspace{0.5cm}
\includegraphics[height=7.0cm,width=10.0cm,angle=0]{f12.eps}
\caption{Similar to Fig. \ref{fig:ageCCF1}, but  for halos in the
  voids. }
\label{fig:ageCCF4}
\end{figure*}

\begin{figure*}
\center
\vspace{0.5cm}
\includegraphics[height=10.0cm,width=10.0cm,angle=0]{f13.eps}
\caption{Halo biases as a function of halo mass. Each panel represent
  a different cosmic web environment. Halo biases are computed using
  the CCF from all halos (filled black circle), the 20\% oldest
  (filled red squares) and the 20\% youngest (open blue squares)
  halos.  For comparison, we also show the model prediction of
  \citet{Tinker2010} using a solid line.  }
\label{fig:agebias}
\end{figure*}

\begin{figure*}
\center
\vspace{0.5cm}
\includegraphics[height=10.0cm,width=10.0cm,angle=0]{f14.eps}
\caption{Similar to Fig. \ref{fig:agebias}, but here for halos in
    the controlled samples. The results shown in the lower-right panel
    for void halos are the same as those in Fig. \ref{fig:agebias}. Halo
    biases computed in other panels for the 20\% oldest (filled red
    squares) and the 20\% youngest (open blue squares) are obtained
    from the controlled samples. }
\label{fig:agebias2}
\end{figure*}

\section{Assembly bias of halos in different cosmic web
  environments}
\label{sec_age}

In recent years, great effort has been made to quantify the assembly
bias of halos, among which the most notable one is the age dependence.
Having quantified the cosmic web environment dependence of halo
biases, we come to the second purpose of this work: to investigate
whether or not the age dependent biases of halos can be explained
using the cosmic web environment dependent halo biases.  More
precisely we try to confirm the presence or absent of prominent age
dependent biases for halos in different cosmic web environments.  To
this end, we separate halos in the two tails of the formation redshift
distribution, building 2 sets of halo sub-subsamples representing the
20\% oldest and 20\% youngest ones and measure separately their
clustering properties.

We first measure the CCFs of halos in the clusters. The open squares
and solid dots in Fig. \ref{fig:ageCCF1} indicate the resulting CCFs
for the oldest (high z) and youngest (low z) halos. For halos with
mass $\la 10^{12.5}\>h^{-1}\rm M_\odot$, the clustering strengths of the two
sub-subsamples are quite different, the oldest sub-subsample having
much stronger clustering strength than the youngest
sub-subsample. However, for more massive halos, the two CCFs are quite
consistent with one another indicating a lack of assembly bias. As the
assembly bias features found in \citet{Gao2005} are prominent within
mass range $\la 10^{13.5}\>h^{-1}\rm M_\odot$, or
$\la 10^{13.0} \sim 10^{13.5} \>h^{-1}\rm M_\odot$ for different definitions of
formation time \citep[see, e.g.][]{Li2008}, the assembly bias feature
found here is at least limited to a smaller mass range.

Next, we focus on the filaments, where the results are
shown in Fig. \ref{fig:ageCCF2} following the same legend as
Fig. \ref{fig:ageCCF1}. Compared to halos in the clusters,
the assembly bias features differ in two aspects: (1) the overall
strength decreases and (2) the reduction is more significant in more
massive halos.

Finally in Figs. \ref{fig:ageCCF3} and \ref{fig:ageCCF4}, we show the
halo CCFs respectively in the sheets and the voids. Compared to the
clusters and the filaments, assembly bias features are further reduced
in the sheets, especially in terms of amplitude. In the void
environment, halo assembly bias features are no longer apparent, with
the oldest and youngest halos overlapping with the overall void halo
population.

In order to quantify the assembly biases for halos in different cosmic
web environments, we use once again the ratios of the halo CCFs shown
in Figs. \ref{fig:ageCCF1} - \ref{fig:ageCCF4} and the dark matter
ACFs within radii $15<r<45\>h^{-1}{\rm {Mpc}}$.  The average bias measurements are
displayed as a function of mass in Fig. \ref{fig:agebias}, with each
panel corresponding to a specific environment. In each panel, the
biases for overall population, oldest 20\% and youngest 20\% halos are
shown using solid dots, solid squares and open squares, respectively.
The error bars again are obtained using the variances of the CCF
ratios (biases) at different radii.  For the cluster environment in
the upper-left panel, the assembly biases is clearly apparent with the
oldest and youngest halos results being located respectively above and
below the overall cluster population.  The assembly bias of halos in
clusters is found here to be of similar amplitude to the one measured
by \citet{Gao2005}. However it appears in our case in less massive halos
with mass $\la 10^{12.5}\>h^{-1}\rm M_\odot$. As we explore the filament
environment (upper-right panel) we notice a reduction in the amplitude
of the assembly biases. The reduction is even more pronounced in the
sheets (lower-left panel) and the assembly bias entirely absents in
the voids (lower right panel).

Note however, as the halos in different environments have different
age distributions (see Fig. \ref{fig:age}), we carry out an additional
test to check if the reduction of assembly bias, especially that in
voids, is really due to the fixed environment.  Here we take the halos
in the voids as the reference sample and select a set of controlled
halo samples from other environments that match the same mass and
formation time distributions. Following the same procedures we carried
out for the reference sample in voids, we measure the biases of the
oldest 20\% and youngest 20\% halos in the controlled samples in
clusters, filaments, and sheets, respectively. Thus obtained results
are shown in Fig. \ref{fig:agebias2}.  Here only halos with mass
$\le 10^{12.5}\>h^{-1}\rm M_\odot$ are used for our investigation. Compare to the
original halos shown in Fig. \ref{fig:agebias}, the ones in the
controlled samples show very similar, although somewhat less
prominent, assembly bias features.  These features indicate that the
reduction of assembly bias from clusters, filaments to sheets and
voids is real.

Although the results are not displayed in the paper, the measurements
using the ACF alternatives (as in Fig. \ref{fig:bias1}) were performed
and found to give very similar results.

\section{Summary}
\label{sec_conclusion}

In this paper, we have probed the clustering properties of halos in
different cosmic web environments using the ELUCID simulation. Halos
were separated into four cosmic web environments defined through the
Hessian matrix of the smoothed density field.  Out of a total of
$48,129,323$ halos in the ELUCID simulation, $19.8\%$ are located in
cluster, $57.0\%$ in filaments, $22.1\%$ in sheets and $1.1\%$ in
voids.  In order to probe the related mass dependence of the
clustering properties, we also separated the halos into nine halo mass
bins, $10.0\le \log M_h <10.5$, ..., $13.5\le \log M_h <14.0$ and
$14.0\le \log M_h$.  Furthermore, so as to confirm existing age
dependent assembly biases in different cosmic web environments,
additional subsamples were made based on the formation redshift
focussing on the 20\% oldest and 20\% youngest halos.

We have measured the cross correlation functions between halos and
dark matter particles, as well as the related auto correlation
functions of halos in these subsamples. The ratios between the halo
CCFs (or ACFs) and the dark matter ACFs within radii $15<r<45\>h^{-1}{\rm {Mpc}}$
are used to estimate the average biases of halos. We find
significantly different biases for halos of {\it same} masses but in
different cosmic web environments. We summarize our main results as
follows;
\begin{itemize}
\item The average biases of halos in  {\it clusters} agree with the
  overall population on both high and low mass ends, but are
  significantly {\it suppressed} in intermediate mass scales. The
  average biases of halos with mass $\sim 10^{12.0}\>h^{-1}\rm M_\odot$ are almost
  by a factor of 3 lower than the overall population.
\item The halos in  {\it filaments} show significantly enhanced
  biases, especially at the massive end with mass
  $\ga 10^{12.5}\>h^{-1}\rm M_\odot$ .
\item Halos in  {\it sheets} show stronger enhanced biases as a
  function of halo mass.
\item Halos in   {\it voids} show the strongest bias
  enhancements. The Milky Way sized halos with mass
  $\sim 10^{12.0}\>h^{-1}\rm M_\odot$ in void region have bias $\ga 3$, which is
  even larger than the overall clustering strength of cluster sized
  halos.
\item The strength of the assembly biases (age dependences)
    decreases from cluster, filament and sheet environments to finally
    disappears in void environment.
\item In addition, the age dependent assembly biases of halos in
    different cosmic web environments exist in a smaller mass range
    $\la 10^{12.5}\>h^{-1}\rm M_\odot$, compared to the overall population at
    $\la 10^{13.0}\sim 10^{13.5}\>h^{-1}\rm M_\odot$.
\end{itemize}

As we have found very prominent -- as strong as the mass dependence --
cosmic web environment dependence of halo biases, a similar study
focussed on galaxy clustering in different cosmic web environments
would be relevant. It would indeed be interesting to obtain the
galaxy-halo connections in different cosmic web environments, which
can be used to better constrain galaxy formation models and better
understand the void-galaxy clustering properties for cosmological
studies, etc.

\section*{Acknowledgments}

We thank the anonymous referee for helpful comments that greatly
improved the presentation of this paper.  This work is supported by
the 973 Program (No. 2015CB857002), the national science foundation of
China (grant Nos. 11233005, 11621303, 11522324, 11421303) and a grant
from Science and Technology Commission of Shanghai Municipality
(Grants No. 16DZ2260200).  We also thank the support of the Key
Laboratory for Particle Physics, Astrophysics and Cosmology, Ministry
of Education, and Shanghai Key Laboratory for Particle Physics and
Cosmology (SKLPPC)

We acknowledge the computing facility (High Performance Computing
Center) at Shanghai Jiao Tong University for providing access to the
PI cluster on which the ELUCID simulation was run. This work is also
supported by the High Performance Computing Resource in the Core
Facility for Advanced Research Computing at Shanghai Astronomical
Observatory.

redpajama_set_name: RedPajamaArXiv


This month, the entire Riddle Village community is excited to celebrate our 25th anniversary. In October of 1993, we opened our doors to our first residents and have continued to grow and welcome more people into our community. Over the years, we have added new buildings, amenities, dining options and much more. We have grown from a community of 78 residents to over 400. To commemorate our anniversary, we would like to take a look back at the journey Riddle Village has gone on over the many years.
In 1993, Riddle Village consisted of three apartment buildings along with our commons building. Williamsburg, Arlington, and Jamestown were the initial buildings that opened. Two years later, the Monticello house opened with 38 personal care units and 60 skilled nursing beds. Our last residential building built, Hampton, was added to provide more independent residence apartments in 1998. The last community expansion was in 2008 when the Monticello House added 11 personal care units and 26 skilled nursing beds.
Changes have not just occurred in the sizing of our community. Inside our walls, we have worked continuously over the years to ensure that our residents are getting top quality services and amenities. In addition to the three dining venues Riddle Village had when we first opened, we have added the Thoroughbred Lounge which features delicious cocktails, appetizers and an outdoor patio for residents to enjoy the courtyard as they dine. The courtyard has been renovated and now includes a bocce ball court and a relaxing fire pit, in addition to the putting green and shuffleboard court.
The fitness center was expanded to include state-of-the-art equipment and is opened 24/7. The wellness center was redesigned to feature additional physician suites for our residents' convenience and the hours of the wellness nurse have been extended to better accommodate our community. All this and more has been redesigned, renovated and/or expanded to continue to ensure we remain strong competitor amongst other communities and offer our residents the amenities and services they deserve.
We are always enhancing our community to make sure residents are living in luxury and comfort. Recently, we started the process of updating the hallways in every building with new lighting, carpeting, and furniture. This fall, dining renovations officially began in the Governour's Inne, with the Chesapeake Room and the restaurant lobby to follow shortly after. Construction is underway to update these venues with new color themes, flooring, and a completely restructured layout. These changes will bring a modern twist to the traditional dining experience that our residents enjoy every day.
After 25 years, Riddle Village Retirement Community has gone through plenty of changes. From physical transformations to more options for our residents, our dedicated staff is always working hard to make sure we are providing the highest quality independent retirement lifestyle. While appearances may change, one thing that has always stayed the same is the friendly atmosphere that everyone experiences when they walk in our doors. Whether you are a resident, employee, or guest, friendly smiles and warm conversation are sure to find you throughout Riddle Village. Contact our team or give us a call at 610-891-3700 to learn more about our retirement community and lifestyle.


Below you will be able to find the answer to "The Simpsons" saloon crossword clue which was last seen on Thomas Joseph Crossword, July 7 2018. Our site contains over 2.8 million crossword clues in which you can find whatever clue you are looking for. Since you landed on this page then you would like to know the answer to... Moe Szyslak /ˈsɪzlæk/ is a fictional character from the American animated television series The Simpsons. He is voiced by Hank Azaria and first appeared in the series premiere episode "Simpsons Roasting on an Open Fire". Moe is the proprietor and bartender of Moe's Tavern, a Springfield bar frequented by Homer Simpson, Barney Gumble, Carl Carlson, Lenny Leonard, Sam, Larry, and others.
In our website you will find the solution for Kodos' alien cohort on "The Simpsons" crossword clue. Thank you all for choosing our website in finding all the solutions for La Times Daily Crossword.... Here you may find the possible answers for: Neighbor of Homer on The Simpsons crossword clue. This clue was last seen on New York Times Crossword January 7 2019 Answers.
Below you will be able to find the answer to "The Simpsons" saloon crossword clue which was last seen on Thomas Joseph Crossword, July 7 2018. Our site contains over 2.8 million crossword clues in which you can find whatever clue you are looking for. Since you landed on this page then you would like to know the answer to... The Simpsons Clue, or The Simpsons Cluedo as it is known in the UK, is a Simpsonfied version of the mystery game Cluedo, which has been produced in two versions since its release in 2000, the first of which was packaged in two different boxes, the second being available in 2003.
Simpsons Clue Board Game Rules Nevertheless, here's your chance to don a detective's hat and catch the murderer! Buzzle, in this article, will tell you about the Clue Board Game, its rules.
In our website you will find the solution for Kodos' alien cohort on "The Simpsons" crossword clue. Thank you all for choosing our website in finding all the solutions for La Times Daily Crossword.


Did you know Rowdy bars are Paleo-friendly? While we don't consider ourselves a Paleo brand, here at Rowdy Prebiotic Foods we want to support health nuts of all sorts. Whether you're a low GI aficionado, a veg-head, or a Paleo patron, we want to create snacks that fill you up and make you smile. This week we're taking a closer look at the benefits of the Paleo diet and how Rowdy Bars qualify as a Paleo snack bars.
Paleo is time tested – The Paleo diet champions eating from an evolutionary perspective. We've been eating as hunter/gatherers for thousands of years. It was only in recent decades that we began to see diet related health problems like obesity, diabetes and heart disease. Paleo doesn't allow most foods that contribute to these health problems.
You eat mean and clean – The Paleo diet is all about eating more like a human, and getting rid of all that toxic junk food.
It's satisfying - Paleo diets are packed with anti-inflammatory, nutrient dense foods that fill you up, so you can get the most out of every day.
What Makes Rowdy Bars Paleo-Friendly?
Usually snack bars are forbidden in a Paleo diet, but Rowdy bars makes the cut! Because our bars are dairy free, honey free, and grain free, Paleo dieters can count Rowdy as a reliable source of Paleo-approved snacks.
Cashews give our bars that buttery, nutty taste and are loaded with minerals like manganese, magnesium and copper.
Coconut, which is one of the most versatile ingredients in the Paleo diet, provides our snack bars with a creamy texture and healthy fats.
Yacon syrup is derived from the Paleo-approved Yacon root and adds both fiber and a low GI sweetener to our bars.
Egg white protein is our main source of protein in our bars and, because it is lactose-free, is totally Paleo-approved!
Dark chocolate is approved in moderation in the Paleo diet because of the nutritional benefits in cacao.
Creating tasty, nutrient dense snacks is what we do best. Whether you're an advocate for Paleo or a different type of health nut, Rowdy Bars thanks you for loving life and filling up on the good stuff. Stay Rowdy!


Problems with private clouds come from users, not technology | Faction Inc.
As the private cloud becomes more popular there is a greater likelihood that companies or individuals that don't understand it will try to use it. This isn't necessarily a problem for those that know what they're doing with the cloud, but it can blur the numbers on cloud approval rates. Unfortunately, there's nothing in the world that works without people understanding what they're trying to do with it. Companies that want to adopt the cloud need a game plan for how their implementation will change their business. In the end, it is those groups that decide to move to the cloud out of necessity, growth potential or unique opportunities will succeed.
Gartner's recent survey asking people what was wrong with their cloud yielded an insight into why people's clouds aren't satisfying them. The clear majority had a problem with changing the operational model of their work with regard to the cloud. In this instance it isn't the cloud itself that is failing the organization. Instead, it's the group's inability to deal with the new way they should work with the cloud in order to realize its benefits. The private cloud allows organizations a large amount of agility. It lets employees and administrators communicate and collaborate more effectively. This means that groups are able to pick up and drop projects quickly, eliminating a lot of wasted time and overhead. However, this can only happen if the company is ready to make these kinds of changes. Those that are stuck in older management styles will find themselves unable to benefit from this change.
In effect, the cloud can be a litmus test for the efficiency of a company's management processes. Those that have agile administration and are effective at discarding old projects while continually realigning the actions of the company towards its vision will find the cloud useful. Part of the problem may be that many who are moving to the cloud are doing so without expert advice, noted Barb Darrow if Gigaom in reaction to the study. A lack of expertise could definitely hinder movement to the private cloud. Due to the inherent complexity of setting up a private cloud and the amount of ways it can be used by a company, partnering with a premium cloud vendor is a good idea. Cloud providers that have expert staff on call to support companies as they move to the cloud are better able to help their clients make sure their new system works for them.
The issue, then, isn't with the cloud itself, but the expertise involved in setting it up and utilizing it. Organizations that are moving to the cloud should be sure everyone is on the same page. A company should be sure of how and why it wants to use the private cloud. moving forward onto a platform without understanding it cloud potentially lead a group into trouble as they struggle to figure out a reason for having it. Thankfully, the private cloud lends itself toward many different opportunities. Taking advantage of mobile computing, allowing for instants spin-ups and spin-downs of private servers to test software, and similar use cases make the private cloud compelling to many organizations. It just that those who are going to use it should know why first. Once that is established, it is easier to train employees on cloud use, and to integrate it into the common workflow of the company. It is this kind of measured approach that will allow people the best use of the benefits of cloud computing.


I consider eating 50% of any trip. I like local budget places as well as fine dining break the budget places.
Here is a mix of restaurants on the Big Island that I would return to. Some of these were recommended by Elanaloo's Big Island Guide and some we happened upon. Every one of Elanoaloo's recommendations was excellent and we didn't put a dent in her list. So many more to try!
I have to give a shout out to Hula Hulas in our hotel in Hilo. They are farm to table and crank out three squares a day. We ate there several times throughout our week in Hilo and didn't have a bad meal.
Pineapple Chili Glazed Pork Belly (above), Ti Leaf Wrapped Sunfish (below) The Sunfish was so good I had it twice during our stay.
A really fun place was Moon and Turtle in downtown Hilo. They don't have online reservations but having to make a phone call was worth it. That is saying a lot for me! I don't understand that in 2018 why any restaurant that requires reservations would refuse to join an online service. If Elanaloo hadn't recommended it so highly I probably would have skipped it.
We loved everything abut this place. It's really small and it has a cool vibe but not hipster-snobby kind of vibe.
The cocktails were inventive and some of the best we had our two weeks on the island.
Our food wasn't very photogenic but it was delicious!
Pineapples is a casual place in downtown Hilo. It was packed so we grabbed two seats at the bar.
I still dream about the Hurricane Furikake Shrimp! I would fly back just to eat those!
The Hilo Bay Cafe is more of a fine-dining establishment within walking distance from our hotel in Hilo.
The stand out here was the surf & turf bowl and the carpaccio. They also have sushi.
During one of our big drives around the island, we ended up in Waimea and Big Island Brewhaus.
This is a really fun Mexican place that has great margaritas and craft beer. If you are a beer lover this is the place for you! It was my husband's favorite. You will see thier beers in many other resturants around the island.
Besides the beer and tacos, you've got to try the fish bites.
Back to fancy, we hit up Jackie Rey's Ohana Grill in downtown Hilo. It definitely has a steakhouse feel. One thing that is hard to find on any Hawaiian island is a good martini. If you are looking for one on the Big Island, this is where you need to go!
Fresh catch and the special of the night.
Finally moving over to the Kona side of the island. We started out pretty poorly at our new digs at a fancy resort. I'll talk more about that later in another post. For now, let's just say we were in need of some comfort. We were pretty down from our dealings with the fancy-pants people and needed uplifting. We had no idea how much The Blue Room would make everything better!
It's family owned and the whole family was there including grandparents and kids. We felt so welcomed and well taken care of it almost brought tears to my eyes. I have no pictures of the food. We were too busy visiting with wonderful people! Our waiter was a riot! He was comedian Stephen Wright in appearance and personality. It was just what we needed!
Oh, and the food was awesome.
We ate a lot of our meals on this side of the island at the resort and it was all good. I'll write more about our resort in my post "When Your Vacation Goes Wrong".
Our last meal before we had to head back to the cold was at Rebel Kitchen.
The Cuban Rolls are the appitizer to try but they were out. We got the Chicken Fajita Wontons and I would only recommned those to those who LOVE garlic. They were a bit heavy for me.
The burgers were awesome! We had the Rebel and a fish sandwich. They also had kombucha on tap.
Just FYI - they don't have a bathroom. You have to get a key an walk up the hill. Just something to keep in mind.


text:
Koji Nakano
Chief Executive Officer & Co-Founder
Hired by TOTO LTD., Koji Nakano was assigned to be Sales and Marketing Supervisor at TOTO USA Inc. and worked for some companies in North and Central America including ones in New York City and Atlanta Headquarters. With his experience as the Manager of International Operations, he became CEO of TOTO Europe GmbH. In 2014 Nakano left the company and established OQTA.
Kiyohisa Takahashi
Chief Philosophy Officer & Co-Founder
Kiyohisa Takahashi graduated from Nihon University College of Art with a bachelor's degree in cinema studies. At the age of 29, he founded a firm which edited live broadcast of sports. At the same time, he majored in media studies at the Graduate School of Waseda University and was awarded a Waseda Student Culture Award. Takahashi joined OQTA in 2015.
Masaru Yamamoto
Chief Software Creator
Masaru Yamamoto graduated from Nihon University with a major in industrial technology. After working for an independent software company, he was assigned to be the Director of Now Village Ltd. His work ranged from development and introduction to management of the construction of web system. He joined OQTA in 2015.
Makoto Kawakami
Makoto Kawakami joined in the construction of MARS 305 provided by JR Group. After that, he worked as a co-founder of Mint Co., Ltd. and Now Village Ltd., and then, he became a board member of the companies. Whether it is a language or a platform, he has a perfect command of computer languages as if they were his native tongues. He joined OQTA in 2015.
Kotobuki Naka
General Manager & Market Development
After she served as a manager of several beauty salons, Naka became a senior leader at a subsidiary of Lawson Group called Best Practice, Inc., where she served as a researcher and analysist. She studied design in general and planning at Tokyo Designplex Institute. She joined OQTA in 2015.
Motoe Haller
Motoe Haller holds a doctor's degree in international development from Nagoya University. She was responsible for marketing and branding strategy and PR when she was working at Dentsu Research Inc., TOTO USA Inc., and InSpec Group. Haller is currently responsible for establishing a US headquarters of OQTA.Inc.
Yoshihiro Suwa
After graduating from Kyoto University with a major in law, Yoshihiro Suwa joined Roland Berger Ltd. and served as a consultant in Japan and Europe. He has worked in strategies of growth, overseas business, marketing, and market penetration (especially to developing companies) for a wide variety of clients. He is currently residing in Jakarta.
Keita Mitsuhashi
Creative Director Design & Technology
Keita Mitsuhashi is currently enrolled in the University of Tokyo, where he majors in engineering. Given business fund by Recruit Holdings Co., Ltd., he built a mobile application called "dood" as a director and engineer. After that, with his experiences of serving as an engineer and digital creator for several companies, he founded Queue Inc. He joined OQTA in 2016.
Naoto Shibata
Naoto Shibata is currently enrolled in the University of Tokyo with a major in engineering, where his study is focused on biorobotics and machine learning. He served as a collaborative researcher in Yutaka Matsuo's laboratory at the University of Tokyo, where he conducted a study on predictive models of Facebook advertisement conversions. After serving as an engineer and data scientist for several companies including building "dood" with Mitsuhashi as an engineer, he founded Queue Inc. He joined OQTA in 2016.
Ren Tsukamoto
After graduating from the technical college, Ren Tsukamoto joined Hitachi, Ltd.
After retiring, He entered the University of Tokyo.
Entrepreneurship in Asian countries while studying abroad.
After that, also advanced to the Middle East · Balkans.
Also, as a social activity, public utility companies are also conducting public utilities business. He joined OQTA in 2016.
OQTA, Inc.
BellMaison 1F, 1-14-7, MinamiAoyama, Minato-ku, Tokyo 107-0062 Japan
37,900,000 yen
April,2015 Established START360.inc.
September, 2015 Moved a head office to Yoyogi.
December, 2015 Released AR santa (for iOS & Android).
July, 2016 Registered a US subsidiary of OQTA Inc. in the State of Delaware.
July, 2016 Succeeded in developing a prototype of OQTA.
August, 2016 Applied for an international patent under PCT. Reference number: 5334-4021
September, 2016 Released HANABEE (for iOS & Android).
September, 2016 Changed the company name into OQTA, Inc.
October, 2016 Launched NepalProject
December, 2016 Applied for a trademark and logo
© 2022 OQTA, Inc.


text:
Mecklenburg County, NCBoard of ElectionsAbout our Board
Information on Elections
Candidate Finance Reports
Campaign Signs and Violations
About our BoardCurrently selected
How do I receive a voter card?
How do I change my party?
How do I update my address?
Mecklenburg County Board of Elections
741 Kenilworth Ave.
Hours: Hours: Mon-Fri 8 a.m. - 5 p.m.
Work and Performance Plan
Our office is responsible for conducting all elections held in Mecklenburg County. Locally, we administer State election laws. Our principal functions include establishing election precincts and voting sites, appointing and training precinct officials, preparing and distributing ballots, voting equipment, canvassing and certifying the ballots cast in elections, and investigating any voting irregularities. We maintain voter registration for Mecklenburg County and provide public information on voters and elections.
Each County in North Carolina has a Board of Elections. It is a five person board - four (4) which are appointed every two years by the State Board of Elections and one (1) the Chair by the Governor. North Carolina General Statute 163-30 states "The State chairman of each political party shall have the right to recommend to the State Board of Elections three registered voters in each county for appointment to the board of elections for that county. If such recommendations are received by the Board 15 or more days before the last Tuesday in June 1985, and each two years thereafter, it shall be the duty of the State Board of Elections to appoint the county boards from the names thus recommended." The local political parties will submit three names to the State political party chairman. Once appointed, County Board members take an oath and begin their two year terms Tuesday following the third Monday in July in odd-numbered years. No more than two members of the County Board of Elections shall belong to the same political party. The Board oversees the functions of our offices and hires a Director to administer all duties.
Carol Hill Williams (Democrat), Chair
Elizabeth M. McDowell (Republican), Secretary
Beverly Earle (Democrat), Member
John Gresham (Democrat), Member
Mary Potter Summa (Republican), Member
Michael G. Dickerson, Director of Elections
Minutes will be posted once approved.
The next Board meeting will be held February 13, 2023 at 5:15pm.
February 13, 2023 Board Meeting Minutes
January 10, 2023 Board Meeting Minutes
December 13, 2022 Board Meeting Minutes
November 8, 2022 Board Meeting Minutes
October 4, 2022 Board Meeting Minutes
September 20, 2022 Board Meeting Minutes
August 5, 2022 Board Meeting Minutes
July 26, 2022 Board Meeting Minutes
June 6, 2022 Board Meeting Minutes
May 27, 2022 Board Meeting Minutes
May 3, 2022 Board Meeting Minutes
April 26, 2022 Board Meeting Minutes


The United States and Russia will begin talks Thursday morning aimed at calming tensions between their opposing military operations in Syria, two senior defense officials told NBC News.
The "very high-level" discussions will begin at 11 a.m. ET, one official said.
Russia defended its latest round of airstrikes in Syria amid mounting questions over their targets, insisting that Moscow's planes had struck ISIS installations.
U.S. officials have questioned whether Vladimir Putin's airstrikes — in the name of defeating ISIS — were genuinely targeting the group or were instead a cover to shore up Syrian President Bashar Assad by bombing anti-government rebel groups.
It also has raised fears over how the Cold War rivals can safely share airspace as they run separate anti-ISIS campaigns and hiked tensions.
Assad is the Kremlin's key ally in the Middle East and Russia maintains a naval facility in the country.
While Russia's defense ministry said its warplanes were conducting "surgical strikes" on ISIS' military equipment, communication hubs and fuel depots, Secretary of Defense Ash Carter said the bombardments didn't appear to be targeting areas held by ISIS forces.
Russia's defense ministry late Wednesday said it had carried out 20 airstrikes, according to The Associated Press. By comparison, the U.S. conducted one airstrike over Syria the same day.
Moscow's warplanes hit four more ISIS targets in Syria overnight, according to a statement Thursday from the Ministry of Defense.
It said the strikes destroyed a terrorist command center and ammunition depot in the Idlib area, a militant-command center in the vicinity of Hama and a facility near Homs producing explosives-rigged cars.
Meanwhile, Russia's ambassador to France said Thursday that targets a day earlier had hit installations for ISIS and the al Qaeda-linked Nusra Front, according to The Associated Press.
It reported that Alexandre Orlov dismissed allegations civilians were killed in the strikes, telling France Info radio that "there has been a certain war of disinformation for some time" and insisting Russia was "acting transparently."
The Russian jets have joined an already-crowded airspace over Syria: U.S. and allied planes have been flying sorties, as are Syrian regime jets.
The Russians gave less than an hour's notice that the bombings were about to begin, according to a U.S. defense official.
State Department spokesman John Kirby said Wednesday that a Russian official in Baghdad had requested American aircraft avoid Syrian airspace during Moscow's missions — but told reporters that the U.S. led coalition would continue to fly over Iraq and Syria "as planned."
The head of the Syrian opposition, Khaled Khoja, said the initial airstrikes killed civilians and that it was "very obvious" Russia didn't go into Syria with ISIS in mind.
"It is clear that the objective of the Russian occupation is to prolong the regime and to support the regime in the killing of innocent civilians," Khoja said Wednesday.
U.S. Rep. Ed Royce, Chairman of the House Foreign Affairs Committee, said "the Russians don't appear to be holding back in their efforts to shore up the murderous Assad regime."
Secretary of State John Kerry said the U.S. would have "grave concerns should Russia strike" areas where ISIS wasn't operating.
"Strikes of that kind would question Russia's real intentions fighting ISIL or protecting the Assad regime," he said, using another name for ISIS.
Courtney Kube and The Associated Press contributed.


It's one of my favorite times of the year at Disney's Grand Floridian Resort!
Every spring in the weeks preceding Easter, the Grand Floridian Bakery Team is given the opportunity to create some absolutely spectacular Easter Eggs for guests to enjoy. And the best part? The Eggs are made of CHOCOLATE. There are other ingredients involved, too, such as fondant, icing, and cocoa butter. But no matter what they are made of, they are all edible!
The Easter Eggs have been a Grand Floridian tradition for 19 years, but this is just the fourth year that the eggs have been on display for every guest who passes through the Grand Floridian lobby.
Something new this year… previously the Eggs were all displayed in one row directly at the lobby entrance. This year, the eggs are grouped in smaller displays in different areas around the lobby. Since some of the eggs are preserved from year to year (you may recognize some familiar ones from the 2014 Easter Egg display), the collection just keeps on growing!
The Easter Eggs are on display through April 10th. But in case Walt Disney World isn't part of your 2015 spring break plans, we wanted to bring the Eggs to you once again this year!
One of the centerpiece eggs for 2015 is an edible replica of Cinderella's Golden Coach.
The classic Disney animated version of Cinderella received a tribute as well.
In an echo of the fountain in the lobby of the Grand Floridian Disney Vacation Club Villas, the penguins from Mary Poppins have come out to play!
There are no shortage of Disney characters on display, including the entire Toy Story gang.
Peter Pan tops off this egg complete with a map of Neverland.
Never one to be outdone, Tinkerbell tops her own egg, too!
And what's a day at Disney World anymore without spotting this face 😉 ?
And the last thing I egg-spected to see (I know, sorry…) was a Great Mouse Detective egg! SO awesome!!
I think this Enchanted Rose egg representing Beauty and the Beast is simply gorgeous.
The Rapunzel eggs make their return this year.
And every side of this egg celebrates something near and dear to many of our hearts… Disney Dogs!
But again, the chefs are given free creative reign, so it's not only Disney characters and film moments represented. Some designs definitely convey a more traditional Easter feel.
The details on the painted eggs are so striking. The next three images are different sides of the same egg.
Not only are the colors on this Peacock egg beautiful, it's almost hard to remember that those feathers aren't real.
Once again, the team at the Grand Floridian has put on an impressive and beautiful display. We hope you enjoyed this tour, and wish you a very Happy Spring!!
Do you have a favorite egg in the display? Please let us know with a comment!
Disney World Grand Floridian Resort Easter Egg Photo Tour!
Wow!!! What amazing talents they have!
Really appreciate this post for those of us who simply can't be there.
And as for the Hercules egg – yaaaaaaaay! One of my favourite movies. An underrated gem getting the love it deserves!
I was thrilled to see the Great Mouse Detective Egg! It's always been one of my favorite Disney movies, and seeing it represented on Disney property in any form was so exciting! I always hold out hope that some of the lesser known but equally brilliant films will start to get more exposure in the parks.
Those elsa and rapunzel eggs are from last year! I thought they were supposed to use new eggs every year.
We were at The Grand Floridian last night to see these beautiful creations and they did NOT disappoint. I absolutely loved every single one of them. The attention to detail and beauty is absolutely stunning. My favorite was the traditional Easter theme with the golden hue and the amazing sugar flowers. You cleared up a mystery for me (it seems so obvious now). I wondered what the marble one was and never dreamed it was Rapunzel's hair!
You're also so right to say how nice it is to see some of the older unappreciated movies as well. Or themed like the Disney dogs. We toured the eggs, ooh-ahhing and taking pictures and then we enjoyed dinner at Trail's End and the Chip and Dale Campfire and movie. It was a wonderful Disney evening!!! Especially for us as we let our annual passes expire for a big UK trip this summer and we are missing our Spring Break week at WDW!!!
Follow my Disney photos at marionwdurham on IG.
Thank you for sharing again!! I loved seeing these pictures of the easter eggs last year and had hoped you would share pictures again this year.
When the display is done I really want to take a hammer crack some of them into pieces and nom nom nom nom nom!
I love the Cinderella eggs and I think the artwork on the first Rapunzel egg is excellent (or should that be eggcellent?). I also think the Toy Story characters are cute and the peacock is exquisite. Thanks for sharing them with us.
These are gorgeous…especially the Enchanted Rose one. Wish I could have been there to see them in person but thanks for sharing since I couldn't!
Wow thank you so much for sharing these fab photos. I never cease to be amazed by Disney only wish I could be there to see them. They are all my favourites!


The Educational Theatre Association is the leading association for theatre educators. We can connect you to thousands of theatre educators and professionals. Through our student honorary organization, the International Thespian Society, we can put you in touch with more than 200,000 high school and middle school students.
Whether through meeting our members in person at one of our national events, reaching them with specific messaging through one of our many advertising channels, or promoting brand recognition and appreciation through a sponsorship, EdTA wants to connect you with our members! For more detailed information, please visit our Media Kit.
Dramatics is the only magazine edited exclusively for students of theatre. The more than 50,000 students who read each issue are committed to excellence, evidenced by attaining membership in the International Thespian Society, a theatre honorary organization. Dramatics offers a high-quality editorial environment to advertisers who want to reach this accomplished group of prospective graduates.
For more information about advertising, please contact Ali Winters at awinters@schooltheatre.org.
Teaching Theatre is the journal published by the Educational Theatre Association for more than 5,000 middle and high school theatre educators, arts education outreach directors, and administrators. Every issue provides advertisers with direct exposure to a niche market of involved consumers and offers a cost-effective way to reach a specialized group of theatre professionals who are interested in your message and product.
EdTA offers several opportunities throughout the year to exhibit at events, affording personal interaction with highly engaged theatre students, educators, and teaching artists.
The International Thespian Festival is a week-long immersion in theatre arts attended by more than 4,200 high-achieving middle and high school drama students and their teachers.
The EdTA National Conference attracts approximately 400 theatre educators from across the country for state-of-the-art presentations by national thought leaders, workshops, and professional development intensives.
The EdTA Leadership Summit brings together the 150 decision-makers for the organization from the state and national levels for three days of strategic planning, briefings, and workshops focused on organizational best practices.
For more information about exhibiting, please contact Angel Wuellner at awuellner@schooltheatre.org.
EdTA offers our college and business partners the opportunity to be part of a robust event sponsorship program, demonstrating their commitment to EdTA and the International Thespian Society through a partnership with EdTA. EdTA works closely with these institutions to provide maximum exposure to our members and promotional opportunities for our sponsors.
For more information about sponsorships please contact Angel Wuellner at awuellner@schooltheatre.org.
EdTA offers an opportunity to advertise on the organization's website and member e-newsletter. Schooltheatre.org is the comprehensive website for the membership of EdTA and also provides information and resources for the larger theatre education community. It averages about 18,000 users and 163,000 page views per month. The News & Notes e-newsletter is distributed to approximately 5,400 adult members of EdTA on the 5th and 20th every month. Since its inception in 2015, the open rate has been steadily growing and is now averaging over 22%. The click-through rate is currently at 2.25%. And, most recently, the opt-out rate is zero. The contents include a variety of updates about association and related programs relevant to members' roles as theatre teachers, teaching artists, and leading industry professionals.
EdTA offers advertising in the 8.5 x 11, four-color program books that serve as the go-to resources during and after major annual events. The International Thespian Festival Program is a souvenir for many participants with detailed listings of participating schools and shows as well as descriptions of every workshop and its presenter. 7,500 copies are printed. The EdTA National Conference Program has detailed lists of every workshop and its presenter as well as material about the Conference's theme issue. 1,000 copies are printed.
Contact Angel Wuellner for any additional Marketing Opportunities information.


"Whether its in grandma's pie, giant muffins or American pancakes nothing beats the flavour of sweet juicy apple with punchy cinnamon spice. It's the perfect combination for a lovely fruity, punchy and spicy tea. Thanks go to the team at Olive and Bean, one of our lovely stockists in Newcastle who suggested this blend of apple and cinnamon."
apple, cinnamon, apple pomace, roasted chicory root, citric acid, sweet blackberry leaves, natural flavours.
pommes, cannelle, marc de pomme, racine de chicorée, torréfiée, acide citric, feuilles de mûres de Chine, arômes naturels.


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Learn more about who we are
Ghiras Al-Nahda is a Nonprofit Non-governmental humanitarian organization working to empower people through fulfilling their basic needs and seeking to improve Syrian community stability and resilience.
Ghiras Al-Nahda started its humanitarian efforts in October 2011 via a team of volunteers, it was legally registered in Turkey on September 9, 2016, under: FIDAN DERNEGI
Registration No: 152-017-27
Ghiras Al-Nahda is a co-founder of the Syrian NGO Alliance SNA
Forced Displacement of Syrians and increasing humanitarian needs for host communities and IDPs.
The limited access to education in Syria, the damage and destruction of schools infrastructure and Children dropping out of schools
The destroyed infrastructure of residential buildings and service facilities
Challenges facing vulnerable groups in the community including women, children and people with disability
The deteriorating economic situation of the displaced and refugees and its impact on unemployment and lack of job opportunities.
Secure a decent life for Syrians and empowering them to lift the Syrian community
Independent non-profit, non-political organization that provides humanitarian aid for Syrians neutrally, without any discrimination and seeks to empower people through fulfilling their basic needs.
Our main goal is to protect human lives and dignity therefore we respond to humanitarian needs wherever they are
We aim for the higher level of perfection in our work, that's why we develop policies, coordination mechanisms, annual and monthly implementation plans
We implement our projects and activities through our field team, the value of our honesty is highlighted through our good reputation which we gained through years of work in the humanitarian sector
Engagement and Participation
We strive to engage all actors in humanitarian work as we seek to exchange experiences to serve the community, whether from team members, donors, beneficiaries, partners and other organizations
The incoming money for the organization is traced with transparency before donors, partners, staff, and government through accurate financial audit and procedures to ensure up to date financial reports that can be acquired when needed, in addition to our governance structure which allow accountability for members who violate organization values
Ghiras Al-Nahda Profile
Check our profile