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Conversation of Cde. Nicolae Ceausescu and Cde. Zhou Enlai at the Embassy
Notes regarding the conversation of Cde. Nicolae Ceausescu and Cde. Zhou Enlai at the dinner organized by the [Romanian] embassy in honor of the Chinese leadership. (20.06.1971. 1930 hours)
Cde. N. Ceausescu: spoke with Cde. Zhou Enlai about the fund for aid of communist parties, the Romanian contribution to this fund, as well as the way [the money] is distributed.
Cde. Zhou Enlai: In our relations with certain parties, we encourage them to depend on their own resources. This is because many parties do not really carry on a revolutionary activity.
We too contributed with money to this fund, with sums even bigger than Romania, but we were never consulted to as to how the money would be distributed, we did not know how it was used. It is clear that this method of theirs is hard to change, it has become tradition. They receive, from generation to generation, the role of head of household. In 1961 or 1963 -- I don't remember exactly -- we stopped contributing to this fund.
Cde. NC showed that a direct air connection between Romania and China between the two countries, that we will need to think about newer planes, faster planes. He stated that Turkey and Iran were, in principle, agreeable to allow [the planes] to cross their territory. Iran told us that during the negotiations for establishing diplomatic relations, this could be one of the problems addressed. He said that the Shah of Iran was very pleased with the reception of the Iranian princesses in China. He said that in October he will travel to Iran to participate in the festivities celebrating 2500 years of the Persian Empire.
Cde. ZE: at the funeral of Gheorghe Gheorghiu-Dej, an emissary of the Shah was also present.
Cde. NC asked about the evolution of the situation in Pakistan.
Cde. ZE: presently they are controlling the situation. The situation in East Pakistan is very complicated. There are two religions there: Hindi and Islam. During the events, a number of people became refugees, a majority of which were Hindi. Quite a few Muslims also became refugees, but because of the religious contradictions, some of them have returned. During the battles, there were many victims. Later, the Hindi rebelled again, but the movement was put down by the army. Presently, the central government is controlling the situation.
Initially, the CIA paid a great deal of attention to the events, and was involved in them. Afterwords, seeing the size of the developments, it advise them to relax.
The Americans offered to help the refugees. Pakistan accepted this, but did not allow the aid to be dropped from American planes.
The Indian government has recognized, semi-officially, the government of the Oriental [East] Bengal. It did not dare to recognize it officially, completely. The US and the Soviet Union have advised the Pakistani and Indians to make peace. The issue is not resolved, it can continue to evolve.
The Pakistani government intends to attract to its side the majority of members of parliament in the Oriental Bengal which are part of Rahman's movement.[1] They also intend to create a new party - "People's Will." The issues are currently churning. Yahya Khan declared that, based on [the evolution of] this process, he'll decide if there will be general or partial elections. They have to act carefully because a rebellious East Bengal could unite with a rebellious West Bengal and create a third Bengal.
The population in West Bengal is having having a very hard time, it's not pleased by India's domination. That is why, every time during elections, the winners were the opposition parties. That is why it was possible that, for a period of time, the power was held by the Communist party.
Cde. NC mentioned that the Indian PM, Indira Gandhi, sent a letter to Romania requesting help for the repatriation of the 3.5 million refugees.
Cde. ZE said that this number, published in several countries, is exaggerated. Maybe there are over 1 million refugees, but there is no way there can be 3.5 million.
They asked everyone for help. The Soviet Union wants to recreate the spirit of Tashkent,[2] which was the creation of Kosygin. This idea, which was imposed on the two sides, ended with the death of Shastri.[3]
India suggested to us to exchange ambassadors. We are looking at their proposal, and I think we will be able to accept this suggestion, since we sent ambassadors to all countries with which we have diplomatic relations.
Cde. NC stated that this is a very good thing. Indira Gandhi said she is looking for solutions to improve [India's] relations with China. Indira Gandhi has obtained good results in the elections. The measures they have adopted are a good beginning.
Cde. ZE: they have a lot of problems. They took out a lot of loans. Receive credits and pay back notes plus the interest. The US demands that the loans be paid back in rupees, and thus the Americans have a lot of rupees with which they can control the Indian market.
Cde NC said that in industrial development, India has had a good beginning. He also said that he had visited one of the three Indian atomic reactors. India can even produce the atomic bomb.
Cde. ZE: India produces a lot of conventional armament, which is why Pakistan is worried. As far as the production of the atom bomb is concerned, probably India wants to create an equilibrium in its relations with China.
Between Pakistan and India, the issues are very complicated, and those issues were created by England through its policy of divide and conquer. The last British governor in India favored Nehru. Dividing India into India and Pakistan, he left a problem unresolved -- Kashmir.
Cde. NC: Improving relations with India would be a good way to prevent the expansion of American influence in India.
Cde. ZE: the two [super]powers are fighting for advantages. We have no wish to get involved in the triangle everyone is talking about.
Cde. NC said that, historically, there were no clashes between China and India.
Cde. ZE: Indeed, there were no clashes between China and India, except the two in 1959 and 1962, which were provoked by India.
Recently, a British journalist published in "Times" a long article entitled "India's War against China."[4] From the title of the article it is clear that India and not China provoked the war. This journalist[5] lived 20 years in India, and never once visited China, and he wrote the entire article on the basis of Indian documents. Thus, he had no reason to go easy on us, and his article clearly shows the Indian plan. Both incidents happened during Nehru's time, the first in the region of Aksai Chin[6] and the second in 1962 on the McMahon line,[7] which was an arbitrary line, and was never recognized by any Chinese government. We repelled the Indian attacks, but Khrushchev said we did not act correctly. The British journalist was fair.
Cde. NC said that, it seems, India wants to reach an understanding, to resolve the problems.
Cde. ZE: That is what they tell you. They never tell this to us. I know Indira Gandhi very well. We do not wish to get involved in the issues there which are being planned by the Soviet Union, the US, and India. It is not just about them, but, rather, about our neighbors to the North.
Cde. NC asked about the situation in Burma.
Cde. ZE: Burma has a lot of economic difficulties. With respect to our relations with them, we exchanged ambassadors, thus raising the level of diplomatic representation.
Ne Win[8] was, until very recently, very sick. Once recently has he returned to his country.
(Cde Zhou Enlai made a toast)
Cde. ZE: A year and a half ago, Cde. Huang Treng-Sang [sic], at the direction of Cde. Mao Zedong, inspected in Northeast China the bomb shelters. I did not go there, I did not see them. The experience used in Northeast China we applied in Beijing, then we generalized in the entire country. Had there not been pressure from outside, we could not have mobilized the people for the creation of these underground constructions, just as you yourself could not have reorganized the patriotic guards in such a short time.
I know that during the events in Czechoslovakia you worked very hard, you did not sleep several nights.
Cde. NC confirmed [this] and talked about the measures undertaken. He mentioned that the Soviets asked why these measures were undertaken, and why the Romanians keep talking so much about independence.
Cde. ZE: [One] needs to talk about independence every day, so that the people have to understand [it] and remember it.
Recently, [French President] Pompidou reviewed troops from the three branches of the French military, and suggested that all non-Mediterranean countries should withdraw their troops from the Mediterranean Sea. The two [super]powers are viewed with hostility everywhere. This is a big change.
Presently, there are several American journalists in Beijing. They told us that even they did not expect the changes that took place in attitudes vis-a-vis the United States. The Americans think that they can have advantages everywhere, that everyone needs to listen to them. But, as the war in Indochina continues, the people's attitudes are changing. In the US, especially young people, seek a way out of the difficult situation in which they find themselves. However, the in Soviet Union, there are no such signs of change as in the US.
Cde. NC talked about the [many] possibilities of getting informed in the US, and about the control of information toward the public in the Soviet Union.
Cde. ZE: the Soviets do not take into account other people's opinions.
We have an internal bulletin of news from the foreign press which is published in 3 million copies. It is being read as far down as the local organizations so that they will know the international developments and the interpretation of these events.
Cde. Li Xiannian[9] mentioned that on 23 August 1968, Cde. Zhou Enlai made a speech in the courtyard of the Romanian Embassy.
Cde. ZE: The actions of the Soviet Union in Czechoslovakia is not appreciated by anyone, it only created heartbreak for the people of that country.
Cde. NC said that, presently, there is a very interesting situation in Africa.
Cde. ZE: There is a conference of Foreign Ministers. They are preparing a conference for the heads of state. First, it was suppose to take place in Uganda, but given the situation in that country, they decided for Addis Ababa.
Some countries with right wing governments like Uganda, Congo (K[inshasa]), and countries in south Africa and Central Africa are creating obstructions. The emperor of Ethiopia sent the Minister of Foreign Affairs in those countries to advise them to participate.
[1] The 6 Point Movement was a Bengali nationalist movement in East Pakistan spearheaded by Sheikh Mujibur Rahman, which eventually led to the liberation of Bangladesh. The movement's main agenda was to realize the six demands put forward by a coalition of Bengali nationalist political parties in 1966, to end the perceived exploitation of East Pakistan by the West Pakistani rulers. The demands were drafted by leading Bengali intellectuals Rehman Sobhan, Govinda Chandra Dev, Munier Chowdhury and Kamal Hossain.
[2] The Tashkent Declaration of 10 January 1966 was a peace agreement between India and Pakistan. In September 1965 before the two had engaged in the short run Indo-Pakistani War of 1965. Peace had been achieved on 23 September by the intervention of the great powers who pushed the two nations to a cease fire for fears the conflict could escalate and draw in other powers.
[3] Lal Bahadur Shrivastav Shastri (2 October 1904 - 11 January 1966) was the second Prime Minister of the Republic of India and a significant figure in the Indian independence movement.
[4] Maxwell, Neville. India's China war. New York: Pantheon Books, 1970.
[5] Neville Maxwell (b. 1926) is a British journalist. In 1959 he was posted to New Delhi as South Asia correspondent. In the next eight years he traveled from Kabul to East Pakistan and Katmandu to Ceylon, reporting in detail the end of the Nehru era in India and the post-Nehru developments. In 1967 he went as a senior fellow to the School of Oriental and African Studies in London in order to write India's China War.
[6] Aksai Chin, also Aksayqin, Akesaiqin or Akesai Qin is a disputed region located in the northwestern region of the Tibetan Plateau north of the western Kunlun Mountains.[1] It is entirely administered by the People's Republic of China as a part of Hotan County in the Hotan Prefecture of Xinjiang Autonomous Region. It is, however, claimed by India as a part of its state of Jammu and Kashmir.
[7] The McMahon Line marks boundary between Chinese-held and Indian-held territory in the eastern Himalayan region. The line was the focus of a brief war in 1962, when Indian and Chinese forces struggled to control a disputed area (shown in red), much of which is a thinly populated high altitude mountain area.
[8] Ne Win (24 May or 14 May 1911 or 10 July 1910 -- 5 December 2002) was a Burmese politician and military commander. He was Prime Minister of Burma from 1958 to 1960 and 1962 to 1974 and also head of state from 1962 to 1981.
[9] Mr. Li Xiannian, Deputy. Premier of the State Council of the PRC
Notes regarding the conversation of Cde. Nicolae Ceausescu and Cde. Zhou Enlai at the dinner organized by the [Romanian] embassy in honor of the Chinese leadership.
Zhou, Enlai
Ceaușescu, Nicolae
Soviet Invasion of Czechoslovakia
Conversations with Zhou Enlai
Prague Spring, 1968
Subjects Discussed
Czechoslovakia--History--Intervention, 1968
Sino-Indian Border Dispute, 1957-
Vietnam War, 1961-1975
Pakistan--Military relations--United States
India--Foreign relations--Pakistan
India--Foreign relations--United States
China--Foreign relations--Pakistan
China--Foreign relations--Romania
Vietnam War, 1961-1975--Public opinion
China--Foreign relations--India
Burma--Foreign relations--China
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"Conversation of Cde. Nicolae Ceausescu and Cde. Zhou Enlai at the Embassy", June 20, 1971, Wilson Center Digital Archive, CWIHP archive.
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\section{Introduction\label{one}}

According to the standard theory of cosmological structure formation, most of the mass in galactic halos is composed of non-baryonic matter with negligible primordial velocity dispersion, commonly called cold dark matter (CDM), the constitution of which remains a mystery.  Many theories have been proposed to account for the dark matter.  Dark matter candidates may be non-thermal relics or thermal relics, depending upon the underlying particle physics. Non-thermal relics are particles which decoupled from the standard model particles without being in thermal equilibrium with them, the best example being the axion~\cite{ref1}. Thermal relics on the other hand, were once in thermal equilibrium with other particles, but decoupled when their interaction rate became comparable to the Hubble rate. These particles are collectively known as Weakly Interacting Massive Particles or WIMPs~\cite{ref2}.

There are many collaborations currently trying to detect dark matter, which include ADMX~\cite{ref3}, DAMA/NaI~\cite{ref4}, DAMA/LIBRA~\cite{ref5}, CDMS~\cite{ref6}, XENON~\cite{ref7}, EDELWEISS~\cite{ref8}, ZEPLIN~\cite{ref9}, etc.  Dark matter detection experiments are usually of two kinds - direct detection experiments look for the recoil that occurs when a WIMP scatters off a target nucleus, while indirect detection experiments look for standard model particles which result from dark matter particle annihilation. In this article, we investigate the flux of gamma ray photons produced by WIMP annihilation in dark matter caustics. Previous work on particle annihilation in  caustics includes \cite{ref10,ref11,ref12,ref13,ms}.  For the possibility of detecting caustics by gravitational lensing, see \cite{ref14,ref15,onemli}. Caustics and their associated cold flows are also relevant to direct detection experiments \cite{ref16,ref17,ref18,ref19,ref20}.

Cold dark matter particles exist on a thin 3-dimensional hypersurface in phase space. To obtain the density in physical space, we must make a mapping from phase space to physical space. Caustics are locations where this mapping is singular~\cite{asz,ref21, ref22, ref23, ref24, ref25, ref26, ref27, ref28, ref29, ref30, ref31, ref32,zs}. Caustics are made up of sections of the elementary catastrophes, which are structurally stable and have a definite geometry that depends on the structure of the phase space manifold. In the limit of zero velocity dispersion, caustics are singularities in physical space. In real galactic halos, the velocity dispersion cuts off the divergence \cite{zs}.

It is important to ask whether the finite velocity dispersion of dark matter can soften the density contrast of caustics to the extent that the caustics are made irrelevant. The inner regions of phase space may well have thermalized over the age of the Universe. The infall of thermal dark matter does not produce observable caustics. However, it is believed that in large galaxies like our own, there is a lot of dark matter well outside the virial radius, yet gravitationally bound to the halo. These dark matter particles are in the process of thermalizing and have velocity dispersions that are small compared to the virial velocity dispersion of the galaxy~\cite{ref28,ref30}. The dark matter particles reaching us today for the first time for example, are cold and are likely to produce a physically significant caustic. Similarly the particles that have fallen into the inner regions of the halo only a few times in the past may be expected to produce observable caustics. Thus caustics are formed if the outer regions of phase space are well resolved. An analysis of the rotation curves of 32 galaxies~\cite{ref33} seems to provide evidence for the existence of dark matter caustics. The rotation curve of our galaxy also shows rises at the expected locations of the caustics~\cite{ref34}.

Perhaps the best example of caustics on galactic scales is the occurrence of shells around giant elliptical galaxies~\cite{ref35, ref36, ref37} (e.g. NGC 3923, see~\cite{ref37}). These shells are caustics in the distribution of starlight. They form when a dwarf galaxy falls into the gravitational potential of a much larger galaxy and is assimilated by it. The velocity dispersions of the stars of the dwarf galaxy are much smaller than the virial velocity dispersion of the giant galaxy. The infall of stars is therefore cold and presumably, collisionless. The occurrence of these caustics show us that cold flows are not unstable and that caustics do not require special initial conditions to form~\cite{ref30}. This leads us to believe that the infall of non-thermal dark matter also produces caustics.

There are two kinds of caustics - outer and inner~\cite{ref29}. The outer caustics are thin topological spheres surrounding galaxies (like the caustic of stars discussed previously). They are simple fold catastrophes and typically occur on scales of 100's of kpc for a galaxy like our own. The inner caustics have a more complicated geometry and are made up of sections of the higher order catastrophes~\cite{ref31}. Inner caustics typically occur on scales of 10's of kpc.

To see the formation of inner caustics, let us consider the infall of a perfectly cold flow of dark matter. If the infall is exactly spherically symmetric, the particle trajectories are radial and the infall produces a singularity at the center. If instead, the dark matter particles possess some distribution of angular momentum with respect to the halo center, the particle trajectories are non-radial, particularly in the inner regions of the halo. Fig.~\ref{fig1} shows an example of non-radial infall (in cross section) with the result that the dark matter density is enhanced along two thin fold catastrophe lines (surfaces in 3-dim. space) which meet at a cusp catastrophe point (line in 3-dim. space)~\cite{ref38,ref39}. The caustic divides the $xy$ space into two regions - one region with 1 particle trajectory passing through each point (outer region) and the other with 3 particle trajectories passing through each point (inner region).

\begin{figure}[]
\includegraphics[width=3in,height=3in] {fig1.eps}
\caption{ Dark matter trajectories forming a caustic. The caustic is the envelope of the family of dark matter trajectories. Thus the dark matter density is large at the location of the caustic. }
\label{fig1}
\end{figure}

Close to the cusp, the dark matter trajectories are specified by the family of curves
\begin{equation}
\frac{y}{y_0} = \alpha^3 - \alpha \frac{x}{x_0} \\
\label{eq_1}
\end{equation}
where $(x=0,y=0)$ are the co-ordinates of the cusp and $x_0,y_0$ are constants. $\alpha$ parametrizes the family. The caustic is the envelope of the family of curves, i.e. the locus of points tangent to the curves. The envelope is obtained by solving Eq.~\ref{eq_1} together with the tangency condition $3\alpha^2 - \frac{x}{x_0} = 0$, using which we obtain the caustic curve
\begin{equation}
\frac{y}{y_0} = \pm \frac{2}{3\sqrt{3}} \left( \frac{x}{x_0} \right )^{3/2}.
\label{eq_3}
\end{equation}
The density is proportional to the sum $ \sum_{i}   \left| 3 {\alpha_i}^2 - \left(x/x_0\right ) \right | ^{-1} $ where $\alpha_i$ are the real roots of the cubic Eq.~\ref{eq_1}. When $y=0$, the dark matter density is given by  $ \rho(x,0) = \rho_c  \left|\frac{x_0}{x}\right| $ for $x < 0$ and $ \rho(x,0) =  \rho_c \left( \frac{x_0}{x} + \frac{x_0}{2x} + \frac{x_0}{2x} \right ) = 2\,\rho_c \frac{x_0}{x}$ for $x > 0$ where $\rho_c$ is a constant. For $x=0$, we have $\rho(0,y) = \frac{\rho_c}{3} \left(\frac{y_0}{y}\right)^{2/3}$. Close to one of the fold lines and in the inner region, the density falls off as the inverse square root of the distance to the fold along the direction perpendicular to the fold.  For arbitrary $(x,y)$, we need to solve Eq.~\ref{eq_1} to obtain $\alpha_i$.  The general solution is worked out in~\cite{ref14}.

For arbitrary initial conditions, other catastrophes can occur. In general, we may parametrize the flow of cold dark matter particles by a three parameter label $\vec\alpha(\alpha_1, \alpha_2, \alpha_3)$ where $\alpha_1, \alpha_2, \alpha_3$ are three conveniently chosen parameters that describe the flow~\cite{ref29}. Let $\vec x(t, \vec \alpha)$ be the physical space location at time $t$, of the particle labeled $\vec\alpha$ and is obtained by solving the equations of motion for given initial conditions. The physical space density is proportional to the sum $ \sum_i \, | \partial \vec x / \partial \vec \alpha_i |^{-1} $ ( the Jacobian determinant of the map from $\vec\alpha$ space to $\vec x$ space ) and is infinite (for a perfectly cold flow) at those points where $ \partial \vec x / \partial \vec \alpha_i  = 0$. For a perfectly cold flow, it can be shown that such a singularity necessarily occurs~\cite{ref31}.

A perfectly cold flow cannot be realized in practice. The primordial velocity dispersion of WIMPs is estimated to be $ \delta v = 3 \times 10^{-7} \sqrt{ 100 \, \textrm{GeV} / m_\chi }$ km/s~\cite{ref29}. This causes the caustic surface to spread by an amount $ \delta a \approx \delta v \times a / v $~\cite{ref40} where $a$ is the outer turnaround radius (few hundred kpc) of the flow of particles forming the caustic and $v$ is the speed of the particles at the location of the (inner) caustic (few $\times$ 100 $\,$ km/s~\cite{ref19}). This minimum spread in the caustic surface sets an upper limit to the density. For the nearby caustics, we can estimate the spread in the caustic location
\begin{eqnarray}
\delta a &\sim & \frac{200 \times 3 \times 10^{-7}}{500} \, \textrm{kpc} \, \sqrt{\frac{100 \, \textrm{GeV}}{m_\chi} } \;  \nonumber \\
  &\sim& 10^{-4} \; \textrm{pc} \; \sqrt{\frac{100 \, \textrm{GeV}}{m_\chi} }
\end{eqnarray}

\begin{figure}[!h]

\subfigure[]{\label{fig2-a}\includegraphics[width=3.2in,height=2in]
{fig2a.eps}}
\subfigure[]
{\label{fig2-b}\includegraphics[width=3.2in,height=2in]
{fig2b.eps}}
\subfigure[]
{\label{fig2-c}\includegraphics[width=3.2in,height=2in]
{fig2c.eps}}
\subfigure[]
{\label{fig2-d}\includegraphics[width=3.2in,height=2in]
{fig2d.eps}}

\caption{ (color online) The effect of averaging the density over a finite volume. Fig.~\ref{fig2-a} shows the variation of dark matter density (in Gev/cm$^3$) with distance to the caustic ( in parsec ). A cut-off density of 100 Gev/cm$^3$ was assumed. Figures~\ref{fig2-b},~\ref{fig2-c} and~\ref{fig2-d} show the effect of averaging the density over a cube of side $\delta$ for $\delta = 0.01, 0.1$ and $1$ parsec respectively.
\label{fig2}}
\end{figure}

Let us now examine the effect of averaging the density over a finite region of space. Fig~\ref{fig2-a} shows the density along the line of sight, close to one of the fold lines of Fig~\ref{fig1}. Close to the fold, but outside it, the dark matter density is very small. The density changes abruptly at the location of the fold and becomes very large (100 GeV/cm$^3$ was chosen as the density cut-off), decreasing smoothly thereafter. Figures~\ref{fig2-b},~\ref{fig2-c} and~\ref{fig2-d} show the density averaged over a cube of side 0.01 parsec, 0.1 parsec and 1 parsec respectively. In Fig.~\ref{fig2-b}, we see that the averaged density follows the true density faithfully, though the maximum averaged density does not quite reach the cut-off value. Fig.~\ref{fig2-c} no longer shows a sharp rise in density and  Fig.~\ref{fig2-d} misses the caustic completely. We conclude that caustics are sub-parsec scale structures and are therefore difficult to resolve with large scale cosmological simulations which typically have spatial resolutions of 100's of pc.

\section{The annihilation flux}

In the minimal supersymmetric extension of the standard model (MSSM), a good candidate for the WIMP is the lightest neutralino which is a linear combination of the supersymmetric partners of the neutral electroweak gauge bosons and the neutral Higgs bosons. The characteristics of the annihilation signal depend both on the composition of the WIMP and its mass $m_\chi$. The line emission signal ( $\chi\chi \rightarrow \gamma\gamma, \chi\chi \rightarrow Z \gamma$ ) is loop suppressed and is therefore smaller than the continuum signal. The continuum flux (number of photons received with energies ranging from $E_1$ to $E_2$ per unit detector area, per unit solid angle, per unit time) is given by~\cite{ref12, ref41,ref42}
\begin{equation}
\Phi(E_1, E_2, \theta, \phi, \Delta\Omega) = S(E_1,E_2) \times \frac{< EM >}{4\pi} (\theta,\phi,\Delta\Omega)
\end{equation}
where
\begin{eqnarray}
S(E_1,E_2) &=& \int_{E_1}^{E_2} dE \, \sum_i b_i \, \frac{dN_{\gamma,i}}{dE}(E_\gamma) \; \frac{ <\sigma v> }{2\, m^2_\chi}  \nonumber \\
< EM >(\theta,\phi,\Delta\Omega) &=& \frac{1}{\Delta\Omega} \int_{\Delta\Omega} d\Omega \;\; EM(\theta,\phi)
\end{eqnarray}
$dN_{\gamma,i}/dE$ is the number of photons produced per annihilation channel per unit energy, $b_i$ is the branching fraction of channel $i$ and $<\sigma v>$ is the thermally averaged cross section times the relative velocity. The factor of 2 in the denominator accounts for the fact that two WIMPs disappear per annihilation.   The quantity $EM(\theta,\phi)$ is called the emission measure and is the dark matter density squared, integrated along the line of sight, i.e.
\begin{equation}
EM(\theta,\phi) = \int_{los} dx \, \rho^2(x).
\label{eq_7}
\end{equation}
and $< EM >(\theta,\phi,\Delta\Omega)$ represents the emission measure in the direction $(\theta,\phi)$ averaged over a cone of angular extent $\Delta\Omega$. We note that $S$ depends solely on the particle physics while $< EM >$ depends solely on the dark matter distribution.

\subsection{Estimating S}

Assuming that all the dark matter is composed of neutralinos, the quantity $ < \sigma v > $ is constrained by the known dark matter abundance~\cite{ref2}
\begin{eqnarray}
< \sigma v > &\approx & \frac{ 3 \times 10^{-27} \textrm{ cm$^3$ s $^{-1}$ } }{ \Omega_\chi h^2 }  \nonumber \\
& \approx & 3\times 10^{-26} \textrm{ cm$^3$ s $^{-1}$ }
\end{eqnarray}
The quantity $dN_{\gamma}(E_\gamma) / dx$ for the dominant channels may be approximated by the form~\cite{ref43, ref44, ref45} $dN_{\gamma} / dx = a \, e^{-bx} / x$ where $x$ is the dimensionless quantity $E_\gamma / m_\chi$ and $(a,b)$ are constants for a given annihilation channel. The values of $(a,b)$ for the important channels are given in~\cite{ref43}. Using these values, we may calculate the number of photons produced per annihilation within a specified energy range. Let us consider four energy bands: Energy Band I with photon energies from 30 MeV to 100 MeV, Band II with energies from 100 MeV to 1 GeV, Band III with energies from 1 GeV to 10 GeV and Band IV containing photon energies 10 GeV upto $m_\chi$. The values of $N_\gamma / m^2_\chi$ are tabulated for the different  energy bands, for $m_\chi = 50, 100, 200$ GeV.

\begin{table}[!h]
\caption{ $ N_\gamma / {m^2_\chi} $ in units of $10^{-4} $ GeV$^{-2}$ for $m_\chi = 50 \, \textrm{GeV} $ }
\centering
\begin{tabular}{l c c c c }
\hline\hline
Channel & I  & II & III &  IV \\ [0.5ex]
\hline
    $ WW,ZZ (0.73, 7.76)$   &  106.8  &   85.2   &  18   &  0.52  \\
    $b \bar b  (1, 10.7)$     &  146     &  114.4  &  21.6  & 0.32 \\
    $ t \bar t (1.1, 15.1) $   &  160  &   122.4  &   19.6  &   0.12  \\
    $ u \bar u (0.95, 6.5)$  &  139.2  & 111.6  &   25.2  &   0.96 \\ [1ex]
\hline
\end{tabular}
\label{table:table1}
\end{table}

\begin{table}[!h]
\caption{ $ N_\gamma / {m^2_\chi} $ in units of $10^{-4} $ GeV$^{-2}$ for $m_\chi = 100 \, \textrm{GeV} $ }
\centering
\begin{tabular}{l c c c c }
\hline\hline
Channel & I  & II & III &  IV \\ [0.5ex]
\hline
    $ WW,ZZ (0.73, 7.76)$   &  38  &   30.8   &  7.9   &  0.6  \\
    $b \bar b  (1, 10.7)$     &  51.9     &  41.8  &  10  & 0.5 \\
    $ t \bar t (1.1, 15.1) $   &  57  &   45.4  &   9.8  &   0.3  \\
    $ u \bar u (0.95, 6.5)$  &  49.4  & 40.3  &   10.7  &   1.0 \\ [1ex]
\hline
\end{tabular}
\label{table:table2}
\end{table}

\begin{table}[!h]
\caption{ $ N_\gamma / {m^2_\chi} $ in units of $10^{-4} $ GeV$^{-2}$ for $m_\chi = 200 \, \textrm{GeV} $ }
\centering
\begin{tabular}{l c c c c }
\hline\hline
Channel & I  & II & III &  IV \\ [0.5ex]
\hline
    $ WW,ZZ (0.73, 7.76)$   &  13.5  &   11.0   &  3.1   &  0.4  \\
    $b \bar b  (1, 10.7)$     &  18.4     &  15.0  &  4.1  & 0.4 \\
    $ t \bar t (1.1, 15.1) $   &  20.2  &   16.4  &   4.3  &   0.3  \\
    $ u \bar u (0.95, 6.5)$  &  17.5  & 14.4  &   4.2  &   0.6 \\ [1ex]
\hline
\end{tabular}
\label{table:table3}
\end{table}

\subsection{Estimating $< EM >$}

The geometry of dark matter caustics depends on the spatial dark matter velocity distribution. In the linear velocity field approximation~\cite{ref31}, the velocity field is a linear function of position, i.e. $\vec v(\vec r) = M \, \vec r$ where $M$ is a matrix. In general, $M$ contains both anti-symmetric and symmetric parts. If $M$ is dominated by the anti-symmetric part (rotational flow), the infall is greatly simplified and the resulting caustics have the appearance of rings~\cite{ref29}. If $M$ contains a significant symmetric part, the caustic geometry is more complicated. See~\cite{ref31} for a description. In this article, we assume that the caustics have the appearance of rings. If the flow has axial symmetry, the caustic ring is circular with constant cross section. Otherwise, the cross section will vary along the ring and the ring will not be circular.

Let us consider cylindrical co-ordinates $(s,z)$ where $s = \sqrt{x^2 + y^2}$.  We assume axially symmetric infall about the $z$ axis and reflection symmetry about the $z=0$ plane. We can then obtain an analytic solution for the dark matter density at points close to the caustic. With these assumptions, the caustic is circular with a tricusp cross-section described by the curve
\begin{eqnarray}
z =
  \left \{
    \begin{array}{ll}
        \pm \frac{q}{2}\sqrt{ 1 - \frac{2}{3} \xi \pm \frac{8}{27} \xi^{3/2} - \frac{\xi^2}{27} }   &   \mbox { $0 \le \xi \le 1$ } \\
\\

        \pm \frac{q}{2}\sqrt{ 1 - \frac{2}{3} \xi + \frac{8}{27} \xi^{3/2} - \frac{\xi^2}{27} }   &   \mbox { $1 < \xi \le 9$  }
    \end{array}
\right.  \label{tricusp_curve}
\end{eqnarray}
where
\begin{eqnarray}
\xi &=& 1 + 8 \frac{s-a}{p}.
\end{eqnarray}
Here, $a$ is the caustic radius ($s$ co-ordinate of the point of closest approach of the particles in the $z=0$ plane), $p$ and $q$ are the horizontal and vertical extents of the tricusp. See~\cite{ref29} for a detailed description.

Let us use the self-similar infall model~\cite{ref46,ref47} to estimate the mass infall rate for the flow of particles forming the caustic
\begin{equation}
\frac{d^2\,M}{d\Omega dt} = v\,f\,\frac{v^2_{rot}}{4\pi G}
\end{equation}
where $v$ is the velocity of the particles forming the flow, $f$ is a dimensionless quantity that characterizes the density of the flow and $v_{rot}$ is the rotation speed of the galaxy.

Let us define the two dimensionless co-ordinates $R = (s-a)/p$ and $Z = z/q$.  In the $Z=0$ plane, the density is given by
\begin{equation}
\rho(R,0) \approx 0.34 \frac{\textrm{GeV}}{\textrm{cm$^3$}} \; \frac{(f/10^{-2})\;( V_{rot} / 220 \, \textrm{km\,s$^{-1}$})^2 } {s_{kpc} \; p_{kpc}}   \left \{
    \begin{array}{lll}
         \frac{1}{1-R}   &    \mbox{ when $R \le 0$   } \\
         \frac{1}{1-R} \left( 1 + \frac{1}{\sqrt{R}} \right )  &  \mbox{ when $0 \le R \le 1$ } \\
         \frac{1}{R-1}   &    \mbox{ when $R \ge 1$   }
     \end{array}
  \right.
\end{equation}
 $s_{kpc}$ and $p_{kpc}$ are distances measured in kpc.  For $R \rightarrow 0$ the dark matter density diverges as $R^{-{1/2}}$ for $ R > 0$. For $R \rightarrow 1$, the divergence $ \sim |(R-1)|^{-1}$.   When $Z \ne 0$, the density takes the form~\cite{ref48}
\begin{equation}
\rho(R,Z) \approx 0.17\, \frac{\textrm{Gev}}{\textrm{cm}^3} \; \frac{(f/10^{-2})\;( V_{rot} / 220 \, \textrm{km\,s$^{-1}$})^2 } {s_{kpc} \; p_{kpc}}  \sum_i \frac{1}{ \left| 2\,T_i \left( T_i - \frac{3}{2} \right ) + \left(1 - R\right ) \right | }
\end{equation}
where $T_i$ are the real roots of the quartic
\begin{equation}
T^4 - 2\,T^3 + (1-R)\,T^2 - \frac{27}{64} Z^2 = 0
\end{equation}
The above formulae are only valid at points close to the caustic.

The emission measure is calculated by integrating the density squared along the line of sight. Let $b = \pi/2 - \theta $ be the galactic latitude. $l$ is the galactic longitude chosen so that the galactic center is located in the direction $l=0, b=0$. We will assume that the caustics are spread over a distance $ \sim 10^{-4}$ pc. $f$ is set equal to $2 \times 10^{-2}$~\cite{ref14}. The cut-off density close to the fold surface(near $R=0, Z=0$) is then $ \approx 2.15 \times 10^3 / a \sqrt{p} $ Gev/cm$^3$. The density close to the cusp will be larger than this (the density falls off as the inverse of the distance to the cusp), but we will use the density close to the fold surface to set the density cut-off.

\begin{figure}[ht]
\subfigure[$\,(a=7.5,p=0.5,q=0.5)$ kpc]{\label{fig3-a}\includegraphics[width=3in,height=2in]
{fig3a.eps}}
\subfigure[$\,(a=8.0,p=0.1,q=0.2)$ kpc]
{\label{fig3-b}\includegraphics[width=3in,height=2in]
{fig3b.eps}}
\subfigure[$\,(a=8.0,p=0.1,q=0.5)$ kpc]
{\label{fig3-c}\includegraphics[width=3in,height=2in]
{fig3c.eps}}
\caption{  Figures~\ref{fig3-a},~\ref{fig3-b},~\ref{fig3-c} show the emission measure averaged over a solid angle $\Delta\Omega = 10^{-5}$ sr for the three sets of caustic parameters.
\label{fig3}}
\end{figure}

Fig.~\ref{fig3} shows the emission measure averaged over a solid angle $10^{-5}$ sr for three different sets of caustic parameters, as a function of longitude $l$. $b$ is set equal to 0 and we assume that the caustic lies in the galactic plane. Figures~\ref{fig3-a},~\ref{fig3-b} and~\ref{fig3-c} are plotted for $(a,p,q) = (7.5,0.5,0.5), (8.0,0.1,0.2)$ and $(8.0,0.1,0.5)$ respectively with all distances measured in kpc. The earth's location is set equal to $8.5$ kpc from the center. We expect the signal to be strongest when the line of sight is tangent to the ring. From the figures, we see that the emission measure is sensitive to the caustic geometry. The prominent features are the pair of peaks, or `hot spots' separated by a few degrees. The first peak occurs when the line of sight is tangent to the fold surface (when $s = a$). The second peak occurs when the line of sight is tangent to the cusp line (when $s = a+p$). (In the limit $p,q \rightarrow 0$, the two peaks coincide, see~\cite{ref12}). For the case when $p=0.5$ kpc (Fig.~\ref{fig3-a}), the cut-off density was set equal to $400$ GeV/cm$^3$ everywhere, while for the plots with $p = 0.1$ kpc (Figs~\ref{fig3-b} and~\ref{fig3-c}), the cut-off density was set equal to $800$ GeV/cm$^3$ everywhere. The magnitudes of $< EM >$ for the hot spots depend on the values of the caustic parameters and also on the averaging scale (here chosen to be $10^{-5}$ sr).  Table IV shows the annihilation flux for the two hot spots for different values of the averaging scale $\Delta\Omega$, for the case $(a=8.0, p=0.1, q=0.2)$ kpc. It is worth pointing out that if the triangular feauture in the IRAS map is interpreted as the imprint of the nearest caustic on the surrounding gas as in~\cite{ref40}, the implied caustic parameters are close to what we have assumed for Fig~\ref{fig3-b}.

\begin{table}[!h]
\caption{ Peaks of $< EM >$ for $(a=8.0, p=0.1, q=0.2)$ kpc}
\centering
\begin{tabular}{ | c | c | c | }
\hline\hline
$\Delta\Omega$   &   Fold peak  &  Cusp peak \\
(sr)  &  (GeV/cc)$^2$ kpc  &  (GeV/cc)$^2$ kpc   \\ [1ex]

\hline

$10^{-7}$ &   1549.8  &   2177.6 \\
$10^{-6}$ &   1048.3  &   1283.3 \\
$10^{-5}$ &    469.9 &   718.1 \\
$10^{-4}$ &   269.6 &    239.4 \\
$10^{-3}$ &   115.4   &   52.0 \\ [1ex]
\hline
\end{tabular}
\label{table:table4}
\end{table}

\section{Comparing the signal with the background}

The annihilation flux from caustics is thus given by
\begin{eqnarray}
\Phi &=& S \times \frac{< EM>}{4\pi} \nonumber \\
       &\approx & 110 \frac{N_\gamma}{ \left( m_\chi/100 \; \textrm{GeV} \right )^2 } \; \frac{ < EM > }{ (\textrm{Gev/cc})^2 \; \textrm{kpc} } \; \left[ \textrm{ m$^2$ sr year }\right]^{-1}
\label{flux}
\end{eqnarray}
Let us compare this flux with the expected background. The EGRET measured background flux $\Phi_{bg}(E_1,E_2)$ from energies $E_1$ to $E_2$ is given by~\cite{hunter,ref44}
\begin{equation}
 \Phi_{bg} (E_1,E_2,\theta,\phi) = N_{\gamma,bg}(E_1,E_2) \times N_0(\theta,\phi) \times 10^{-6} \textrm{ cm$^{-2}$ s$^{-1}$ sr$^{-1}$ }
\end{equation}
where
\begin{equation}
N_{\gamma,bg}(E_1,E_2) = \int_{E_1}^{E_2} dE\, \left(\frac{E}{\textrm{GeV}}\right)^{-2.7}
\end{equation}
The function $N_0(\theta,\phi)$ is energy independent and follows the fitting form given in~\cite{ref44}. For the four energy bands we have considered, $N_{\gamma,bg}$ = 198.8 for Band I (30 MeV - 100 MeV),  28.9 for Band II (100 MeV - 1 GeV), 0.58 for Band III (1 GeV - 10 GeV) and     0.012 for Band IV (above 10 GeV).

We now compare the caustic signal with the expected background. Since the gamma ray background falls off with energy ($E^{-2.7}$) faster than the annihilation signal ($E^{-1.5}$), we expect that the best chance for detection is at moderately high energies. At low energies, the background flux overwhelms the signal, while at very high energies, the signal is weak. We choose $m_\chi = 50$ GeV since this choice gives the largest flux. For the quantity $ N_\gamma / {m^2_\chi} $, we use the average value for the band. The averaging scale $\Delta\Omega$ is set to $10^{-5}$ sr.

Figures~\ref{fig4-a} and~\ref{fig4-b} show the expected annihilation flux (number of photons per square meter, per steradian, per year) as a function of angle $l$ near the plane of the galaxy ($b = 0$) for the three sets of caustic parameters we considered, for Energy Bands III and IV respectively. This is contrasted with the expected diffuse gamma ray background. The figure shows only the flux from the caustic and does not include the smooth component of the halo. For a standard isothermal with core type of halo profile, we expect the signal from the smooth component of the halo to be much smaller than the signal from the caustic. However,  if there are dark matter clumps along the line of sight, annihilation from the clumps may be significant \cite{ms}. In principle, the peaks in the signal and the sharp fall-off of flux are helpful in identifying the annihilation signal, particularly for the more optimistic caustic parameters and for small WIMP masses. For large WIMP masses, the annihilation signal is significantly smaller.

Let us estimate the significance of detection by assuming an angular resolution $\Delta\Omega = 10^{-5}$ sr, an integration time of 1 year, a detector area of 1 $m^2$ and an optimistic value of $m_\chi = 50$ GeV. Further let us consider the 1 GeV - 10 GeV band, for which the mean value of $ \frac{N_\gamma}{(m_\chi / 100 \, GeV)^2}$ is 21.1 (Table \ref{table:table1}). The number of photons received, assuming $100\%$ detector efficiency, from a region with angular extent $\Delta\Omega = 10^{-5}$ sr is then (Eq. \ref{flux}), $ N_{\gamma,signal} \approx 0.02 \, \frac{< EM >}{(GeV/cc)^2 \, kpc}$. Since an angular size of $10^{-5}$ sr corresponds to a spot of diameter roughly $0.2^\circ$ at the equator, we may expect about 10 distinguishable spots in the angular range $-0.1^\circ < b < 0.1^\circ, 68.2^\circ < l < 70^\circ$. Here $b$ is the latitude ($\pi/2 - \textrm{polar angle} \; \theta$) and $l$ is the longitude. For the moderately optimistic case of caustic parameters $(a=8,p=0.1,q=0.2)$ kpc, we find approximately 60 signal events and for the very optimistic case $(a=8,p=0.1,q=0.5)$ kpc, we find approximately 101 signal events. In this range, we find 716 background events.  Assuming that the fluctuation in the background varies as the square root of the number of background events ($N_{\gamma,bg}$), we may define the detection significance $\sigma = N_{\gamma,signal} / \sqrt{N_{\gamma,bg}}$. For the case $(a=8,p=0.1,q=0.2)$ kpc, we find $\sigma = 2.2$ while for $(a=8,p=0.1,q=0.5)$ kpc, we find $\sigma = 3.8$. A similar calculation shows that in the range $-0.1^\circ < b < 0.1^\circ, 70.2^\circ < l < 72^\circ$, we find 93 signal events for the case $(a=8,p=0.1,q=0.2)$ kpc, and 148 signal events for the case $(a=8,p=0.1,q=0.5)$ kpc, with 700 background events. The values of $\sigma$ for the two sets of caustic parameters is found to be 3.5 and 5.6 respectively.

\begin{figure}[ht]
\subfigure[$\,$Energy Band III]{\label{fig4-a}\includegraphics[width=3in,height=2in]
{fig4a.eps}}
\subfigure[$\,$Energy Band IV]
{\label{fig4-b}\includegraphics[width=3in,height=2in]
{fig4b.eps}}
\caption{  (color online) The annihilation flux for the three different sets of caustic parameters ($m_\chi = 50$ GeV), compared with the EGRET measured diffuse background. The background signal appears as a line of nearly constant slope. The characteristic peaks and the sharp fall-off of the signal may help in signal detection. Among the three curves that show the signal flux, the largest flux curve corresponds to the case $(a=8.0,p=0.1,q=0.5)$, the middle curve is for $(a=8.0,p=0.1,q=0.2)$ and the smallest flux is for $(a=7.5,p=0.5,q=0.5)$. Energy Band III is favored to Energy Band IV owing to the very small flux in Band IV.
\label{fig4}}
\end{figure}

\section{Conclusions}

We calculated the gamma ray annihilation signal from a nearby dark matter caustic having the geometry of a ring with a tricusp cross section near the plane of the galaxy, in different energy bands. For such a caustic, the annihilation signal has two peaks, separated by a few degrees, depending on the size of the caustic. There is an abrupt fall-off of flux after the second peak.  Since the diffuse gamma ray background flux falls off with energy faster than the signal, it is advantageous to look for the signal at moderately high energies. We compared the expected annihilation flux with the expected diffuse gamma ray background. The characteristics of the annihilation flux can in principle, be used to discriminate between the signal and the background. In practice however, we expect this to be a challenging task.

\acknowledgments{ I thank Paolo Gondolo, Konstantin Matchev, Pierre Sikivie and Richard Woodard for helpful discussions. This work was supported by the U.S. Department of Energy under contract DE-FG02-97ER41029. }

redpajama_set_name: RedPajamaArXiv


Archive for the tag "hit"
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We are delighted to announce that students, staff, parents and governors can take great pride in Harington School having been judged Outstanding by Ofsted. The thorough inspection took place in the school between 17-19 January 2017.
Particular strengths identified by Ofsted included the culture of high expectation established by the school leaders, effective collaboration between school leaders and excellent partnerships with local feeder schools. The wealth of experience in education offered by Harington's governors was also noted, as was the quality of support for students making decisions about higher education and careers.
A full copy of the inspection report can be downloaded here.
If you wish to view the report via the Ofsted website, please click here.


text:
".....THE SCHOOL WILL ALWAYS KEEP THEIR MEMORY GREEN"
….. some have made the greatest sacrifice of all. They felt that their country called them, and they did not hesitate to answer the call. And while we deeply mourn their loss, the School will always keep their memory green, and when happier times come back again, the example of their self-sacrifice will still remain for all the succeeding generations who will receive their education within these walls.
Mr G.W Arnison, RGS Headmaster, 1915
This year, whole school community, including governors, neighbours and friends of the school gathered in the Quad this morning for our Annual Service of Remembrance. We were honoured to have Wg Cdr T Benjamin (RAF High Wycombe) present a wreath in memory of our OW casualties of war during the morning's service.
RGS has a long history of association with the armed forces, dating back to 1909 when the School's Officers' Training Corps (OTC) was founded. Today, 180 boys participate in the Combined Cadet Force (CCF), with Royal Navy, Arm and Royal Air Force Sections. We are the only state school in Bucks offering a tri-service CCF.
Two of the three sections at RGS are named in memory of highly decorated OW war veterans, Frederick Youens and Ian Fraser, who fought in the First and Second World War respectively. They continue to be an inspiration to us all, and a source of pride. Both were awarded the Victoria Cross, the highest and most prestigious award 'for gallantry in the face of the enemy' that a serviceman in the British and Commonwealth forces can aspire to attain.
Sports Fixtures

redpajama_set_name: RedPajamaCommonCrawl


text:
DEM BIG MANTON DIES AT 73
By Hasani Gittens
Queens Democratic Party leader Thomas Manton died yesterday evening after a long illness. He was 73.
Manton died at Calvary Hospice in The Bronx, according to longtime friend and spokesman Michael Reich.
His family did not want to disclose the nature of the sickness which had debilitated the party leader for at least the past two months, causing him to miss party meetings.
"Tom was a very proud guy," said Reich. "The one thing that Tom didn't want was for people to have pity on him or anything like that."
"Tom put a very brave and solid face forward for the last few months," said friend and Queens Democratic councilman John Liu. "He's held everybody together until the very end."
Manton, a former Marine, became the head of the Queens County Party Organization in 1986 after serving as a U.S. congressman from 1985 to 1999.
He leaves behind his wife, Diane, and four adult children, Tom Jr., John, Cathy and Jeanie.
"From the Marine Corps, to the NYPD, to the City Council to Congress, Tom Manton dedicated his life to serving the people of Queens and New York City," said Mayor Bloomberg in a statement.
"On behalf of all 8.1 million New Yorkers, our thoughts and prayers are with his family and friends."
WEIRD BUT TRUE


Arcanic Affinity: You have a +4 to Arcane based challenge checks. Negated by Weakness to Arcane.
Night Vision: Whenever your character is in an encounter where fog of war is present, their vision is increased by +2 and they gain +10 to perception.
Manipulator: Replaces plead with Lie. Lies have a -4 threshold to social challenge checks, but the target lied to may attempt to roll perception to determine if they can see through the lie. A 70+ is required to detect the lie. If detected, the liar takes 2 DP damage.
Demonic: Your character may negate all campaign wound penalties by rolling 1d3, where a 1 is considered successful.
Fel Tainted: Your character has a +4 to fel based challenge checks.
Touched By Shadow: Your character has a +4 to all shadow based challenge checks.
Frail I: Your character has a +4 to wounds and suffers an +1 to wound duration.
Crass I: Your character have a -4 to etiquette challenge checks.
Greedy I: Your character has a +15 to their loot rolls, but if they do not win, you will take "Heavy Wounds" as they are stricken with envy. Does not stack with regular wounds. The heavy wounds are not actual wounds but your character will gain the mechanical debuff -1 week. They cannot give loot earned in events to other players.
Wanton II: If an opponent rolls a successful charm or seduction roll, it deals double the DP damage during diplomacy. In combat, it stuns your character for a turn.
Violent I: Whenever your character enters a situation that becomes overly tedious, they must roll a violence check of 1d4. If they roll a 4, they will then violently attack someone present.
Addict I: At the start of each turn, your character must attempt to manage the side effects of withdraw. Roll 1d3 to attempt manage the symptoms, if your characters rolls a 3, they take 1d20 damage.
Weakness to Arcane II: (Negates Arcane Affinity) Your character cannot pass an arcane based challenge check.
Weakness to Light II: Your character cannot pass a light based challenge check.
Weakness to Nature II: (Negates Nature's Gift) Your character cannot pass nature based challenge checks.
Achille's Heel II: Your character has a -2 to their dueling defense dice.
Bonus: +5 max and +2 mod. Increases Intimidation and Seduction rolls by +2.
Bonus: +5 max and +2 mod. Increases crit by +5.
Rain of Fire: The warlock brings down a firestorm of flaming rock and ruin. Using a large explosion template, deal 1d66+6 damage to all enemy targets within it.
Life Siphon: The warlock drains their enemy of precious vitality restoring themselves. The warlock drains an enemy target of 3d8+8 and heals themselves for damage dealt. If the Warlock is at full HP, it will add a shield for the damage dealt, up to 30HP.
Possession : The Ascendant is one who has calculated the exact means necessary to exert their will over their enemy, though it demands such strain that should only be used in the most dire of circumstances.The Ascendent will control the mind of a non-boss enemy unit and that target will move and act on the Ascendent's turn. Each turn the Ascendent must roll 1d20>8 to maintain control of the enemy target. Should they fail the challenge roll to maintain control, the target will die.
Shadow Orbs [Passive]: The Ascendant manifests the power of the void into shadow orbs. They must roll 1d3 every turn to determine how many orbs are available to use. Then, based upon the amount of orbs summoned will determine how many times the Ascendant can use their regular attack on their chosen target.
Suncaster Demonologists summon a horde of imps to the battlefield that deal 5d5+5 damage and have 30hp. They move and attack at the same range/distance as the Suncaster Demonologist. This is a minor action.
Bonus: Suncasters Demonologist summons an infernal to the field to stun a target and deal 5d10+10 damage to them at a range. The Infernal has 100hp and deals 2d30+10 damage in melee. They have the same movement distance as the Suncaster Demonologist. Infernals cannot be healed. This is a minor action.
Bonus: Whenever taking melee damage the player may roll a 1d10 to avoid the damage by blinking. A +5 is a successful dodge.


NEW CONTENT! Geoff interviews Vlad Niculae of Cornell about his recent research on predicting betrayal via written communications. The foundation of the study? An only repository of 300 Diplomacy games and all 150,000 messages they generated.
Vlad's new project is the online game StreetCrowd, which is also exploring communications and team dynamics.
Mike and Geoff select their top 10 entries from the Ludology contest, and reveal the winner!


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Inviata: Bioinformatics Scientist - Statistical Genomics
Thursday, December 17, 2020 - Inivata -
This role will involve the understanding and application of statistical methodologies to genomic data sets for the analysis of NGS cancer genomics data, biomarker development, innovative algorithm design and optimisation of Inivata's technology
Inivata: Medical Science Liaison
The Medical Science Liaison (MSL) is a member of a field-based team of scientists who function as an extension of the Inivata Medical and Scientific Affairs organization. MSLs are responsible for developing and enhancing professional relationships with medical thought leaders involved in various phases of product development and clinical use. MSLs provide medical and scientific information through unbiased exchange and provide clinical/scientific support for Inivata and the Medical Affairs department at the direction of Medical and Scientific Affairs management and in collaboration with the Chief Commercial Officer and commercial field leadership, Clinical Operations and other teams as needed.
OMASS: Computational Chemist (Senior Scientist II / Principal Scientist DOE)
Thursday, December 17, 2020 - Kathryn North -
OMass Therapeutics is inviting applications for the position of Computational Chemist (Senior Scientist II / Principal Scientist depending on experience). This is an exciting opportunity to participate in cutting edge drug discovery and undertake an extremely dynamic and diverse role as OMass seeks to expand computational chemistry capabilities. The company offers a thriving and creative environment for a well-suited candidate to become an integral part of our future vision.
The successful candidate will possess expert Computational Chemistry knowledge with experience across all stages of a project from hit ID through to candidate nomination.
Medicinal Chemist (Senior Scientist II / Principal Scientist DOE)
OMass Therapeutics is inviting applications for the position of Medicinal Chemist (Senior Scientist II / Principal Scientist depending on experience). This is an exciting opportunity to participate in cutting edge drug discovery and undertake an extremely dynamic and diverse role as OMass seeks to expand medicinal chemistry capabilities. The company offers a thriving and creative environment for a well-suited candidate to be exposed to the drug discovery and development process and state-of-the-art technology developments. You will acquire extensive knowledge of the company's operations and become an integral part of our future vision.
The successful candidate will have expert synthetic organic chemistry and medicinal chemistry knowledge and be passionate about applying these skills to the discovery of novel medicines. You will have a proven track record of scientific achievement and of delivering high quality candidates into development.
UKRI: Biological sciences or biopharma – Infrastructure Advisory Committee
Tuesday, December 15, 2020 - Rebecca Wilkes -
A fantastic opportunity for new biosciences IAC members to influence future strategic direction as regards science and innovation infrastructure!
Our Human Resources Sponsor
AggioSergeant is an international boutique retained search firm that has been delivering life science leadership and connecting extraordinary businesses to outstanding people for more than 30 years. Working globally, they have an unparalleled network within the life science community and offices in California, the UK, and the EU.
Our Membership also includes several other companies that provide recruitment, HR, headhunting and interims and which participate in OBN's programme of events. These companies can be located using the Members Directory.
Tweets by OBN_UK


text:
David Vandenbroeck – calciatore belga
 Jonathan Vandenbroeck, noto come Milow – cantautore belga
 Sven Vandenbroeck – allenatore di calcio ed ex calciatore belga

redpajama_set_name: RedPajamaWikipedia


Our dedication to quality doesn't stop at the food we prepare. Ordering, preparing and serving our meals is easy with apetito's innovative solutions and support.
When you partner with apetito, you're immediately assigned a dedicated account management team who'll provide continued support. They'll also assist you with getting started, planning menus, placing orders and meeting your customers' nutritional needs, all within your budget.
You can view the full meal ranges on offer, place orders and check the nutritional information of every meal online, 24/7. Our customer service team is also on hand to assist you every step of the way.
Your meal deliveries will arrive on the same day each week by our own trained delivery staff, in reusable crates that not only make it easy for you check, store and prepare meals, but also reduce cardboard waste.
Our extensive range of delicious, nutritionally balanced meals and flexible portion sizes make it easy to delight customers, manage costs, streamline your service and reduce your food waste.


Leslie Faught is a full time REALTOR® for Alain Pinel REALTORS®, the 5th largest residential, family owned, independent Bay Area broker in the nation. She proudly serves her clients throughout the east bay.
For more than 25 years, Leslie's career has always revolved around serving people in the real estate industry. She is dedicated to partnering with her clients and achieving their real estate goals from their first meeting, through the home buying and selling process, and after the transaction is completed. Prior to her career as a REALTOR®, Leslie was a Platinum Affiliate with the Bay East Association of REALTORS® as a Sales and Marketing Manager in the title insurance and escrow industry. Her vast experience in the transaction process helps insure a smooth and positive experience for her clients.
Living in the East Bay for more than 30 years, Leslie is passionate about the community she serves. She has fun being a "Rosette" with the Annual Pleasanton Rose Show where the proceeds help support the Alameda County Community Food Bank. "I love seeing our community and generations come together, one rose a time while providing food for many of our local families".
Pleasanton, Dublin, Livermore, Sunol, Fremont, Newark, Union City, Castro Valley, Hayward, San Leandro, San Lorenzo, San Ramon, Danville, Brentwood - Leslie is a part of the Relocation Team and is a great resource for your local and global home buying and selling needs can refer you a REALTOR® in the community your are interested in.
Local or global, Leslie will find a buyer for your home and a home for you to buy.


These opening hours don't take account of public holidays and of Sundays. You can also check if Clay County Personal Injury Attorney Green Cove Springs is open on lundi by calling it.
Usually Clay County Personal Injury Attorney Green Cove Springs is closed on Sundays. Careful, stores-locator.com is a participative site, where anyone can indicate opening hours. If you see any mistake, please contact us.
You are a customer or you know the store Clay County Personal Injury Attorney Green Cove Springs?


Feel free to support my work by donating.
Doh! Just realized this was included in your Challenger add-on. Thank you!
i love this car very much,i want this car to be the unique one in lostans,so could u make an add on ?please!
@EliteSamOfficial No need, this car is already an add-on in my challenger car download.
Very cool. Is there a way that I can make other cars NOT have broken windshields or broken glass?
Nice model. But you should definitely put the lodDistances in the README too.
@CrzBonKerz Only if you download the 1.2 version on the challenger download page.
PLEASE MAKE VANQUISH S !!!!!!
hey bro pls can you create DBS with better qualite pls its my favourite car i pay you for private car i have some your your cars on patreon pls can it be possible ?


and fell in "like" with a beautiful mirror, B., on the back cover.
Beveled. Thick molding. Trimmed in antique silver.
Then, as all epiphanies do, it happened!
in the basement office closet.
I painted two coats of Valspar's Gray Teal to cover the red.
And with these little fellas, I painted the molding edges.
I mixed some Metallic Silver Sterling with Burnt Umber.
I painted over that with Metallic Pearl White.
With a paper towel, and more Burnt Umber, I aged the blue area.
I used the flash so you could see how the pearl paint glows.
That is GREAT! You should submit it to Knock Off Decor - totally would get featured!!!
OK. I'll take a pair, please.
A pair of pairs, please.
Oh my! That looks great! I also adore that color!
I think you did great, Leslie! Love the color and those chunky frames!
Fantastic!! And it looks great on the wall!
This is fab! So glad I clicked on this post, I have a mirror in the garage waiting for a revamp, so may have to pinch this idea. If I do I will be linking all my readers to where I got my inspiration from.
Great job Leslie! Looks awesome!
Fabulous....as always! I just love free stuff, especially when it looks that good :). We made a sign for the baby's side of the room last week with stuff we had lying around - free art, gotta love it!
You did a wonderful job. I think it is great and look at the money you saved by using what you had already!
And you know I love the color.
You do realize that's what made them even more special, right?
Lovely job on that mirror, Leslie. That teal color is yummy.
Don't you just love that moment, when you're like, aw mannnn...I wish I had that (item, whatever it is)...and you go...holy crap I have that in my stash!!! :) looks great!
Beautiful! I saw that mirror in my Ballards catalog and "swooned". Great job!
I need to look for that pearl paint. I've never heard of it before, but I love that pretty sheen. Thanks for the tip!
That's awesome! You did amazing!
You did a fantastic job, Leslie - love it! You have me inspired to paint an ugly brown mirror I have hanging in my hallway. How did you protect the mirrored part as you were painting?
That looks FABULOUS!!!! Love it! You did a fantastic job!
Your work is such a impressive. I think it is great and look at the money you saved by using what you had already, for me it is very much inspirational.
How'd you do? You did very well!
You did awesome! Found you via Knock Off Decor. I love how you mixed B.Umber w/Silver. Brilliant - I've gotta try that.
I just used a pearl glaze in a baby's room. It's my new fav 'color'.
I honestly like yours a bit better.


That makes the Senate Judiciary Committee vote a done deal — and likely the floor vote for Brett Kavanaugh's confirmation, too. Retiring Senator Jeff Flake was the only Republican committee member who remained uncommitted on Kavanaugh, and who took to the Senate floor earlier in the week to appeal to the better angels of both parties.
Flake's support means that Judiciary will pass Kavanaugh's nomination to the Senate with a recommendation for confirmation, likely on an 11-10 vote. That will give Mitch McConnell all the impetus he needs to fast-track the vote over the weekend, with a final vote likely by Tuesday at the latest.
Still, 49 is not 50, where Mike Pence could cast a tiebreaking vote. McConnell needs either Susan Collins or Lisa Murkowski to vote aye in both the procedural motions and the final vote. That seems a lot more likely with Flake's decision to back the nomination; Collins seemed to be leaning Kavanaugh's way already, and Murkowski sounded annoyed with the circus that had developed around him. But even without them, there is a better-than-zero chance that Joe Manchin will cross the aisle to support Kavanaugh, given the politics in West Virginia and his need to be seen as independent from Chuck Schumer.
Judge submitted a second sworn statement to the committee last night largely reiterating the first statement. He added that he didn't want to publicly testify because of a fear of public speaking and his recovery from addiction, and also fixed a technical issue with the first statement by signing it.
Update: The committee will take its final vote at 1:30 ET today. The result is a foregone conclusion now.
BREAKING: Some Democratic senators are walking out of cmte. hearing as Republican Chairman Grassley continues with Judge Kavanaugh's confirmation process.


Summer romances are tricky things. You get caught up in the whirlwind of the moment and the feeling of the freedom. So much of what fuels the summer mind is the prospect of living in the moment, saying yes to things you normally wouldn't have and hoping what you felt in that exact moment is a feeling that will last forever, like that one Grease song.
Of course, all summer romances differ slightly in their contexts and conceptions, but one thing can be said of all summer loves: they are wonderful and spectacular things. But once August comes, the feelings dwindle, and that moment and the sheer freedom get lost in the routine of normal life.
Why are summer romances so different from ones at any other time of the year? What makes your feelings during hazy summer nights and hot summer days so unique? As college students, summer provides us with the escape from the monotony and predictability of school life. After our last final, a weight is lifted from our shoulders, and we feel the freedom of the absence of routine and the constant demand of schoolwork — at least for the next three months.
You can't go through your entire break wanting to have a summer romance or fling. Those things just happen. Forcefully trying to create some kind of connection with another person usually turns out disastrous for both. Summer romances are different because they happen by chance. They catch you in your most carefree state, caught up in the haze of the season.
But if you're looking for opportunities to encounter a possible summer fling, your best bet would probably be at a party. Parties are the best places to meet people. Everyone is carefree and having fun, so this is the easiest place to make a connection.
Say you're at a bonfire on a hot summer night, chilling with a few of your friends and the friends of those friends. You end up sitting by an engaging and interesting stranger. So, of course, you make small talk. Small talk turns into talking about your interests, and that, in turn, shifts into talking about what you have in common. Thus, a connection is made.
This connection, fueled by the lightness of the season and the extra time you have from not being in school, sparks the flame that is the beginning of a fling. The extra time means you are able to easily balance a romance with the rest of your life because you aren't too busy. Summer romances are wrapped up in themselves, and you forget come August, your responsibilities return.
This is the downfall of the fling. For most, routine will eventually catch up with you. At the start of the new semester, you'll both go back to your busy schedules and expectations, and what you based your summer romance around will slowly fade to a memory of that free, passionate feeling until the hazy heat of the next summer rolls around once again.


It's the perfect crime, meaning it wasn't their fault. When Adam goes missing an investigation begins to unfold that targets exactly the wrong person. Those really responsible just need to keep their mouths shut until it all blows over.
In Dennis Kelly's 'DNA' a group of teenagers try to see if Adam really will do anything to be a part of their little gang. But nothing turns out as they'd planned. Sure, they meant everything else they did to him – and have done for years – but they didn't mean to make him fall through the old grate at the top of the hill. It's dark, and it's a long way down. Adam may be missing, but unlike everyone else at school, they know he won't be coming back.
Through the weeks that follow we watch as the lives of the eleven teens involved begin to twist out of shape. Leah notices that somehow everyone is happier, somehow. Whether repentant or relieved the group begins to change after what they did to Adam. Each member of the eleven-strong cast delights and unnerves their audience in equal measure, with a notably powerful performance from Daniel J Kenton as the disturbingly pragmatic Phil.
The Young REP has always had a reputation for staging brilliant productions and nurturing local talent, and DNA is as much a testament to that as anything else. But what is also wonderful to see is how many young people filled the audience. And not just school groups. The REP proves again to be one of those theatres with a seemingly effortless ability to encourage and engage young people in theatre, especially with this production of DNA.
My one criticism of the piece is that it is played with too much comedy. DNA has its moments of laughter but sometimes this is stretched too far, often to the point where the truth of the words is lost. Though it entertains audiences it causes key monologues, plot shifts, and whole character developments to lose their weight. Ultimately many grittier aspects end up being undercut by the comedy flaring up around them.
What began to redeem the push for laughs, however, were the technical aspects of the production. We're dragged kicking and screaming through the teenager's ordeal through the vivid projections, stark lighting, and scratching audio that link it all together. Lighting designer Simon Bond, sound/AV designer Andy Gregory, and AV photographer Hannah Kelly encapsulate not only the enormously varied settings of the piece but also draw out the fear and guilt present in every character, and thrust it onto the audience too.
'DNA' is showing at The Birmingham REP until 7th April.
Incredible performance! Went with my school and it was absolutely fantastic! The cast were phenomenal, especially Phil and Leah's characters. loved it so much that me and my friend came to watch again. Deserves a strong 5 STARS!!!!!!!


Begin by being in an experimental mood and a meta frame of mind.
Post a series of photographs called "Safeway Park Lines" on Instagram.
Put the new photo of the screen image of your Instagram post of your photograph on Facebook.
Proceed to quickly and methodically repeat the process over and over, alternating between Instagram and Facebook (e.g., Instagram screen of FB screen of Instagram screen of FB screen of Instagram screen of FB screen of Instagram screen of FB screen of Instagram screen of "Safeway Park Line" photograph).
Be prepared to annoy all your "friends" on Instagram and Facebook with lots of posts that all look rather alike. Wonder if anyone can tell that, instead of posting images that are complete and ready for consumption, you are attempting to use the very act of posting (and re-posting) as a method for creating images.
Finally stop around the twenty-first post. You notice that the changes between images are not exactly linear and that an oddly blurry, yet bright, area started growing in the center as each image became more distorted.
Be reminded of an early experiment with tape by musician Steve Reich, of two stereos facing each other, with the first playing a tape recording and the second recording the tape recording and then switching, so that the second plays the recording of the first while the first then records (and repeat, back and forth, again and again, until the original recording slowly turns into white noise).


January 2015 Friends of the Planetarium Programming: LASERS!
In December of 2013, the United Nations General Assembly proclaimed 2015 as the International Year of Light and Light-Based Technologies (IYL2015.) To kick off the special events of the Year of Light, the Friends of Arlington's David M. Brown Planetarium is focusing its January weekend on LASERS! All events on the weekend of January 16 through 18, 2015, will include special presentations, short videos, and displays that highlight the uses of lasers in astronomy and geophysics. There will also be free gifts, door prizes, and an amazing laser display on the dome! Come join in the fun and help us kick off the International Year of Light!
Screening of the full-dome digital program Supervolcanoes, followed by an Interactive Star Talk (for adults & children five and older).
Screening of the digital program Magic Tree House® Space Mission.
To download a colorful 8x10 poster advertising this month's weekend, click here [3 MB jpg].


In the latter part of the 19th century, F. H. A. Scrivener produced an edition of the Greek New Testament which reflects the Textus Receptus underlying the English Authorised Version.
F. H. A. Scrivener (1813-1891) attempted to reproduce as exactly as possible the Greek text which underlies the Authorised Version of 1611. However, the AV was not translated from any one printed edition of the Greek text. The AV translators relied heavily upon the work of William Tyndale and other editions of the English Bible. Thus there were places in which it is unclear what the Greek basis of the New Testament was. Scrivener in his reconstructed and edited text used as his starting point the Beza edition of 1598, identifying the places where the English text had different readings from the Greek. He examined eighteen editions of the Textus Receptus to find the correct Greek rendering, and made the changes to his Greek text. When he finished he had produced an edition of the Greek New Testament which more closely underlies the text of the AV than any one edition of the Textus Receptus.


Have a migraine kind headache that will not go away even with can.
Dizziness is what caused all the convert to body.
Carrots, broccoli, salads, green beans and zucchini amounts of energy all the time, the sugar must.


PALO ALTO, Calif., February 10, 2015 — HP today released results of a security testingstudy revealing that owners of Internet-connected home security systems may not be the only ones monitoring their homes. The study found that 100 percent of the studied devices used in home security contain significant vulnerabilities, including password security, encryption and authentication issues.
Home security systems, such as video cameras and motion detectors, have gained popularity as they have joined the booming Internet of Things (IoT) market and have grown in convenience. Gartner, Inc. forecasts that 4.9 billion connected things will be in use in 2015, up 30 percent from 2014, and will reach 25 billion by 2020.(1) The new HP study reveals how ill-equipped the market is from a security standpoint for the magnitude of growth expected around IoT.
Manufacturers are quickly bringing to market connected security systems that deliver remote monitoring capabilities. The network connectivity and access necessary for remote monitoring presents new security concerns that did not exist for the previous generation of systems that have no internet connectivity.
The HP study questions whether connected security devices actually make our homes safer or put them at more risk by providing easier electronic access via insecure IoT products. HP leveraged HP Fortify on Demand to assess 10 home security IoT devices along with their cloud and mobile application components, uncovering that none of the systems required the use of a strong password and 100 percent of the systems failed to offer two-factor authentication.
Insufficient authorization: All systems that included their cloud-based web interfaces and mobile interfaces failed to require passwords of sufficient complexity and length with most only requiring a six character alphanumeric password. All systems also lacked the ability to lock out accounts after a certain number of failed attempts.
Insecure Interfaces: All cloud-based web interfaces tested exhibited security concerns enabling a potential attacker to gain account access through account harvesting which uses three application flaws; account enumeration, weak password policy and lack of account lockout. Similarly five of the ten systems tested exhibited account harvesting concerns with their mobile application interface exposing consumers to similar risks.
Privacy Concerns: All systems collected some form of personal information such as name, address, date of birth, phone number and even credit card numbers. Exposure of this personal information is of concern given the account harvesting issues across all systems. It is also worth noting that the use of video is a key feature of many home security systems with viewing available via mobile applications and cloud-based web interfaces. The privacy of video images from inside the home becomes an added concern.
Lack of transport encryption: While all systems implemented transport encryption such as SSL/TLS, many of the cloud connections remain vulnerable to attacks (e.g. POODLE attack). The importance of properly configured transport encryption is especially important since security is a primary function of these systems.
As IoT product manufacturers work to incorporate much needed security measures, consumers are urged to consider security when choosing a monitoring system for their home. Implementing secure home networks before adding insecure IoT devices, instituting complex passwords, account lockouts and two-factor authentication are only a few measures consumers can take to make their IoT experience more secure. Legislators are also getting involved, with the U.S. Federal Trade Commission releasing a recent report analyzing the balance between security and privacy concerns with development of the IoT devices.
For more information, visit the first report in this IoT series, 2014 HP Internet of Things Research Study, which reviews the security of the top 10 most common IoT devices. Additionally, the most recent HP Security Briefing, Episode 20: The Internet of Things: A Security Overview looks at how the advent of millions of connected devices affects network security from a practical standpoint.
Conducted by HP Fortify and leveraging HP Fortify on Demand, HP's Home Security Systems study tested 10 of the most commonly used home security IoT devices for vulnerabilities using standard security testing techniques that combined manual testing along with the use of automated tools. Devices and their components were assessed based on the OWASP Internet of Things Top 10 and the specific vulnerabilities associated with each top 10 category.
The resulting data and percentages in this report were drawn from the 10 IoT systems tested. Given the popularity and similarity among the 10 devices, HP Fortify believes the results provide a good indicator of where the market currently stands as it relates to security and the Internet of Things.
Additional information about application security and further details resulting from the study are available at hp.com/go/fortifyresearch/iot.
Join HP Software on Linkedin and follow @HPSoftware on Twitter. To learn more about HP Fortify and HP Enterprise Security Products on Twitter, please follow @HPsecurity and join HP Enterprise Security on Linkedin.
(1) Gartner, Press Release, "Gartner Says 4.9 Billion Connected "Things" Will Be in Use in 2015" November 2014. http://www.gartner.com/newsroom/id/2905717.


text:
The General Dutch Union of the Building and Wood Industries (, ANBH) was a trade union representing workers in the construction and wood industries in the Netherlands.

The union was founded on 1 January 1970, when the General Dutch Construction Union merged with the General Industrial Union of Furniture Makers and Woodworkers.  Like both its predecessors, it affiliated to the Dutch Confederation of Trade Unions (NVV).  By 1980, the union had 95,090 members, of whom, 89% worked in construction, and the remainder in woodworking and furniture making.

The union began working closely with the Dutch Catholic Union of the Building and Wood Industries, forming a loose federation in 1973, and a more formal one in 1976, through which both unions then channeled all their activities.  On 1 January 1982, the two unions merged, to form the Construction and Wood Union.  Throughout its existence, it was led by Bram Buijs.

References

Building and construction trade unions
Trade unions established in 1970
Trade unions disestablished in 1981
Trade unions in the Netherlands


I recently sent a lb of 7-8 count shrimp, lb jumbo scallops, lb blue mussels, and lobster bisque to my sister. She's only eaten the bisque this far, which was described as delicious. Her kids will join her for the rest in the next week, but everything was delivered perfectly, and we are both extremely happy. The service was great. I won't hesitate ordering with Oceanside again. You shouldn't either. Mike. Nashville, Tn.
These were easy to prepare and even easier to eat!
This was a perfect purchase. My guests throughly enjoyed their meals especially the shrimp. These large shrimp are not available where I live. When I searched and found Oceanside and made this purchase the results more than I expected Thanks so much!
Colossal Prawns 6/8 Ct. 2 lb.
I purchased 4lbs of Colossal Prawns. The shipping, notifications and delivery were seamless and perfect. The prawns LOOK great, we have not eaten them yet, as we are saving them for Christmas Day. While the price per pound was very competitive...when I added the $35.00 delivery price to my $19/lb price...it drives the price to $27.74 per pound. I probably won't justify that kind of expense again. Unless the prawns are absolutely out of this world. I will try to find a similar product locally at a more competitive "total" price per pound.
Colossal Prawns 6/8 Ct. 1 lb.


The beginning of the year calls for the convening of state legislatures, which in turn brings people into the streets to protest. It began with students in Florida calling on their representatives in government to pass some real, common sense gun laws. It then turned to the streets of West Virginia in late February, lasting until the early weeks of March, when teachers walked out of their classrooms to protest their low wages and low funding within their classrooms.
The teacher protests did not stop in West Virginia; that was just the start. Since the teacher walkouts of West Virginia, teacher walkouts in Oklahoma, Kentucky, Colorado, and, most recently, Arizona have occurred. These teachers, like those in West Virginia, have called for their state legislatures to pass a budget that includes teacher raises and more funding for the teachers in the classrooms because they are paying for basic classroom supplies out of their own pocket.
This naturally leads us to look to how Wyoming ranks nationally in its education funding in light of its recent economic downturn and proposed education funding cuts to examine if there will be a teacher walkout in the state of Wyoming anytime soon. Although the state legislature is not convened, the teachers of Wyoming can go to the streets to voice their opinion and go back to Cheyenne early next year so the legislature gets to literally hear their voices.
According to Census Bureau data from 2015, Wyoming ranks seventh nationally in both spending per pupil and salaries and wages per pupil at $16,055 annually and $9,495 annually, respectively; it also ranks ninth among the fifty states and the District of Columbia for benefits per pupil at $4,041 annually.
Although Wyoming may rank highly in all of these categories, it is not a rarity to hear of a teacher in the state having to buy supplies for their classroom. Just walk into a majority of Kelly Walsh High School classrooms and you will not be able to find the most basic of products: Kleenex. This supply may sound simple and cheap, but with schools having kids in close proximities to each other, sickness spreads quickly, and the most common of those is a cold; with all of the Kleenex being used due to colds, the boxes purchased by a teacher add up quickly, especially with their meager salary, compared to other nations worldwide.
The Brookings Institution conducted a study of American teachers' pay compared to other nations around the globe and found that while the United States does not have the lowest average salary for teachers, there is a major gap between them and at least eighteen other nations worldwide.
The federal government spends so much on their military, yet neglect to pay their teachers for the hard work they do day in and day out. So, if you are a teacher, do not be afraid to walk out and stand up for your rights and livelihood, and if you are a student or parent: stand with your teachers and do not be quick to judge if they do choose to protest their low wages because they work hard to educate you and your children to make their future bright and the future of our great nation even brighter.


In a surprising merging of products, the Solar Energy Bucket serves as a multifunctional tool for anyone who likes to rough it.
At first glance it appears to be a simple water bucket, but turn it upside down and you'll see a small solar panel which harnesses the sun's energy during the day.
The stored energy can then be used to power the built-in light or even gently heat the water.
I read this great article and found it very interesting, thought it might be something for you. The article is called The Solar Energy Bucket and is located at https://grendz.com/pin/319/.


RALEIGH TheN.C. Department of Transportationplans to begin replacing culverts on U.S. Highway 311 at Sycamore Creek and Bob's Branch in Randolph County on Monday, July 13. Crews will remove and replace the existing culverts, one at a time, detouring traffic.
The existing culverts were structurally deficient,meaning that while the culverts were safe, they were in relatively poor condition, or had insufficient load-carrying capacity. The insufficient load capacity could be due to age, the original design or to wear and tear.
There will be a signed detour using Interstate 74 to Cedar Square Road.Motorists are advised to use caution while traveling in the area, stay alert and obey the posted speed limit.
Construction for the project is scheduled to be complete in November with traffic returning to normal, while crews will continue adding vegetation and other work around the area with the overall completion date of May 2016.
Country Boy Landscapingof Harmony is the contractor for the $707,800 project.


The Government has announced that they will create a new tax-free children's savings account following the end of Child Trust Fund (CTF) eligibility.
The Government intends the new accounts to be available by autumn 2011.
there will be no Government contributions into the account.
The new account, described as a 'Junior ISA', will offer parents a simple and tax free way to save for their child's future.
Eligibility for the new account will be backdated, to ensure that no child born after the end of CTF eligibility will miss out on the chance to have one of the accounts. There will be no CTF eligibility for children born from January 2011.


A time-sensitive, single-session, expert consultation for parents when their child is facing any stressful life event. Often done by phone, the consultation serves parents of any age child.
Stressful life events—everything from putting a favorite pet down, to a military deployment, to a life-changing diagnosis—happen to every family. And when they do, it can be difficult to know how to talk to your children about it.
Talking Points is a free, one-hour, time-sensitive consultation for parents dealing with a stressful life event. In a single session, a trained professional will talk you through what behaviors to expect from your child, when to worry, and what you can say and do to best support them, all based on their age and stage of development. At the end of the session, you will be equipped with the words, strategies, and confidence you need to talk through even the most difficult changes in your family.
A mother of daughters 11 and 13 faces her husband's final days at home with hospice care. She worries about how she can support her children.
The family's twelve-year-old beloved golden retriever needs to be euthanized. How to tell the five -and eight-year-old children.
Nana has dementia. Knowing how much to share, when and what words to use to a ten-year-old.
A young Dad takes a nap and never wakes up. His 5th-grade son finds him.
A father of two young girls is being deployed for eight months.
A Dad suffers from late-stage pancreatic cancer. How does the Mom tell her 6- and 8-year-old children he is entering hospice care?
Preparing a four-year-old (and her anxious mom!) for her first pre-school experience.
An estranged Dad, not living at home, died of suicide and the kids haven't been told.
Each session includes a one-hour consultation with a trusted, trained professional.
Sessions can take place in person, on the phone, or by Skype.
This program is provided at no cost.