text:
550 Giant Scale RC Model Airplane Plans Templates, Bombers Military PDF DVD
135+ JETEX Scale Model Airplane Plans, Templates Bombers Jets Glider PDF
The Shadow, + The Whistler, 550 SHOWS, Old Time Radio, OTR, Suspense DVD
Dragnet, Dick Tracy, 443 Shows, ALL Known Episodes, Old Time Radio, OTR DVD
The Whistler + Mysterious Traveler, ALL 601 Shows, Old Time Radio, OTR, DVD
Home - Parks and Fairs - 1964 NYC World's Fair and Unisphere Construction Films
1964 NYC World's Fair and Unisphere Construction Films
Take a trip back in time to the 1964 New York World's Fair. Watch how the Unisphere was conceptualized and built, see the sights.
The 1964 Worlds Fair, New York, DVD Film Collection
This DVD takes you back to the year 1964. You will learn how the World's Fair was set up and planned, with much footage of the famed Unisphere. If you were there, or a parent was, this DVD will let you relive memories of a different time. This culturally significant collection is perfect for educators, students and fans alike. Makes a great gift.
The 1964/1965 New York World's Fair was the third major World's Fair to be held in New York City. The site is Flushing Meadows Corona Park in the Borough of Queens and held both the 1964/1965 New York World's Fair and the 1939/1940 New York World's Fair. Preceding these Fairs is the 1853-54, New York's World's Fair, called the Crystal Palace Exhibition, located on the site of Bryant Park in the borough of Manhattan, New York City. The 1964/1965 New York World's Fair opened on April 22, 1964, and ran for two six-month seasons concluding on October 17, 1965. The World's Fair took place without sanctioning from the Bureau of International Expositions, the only one to do so.
It was the largest World's Fair to be held in the United States, occupying nearly a square mile (2.6 km²) of land. Hailing itself as a "Universal and International" exposition, the Fair's theme was "Peace Through Understanding," dedicated to "Man's Achievement on a Shrinking Globe in an Expanding Universe." The theme was symbolized by a twelve-story high, stainless-steel model of the earth called Unisphere. United States corporations dominated the exposition as exhibitors at the expense of international participation. The Fair is best remembered as a showcase of mid-twentieth century American corporate culture. The nascent Space Age, with its vista of promise was well-covered by the exhibits. More than fifty-one million people attended the Fair, but this was less than the hoped-for seventy million.
We also sell a DVD collection that has very rare footage of the 1939 NY World's Fair. Please see our other items to view that collection.
This DVD has about 1 hour and 45 minutes worth of footage and comes complete with an interactive menu. A list of films contained in this collection is as follows:
1964 New York Worlds Fair Report
Preparation, planning and construction for the Fair, under the imperious direction of Robert Moses. An overview to transform Flushing Meadow into the World's Fair of 1965 is showcased here. Quite interesting background information on how much time is needed to put one of these babies on. Also of fascination, this being 1961, is how many people show up for a bridge opening.
Sound, B&W, 27:00
New York World's Fair 1964
(1) New York World's Fair, symbolized by Unisphere, many bldgs yet to be completed, theme "peace through understanding" with 58 nations to participate, on same site as 1939 Fair (2) Grauman's Chinese Theater - Haley Mills leaves handprints (partial newsreel).
Sound, B&W, 2:31
The Unisphere, Biggest on Earth 1964
Designing and building the symbol of the 1964 New York World's Fair. This film is a wonderful tribute to a perhaps overlooked monument from the enthusiastic early 1960's. You rarely see the unisphere unless it is the backdrop for an action film or science fiction. A pity. This film is a fascinating look at the conceptualization and creation of a truly fine piece of sculpture.
Sound, Color, 14:10
To the Fair 1965
Provides a trip to the New York World's Fair of 1965, showing the various activities at the fair. It follows various groups of people during their day at the fair: a family of five; a couple from India; two women schoolteachers; three Boy Scouts who get separated from their troop; a pair of young women pursued by two very ardent male suitors; and -- the only one to whom I can relate -- a bespectacled nerd who drives to the fair across the water in his amphibious car just so he can listen to the out-of-tune musicians. The beatific look on his face as he cocks his head to take in the cacophony is priceless.
2 Part, Sound, B&W, 56:58
World's Fair Night Aerials
For the amount of second-hand knowledge about the 64-65 World's Fair that I've come across, this film is a revelation. The fountains and New York Pavilion look especially magnificent, as does Shea Stadium (it's so clean and new!). In just four minutes, you will see the scale and magic of the Fair from the air! The camera is shaky, as you'd expect from aerial footage shot with a telephoto lens.
Silent, Color, 4:19
DVD Menu Sampler:
Model: DVD-TCA-J09
1939-1940 New York Word's Fair with Medicus Films, 4 DVD's
300+ Sherlock Holmes Audiobooks, and OTR Radio Drama Shows DVD
The Korean War, A Documentary and Propaganda History
Sergeant Preston, Challenge of the Yukon, 776 Episodes, + bonus OTR MP3 DVD
The General Magazine, Avalon Hill, All 200 Vintage issues with extras DVD
Learn How To Speak Spanish, Fast Foreign Language Training Course, DVD


An influential hypothesis in family research is that having many economic resources decreases women's and increases men's rate of entering a union. A more recent hypothesis is that the strength of the association between economic resources and union formation has weakened over time, given decreasing role differentiation by gender. Rather than looking at the timing of union formation, we look at its non-occurrence. Using the Netherlands Kinship Panel Study, we find that, as predicted, high-resource women and low-resource men are more likely to remain single. Contrary to predictions, university-educated men are also more likely to remain single. The association between economic resources and permanent singlehood shows little change over time. Several explanations for this unexpected finding are discussed.


As if straight out of a sci-fi movie, rather a time travel movie, People are going bonkers over this incident that Massachusetts county. The riddle of how two twins born almost half an hour apart, being older than each other, is becoming a huge puzzle. However, on further research, the incidence lays bare on a simple Time calculation. On a fine Sunday Morning, Emily and Seth Peterson, welcomed two twin boys into their family. One named Samuel and the other Ronan. However, the intricate puzzle comes to this – Although Samuel was born before Ronan, Ronan ended up being the older twin. And the same is being reflected in the respective birth certificates.
The official reasoning behind this, is the following explanation. Daylight Savings Time, tricked the mathematicians and general public with this conundrum. Take this- Samuel was born at 1:39 AM on Sunday, November 6th, while Ronan took 31 minutes longer. Now, usually the shift of Daylight Savings Time happens at 2 AM. This meant that Ronans birth adjusted for savings, came at 1:10 AM instead of 2:10 AM. This made him elder as well. Thus, making both of the babies older than each other!
"I said earlier that night that they were either going to be born on two different days or the time change was going to come into play," said Seth, who is trooper with the Massachusetts State Police. Cape Cod Hospital Maternity nurse, Deb Totten, said it was the first time she has ever seen this happen in more than 40 years of nursing!


text:
Be Elvis at world record attempt at Harrah's Cherokee
Carol Motsinger
cmotsinger@citizen-times.com
What's the plural of Elvis?
Elvises? Elvi?
No matter what, plural doesn't even seem to cover the more than a thousand Elvis Presley impersonators expected to gather at Harrah's Cherokee Casino Resort Saturday.
That's a whole lot of Kings of Rock 'n' Roll.
The first 1,400 ticket-holding guests who arrive in the event center by 6:30 p.m. will receive a free Elvis costume.
The largest gathering of Elvis impersonators was 645 in 2010 at the Aria Hotel in Las Vegas,
It's part of the casino's Ultimate Elvis Tribute Artist Competition festivities, that start at 6:30 p.m. Thursday with Parade of Kings on Casino Floor.
The contestants will walk through the casino and snap photos with fans at designated locations.
At 7:30 p.m., the Elvis impersonators will perform in a showcase. It's free and standing room only.
On Friday, the contest kicks off with a preliminary round at 1 p.m. at Essence Lounge (reserved seating, ticketed and standing room only).
At 3 p.m., Sam Thompson, a former bodyguard and friend of Elvis, will be part of a question-and-answer session. He was a member of the "Memphis Mafia," the nickname given to Elvis's personal entourage, and also the brother of Elvis's girlfriend, Linda Thompson.
The contest continues at 4 p.m.
The Parade of Kings returns to the Casino Floor at 7 p.m. Saturday, and the top five contestants will compete for the championship at 7:30 p.m.
Purchase tickets for the finals by calling Ticketmaster at 1-800-745-3000 or by visiting www.ticketmaster.com.
For more, visit the website.

redpajama_set_name: RedPajamaCommonCrawl


text:
Jamie Randolph Benn, född 18 juli 1989 i Victoria, British Columbia, är en kanadensisk professionell ishockeyspelare som spelar för det amerikanska ishockeylaget Dallas Stars i NHL.

Biografi
Benn valdes av Dallas Stars som 129:e spelare totalt i 2007 års NHL-draft.

Den 19 september 2013 utsågs Benn till lagkapten för Stars.

2014 var Benn med och vann guld med det kanadensiska landslaget under de Olympiska vinterspelen Sotji.

2013–14
Säsongen 2013–14 valdes Benn till NHL:s First All-Star Team (som vänsterforward) efter att ha gjort 79 poäng på 81 matcher.

2014–15
Säsongen 2014–15 vann Benn Art Ross Trophy som NHL:s främste poängplockare under grundserien efter att ha spelat ihop totalt 87 poäng, en poäng mer än New York Islanders center John Tavares. Den 11 april 2015, i Dallas Stars sista grundseriematch för säsongen (på hemmarink mot Nashville Predators), registrerades Benn för sammanlagt fyra poäng (tre mål och en målgivande passning). Hans sista poäng, en andrahandsassist på ett mål av lagkamraten Cody Eakin med 8.5 sekunder kvar av matchen, gjorde att han övertog ledningen i poängligan från Tavares. Hade Benn och Tavares slutat på delad första plats poängligan (med 86 poäng vardera) så hade Tavares vunnit Art Ross Trophy eftersom han gjort fler mål under säsongen (38 gentemot Benns 35). Under säsongens tre sista matcher (mot San Jose Sharks, Anaheim Ducks och Nashville Predators) gjorde Benn 10 poäng (fem mål och fem assists).

2015–16
Nästkommande säsong, 2015–16, slutade Benn på andra plats i NHL:s poängliga efter att ha spelat ihop 89 poäng, dock hela 17 poäng bakom Chicago Blackhawks högerforward Patrick Kane.

Personligt
Jamie Benn är yngre bror till Jordie Benn som spelar som back för Vancouver Canucks.

Statistik

Klubbkarriär

Internationellt

Referenser

Noter

Externa länkar
Jamie Benn på nhl.com
Jamie Benn på hockey-reference.com

Födda 1989
Kanadensiska ishockeyspelare
Levande personer
Män
Spelare i Dallas Stars
Personer från Victoria, British Columbia
Idrottare från British Columbia
Kanadensiska olympiska guldmedaljörer
Olympiska guldmedaljörer 2014
Tävlande vid olympiska vinterspelen 2014 från Kanada
Tävlande i ishockey vid olympiska vinterspelen 2014
Spelare i Kelowna Rockets
Vinnare av Art Ross Trophy
Spelare valda i NHL Entry Draft 2007
Lagkaptener i Dallas Stars
Spelare valda av Dallas Stars i NHL Entry Draft
Spelare som har spelat minst 1000 matcher i National Hockey League

redpajama_set_name: RedPajamaWikipedia


text:
\section{Introduction}
Gravitational waves (GWs) are ripples in the curvature of space and time which propagates at the speed of light. They are the mechanism by which the field of a changing mass distribution propagates, similar with the electromagnetic (EM) waves which represent the way by which a changing electric charge distribution tells remote observer that the source is varied \cite{LB}.

During their travel, the GWs squesh and stretch spacetime in the plane perpendicular to their direction of propagation. They however induce very tiny deformations: even very strong GWs from astrophysical sources are expected to perform relative length variations of order $10^{-21}$ \cite{EB}. Cabral and Lobo \cite{CL} showed that, in principle, the passage of a GW in a region with EM fields will have a measurable effect that may be computed studying Maxwell's equations on the perturbed background (the Minkowski space) of a GW. One obtains oscillations of the electric field which is aligned with the direction of the GW propagation. Even if in the absence of the GW the field was static, during the passage of the wave the electric field will become time-dependent, oscillating with the same frequency as the GW. Therefore, EM waves propagating along the same direction of the GW will be generated \cite{CL}.

Goswami et al. \cite{GMP} have shown that GWs propagate through ideal fluids without dissipation, but a nonzero shear viscosity will dissipate them. They calculate the dissipation of GW150914 \cite{BA} which propagated over a distance of 410 Mpc through the dissipative fluid and tested the data with the theoretical predictions. In their opinion, future observation of GWs at LIGO will give the possibility of detecting the viscosity of dark matter and dark energy.

As spacetime fluctuations that usually do not reflect from any matter surface, in the brane-world scenario zero-mode gravitons are trapped on a brane due to a nonlinear warping effect \cite{GM} and so Gogberashvili and Midodashvili expressed a radical possibility that GW151014 signal was caused by a short duration source in the brane-world scenario \cite{RS}. Liu et al. \cite{ML} check the Equivalence Principle (EP) about GW transient GW150914 associated with weak EM signal GW150914-GBM \cite{VC}, observed by Gamma-ray Burst Monitor. Their results show that the violation of the EP is quite insensitive to the location of the source. If the EP is right, initial gravitons will arrive the Earth (at Livingston and Hanford) in the same time. Caldwell, Devulder and Maksimova \cite{CDM} studied the general phenomenon of the conversion of a GW into a stationary gauge field. They show that GWs transform into tensor waves of a gauge field, similar with their conversion into an EM wave and back, when propagating through a stationary magnetic field. Lasky et al.\cite{PL} studied the so-called ''GW memory''- a permanent displacement of spacetime that comes from relativistic strong-field effects. They showed how the accumulation of several measurements will allow the detection of that effect.

 In the weak gravitational field limit, one can expand Einstein's field equations $G_{ab} = 8\pi T_{ab}$ in powers of $h_{ab}$, with
  \begin{equation}
  g_{ab} = \eta_{ab} + h_{ab},~~~|h_{ab}| << 1
 \label{1.1}
 \end{equation}
using a coordinate frame where (1.1) holds ($a, b$ run from 0 to 3, with $x^{0} = t,~ x^{1} = x,~ x^{2} = y,~x^{3} = z$) \cite{MTW, BS, EG, PG}. This is the linearized theory of gravity or tensor-field theory of gravity in flat spacetime. $h_{ab}$ in (1.1) is taken to be a perturbation of the flat spacetime caused, for example, by GWs, which are assumed to be plane waves at large distances from the source, as compared to their wavelength \cite{EG}. Let us mention that $h_{ab}$ is not a tensor. Nevertheless, it is convenient to think of a slightly curved spacetime as a flat spacetime with a ''tensor'' $h_{ab}$ defined on it \cite{BS}. One may therefore express, for instance, the curvature tensor $R^{a}_{~bcd}$ in terms of $h_{ab}$.

Poplawski \cite{NP} showed that real GWs may differ from solutions of the linearized field equations due to the fact that the two polarization modes are not independent and the monochromatic GW loses its periodic character because of the nonlinearity of Einstein's equations.

Pazouli and Tsagas \cite{PT} start from the fully nonlinear Einstein's equations before reducing them to their linear and second-order limits (around a chosen background), by employing the covariant $1+3$ splitting of the Weyl tensor for to describe the GWs instead of perturbing the background metric (see also \cite{RJS}). Their second order study suggest that Weyl-curvature distorsions could dictate the large-scale density perturbations. The key kinematical parameter is the shear tensor (in a $3+1$ covariant decomposition of the 4-velocity gradient) that is directly related to GWs in perturbed FLRW cosmologies.

  Usually, cosmologists take the linearized version of Einstein's equations for to deal with GWs. Even for the GW150914 event one assumes the linearized gravitational equations and implicitly the quadrupole formula may be used for the two BHs merger. In that case, strong gravity plays an important role and, therefore, the linear approximation should be used with caution. That is the main reason  which motivate us to work with the fully nonlinear Einstein's equations, to get the exact solutions and make approximations at a later stage of calculations. Therefore, we intend in this paper to follow Pazouli and Tsagas approach and to look for an exact solution of Einstein's equations that represents a nonlinear GW. We work firstly in Cartesian coordinates and seek a finite perturbation in spacetime, propagating with the velocity of light. We stress that that perturbation plays the role of a source of curvature and does not move in a given background. In section 2 we  compute the components of the source stress tensor in a spacetime which depends on a constant length, chosen to be of the order of the Planck length. The source fluid is anisotropic and can be expressed in terms of a null 4-vector and has negative energy density and pressure. Section 3 treats the same spacetime but in double-null coordinates $(v,~u)$ where the only nonzero component of the stress tensor is $T^{u}_{~v}$. Timelike and null geodesics are investigated in section 4. Finally, we discuss the implications of our results in section 5.

Throughout the paper we set $G = c = \hbar = 1$, unless otherwise specified.

\section{Nonlinear wave in Cartesian coordinates}
Prior to look for a suitable spacetime of a nonlinear wave as an exact solution of the Einstein field equations, let us comment a little on the Eq. (1.1). Firstly we notice that the condition $|h_{ab}| << 1$ refers not to a weak field but to a weak (gravitational) potential. But what does ''1'' represent above? It is related to the background geometry, namely the Minkowski spacetime. However, Minkowski space is flat, which means no gravity. In other words, the ''weak'' perturbation $h_{ab}$ is compared to a background with zero gravity. Therefore, it turns out to be ambiguous to claim that a perturbation is small w.r.t. zero. The way out, in our opinion, is that the Minkowski space corresponds not to lack of gravity but to a constant gravitational potential, which is $c^{2} = 1$, where $c$ is the velocity of light in vacuo, so that a weak potential $h_{ab}$ means a potential much less than $c^{2}$. Put it differently, flat space concerns physics at constant gravitational potential, rendering it more Machian. That is valid even classically, i.e. the Newton potential at a distance $r$ from a point mass $m$ is not $-mG/r$ but $c^{2} - mG/r$. That will not change, of course, the equation of motion of a test particle but, however, it changes the sign of the potential.

A similar situation arises when we consider ripples on the surface of a quiet lake. When we say ''small ripples'' we must add: w.r.t. what background? If the background means ''no ripples'' it is a nonsense to add the adjective ''small''. Therefore, the GWs are considered to be ''weak perturbations'' because from the very beginning they are taken to be ''weak''. So, it is not useless to look for strong GWs, to whom the linear approximation will no longer be valid. The fact that they are not observed experimentally is not a flaw. For example, Dark Energy and Dark Matter are not perturbations to some background and, nevertheless, they are still not observed experimentally.

We look for an exact plane-wave solution of Einstein's equations in the form given by Misner, Thorne and Wheeler \cite{MTW} (see also \cite{BS})
   \begin{equation}
  ds^{2} = - dt^{2} + \Psi^{2}(e^{-2\Phi} dx^{2} + e^{2\Phi} dy^{2}) + dz^{2},
 \label{2.1}
 \end{equation}
where $\Psi = \Psi(t-z),~\Phi = \Phi(t-z)$ are ''the background factor'' and ''the wave factor'', respectively. The linearized theory corresponds to $\Psi = 1$ and $\Phi << 1$. Then the metric (2.1) takes the form
   \begin{equation}
  ds^{2} = - dt^{2} + (1 - 2\Phi) dx^{2} + (1 + 2\Phi) dy^{2} + dz^{2},
 \label{2.2}
 \end{equation}
which is a plane wave propagating along the z - direction. It represents a perturbation of the Minkowski space. The line-element (2.2) is a solution of Einstein's field equations in the linear approximation in the so called (transverse-traceless) Lorentz gauge \cite{CL}.

Motivated by our purpose to look for an exact solution of the fully nonlinear Einstein's equations, we introduce the following nonlinear gravitational wave
   \begin{equation}
  ds^{2} = - dt^{2} + e^{-\frac{b}{\sqrt{(t - z)^{2} + b^{2}}}} dx^{2} + e^{\frac{b}{\sqrt{(t - z)^{2} + b^{2}}}} dy^{2} + dz^{2},
 \label{2.3}
 \end{equation}
where $b$ is a constant length that will be considered of the order of the Planck length. When $t - z >> b$, we may approximate $e^{-2\Phi} \approx 1 - 2\Phi,~ e^{2\Phi} \approx 1 + 2\Phi ,(\Phi = b/(2\sqrt{(t - z)^{2} + b^{2}})$) and (2.3) gives us (2.2), i.e. the linearized version. Our purpose now is to find what stress tensor $T_{ab}$ we need on the r.h.s of the Einstein equations in order (2.3) to be an exact solution. One finds that the only nonzero components of $T_{ab}$ are
   \begin{equation}
	8\pi \rho = 8\pi p_{z} = -8 \pi T^{t}_{~t} = 8 \pi T^{t}_{~z} = -8 \pi T^{z}_{~t} = -\frac{b^{2} (t - z)^{2}}{2[(t - z)^{2} + b^{2}]^{3}},
 \label{2.4}
 \end{equation}
where $\rho$ is the energy density of the anisotropic source, $p_{z} = T^{z}_{~z}$ is the pressure along the z-direction and $T^{t}_{~z}$ is the energy flux along the z-axis. It is worth noting that the source is a null fluid which can be put in the form \footnote{$l_{a}$ may be also expressed in terms of the null retarded coordinate $v = t - z$ as $l_{a} = -\partial_{a} v = (-1, 0, 0, 1)$}.
   \begin{equation}
	T_{ab} = \rho l_{a} l_{b},
 \label{2.5}
 \end{equation}
with $l_{a} l^{a} = 0,~l^{a} = u^{a} + s^{a},~u^{a} = (1, 0, 0, 0),~s^{a} = (0, 0, 0, 1),~l^{a} = (1, 0, 0, 1),~u_{a} s^{a} = 0,~u_{a} u^{a} = -1,~s_{a} s^{a} = 1,~l_{a} u^{a} = -1,~l_{a} s^{a} = 1$. $u^{a}$ here is the velocity vector field of a static observer ($x,y,z - const.$), $s^{a}$ is a spacelike vector orthogonal to $u^{a}$ and $l^{a}$ is a null vector related to the flow of energy on the z-direction. Comparing to the general form of an anisotropic fluid with energy flux \cite{HC}
  \begin{equation}
  T_{ab} = (p_{\bot} + \rho) u_{a} u_{b} + p_{\bot} g_{ab} + (p_{z} - p_{\bot}) s_{a}s_{b} +  u_{a} q_{b} + u_{b} q_{a},
 \label{2.6}
 \end{equation}
we see that
  \begin{equation}
  p_{\bot} \equiv p_{x} = p_{y} = 0,~~~ q^{a} = - T^{a}_{~b}u^{b} - \rho u^{a},
 \label{2.7}
 \end{equation}
 where $q^{a} = (0, 0, 0, q^{z})$ is the energy flux 4-vector, with $q^{z} = T^{t}_{~z}$ the only nonzero component and $\sqrt{q^{a}q_{a}} = |\rho|$. The stress tensor may be also written in the form
  \begin{equation}
  T_{ab} = -\nabla_{a}\bar{\Phi} \nabla_{b}\bar{\Phi},~~~\bar{\Phi} = \Phi/\sqrt{4\pi}
 \label{2.8}
 \end{equation}
where $\nabla_{a}\bar{\Phi}$ is a null vector and $\bar{\Phi} = b/\sqrt{4\pi}(2\sqrt{(t - z)^{2} + b^{2}})$ could be interpreted as a scalar field with a ''wrong sign'' kinetic term \cite{HE,EH} and negative energy density (Ellis related his scalar field to a drainhole model but in Harris' approach the scalar field refers to a wormhole connecting two Reissner-Nordstrom (RN) black holes).

Let us observe that the energy density and pressure are negative but finite for any $t$ and $z$. They vanish at the null surface $t - z = 0$ and when $t - z \rightarrow \infty$. However, they acquire a minimum value $-1/108\pi b^{2}$ at $t - z = b/\sqrt{2}$. The density $\rho$ represents a lump of negative energy that moves on the z-direction with the speed of light. Far from the surface $t - z = 0$ (i.e. for $t - z >> b$) the energy density may be written as
 \begin{equation}
 \rho = -\frac{\hbar c}{16\pi (t-z)^{4}},
 \label{2.9}
 \end{equation}
where we put $b = l_{P}$, with $l_{P}$ - the Planck length. Noting that in that region $\rho$ (and $p_{z}$) have a structure which remind us of the Casimir energy. We also have that the scalar curvature and the Kretschmann scalar are vanishing in the spacetime (2.3).

How could we approach the null surface $t - z = 0$ , where the effects of the GW are stronger? To bring near that surface, we have to accelerate (of course, a huge acceleration is necessary), when the causal horizon $t - z = 0$ becomes a Rindler horizon for that accelerating observer \cite{MM}. The larger the acceleration, the closer to the null surface we are.

We consider now a congruence of static observers with the velocity vector field $u^{a} = (1, 0, 0, 0)$. All those observers are geodesic, namely the acceleration vector $a^{b} \equiv u^{a} \nabla_{a}u^{b} = 0$. In addition, the expansion scalar $\Theta \equiv  \nabla_{a}u^{a}$ also vanishes. However, the shear tensor
\begin{equation}
\sigma_{ab} = \frac{1}{2}(h_{~b}^{c} \nabla_{c} u_{a}+ h_{~a}^{c} \nabla_{c} u_{b})-\frac{1}{3} \Theta h_{ab}+ \frac{1}{2}(a_{a} u_{b} + a_{b} u_{a}),
\label{2.10}
\end{equation}
where $h_{ab} = g_{ab} + u_{a}u_{b}$ is the projection tensor onto the direction perpendicular to $u_{a}$, has the nonzero components
 \begin{equation}
 \sigma^{x}_{~x} = - \sigma^{y}_{~y}= \frac{b(t - z)}{2[(t - z)^{2} + b^{2}]^{3/2}}.
 \label{2.11}
 \end{equation}
In other words, the gravitational wave distorts the spacetime in the plane $xOy$, orthogonal to the direction of propagation. We also notice that the distortion changes sign beyond the surface $t - z = 0$.

We look now for the expression of the total energy flow $W$ measured by an observer laying at $z = z_{0} = const.$. It is given by \cite{HC}
 \begin{equation}
 W = \int{T^{a}_{~b}u^{b}n_{a}\sqrt{-\gamma}}dt~dx~dy
 \label{2.12}
 \end{equation}
 where $n^{a} = (0, 0, 0 , 1)$ is the unit normal to the surface of constant $z$, $\gamma_{ab} = g_{ab} - n_{a}n_{b}$ is the induced metric on that surface and $\gamma = det(\gamma_{ab}) = -1$. Eq. (2.12) yields
  \begin{equation}
 W = \frac{b^{2}}{16\pi}\int{\frac{(t - z_{0})^{2}}{[(t - z_{0})^{2} + b^{2}]^{3}}} dt~dx~dy
 \label{2.13}
 \end{equation}
If we change the variable of integration to $T = t - z_{0}$ and keeping in mind that
  \begin{equation}
 \int{\frac{T^{2}}{[T^{2} + b^{2}]^{3}}dT} = \frac{T (T^{2} - b^{2})}{8b^{2}(T^{2} + b^{2})^{2}} + \frac{1}{8b^{3}} arctan\frac{T}{b},
 \label{2.14}
 \end{equation}
one obtains, after an integration from $0$ to $\infty$, that $W = (c^{4}/G) \Delta x \Delta y/256b$, where $\Delta x , \Delta y$ gives the domains of integration for $x$ and $y$, respectively.

\section{Nonlinear wave in double-null coordinates}
Given the flat form of the $t - z$ plane from the metric (2.3) and its dependence on its retarded null coordinate only, we find more practical to use the double null coordinates $v = t -z$ and $u = t + z$. The line-element (2.3) becomes now
 \begin{equation}
  ds^{2} = - dv du + e^{-\frac{b}{\sqrt{v^{2} + b^{2}}}} dx^{2} + e^{\frac{b}{\sqrt{v^{2} + b^{2}}}} dy^{2} ,
 \label{3.1}
 \end{equation}
with $u$ - the advanced null coordinate. In this frame, the energy-momentum tensor of the source has a more simple form: there is only one nonzero component
 \begin{equation}
 8\pi T^{u}_{~v} = G^{u}_{~v} = \frac{b^{2}v^{2}}{(v^{2} + b^{2})^{3}},
 \label{3.2}
 \end{equation}
i. e. the energy flux on the null direction $u$ (we take $v$ to play the role of time and the coordinates are $v,u,x,y$). The lump of gravitational energy travels with the speed of light and has a maximum $(T^{u}_{v})_{max} = 1/54\pi b^{2}$ at $v = b/\sqrt{2}$. One sees that  $T^{u}_{~v}$ vanishes on the surface $v = 0$ and very far away from that surface. It acquires there the form $T^{u}_{~v} \approx b^{2}/8\pi v^{4} = \hbar c/8\pi v^{4}$, which is a purely quantum quantity.

In the spacetime (3.1) the source tensor is given by the same general form (2.6), but now we have $u_{a} u^{a} = -1$, $u^{a} = (1, 1, 0, 0)$, $s^{a} = (-1, 1, 0, 0)$ and $l^{a} = (0, 2, 0, 0)$. The energy flux vector has the components
   \begin{equation}
  q^{a} =  - T^{a}_{~b}u^{b} - \rho u^{a} = \left(\frac{1}{2}T^{u}_{~v},-\frac{1}{2}T^{u}_{~v}, 0,0\right).
\label{3.3}
 \end{equation}
The energy density and pressures, rooted from (2.6) give now
   \begin{equation}
 \rho =  T_{ab}u^{a}u^{b} = -\frac{1}{2}T^{u}_{v} = -\frac{b^{2}v^{2}}{16\pi (v^{2} + b^{2})^{3}},~~~p_{u} = \rho,~~~p_{\bot} = 0,
 \label{3.4}
 \end{equation}
where $p_{\bot}$ represents the transversal pressures $p_{x}$, $p_{y}$ and $p_{u}$ is the pressure on the $u$-direction.  $q \equiv \sqrt{q^{a}q_{a}} = (1/2)T^{u}_{~v}$ and the acceleration of the congruence is again null, so that the congruence is geodesic. For example, taking $v = 10^{-15}s$ we have $q\approx b^{2}/16\pi v^{4} = 2\cdot 10^{-10} ergs/cm^{2}\cdot s$, a low value. It could be increased with a shorter value of the duration of measurement given by $v$.

The two nonzero components of the shear tensor appears now as
 \begin{equation}
 \sigma^{x}_{~x} = - \sigma^{y}_{~y}= \frac{bv}{2(v^{2} + b^{2})^{3/2}}.
 \label{3.5}
 \end{equation}
We further write down the nonzero components of the Riemann tensor in the geometry (3.1). One obtains
 \begin{equation}
 \begin{split}
 R^{u}_{~xvx} = \frac{b}{2}\frac{bv^{2} - 2(2v^{2} - b^{2})\sqrt{v^{2} + b^{2}}}{(v^{2} + b^{2})^{3}} e^{-\frac{b}{\sqrt{v^{2} + b^{2}}}}\\
  R^{u}_{~yvy} = \frac{b}{2}\frac{bv^{2} + 2(2v^{2} - b^{2})\sqrt{v^{2} + b^{2}}}{(v^{2} + b^{2})^{3}} e^{\frac{b}{\sqrt{v^{2} + b^{2}}}}\\
   R^{x}_{~vvx} = \frac{b}{4}\frac{bv^{2} - 2(2v^{2} - b^{2})\sqrt{v^{2} + b^{2}}}{(v^{2} + b^{2})^{3}}\\
 R^{y}_{~vvy} = \frac{b}{4}\frac{bv^{2} + 2(2v^{2} - b^{2})\sqrt{v^{2} + b^{2}}}{(v^{2} + b^{2})^{3}}
 \label{3.6}
 \end{split}
 \end{equation}
It is worth noting that, close to $v = 0$, the above expressions behave as
 \begin{equation}
 R^{u}_{~xvx} \approx  \frac{1}{eb^{2}},~~~R^{u}_{~yvy} \approx  -\frac{e}{b^{2}},~~~ R^{x}_{~vvx} =  -R^{y}_{~vvy} \approx  \frac{1}{2b^{2}},
 \label{3.7}
 \end{equation}
which are of the order of the Planck value. That takes place very near the null surface $v = 0$. However, in the region $v >> b$, the curvature tensor acquires negligible values
 \begin{equation}
 R^{u}_{~xvx} = -R^{u}_{~yvy} \approx  -\frac{2b}{v^{3}},~~~ R^{x}_{~vvx} =  -R^{y}_{~vvy} \approx  -\frac{b}{v^{3}},
 \label{3.8}
 \end{equation}
so that the spacetime becomes Minkowskian asymptotically.

\section{Geodesics}
To find the timelike geodesic equations in the spacetime (3.1), we start with the Lagrangean
  \begin{equation}
	L = \frac{1}{2} g_{ab} \dot{x}^{a} \dot{x}^{b} = -\dot{u} \dot{v} + \frac{1}{2}( e^{-\frac{b}{\sqrt{v^{2} + b^{2}}}} \dot{x}^{2} + e^{\frac{b}{\sqrt{v^{2} + b^{2}}}} \dot{y}^{2}),
 \label{4.1}
 \end{equation}
where a dot means a derivative w.r.t. the proper time $\tau$. If we keep track of the fact that the metric coefficient $g_{ab}$ do not depend on $u, x, y$, one obtains
  \begin{equation}
	  \dot{x} = C_{1} e^{\frac{b}{\sqrt{v^{2} + b^{2}}}},~~~ \dot{y} =  C_{2} e^{-\frac{b}{\sqrt{v^{2} + b^{2}}}},~~~ \dot{v} = C_{3},
 \label{4.2}
 \end{equation}
 where $C_{1}, C_{2}, C_{3}$ are dimensionless constants.
We take above $C_{3} = 1$ and so the variable $v$ will replace the proper time. The trajectories $x(v)$ and $y(v)$ may be obtained, in principle, from Eqs. 4.2, by integration. As far as the $u$ - coordinate is concerned, the function $u(v)$ may be obtained from the constraint $u_{a} u^{a} = -1$, where we have here $u^{a} = (\dot{v}, \dot{u}, \dot{x}, \dot{y})$. Therefore,
  \begin{equation}
	  \dot{u} = e^{-\frac{b}{\sqrt{v^{2} + b^{2}}}} \dot{x}^{2} + e^{\frac{b}{\sqrt{v^{2} + b^{2}}}} \dot{y}^{2} + 1,
 \label{4.3}
 \end{equation}
where now $\dot{u} = du/dv$, etc. In order to satisfy that $\dot{x} < 1,~\dot{y} < 1$, we choose $C_{1} = 1/e$ and $C_{2} = 1$, to obtain
  \begin{equation}
	\dot{x}(v) = e^{\frac{b}{\sqrt{v^{2} + b^{2}}} -1},~~~\dot{y}(v) = e^{-\frac{b}{\sqrt{v^{2} + b^{2}}}}
 \label{4.4}
 \end{equation}
While $\dot{y}(v)$ grows from $1/e$ at $v = 0$ to unity at $\infty$, $\dot{x}(v)$ drops from unity to $1/e$. They reach the same value $1/\sqrt{e}$ at $v = b\sqrt{3}$. Eq. (4.3) gives us now
  \begin{equation}
	  \dot{u}(v) = e^{\frac{b}{\sqrt{v^{2} + b^{2}}} -2} + e^{-\frac{b}{\sqrt{v^{2} + b^{2}}}} + 1
 \label{4.5}
 \end{equation}
whence
  \begin{equation}
	  \dot{u}(v) = \frac{1}{e} \dot{x}(v) + \dot{y}(v) + 1,
 \label{4.6}
 \end{equation}
or
  \begin{equation}
	  u(v) = \frac{1}{e} x(v) + y(v) + v,
 \label{4.7}
 \end{equation}
where a constant of integration has been absorbed by $v$. In terms of the previous coordinates $(t,z)$ (4.7) yields
  \begin{equation}
	 x(t) + ey(t) -2ez(t) = 0
 \label{4.8}
 \end{equation}
Eq. (4.8) shows that the trajectory of the test particle is contained in a plane to which $\vec{n}(1, e, -2e)$ is a normal vector. If the test particle has constant $x$ and $y$, say $x = x_{0},~y = y_{0}$, then $z = (x_{0} + ey_{0})/2e$ will also be constant, i.e. the particle will be at rest. That is a confirmation that the velocity field $u^{a} = (1, 0, 0, 0)$ corresponds to a geodesic.

To obtain the null geodesics we have only to get rid of the last term in Eq. (4.6). Hence
  \begin{equation}
	  \dot{u}(\lambda) = \frac{1}{e} \dot{x}(\lambda) + \dot{y}(\lambda),~~~\dot{v}(\lambda) = const.,
 \label{4.9}
 \end{equation}
where $\lambda$ is the parameter along the null geodesic. But we have again $\dot{v} = const.$ so that $v = \lambda$ is a suitable choice. Passing from $(v,u)$ to Cartesian coordinates $(t,z)$, (4.9) yields
  \begin{equation}
	  \frac{1}{e} x(t) +  y(t) - z(t) = t,
 \label{4.10}
 \end{equation}
which describes a plane moving with the speed of light along the direction given by its normal vector $\vec{n}(1/e, 1, -1)$. If the null test particle moves such that $x = x_{0},~y = y_{0}$, we get $z(t) = - t + (1/e)x_{0} + y_{0}$, which is a straight line.

\section{Nonlinear wave with cross-polarization}
In the linear version of the previous GW (Eq.2.2) the $+$ polarization mode
  \begin{equation}
	h_{xx} = -h_{yy} = -2\Phi = -\frac{b}{\sqrt{v^{2} + b^{2}}}.
 \label{5.1}
 \end{equation}
 appeared. Let us introduce a $\times$ polarization through the last term of the metric
  \begin{equation}
	  ds^{2} = - dv du + e^{-\frac{b}{\sqrt{v^{2} + b^{2}}}} dx^{2} + e^{\frac{b}{\sqrt{v^{2} + b^{2}}}} dy^{2} + \frac{2b}{\sqrt{v^{2} + b^{2}}} dxdy
 \label{5.2}
 \end{equation}
where $h_{xy} = b/\sqrt{v^{2} + b^{2}}$. The source stress tensor gives us now an anisotropic fluid with energy flux and positive energy density
  \begin{equation}
	\rho (v) = p_{u}(v) = \frac{b^{2}}{4\pi (v^{2} + b^{2})^{2}},~~~q^{a} = (-\rho, \rho, 0, 0),~~~p_{\bot} = 0,~~~q = \rho,
 \label{5.3}
 \end{equation}
with $\rho_{max} = \rho(0) = 1/4\pi b^{2}$. However, the scalar expansion
  \begin{equation}
	\Theta \equiv \nabla_{a}u^{a} = \frac{b^{2}}{v(v^{2} + b^{2})}
 \label{5.4}
 \end{equation}
is nonzero and diverges at $v = 0$. We have again $u^{a} = (1, 1, 0, 0)$. Let us evaluate the order of magnitude of $\rho (v)$ from (5.3) for $v = 10^{-15}s$. With all fundamental constants inserted, one obtains $\rho = \hbar /c^{3}v^{4} = 3~ ergs/cm^{3}$ (the approximation $v >> b$ has been used). Here $v$ was taken as the duration of measurement. If the space were filled with these nonlinear GWs, to find a larger value of the energy density a very short-in-time measurement should be performed. We note that $\rho$ might be considered to be related to the dark energy. In addition, we have to keep in mind that the geometry (2.3) is not a vacuum solution of gravitational equations; the curvature is rooted from the gravitational wave itself, through the energy-momentum tensor (2.4).
The $u-v$ components of the shear tensor are given by
  \begin{equation}
	\sigma^{v}_{~v} = \sigma^{u}_{~u} = -\sigma^{u}_{~v} = -\sigma^{v}_{~u} = -\frac{b^{2}}{6v (v^{2} + b^{2})}
 \label{5.5}
 \end{equation}
and
  \begin{equation}
	\begin{split}
	\sigma^{x}_{~x} =  \frac{b(b + 3\sqrt{v^{2} + b^{2}})}{6v (v^{2} + b^{2})},~~~\sigma^{y}_{~y} =  \frac{b(b - 3\sqrt{v^{2} + b^{2}})}{6v (v^{2} + b^{2})} \\
		\sigma^{x}_{~y} =  \frac{b(b - \sqrt{v^{2} + b^{2}})}{2v (v^{2} + b^{2})} e^{\frac{b}{\sqrt{v^{2} + b^{2}}}},~~~\sigma^{y}_{~x} = - \frac{b(b + \sqrt{v^{2} + b^{2}})}{2v (v^{2} + b^{2})} e^{\frac{-b}{\sqrt{v^{2} + b^{2}}}}
\end{split}
 \end{equation}
It is worth noting that all nonzero components of the $\sigma^{a}_{~b}$ are vanishing when $v \rightarrow \infty$ and diverge at $v = 0$, excepting $\sigma^{x}_{~y}$ which vanishes at the origin.

\section{Conclusions}
We followed in this paper the Pazouli and Tsagas recipe and used the fully nonlinear Einstein equations, assuming a certain form of the starting geometry. Our ''perturbation'' solution plays the role of a source of curvature and does not act in a given background. The source stress tensor is given by a null fluid with no transversal pressures in Cartesian coordinates and with $\rho = p_{z} < 0$, which are very large near the null surface $t - z = 0$, with $z$ - the direction of propagation. We conjectured a new interpretation of the lack of gravitation in Minkowski space, concluding that flat space means constant Machian gravitational potential $c^{2}$. We also studied general timelike and null geodesics and found that they belong to a plane which has a constant direction, given by its normal vector. A static observer is not affected by the presence of the wave and a massless particle continues to move with the velocity of light.
We found also that the energy density $\rho$ becomes positive when the $\times$ polarization is included.\\

\textbf{Acknowledgement}\\
I am grateful to the anonymous referee for useful suggestions which improved the quality of the manuscript.

redpajama_set_name: RedPajamaArXiv


Craig Clarke has accumulated decades of experience in Sales and Customer Service both locally and abroad. Upon completing college with his Bachelor's Degree from St. Louis University he joined the Bahamas Ministry of Tourism and was subsequently stationed in its Detroit office for three years prior to opening the office in Vancouver, Canada.
Upon his return to the Nassau office he served in various capacities in Advertising and Marketing before leaving for the private sector. He has held the position of Director of Sales for the Paradise Island Resort & Casino and Carnival's Crystal Palace Resort & Casino, Sales & Family Island Development Manager for Cable Bahamas, Director of Customer Service at Bahamasair and Sales Executive for Harborside Resort at Atlantis receiving numerous sales and service awards over the years.
Craig is a people person who brings his years of experience and skills to service his clients here at C.A. Christie Real Estate.


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text:
\section{Introduction}
Even galaxies with little star formation activity continue to evolve,
as evidenced by the substantial increase of their cosmic stellar mass
density over the past 7 billion years \citep{bell04b, faber07,
  brown07}.  This must be related to the decreasing star formation
activity over the same period \citep[e.g.,][]{lefloch05}, and the
production of such quiescent galaxies through the truncation of star
formation \citep[e.g.,][]{faber07, bell07}; the color scatter among
quiescent galaxies and its evolution are in precise agreement with
such a scenario \citep{ruhland09}.  There are, however, quiescent
galaxies at all redshifts $z\lesssim 1.3$ that are more massive than
the most massive star-forming galaxies. This implies that star
formation in the most massive galaxies was truncated even earlier,
and/or that mergers play an important role in producing massive
galaxies.

Evidence for the early formation of massive galaxies is provided by
their old stellar populations. However, we need to bear in mind that
there can be a large difference between the age of the stellar
population and the assembly age, especially if mergers are important,
as is the case in a hierarchical framework for galaxy formation
\citep{delucia07}.  Hence, the number density evolution of galaxies is
important in constraining their assembly history.  Measuring this is
difficult because of its sensitivity to the luminosity evolution
correction, especially for massive galaxies at the exponential cut-off
of the mass function.  As a result, there is no consensus among the
currently available measurements \citep{cimatti06, wake06, brown07,
  cool08}.

Given these difficulties, other observations have been used to either
directly or indirectly constrain the assembly of galaxies.  Merging
activity among the massive galaxy population is observed
\citep[e.g.,][]{vandokkum99, vandokkum05, bell06a, bell06b, lin08},
and has been shown to produce a color-magnitude relation that is in
agreement with observations \citep{skelton09}.  However, its
cosmological relevance has always been difficult to determine, given
the uncertainties in converting observed merger fractions to merger
rates and the associated growth in mass.  An independent and indirect
indication that massive galaxies undergo continuous evolution is
provided by the recent result that high-redshift quiescent galaxies
are substantially smaller than local galaxies with the same mass
\citep[see,][and references therein]{vanderwel08c}.  This strongly
suggests that mergers are important \citep[see,
e.g.,][]{vanderwel09a}, and that the assembly of massive galaxies is
continuing up until the present day.  Another indirect, yet powerful,
constraint is provided by the evolution in the clustering and halo
occupation distribution of red galaxies \citep{white07, conroy07,
  brown08}: the evolution in the clustering strength of red galaxies
is slower than expected in the absence of merging.

In this Letter we address the question whether major merging is the
dominant mechanism for the production of very massive, quiescent
galaxies.  The argument that we invoke is simply that major merging
generally leads to rounder galaxies.  An analysis of the shape
distribution of quiescent galaxies can therefore constrain the
importance of merging.  Since merging among galaxies with mass ratios
of $\lesssim 3$ is the only known mechanism to produce round galaxies
(see Section 3 for further discussion), this is a powerful test.  The
disadvantage of this method, compared to those mentioned above, is
that no information about the time scale and epoch of galaxy assembly
can be inferred.

\citet{vincent05} and \citet{padilla08} were the first to
systematically study the axial ratio distribution, $p(b/a)$, of a
large number of galaxies, selected from the Sloan Digital Sky Survey
(SDSS).  Through a detailed analysis, they infer the intrinsic shape
distribution and the effect of extinction.  Both divide the sample
into 'elliptical' and 'spiral' galaxies, and confirmed that luminous
'elliptical' galaxies are, on average, rounder and tri-axial, compared
to low-luminosity 'ellipticals', which are more elongated and oblate
\citep{davies83, franx91}, and display disky isophotes
\citep{jorgensen94}. This phenomenon is not recent: \citet{holden09a}
showed that this trend persists at least out to $z\sim 1$.  Here we
present a complementary, modified analysis, focusing on $p(b/a)$ as a
function of stellar mass for quiescent, i.e., non-star-forming,
galaxies.  Because mass-to-light ratios are well constrained by
broad-band colors for quiescent galaxies, stellar mass estimates are
robust.  This is essential for our purposes, as we are interested in
the most massive objects, i.e., those that populate the exponential
tail of the mass function.  Furthermore, as opposed to previous
studies, we pre-select galaxies independent of their photometric
properties.  Our shape-independent, spectroscopic selection criteria
circumvent the biases that are potentially introduced by selecting
galaxies by their 'morphological' properties, or some pre-defined
surface brightness profile.

With this sample, for which we have determined axial ratios from our
own fits to two-dimensional light distributions, we address the
following specific questions. Are high-mass, quiescent galaxies
rounder than low-mass quiescent galaxies? If so, is there a mass limit
at which $p(b/a)$ distinctly changes, and above which disk-dominated
are completely absent?  Such evidence would imply that the only
evolutionary path to such masses is a disk-destroying mechanism, i.e.,
major merging.

\section{The Sample}

We select a sample of 17,480 quiescent galaxies from Data Release 6 of
the SDSS \citep{adelman08}.  Our sample includes galaxies at redshifts
$0.04<z<0.08$ without detectable $[\rm{OII}]$ and $\rm{H}\alpha$
emission lines. The selection criteria are described and motivated in
full by \citet{graves09b}; but as opposed to that work, we do not
exclude galaxies with a low concentration index and galaxies that are
fit better by an exponential profile than by a \citet{devaucouleurs48}
profile, because this may exclude quiescent, yet disk-like galaxies,
which are obviously relevant for quantifying $p(b/a)$ of quiescent
galaxies. As a consequence, our sample may include galaxies with star
formation in an extended disk outside the SDSS spectroscopic fiber.
This effect, however, does not affect our main conclusion that
quiescent massive galaxies with prominent disks are extremely rare
(see Section \ref{res}). Rather, such a bias works in the opposite
direction in the sense that it would lead to the mistaken inclusion of
galaxies with large disks.

The exclusion of all galaxies with emission lines also excludes
quiescent galaxies with active galactic nuclei.  Their number,
however, is small, and make up a small fraction of the population
\citep[e.g.,][]{pasquali09a} that is negligible for our purposes.

The axial ratios were obtained as described by \citet{vanderwel08c}.
Briefly, GALFIT \citep{peng02} is used to determine from the $r$-band
the radii, axial ratios, position angles, and total magnitudes,
assuming a \citet{devaucouleurs48} surface brightness profile.  We
have verified that adopting surface brightness models with a free
S\'ersic index does not lead to a significantly different
$p(b/a)$.

The stellar masses are derived with the simple conversion from color
to mass-to-light ratio \citep{bell03}, but are normalized to
correspond to the \citet{kroupa01} stellar initial mass function.  The
assumed cosmology is $(\Omega_{\rm{M}},~\Omega_{\Lambda},~h) =
(0.3,~0.7,~0.7)$.

The sample is complete over the entire redshift range $0.04 < z <
0.08$ down to $M_* \sim 4\times 10^{10}M_{\odot}$, set by the
spectroscopic magnitude limit of the SDSS ($r=17.7$).  The SDSS may be
incomplete for low-luminosity, low-surface brightness galaxies
\citep{blanton05c}, which could, in addition, depend on their
orientation \citep[see, e.g.,][]{odewahn97}.  However, since we are
concerned with the high-mass end of the galaxy population, this does
not play a role.  Moreover, simulations of images with even lower
signal-to-ratio than those of the massive galaxies analyzed here
demonstrate that axial ratio measurements from GALFIT are robust and
accurate \citep{holden09a}.  In summary, the lack of galaxies with
small $b/a$, reported in the following section, is not in any way
compromised by selection effects or measurement errors.

\section{Results and Discussion}\label{res}

In Figure \ref{M_q}(a) we show $p(b/a)$ of the 17,480
spectroscopically selected, quiescent galaxies as a function of
stellar mass.  $p(b/a)$ is shown in gray scale, with the percentiles
of the cumulative $b/a$ distribution shown as (red) lines.  Figure
\ref{M_q}(a) immediately demonstrates that for quiescent galaxies, the
projected axial ratio distribution is a strong function of stellar
mass. In the narrow mass range $8\times 10^{10} \lesssim M_*/M_{\odot}
\lesssim 2\times 10^{11}$ there is a rapid decrease in the number of
galaxies with small axial ratios.  As further illustrated by Figure
\ref{M_q}(b), above $M_*\sim 2\times 10^{11}~M_{\odot}$ quiescent
galaxies with $b/a<0.6$ are essentially absent.

This result shows that evolutionary paths that lead to quiescent
galaxies with stellar mass $M_* \gtrsim 2\times 10^{11}~M_{\odot}$ all
but exclude the existence, or the survival, of highly flattened,
disk-like stellar components.  As highly flattened stellar systems are
quite common at lower masses, in the possible realm of plausible
progenitors of high-mass galaxies, this result implies the destruction
of the flattened component in whatever process causes growth beyond
$M_*\sim 2\times 10^{11}~M_{\odot}$.  Therefore, our result that
essentially all quiescent galaxies with masses larger than $M_*\sim
2\times 10^{11}~M_{\odot}$ are round strongly suggests that for such
galaxies major mergers are the dominant, perhaps even unique,
formation channel.  The destruction of a stellar disk requires a major
merger, i.e., a merger involving progenitors with a relatively small
mass ratio of at most $\sim 3$, mergers with a larger mass ratio
leaving stellar disks intact \citep[see, e.g.,][]{bekki98,
  bournaud04}.  Moreover, most likely, the progenitors are not very
gas rich, as this would produce a disky remnant
\citep[e.g.,][]{naab06b}.

It has been suggested that cold flows are responsible for the
formation of massive, classical bulges at high redshift
\citep{dekel09, ceverino09}.  In this scenario, intensely star-forming
'knots' merge, forming a massive bulge \citep[see also][]{noguchi99}.
However, a substantial fraction of the mass ($\sim 50\%$) is still
predicted to reside in a disk.  Even at later stages, when the gas
disk has become stable against fragmentation and collapse
\citep[``morphological quenching'';][]{martig09}, the stellar disk
remains intact and contains a non-negligible fraction of the total
mass.  In short, although cold flows plausibly produce quiescent
galaxies, the end-products will not be uniquely round.  Only in the
case of sufficient merger activity would galaxies become spheroidal.

In passing, we note that the sharp decrease in the fraction of very
round galaxies ($b/a > 0.8$) at the very highest masses ($M>3\times
10^{11}~M_{\odot}$) signifies that such high mass galaxies are typically
brightest group/cluster galaxies, which tend to be slightly more
elongated than 'normal' massive elliptical galaxies
\citep[see,][]{bernardi08}.

As already noted above, at masses lower than $M_*\sim 10^{11}~M_{\odot}$,
quiescent galaxies display a large range in axial ratios, which
implies that star formation truncation mechanisms below
$10^{11}~M_{\odot}$ are often not associated with the destruction of the
disk.  It remains to be tested whether $p(b/a)$ of low-mass quiescent
galaxies is similar to or different from $p(b/a)$ of star-forming
galaxies in the same mass range. Such an analysis, which is
non-trivial because of the effects of extinction and color gradients,
will constrain the degree to which mergers or bulge growth regulate
star formation at these lower masses.

Another open question concerns the number and properties of massive,
star-forming galaxies.  Morphological studies suggest that a large
fraction ($20\%-40\%$) of all galaxies more massive than $M\sim
10^{11}~M_{\odot}$ are late-type galaxies \citep{vanderwel08a,
  bamford09}, and their high masses of at least some of these objects
are confirmed by their rotational velocities
\citep[e.g.,][]{courteau07}. Yet, the degree to which such galaxies
are disk-dominated and should be considered actively star forming
remains to be determined.  It would, therefore, be premature to
conclude that merging is the only way to produce a massive galaxy in
general, and therefore restrict this proposition to the formation of
massive, quiescent galaxies.

The picture sketched by the axial ratio distribution of quiescent
galaxies is in agreement with the strong correlation between structure
and mass for galaxies in general \citep[e.g.,][]{kauffmann03b,
  vanderwel08a} and early-type galaxies in particular
\citep[e.g.,][]{caon93, graham03}: high-mass galaxies are more
concentrated and have higher S\'ersic indices than low-mass galaxies.
These trends are an indirect indication of a decreasing importance of
disks for galaxies with higher masses, although part of this trend is
caused by the increase in S\'ersic index with galaxy mass among
spheroidal galaxies.  In our sample we see a similar trend: in the
mass range $10^{10} < M_*/M_{\odot} < 2\times 10^{10}$, 41\% of the
galaxies have S\'ersic indices $n<3$, whereas at higher masses,
$M_*>2\times 10^{11}M_{\odot}$, only 3\% have such low S\'ersic
indices. We postpone a full exploration of the joint behavior of shape
and structure as a function of galaxy mass until a future paper, but
it is encouraging that the apparent absence of prominent disks in
high-mass, quiescent galaxies is reflected in both the S\'ersic index
and $p(b/a)$.

\acknowledgements{The authors thank the referee for positive feedback.
  A.v.d.W. thanks Marijn Franx for helpful discussion.  H.W.R. thanks
  Simon White for his insistence on eventually 'publishing the last
  thesis chapter'. This Letter makes use of the Sloan Digitial Sky
  Survey (www.sdss.org).}

\bibliographystyle{apj}


text:
Q: How to control JSON.NET serialization of System.Data.Spatial.DbGeometry I have a DB First Entity Framework 5 Data Access Layer that is mapped to a table containing a SQL geometry type field called CenterCoordinate.  The resulting entity contains this:
public System.Data.Spatial.DbGeometry CenterCoordinate { get; set; }
My client javascript requests the API and only accepts JSON.  I then use the Asp.net Web API to serve this using the default formatter (JSON.NET).  In the API controller the field has a long list of properties including an XCoordinate and a YCoordinate.
In the client the JSON only contains this:
Geometry: Object
    CoordinateSystemId: 3498
    WellKnownBinary: null
    WellKnownText: "POINT (6438089.715 1801515.828)"
I really don't want to have to parse out the WellKnownText to get to the values of X and Y.
So the question is how can I control the serialisation/de-serialisation of System.Data.Spatial types to/from JSON such that I get something more useful?  How does the JSON.net formatter know what to include/exclude?
Note:  I really don't want decorate the entity with attributes as these will be lost each time I regenerate the model from the database (I have no idea why we can't add attributes to model fields through VS2012 and have it remember them after a regeneration).  So can this be with partial classes or overriding the formatter?
Thanks, Matt

A: Unfortunately, you're more or less stuck parsing the WellKnownText field if you want to manipulate the coordinates with Javascript.
Geometry is a SQLSpatial type that is saved to a database via the WKT field, so that's why your DbGeometry type is converting the JSON to that format.
If it makes you feel any better, it's causing me just as much of a hassle right now.

Edit: These resources might help a bit:
GeoJSON has a structure much more similar to SpatialSQL:

*

*http://www.geojson.org/geojson-spec.html

*https://github.com/Esri/geojson-utils/blob/master/src/jsonConverters.js
This is a solution used to serialize/deserialize DbGeo types as JSON:

*

*http://www.arcgis.com/home/item.html?id=6d28a606369c43fd9a6f929541ae7c93

redpajama_set_name: RedPajamaStackExchange


WASHINGTON (AP) — Countering China's rapidly expanding military and an increasingly aggressive Russia are now the U.S. military's top national security priorities, outpacing the threat of terrorism, the Pentagon said Friday.
A new national defense strategy says that competition with China and Russia has threatened America's military advantage around the world. And it will require increased investment to make U.S. forces more lethal, agile and ready for war.
"We will continue to prosecute the campaign against terrorists, but great power competition — not terrorism — is now the primary focus of U.S. national security," Defense Secretary Jim Mattis said in prepared remarks at the Johns Hopkins School of Advanced International Studies in Washington.
He declared the defeat of the Islamic State group's "physical caliphate" in Iraq and Syria, but warned that IS, al-Qaida and other extremists continue as threats across the globe.
The document reflects persistent U.S. worries about China's military build-up in the South China Sea, its moves to expand its political and economic influence around the globe, and what has long been described as Beijing's systematic campaign of cyberattacks and data theft from government agencies and private U.S. corporations.
And it underscores American concerns about Russia's aggressive military moves, including the invasion of Ukraine and involvement in the Syria war, as well as its meddling in the 2016 election.
Pentagon officials released an 11-page unclassified version of the strategy on Friday, saying it mapped out a "fundamental shift" in focus for the military.
Previous defense chiefs have long warned about a rising China — triggering the Obama administration's move to put a greater focus on the Asia Pacific region, including added ships and troops. And the new strategy's call for strengthening alliances sounds more like previous administrations, rather than the "America First" message of President Donald Trump's national security strategy that was released in December.
The Pentagon document says that allies and partners are crucial and can provide additional capabilities and access to other regions.
The U.S. has been urging China to take a more active role in convincing North Korea to set aside its nuclear ambitions, and the U.S. has held talks with Russia to ensure there are no conflicts or accidents in the skies over Syria, where both nations are flying in the war against the Islamic State group.
In the strategy's conclusion, Mattis makes clear that his goal is to "pursue change at significant scale" with sustained investment and creative approaches. That plan, however, will face grim budget hurdles.
Congress has been deadlocked and unable to pass a spending bill, bringing the federal government once again to the brink of a shutdown at midnight Friday. And lawmakers are still constrained by the Budget Control Act of 2011, which put mandatory spending caps in place.
The Pentagon strategy acknowledges the budget limits, and calls for greater spending discipline and management, as well as a commitment to again seek more base closings to save money. Congress has repeatedly rejected additional base closings.
The new plan cannot survive, Mattis said, without needed and stable funding.


My name is GADE AMMAJI and I am working as a Supervisor in the Private sector. I have completed my B.Sc.. I grew up in a Upper middle class, Nuclear family with Traditional values.
My sister has a Master's degree and she is employed in private Sector as a supervisor currently based in Nizamabad. We come from a middle class, joint family background with orthodox values.
My daughter is a supervisor with a Bachelor's degree currently working in private sector in Gajuwaka. We belong to a middle class, nuclear family with traditional values.


text:
Home / Collection / Research Guides
Slave narratives recount the personal experiences of antebellum slaves or former slaves, and comprise one of the most extensive and influential traditions in African American literature and culture. Slave narratives were hugely popular in the 19th and early 20th centuries, with many going through multiple reprintings and selling tens of thousands of copies. In fact, until the 1930's slave narratives outnumbered novels written by African Americans.
This pathfinder focuses on reference sources that identify individual slave narratives, as well as how to go about finding items in our collections. While the library holds many sources concerning slavery (e.g. periodicals, newspapers, music), this pathfinder concentrates primarily on autobiographies and biographies published in book or pamphlet form. Also included is a short section on fictionalized accounts of slavery. Not included in this pathfinder is information about the United States Works Progress Administration (WPA) Slave Narrative Collection.
Background Reading
Andrews, William L., Frances Smith Foster, Trudier Harris, eds. The Oxford Companion to African American Literature. New York: Oxford University Press, 1997. Call Number: Ref PS153.N5 O96 1997. This book gives a very general, but helpful overview. It is arranged alphabetically, so you can check the main entries under slave narratives and slavery; or you can check the index for entries that cross-reference slave narratives or slavery.
The following two books examine slave autobiographies as a literary genre. Andrews provides an annotated bibliography of slave autobiographies and biographies; Foster provides a particularly helpful selective bibliography of secondary sources.
Andrews, William L. To Tell a Free Story: The First Century of Afro-American Autobiography. Urbana, IL: University of Illinois Press, 1986. Call Number: E 185.96 .A57 1986.
Foster, Frances Smith. Witnessing Slavery: The Development of Ante-Bellum Slave Narratives. Madison, WI: University of Wisconsin Press, 1994. Call Number: PS 366 .A35 F6 1994.
Searching the Online Catalog
When searching for materials in the Newberry's collections, check the online catalog. If you know the author or title of the item you want, simply search using the Author or Title search options within the online catalog. If you do not know the author or title, you may try searching under the following subject headings:
Slaves' writings, American
Slaves--United States--Biography
You may also want to consult one of the bibliographies listed below to find specific authors or titles.
North American Slave Narratives
Put together by the University of North Carolina at Chapel Hill, the North American Slave Narratives collection includes all the existing autobiographical narratives of fugitive and former slaves published as broadsides, pamphlets, or books in English up to 1920. Also included are many of the biographies of fugitive and former slaves and some significant fictionalized slave narratives published in English before 1920. Although this collection does not claim to be complete and final, it is fairly comprehensive. It is particularly helpful in that the bibliography can be viewed both alphabetically and chronologically. Many of the narratives have also been digitized.
Arksey, Laura, Nancy Pries, and Marcia Reed. American Diaries. Volume 1: Diaries written from 1492 to 1844; Volume 2: Diaries written from 1845-1980. Call Number: Ref Z5305.U5 A74 1983. These two volumes are guides to more than 5000 published diaries and journals; there is a focus on books that are day-to-day records as opposed to narratives or memoirs. The entries are arranged chronologically. In volume one, many of the entries concerning the subject of slavery will not be by slaves, but by slave owners and traders, visitors to the South, and abolitionists; check the index under the subject headings of slave; slavery; and slaves. In volume two, check under the same headings in the index, as well as civil war, contrabands and freedmen.
Bibliography of American Imprints to 1901. New York: K.G. Saur, 1993. Call Number: Ref Z1215 .B47 1993. An extremely handy resource for finding printed materials. In the Subject Index, check under a variety of headings, including:
Slaves. Autobiography
Slaves. Country. Biography (e.g. Slaves. United States. Biography)
Slaves. State. Biography (Slaves. Illinois. Biography)
Slaves. Personal Narratives
You can also check for titles in the Main Index: for example, "Narrative of . . ." yields some possibilities. You can also check the Date and Place Indexes if you are interested in narratives from particular years or places.
Brignano, Russell C. Black Americans in Autobiography. Durham, N.C.: Duke University Press, 1984. Call Number: Ref Z1361 .N39 B67 1984. While this bibliography broadly covers all African-American autobiography, it can still be helpful in searching out the narrower category of slave narratives. Arranged alphabetically by Author, each entry includes information about reprints; symbols for up to ten known library locations; and cross-references to other autobiographical volumes by the author or by a member of his or her family. Brignano adds short but informative descriptions for each entry as well. Also included is a checklist of post-World War II reprintings of autobiographies published before 1865.
Dumond, Dwight Lowell. A Bibliography of Antislavery in America. Ann Arbor: University of Michigan Press, c1961.
Call Number: Ref Z1249 .S6 D8. This bibliography includes literature written and circulated by those active in the antislavery movement. It includes not only American publications, but also British ones that were widely circulated in the U.S. The bibliography is arranged alphabetically by author.
Matthews, Geraldine O. Black American Writers, 1173-1949: A Bibliography and Union List. Boston: G. K. Hall, 1975.
Call Number: Ref Z1361 .N39 M35. This bibliography is an attempt to identify African-American materials held in repositories in six southeastern states: Alabama, Georgia, North Carolina, South Carolina, Tennessee, and Virginia. It includes a section on "Slavery, Anti-Slavery, Slave Trade, and Personal Narratives" which is organized alphabetically by author.
Parrish, T. Michael and Robert M. Willingham, Jr. Confederate Imprints: A bibliography of Southern Publications from Secession to Surrender. Call Number: Ref Z1242.5 .P37 1987. This is a bibliography of Confederate publications, and one can find some slave narratives in the section titled "Politics, Economics, and Social Aspects." Although this section is arranged alphabetically by author, it is a bit difficult to skim because of the variety of subjects included.
Southern, Eileen and Josephine R. B. Wright. African-American Traditions in Song, Sermon, Tale, and Dance, 1600s-1920: an Annotated Bibliography of Literature, Collections, and Artworks. New York: Greenwood Press, 1990. Call Number: Ref Z5956 .A47 S68 1990. While not a bibliography of slave narratives per se, this book is still immensely useful, as it provides a unique perspective to writings by and about African-Americans. It is a compilation of both primary and secondary sources, and includes works known for their explication and interpretation of African-American culture; the compilers also give priority to "firsts" in various areas first collection of slave songs, first compilation of Brer Rabbit tales, first description of a black church religious service. It is organized by time period, and then sorted into the categories of "Social Activities" (incl. items related to social customs, and holiday festivals); "Religious Experience;" and "Song." Short descriptions are given for each entry, and the book is fairly easy to browse.
Work, Monroe N. A Bibliography of the Negro in Africa and America. New York: The H.W. Wilson Company, 1928. Call Number: Ref Z1361.N39 W8. Despite the early publication date, this book remains a standard used by researchers. Work devotes an entire section to slave narratives, as well as publications concerning other facets of slavery including: economic aspects, social aspects, the abolition movement, fugitive slaves and the underground railroad, and African-Americans as soldiers. Entries are arranged alphabetically by author within each section.
Yellin, Jean Fagan. The Pen is Ours: A Listing of Writings by and about African-American Women before 1910 with Secondary Bibliography to the Present. New York: Oxford University Press, 1991. Call Number: Ref Z1229. N39 Y44 1991. Part II of this bibliography contains a list of writings by and about women who had been held in slavery and whose dictated narratives or biographies were published before the end of 1910. Entries are arranged alphabetically by author.
Fictionalized Slave Narratives
The antislavery movement in the nineteenth century generated a number of narratives about slavery, some widely read, that were subsequently revealed to be fictitious or heavily fictionalized, though sometimes based on an actual case or person.
If you know the author or title (check the North American Slave Narratives online bibliography), search using those commands from the main catalog search page. You may also search using the following subject headings:
Slavery—Fiction
Women Slaves—Fiction
Fugitive Slaves—Fiction
Slavery—United States—Fiction
Slaves—United States—Fiction
Harriet Beecher Stowe and Uncle Tom's Cabin
The Newberry owns several interesting items related to Harriet Beecher Stowe's Uncle Tom's Cabin, including sheet music, plays, ballets, and translations. To find these items in the online catalog, you can search under Author for Stowe, Harriet Beecher, 1811-1896, or Title for Uncle Tom's Cabin.


Besides the hotel offers in Kashan (see this post), we received many, many more messages after our ask for three-phase electricity on Instagram. Most people who messaged us either told us what touristic places to visit or they asked when they can see us.
In fact, our number 1 problem always is, how to charge the car. After that we need to find a place to sleep and eat. Sometimes the order and priority is different ;-). Only after those three problems (and sometimes additional ones like laundry, grocery shopping and so on) are solved, we start thinking about what sights to see or whom to meet.
Soheil in Isfahan was the only one who clearly understood what our problem is (the need for a place to charge the Tesla). He offered us three-phase electricity in his father's factory.
Of course, we didn't know what to expect when we drove to the industrial town of Isfahan. But the surprises couldn't have been bigger. We were welcomed by Soheil, his mother and his sister, Mehrnoush, as well as one of his friends, Ali. Soheil and Ali were very curious about the car. Benedikt spend the afternoon talking to them and explaining. I spend the same time with Mehrnoush and her mom, wonderful people, who it was so great talking to. We all share the same interest in mountaineering. Especially the dad of the family, who unfortunately died last fall and who we would have loved to meet, was a great climber and hiker. He started in the 1980s a company for everything climbers need out of metal (carabiners, pitons, crampons, ice picks…) and other metal products (tea pots).
While we were chatting, and visiting the factory, the Tesla was charging on a stable three-phase outlet (Montenegro style) with 32 amperes and 22 kW.
It was really a great afternoon we spend together with the Samavatis. We just couldn't refuse an invitation from the family to stay at their place overnight and have dinner together. This kind of hospitality is just amazing and we had a wonderful time at their apartment.
I was sick the third day in Isfahan (probably eat/drank something wrong). Due to that Benedikt had to go to a meeting of our "fans" by himself. We set up this meeting since many people waned to meet us (and see the car). We didn't want them all at our hotel. About 25 to 30 people showed up for this meeting. Like any Tesla-newbie Benedikt could easily entertain them with the soundless car, suspension control, the car key, frunk and so on.
Before we left we went another time to Soheil and his family. Again, we had a great time together and the car charged up to 98%. This time, the cable/fuse didn't really take the 32 amperes though. After about 1 hour charging, a fuse blew and the charging stopped. We only noticed at that point that the fuse was made for 25 amperes and the outlet for 16 amperes. It worked the first time to push 32 amperes through them, but after the fuse-blow we continued charging only with 20 amperes (on all three phases).
That is amazing. Thanks to the Isfahani family. Also why don't you guys record video? That would be much better if you a share videos of the car and the fans!!
We want to! It just really takes some time to produce good videos. Right now, we still enjoy it more to travel, discover and meet new people. We have really great video material and will make many videos as soon as the journey is getting more quite.


A High Court bench yesterday felt "embarrassed" to hear the bail petition of noted photographer Shahidul Alam in a case filed for "spreading propaganda and false information against the government".
The bench of Justice Md Ruhul Quddus and Justice Khandaker Diliruzzaman was set to hear the petition. But it forwarded the petition to the chief justice for a decision, saying one of the bench members felt embarrassed to hear the matter.
Petitioner's counsel Barrister Sara Hossain wanted to know from the judges why one of them felt embarrassed to hear the petition.
However, the HC bench neither disclosed the reason nor the name of the judge who felt embarrassed.
Asked, Shahdeen Malik, another lawyer for Shahidul, said he was surprised that the HC bench suddenly felt embarrassed.
"It was unexpected for us ... A judge may feel embarrassed at the beginning of the proceedings of a case but it is unusual that a judge would feel so three days after the start of the proceedings," he told The Daily Star.
Contacted, Attorney General Mahbubey Alam said an HC judge is not obligated to disclose in the courtroom the reason for feeling embarrassed to deal with a case. The judge may disclose the reason to the chief justice.
He further said the CJ will now assign another HC bench to hear Shahidul's petition.
The 63-year-old eminent photographer was picked up by law enforcers from his home in the capital's Dhanmondi area on August 5 night.
The following day, the police filed a case against him under the Information and Communication Technology (ICT) Act.
Shahidul was placed on a seven-day remand after police produced him at a Dhaka court the same day, seeking 10-day remand. He told the court that he was tortured in custody.
Police, however, refuted the allegation.
Shahidul filed the bail petition with the HC on August 28 through his lawyers -- Sara Hossain and Jyotirmoy Barua -- saying he may be granted bail as he is ill.
The petition also mentioned that Shahidul will face the trial proceedings and will not leave the country if he is granted bail in the case.
The petition was included in the hearing list of the HC bench of Justice Ruhul and Justice Diliruzzaman on August 29.
On that day, the HC bench told the lawyers that it would examine the decisions of the HC and the Supreme Court in such cases, and asked them to move Shahidul's bail petition this week.
The HC bench was scheduled to hear the petition on Monday. But it deferred the hearing till yesterday, as the attorney general sought time from the bench for making preparations to place arguments on the petition.


Excellent work. Professionally done. Keep it up!
Ingenious idea. This is what instructables is about.
Great project. Your ible is very well laid out, easy to follow!
Well made. Thanks for sharing.
Good idea. I need to make one of these soon.
Wonderful idea and thank you for sharing.
Pics look good enough to eat. I'm sure it must taste great too. Thanks for sharing.
Thanks for the idea. God instructable. I have a B+ with 40 pins. I made my breakout cable from an old 40 pin IDE cable. I dug out the blanked pin socket. I preferred not to use a breakout board, instead I just use dupont wires at the outer end. I will label the pins by sticking a printed label on either side of the connector end. Haven't done that yet. Here's some pics of the cable.
Great job! And very well laid out instructable.
Great instructable. Easy to follow and well written.
Cut Your Own Hair: Spend Zero-Dinero!


text:
Richard Guy Bowers, né le  à Rawhiti (Nouvelle-Zélande) et décédé le  à Motueka, est un joueur de rugby à XV qui joue avec l'équipe de Nouvelle-Zélande. Il évolue au poste de demi d'ouverture (1,70 m pour 70 kg).

Carrière

En 1953-1954 il est sélectionné à deux reprises avec les All Blacks, qui font une tournée en Europe et en Amérique du Nord. Il dispute son premier test match avec l'équipe de Nouvelle-Zélande le  contre l'Irlande pour une victoire 14-3. Il perd contre la France 0-3 le  pour sa dernière rencontre internationale.

Palmarès
Sélections avec les All Blacks :  2 en 1954
Nombre de matchs avec les All Blacks : 15, 6 points marqués

Notes et références

Liens externes

Joueur international néo-zélandais de rugby à XV
Demi d'ouverture (rugby à XV)
Joueur de la Wellington Rugby Football Union
Naissance en novembre 1932
Décès en juin 2000
Naissance dans la région de Northland
Décès en Nouvelle-Zélande
Décès à 67 ans


For treating erosive esophagitis or GERD in children or babies, the usual dose of Zantac is typically 5 mg to 10 mg per kg (a little less than 2.5 mg to 5 mg per pound) total per day. This is usually split up into two doses per day.
This medication is approved for use in babies and children and comes in two convenient dosage forms. However, you should always talk to your baby's healthcare provider before giving any medication to your baby. Do not give over-the-counter Zantac to babies.


Picture: A total of 317,000 people were registered as unemployed job seekers at Finland's Employment and Economic Development Offices (TE Offices) in March.
The ranks of the long-term unemployed continued to fall in Finland in March, reports the Ministry of Employment and the Economy.
The number of unemployed job seekers who had been without a job for an uninterrupted period of at least one year dropped by 10,400 year-on-year to 112,200 – to account for roughly a third of all unemployed job seekers.
The ranks of the unemployed also included 121,900 over 50-year-old and 38,600 under 25-year-old job seekers. Both of the numbers have dropped from the previous year, by 9,400 and 6,100 respectively, according to the Ministry of Employment and the Economy.
The statistics also show that under 25-year-old job seekers were less likely to remain unemployed for extended periods of time, with 61.8 percent of them finding employment no later than three months after first registration as unemployed job seekers between January and March. The percentage represents an improvement of 2.7 percentage points from the corresponding period in 2016.
Almost 60,000 new job vacancies were reported to the TE Offices in March. The total number of unfilled vacancies, in turn, stood at 123,300, representing an increase of 14,600 from March 2016.
Statistics Finland, meanwhile, reported that the unemployment rate improved by 0.5 percentage points year-on-year to 9.6 percent in March following a year-on-year increase of 19,000 in the number of the employed and a decrease of 14,000 in that of the unemployed.


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Now in its fourth generation, is the most lunatic AMG saloon of them all still a match for the BMW M3? crankandpiston.com finds out on the international launch in Portugal.
Of all the Mercedes-derived AMGs, the C 63 has the reputation for being the most lunatic. As the lightest rear-wheel drive model available, with brutish power and a heavy metal soundtrack, it's the perfect recipe for luxury German hooliganism, and through each generation since has been an intriguing alternative to BMW's M3.
More than 40,000 third generation C 63s were sold around the world, making it the most successful car in AMG's history. And now there's a new one, based on the fourth-generation W205 C-Class. AMG has taken an already accomplished mid-size saloon and worked its brand of beefy magic to give it some serious clout, both on road and on track.
The name of the C 63 comes from its old 6.3-litre, naturally aspirated V8. But that's been replaced by a twin-turbocharged 4-litre V8 – the same one found in the Mercedes-AMG GT. It's notable not just for being smaller than the old V8, but also for being quite clever. The turbochargers are wedged in between the two banks of cylinders, which means the whole caboodle can be mounted low down in the car for better performance. Two versions are available. The standard car has 469bhp and 479lb ft. However, we've been playing with the top-of-the-line C 63 S, which ups the power output to 503bhp and a stonking 516lb ft of torque. That dwarfs the M3's 406lb ft, although the BMW is around 50kg lighter.
Various flavours of C 63 S are lined up outside the hotel on the international launch in Faro, Portugal, and by gum they look good. The AMG design team is confined to the visual boundaries set by the vanilla C-Class, but they've succeeded in making the C 63 look mean without being tacky. The tracks are wider than the standard car, and the wheel arches flared accordingly. The bonnet bulges and the bumper features a grey "A-wing" that serves as an air deflector for the cooling inlets. At the back, a motorsport-style rear diffuser does the same job.
Inside, it's familiar C-Class territory with added steroid. As well as practical and comfort features like the tablet-style centre screen and electric everything, there are hugging sports seats and carbon fibre-backed gauges to remind you that this machine means business.
A twist of the key and the V8 starts with a bark. Pootling around town the C 63 S is docile, but even with Comfort mode enabled and the exhaust on its quietest setting, there's a threatening burble from the back end. The suspension is firm, but damped well enough to dismiss potholes. It's an entirely comfortable experience, meandering behind mid-morning shoppers in the sunshine, with the only slight hiccup being the seven-speed transmission. At very low speeds, it seems to hesitate from time-to-time, resulting in an embarrassing lurch off the line and an accompanying exhaust snarl. People look.
On the highway, a stab of the gas takes us to 130kph almost instantly, accompanied by a glorious flap-assisted exhaust note and a G-force squeeze into the sports seats, but then it settles to an adaptive cruise-controlled canter. Road noise is reasonable, although there's a noticeable buffeting of wind noise from the wing mirrors. It's a good excuse to crank up the excellent Burmester stereo.
The test route takes us off the highway and onto some exquisite hill roads towards Portimao. It's time to play. Sport+ mode is selected, which opens the exhaust flaps, ups the transmission speed and stiffens both the suspension and the steering.
Instantly, the bellow from the back of the car is louder, more metallic, more evocative. Fears about the reduction in engine size are immediately forgotten; the biturbo V8 is superb, with buckets of torque available and no noticeable lag on the throttle. It takes a few kilometres to realise that there's no need to skip up and down the gears – the full band of power is usable.
As the road winds left, right, up and down, the C 63 S comes alive, encouraging the driver to lean harder on the Michelin Pilot Sports and dig into the tarmac. The steering is weighty and direct, although some more textured feedback would be nice. With the gearbox set to manual, the hefty wheel-mounted paddles come into play. The changes are fine, although not as instant and smooth as some other models – no twin-clutch cleverness here. However, the slight jolt on each shift actually adds to the visceral experience. Squeeze the throttle, watch the horizon approach at pace, hard on the carbon-ceramic brakes and turn in as the exhausts pop and crackle away. It's easy, with all that power, to break grip at the back, but feather the throttle on exit and smooth, fast progress is surprisingly accessible.
And so to the wonderful Autodrome Internacional Algarve, a peach of a modern circuit that rides crests over the Portuguese landscape. It's a true test of any car, but one guaranteed to extract maximum excitement if the quality of machine is high enough.
It is. The carbon-ceramic brakes come into their own on this high-speed track, keeping things in check even as the rear of the car tries to squirm under the force of physics. With Race mode enabled (only available on the C 63 S), the full force of AMG is unleashed. The ESP is set to Sport Handling mode, which lifts the electronic reigns just enough to let you hang on the edge of adhesion through the quickest corners, without getting too sideways. It doesn't interfere with the process of going fast, as long as you keep things tidy. And on this exhilarating but slightly scary circuit, it's nice to have a safety net.
The balance of the car is beautifully judged, allowing even decidedly mediocre drivers (like myself) to trail brake into off-camber, downhill corners and then use the throttle to point the nose exactly where it needs to go. The game is then to apply the throttle without slipping at the back. It's really, really fun and really, really fast.
The C 63 S is an excellent machine, the result of AMG treading a near-perfect line between exhilaration, luxury, comfort and accessibility. Extreme, muscular performance is readily available, and not just to the finest drivers that can eke out the limits. Our gripes are minor – an occasionally hesitant transmission, and a slight lack of feel in the steering don't take away from the large amounts of lunacy available. Are you worried, BMW? A twin-test surely awaits.


Set of 5 flat letterpress notecards, measuring 4×6″, with matching metallic navy envelopes.
There's nothing quite like a handwritten note in the mail. These letterpress notecards are the perfect way to let someone special know you are thinking of them. This set of flat notecards is printed with "a little note to say… get well soon", for those occassions when an email just won't cut it, and comes with matching navy envelopes.
Since I first fell in love with the art of letterpress, I have had a mind full of ideas to create my own letterpress plates, and these notecards are the result. Printed from plates I designed using my own calligraphy in combination with a hand-drawn font (used with the designers permission), and then letterpressed with navy ink on beautiful 300gsm paper, these 4×6″ notecards are something I am really excited about. This set of five comes with co-ordinating metallic navy envelopes, wrapped in kraft card & twine with a handstamped "barefoot" charmed, before being protected in a cello sleeve. All stationery sets ship free within Australia.


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Updated on May 11, 2017 9:05am EDT
MARKET SNAPSHOT: Nasdaq's Record Run On The Line, As Snap Tumbles After Results
By Barbara Kollmeyer , MarketWatch Dow Jones Newswires
Macy's stock drops after disappointing earnings
The Nasdaq Composite faces a struggle to log another record on Thursday, with U.S. stocks poised for a modestly lower open.
Meanwhile, shares of Snapchat parent Snap Inc. were set to tumble after reporting a $2.2 billion loss.
Nasdaq 100 futures slipped 13 points to 5,662. Dow Jones Industrial Average futures dipped 30 points to 20,861, while S&P 500 futures eased 5 points to 2,390.
On Wednesday, the tech-heavy Nasdaq closed at a record for a fourth session in a row (http://www.marketwatch.com/story/us-stocks-poised-to-edge-lower-after-trump-fires-fbis-comey-2017-05-10), rising 0.1% to 6,129.14. The S&P 500 scraped out a 0.1% gain, but the DJIA finished 0.2% lower.
Higher oil prices were failing to support stock futures Thursday. U.S. crude prices added to Wednesday's gains (http://www.marketwatch.com/story/oil-boosted-by-signs-us-crude-glut-is-shrinking-2017-05-11) with a 1.3% rise to $47.93 a barrel, on the heels of data showing the biggest weekly drawdown for inventory since December.
Calling the Fed's bluff: The prior session's moves came after the shock firing of FBI Director James Comey, but the stock market's reaction to this was fairly sanguine (http://www.marketwatch.com/story/heres-why-the-stock-market-isnt-freaking-out-about-the-comey-firing-2017-05-10), despite questions over whether it would crimp U.S. President Donald Trump's ability to push through market-friendly policies.
Joel Kruger, currency strategist at LMAX Exchange, said that while politics could factor into stock gains, Federal Reserve policy will likely dictate the direction for equities.
"Conversations about a stock market top are certainly not without merit. But it has also been abundantly clear stocks will only be at risk when the market truly believes the Fed isn't going to fold its hand when it comes to forward guidance," Kruger wrote in emailed comments.
"We may be getting close to that point, but until then, investors will keep pushing their bets and calling the Fed's bluff," he said.
For the week so far, the Nasdaq is showing a 0.5% gain, while the Dow industrials are off 0.3% and the S&P 500 is flat.
Early Thursday, New York Fed President William Dudley said trade protectionism is a "dead end" that will eventually harm the U.S. economy, Reuters reported (http://www.nasdaq.com/article/in-trumps-shadow-fed-official-says-trade-barriers-a-dead-end-20170511-00297). The comments, in a speech on the benefits and challenges of globalization in Mumbai, India, are seen as implied criticism of President Donald Trump's policies, even though Dudley did not mention the U.S. leader by name.
As for economic data, weekly jobless claims fell by 2,000 to 236,000, while continuing claims fell to the lowest level since Nov. 1988. Low levels of layoffs underline a strong labor market.
U.S. producer prices showed a broad-based gain in April, which pushed the annual increase up to the largest advance in five years
Stock movers: Snapchat parent Snap (SNAP) tumbled 22% in premarket trading after the messaging app reported a $2.2 billion loss (http://blogs.marketwatch.com/thetell/2017/05/10/snap-user-growth-to-be-key-focus-in-first-earnings-report-live-blog/) in its first set of earnings since going public.
Read: Snap's CEO is the key to that huge loss (http://www.marketwatch.com/story/why-snap-lost-22-billion-in-its-first-quarter-as-a-public-company-2017-05-10)
Shares of Macy's Inc.(M) dived 11% after the retailer reported a worse-than-expected slide in revenue in the first quarter.
Straight Path Communications Inc.(STRP) shares sank 20% in premarket after the company confirmed an agreement to be bought by Verizon Communications Inc.(VZ) in a deal that values Straight Path at a deep discount to Wednesday's closing price (http://www.marketwatch.com/story/straight-paths-stock-plunges-after-verizon-merger-deal-2017-05-11).
Whole Foods Market Inc.(WFM) shot up 3% in premarket trade after the grocery-store chain announced a new stock buyback plan () and released earnings that met forecasts.
Other markets: Asian markets finished higher (http://www.marketwatch.com/story/oil-gains-lift-most-asian-markets-but-china-sags-on-liquidity-worries-2017-05-11), with China squeezing out a gain of 0.1% as investors fretted over liquidity worries. European stocks were trading mostly flat to lower (http://www.marketwatch.com/story/italian-banks-a-bright-spot-as-european-stocks-fall-back-2017-05-11). The FTSE 100 was holding steady (http://www.marketwatch.com/story/ftse-100-adrift-ahead-of-bank-of-englands-super-thursday-update-2017-05-11) ahead of the Bank of England's update on inflation and interest rates.
Read:Italian banks a bright spot as European stocks fall back (http://www.marketwatch.com/story/italian-banks-a-bright-spot-as-european-stocks-fall-back-2017-05-11)
Gold prices traded modestly higher. The dollar was mostly lower, except against the pound , which fell after disappointing U.K. industrial and trade data (http://www.marketwatch.com/story/uk-industrial-production-shrinks-on-warm-weather-2017-05-11).
The price of a single bitcoin reached a new milestone on Thursday, shooting past the $1,800 level for the first time. Bitcoin prices were up last up 4.9% to $1,827.55. Earlier in the week, bitcoin shot past $1,700 for the first time.
The yield on a 10-year Treasury bond was unchanged at 2.42%.
May 11, 2017 08:55 ET (12:55 GMT)