text:
\section{Introduction
\ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ }%

According to one of the proposed universe models, our perceptible universe is a $3+1$-dimensional ($4D$) brane (the so-called extended dimension or hypersurface), which is submerged in a higher dimensional (i.e., $5D$) anti-de Sitter ($AdS_5$) spacetime, in which the only force spreads through the infinite bulk space, is gravity while other forces are constricted to the brane. In fact, the need for extra special dimensions originates from the fundamental aspects in the string theory (STH). Propounding of the extra dimensions provide the probability of the Planck scale being on an electroweak scale which relieve the problem of gauge hierarchy. It was shown that these models suffer from degradation of unitarity in about three-quarters of the low-impact Planck scale \cite{Antoniadis:2011bi}. STH is the biggest candidate to solve the problem of the unitarity. It was also found that, for the string scale it is essential to become visible lower than the effective Planck scale, in which string resonances are the first mark of these models \cite{Antoniadis:2011bi,Mavromatos:2009xg}.

In 1920s, Kaluza and Klein \cite{2,3} proposed a feasible theory for the existence of extra dimensions (the fifth dimension) point out the electrodynamics as a gravity component. Later on, in 1998, Arkani-Hamed et al  \cite{3s} presented a large extra dimensions theory in which the gravity diverges into its bulk, although the matter fields stay localized. They proved that with the extra large dimensions the famous hierarchy problem can be solved. Namely, the visible Universe might consist of a $4D$-dimensional surface (the so-called \textquotedblleft brane\textquotedblright) immersed in a $4D+D_{extra}$-dimensional spacetime (the so-called \textquotedblleft
bulk\textquotedblright). There are many investigations to consider the impression of the extra dimensions on the physics of the Standard Model (SM) and fields, which are confined to the brane \cite{3ss}.
However, the gravity has an access to reach the bulk. At least one of those additional spatial dimensions might be extremely large in comparison to the Planck scale that it causes to lower the basic gravity scale to the electroweak ($\backsim$TeV) level \cite{Maartens:2010ar}. In other words, those large extra dimensions could come with a electroweak level for quantum gravity (and/or STH) leading to the numerous new observable phenomena in colliders and other fields of the particle physics \cite{4}. The most prominent brane-world model content is  Randall-Sundrum model which was proposed in 1999 \cite{S4,S5}. They presented a different high-dimensional scenario that provides an alternative approach to constructing the hierarchy, which appear between the weak and the fundamental scales of gravity. There have been considerable investigations in the recent years about the higher-dimensional gravity where the classical $4d$ spacetime of general
relativity (GR) is recovered from the effective theories \cite{S6,N6,N7,N8}, which also admit exact solutions \cite{S7,S8}. In Ref. \cite{S9}, the construction of the Einstein field equations on a $4D$-brane planted
in a higher dimensional bulk where the matter fields are constricted to the brane in accordance with the confining potential and the associated spherically symmetric vacuum
(static) black hole solutions were investigated (see also \cite{S10,S11}).

In this paper, we consider two brane world black hole solutions having confining potentials \cite{S10,S9} in which the equation of the vacuum fields are modified by a geometrical quantity $Q_{\mu\nu}$ on the brane which may play the role of the dark energy \cite{S10}. The first solution is a good toy model to represent the galaxy's rotation curves independent of the presence of dark matter and modified Newtonian dynamics theory \cite{10SS}.  The second solution explains a black hole in the space of asymptotically de Sitter (dS). In this context, the reader is also refered to  Refs. \cite{11SS} and \cite{12SS} which do not consider the mirror symmetry that leads to a geometrical interpretation of the dark energy as bend
in the Universe given by the exterior curvature that has no mechanism needed for the confinement of matter on the brane.

In recent years, black hole thermodynamics has been repeatedly applied to test the predictions of quantum gravity candidate theories \cite{5,6,7,8}. The black hole thermodynamics in the brane-world
scenario by considering scalar and axial gravitational perturbations was studied
in Ref. \cite{9}. Besides, inspired from the inflation brane world cosmology, the thermodynamics of a black hole solution in two dimensional dilaton gravity with an arc-tangent potential background was analyzed \cite{10}. The entropy of the Reissner--N\"{o}rdstrom
black hole is regarded within the state of a brane world \cite{11}.
However, the thermodynamics of these brane world black hole solutions have not been adequately considered under the influence of GUP. With this study, we want to fill this gap of the literature for some extent.

The emitted gravitational radiation from the horizon of a perturbed black hole releases information of its interior properties \cite{12} and makes also possible to investigate the quantum structure of the black holes. The outer side of the horizon, the potential
barrier has a frequency dependent black hole parameters that act as if a filter. As a result, some waves are reflected back by the barrier, while others are transported to infinity \cite{13}. However, the radiation emitted (or to be detected by the observer) at spatial infinity differs from its originating value measured near the black hole's horizon. More specifically, Hawking radiation changes from its perfect black body character until reaching to spatial infinity. This phenomenon is known as greybody factor (GF) \cite{14,15,16}, which reveals important information about black holes and can be computed in various methods \cite{17,18,19,20,21,22,23}.\\

On the other hand, QNMs play an essential role within theory of GR, which reveal the presence of gravitational radiation \cite{D23}. Furthermore, they depend on the black hole parameters and
independent of the initial disturbance to the black hole. Namely, QNMs have characteristic oscillation frequencies of the black hole \cite{24,25}. In astrophysics, the detection of QNMs from gravitational wave experiments will lead to the new tests of GR, as well as precise measurements of black hole parameters (like: mass, charge, and spin parameters). For instance, the QNMs related with gravitational-wave radiations from binary black hole coalitions can prepare deep insight into the remnant's properties \cite{DaSilvaCosta:2017njq}. The QNMs represent as a complex form which the  real part mentions the frequency of oscillation, and its imaginary part associates with the decaying or growing (in the case of superradiance \cite{Aliev:2015wla}) characteristic time of the decay \cite{26,27}. One of the most promising approaches to compute the QNMs is the WKB method, which can be calculated in $3^{th}$ and $6^{th}$ orders \cite{D29,H11}. To wrap things up, when a black hole is perturbed, the proceeding behaviors could be expressed in three phases: The first level is correlated with the radiation because of the perturbations conditions. The second level is related to the damped oscillations with complex frequencies, (QNMs). And the third corresponds to the breakdown of a power law decay of waves \cite{Pedraza:2021hzw}.

In this paper, we study the QNMs of spherically symmetric and static (and vacuum)  black hole solutions with a confining potential in the brane-world scenario \cite{Heydar-Fard:2007ahl}. We consider two particular black hole solutions that have constant curvature bulk: (1) Schwarzschild-de Sitter black hole like solution with the existence of a cosmological constant ($\Lambda$), which can be a verification for this point that an extra term in the field equations on the brane can represented as a positive ($\Lambda$) and can be used for explaining the accelerating expansion of the universe. (2) Solution with a suitable potential explaining the galaxy rotation curves without assuming the existence of dark matter.

This paper is organized as follows: In Section 2, we introduce the Brane-World black hole solution via a confining potential (BWBHSCP). The thermodynamical propertis o BWBHSCP including its entropy with GUP are given in Sect. 3. We then study the GFs of the scalar particles in Sect. 4. To this end, we employ the Klein-Gordon equation to derive and analyze the
massless effective potential, which is efficacious in the GFs. In Sect. 5, bosonic QNMs of the BWSBHCP are numerically
computed with the aid of WKB approximation method in $6^{th}$ order. Finally, we provide conclusions in Sect. 6.

(Throughout the paper, we shall use the metric convention of $(-,+,+,+)$ and the geometrized units: $c=G=\hslash=1$.)

\section{REVIEW OF BWBHSCP SPACETIME}

The action of BWBHSCP is given by \cite{Heydar-Fard:2007ahl}%
\begin{equation}
S=\frac{1}{2\alpha^{\ast}}\int_{\aleph}D^{n}X\sqrt{-%
\mathcal{F}%
}\left(  \Re-2\Lambda^{\left(  b\right)  }\right)  +\int_{\Sigma}d^{4}%
x\sqrt{-g}\left(
\mathcal{L}%
_{surface}+%
\mathcal{L}%
_{m}\right)  , \label{1}%
\end{equation}

which, in general, stands for a spacetime $\left(  \aleph,%
\mathcal{F}%
 _{AB}\right)  $ with boundary $\left(  \Sigma,g_{\mu\nu}\right)  $. $\Lambda^{\left(  b\right)  }$ is the bulk cosmological constant and
$\alpha^{\ast}=\frac{1}{M_{\ast}^{n-2}}$ ($M_{\ast}$ represents the basic energy scale in the bulk space and $n$ denotes the dimension number). The effective field equations for vacuum
are found to be as follows \cite{Heydar-Fard:2007ahl}%
\begin{equation}
G_{\mu\nu}=-\Lambda g_{\mu\upsilon}+Q_{\mu\upsilon}-\varepsilon_{\mu\upsilon},
\label{2}%
\end{equation}

where $Q_{\mu\upsilon}$ is a geometrical quantity, which adjusts the vacuum field equations on the brane. Due to the Weyl symmetries, $\varepsilon_{\mu\nu}$  is a symmetric and traceless tensor and it is restricted by the conservation equations: $\varepsilon_{;\upsilon}^{\mu\upsilon}=0$  (ensued from the Bianchi identities). To have a brane, which has a static spherically symmetric
metric, one can use the following ansatz:
\begin{equation}
ds^{2}=-e^{\mu\left(  r\right)  }dt^{2}+e^{\upsilon\left(  r\right)  }%
dr^{2}+r^{2}\left(  d\theta^{2}+\sin^{2}\theta d\varphi^{2}\right).
\label{3}%
\end{equation}

Substituting the metric \eqref{3} into Eq. \eqref{2} and making some straightforward computations, one gets the gravitational field equations of BWBHSCP as follows:
\begin{equation}
G_{0}^{0}=\frac{e^{-\upsilon}}{r^{2}}\left(  1-r\upsilon^{\prime}
-e^{\upsilon}\right)  , \label{9}%
\end{equation}

\begin{equation}
G_{1}^{1}=\frac{e^{-\upsilon}}{r^{2}}\left(  1+r\mu^{\prime}
-e^{\upsilon}\right)  , \label{10}%
\end{equation}

and
\begin{equation}
G_{2}^{2}=G_{3}^{3}=\frac{1}{4re^{\upsilon}}\left(  2\mu^{\prime}
-2\upsilon^{\prime}
-\mu^{\prime}
\upsilon^{\prime}
r+\mu
^{\prime2}r+2\mu^{\prime\prime}
r\right)  , \label{11}%
\end{equation}

where prime symbol indicates derivative with respect to $r$. Thus, two classes of solutions are obtained. The first solution reads

\begin{equation}
e^{\mu\left(  r\right)  }=e^{-\upsilon\left(  r\right)  }=1-\frac{B}%
{r}-\alpha^{2}r^{2}-2\alpha\beta r-\beta^{2}, \label{4}%
\end{equation}

where $B$, $\alpha$, and $\beta$ are the integration constants. However, $\alpha$ is known as the scale of energy on the brane \cite{Heydar-Fard:2007ahl}. In short-range distances regarded with conventional stellar/astrophysical scales (like our solar system scale), metric function \eqref{4} yields a Schwarzschild-like solution. On the other hand, taking into account the small $\alpha$ values which allow us to neglect the $\alpha^2$ term, the larger distance scales associated with galaxies yield the following potential function, which describes a new galaxy model as distinct from the original Einstein's GR theory:

\begin{equation}
\phi(r)=\frac{B}{2 r}+\alpha \beta r+\frac{\beta^{2}}{2}. \label{iz1}
\end{equation}

Without referring to dark matter or assuming any new or modified theories like the modified Newtonian dynamics \cite{Turner:1997npq}, the potential function \eqref{iz1} could be utilized to explain the galactic rotation curves. The corresponding outer ($r_{+}$) and inner ($r_{-}$) horizons of the obtained metric solutions \eqref{4} can be found as
\begin{equation}
r_{\pm}=\frac{d^{1/3}}{6\alpha}+\frac{2}{3}\left(  \frac{\beta^{2}+3}{\alpha
d^{1/3}}\right)  -\frac{2\beta}{3\alpha}, \label{5}%
\end{equation}

where%
\begin{equation}
d=8\beta^{3}-108B\alpha+12\sqrt{3}\sqrt{-4B\alpha\beta^{3}+27B%
^{2}\alpha^{2}-4\beta^{4}+36B\alpha\beta+8\beta^{2}-4}-72\beta\text{.}
\label{6}%
\end{equation}

At the considerable distance scales with
a small $\alpha$, Eq. \eqref{6} becomes

\begin{equation}
r_{\pm}=-\frac{\left(  \beta^{2}-1\right)  \pm\sqrt{\left(  \beta
^{2}-1\right)  ^{2}-16M\alpha\beta}}{4\alpha\beta}. \label{7}%
\end{equation}

For $16M\alpha\beta>\left(  \beta^{2}-1\right)^2$
there are no horizons and $16M\alpha\beta=\left(  \beta^{2}-1\right)^2$ leads to extremal black hole solution.

The second type of solution is obtained by
considering $\beta=0$ and $\alpha\neq0$:
\begin{equation}
e^{\mu\left(  r\right)  }=e^{-\upsilon\left(  r\right)  }=1-\frac{B}%
{r}-\alpha^{2}r^{2}. \label{8}%
\end{equation}

If we consider the GR limit and compare the above result asymptotically with the black hole solution in de-Sitter space with $B=2M$, the cosmological constant is determined as $\Lambda=3\alpha^{2}$. Besides, neglecting the
second order term of $\alpha,$ the Schwarzschild horizon $r=2M$ is recovered. Also, by assuming $M=0$, one can obtain the de-Sitter horizon: $r=\frac{1}{\alpha}$.

\section{PHYSICAL PROPERTIES of BWBHSCP}

In this section, we shall study the thermodynamic and mass features of the BWBHSCP. To this end, we first recall the statistical definition of the Hawking temperature, which is determined in terms of surface gravity $\mathcal{K}$ as follows \cite{Wald,riz}:
\begin{equation}
T_{H}=\frac{\mathcal{K}}{2\pi}=\frac{1}{4\pi}\lim_{r\rightarrow r_{+}}\frac{\partial
_{r}g_{tt}}{\sqrt{g_{tt}g_{rr}}}. \label{12}%
\end{equation}

Thus, the Hawking temperatures of first \eqref{4} and second \eqref{8} kind solutions of the BWBHSCP can be computed as follows%
\begin{equation}
T_{H\left(  1\right)  }=\frac{B-2\alpha^{2}r_{+}^{3}-2\alpha\beta
r_{+}^{2}}{4\pi r_{+}^{2}}, \label{13}%
\end{equation}

\begin{equation}
T_{H(2)}=\frac{B-2\alpha^{2}r_{+}^{3}}{4\pi r_{+}^{2}}. \label{14}%
\end{equation}

In order to define the related masses, one can consider the event horizon of each BWBHSCP solution by considering $B=2M$. Therefore, we get
\begin{equation}
M_{\left(  1\right)  }\left(  r_{+}\right)  =-\frac{1}{2}\left(  \alpha
^{2}r_{+}^{3}+2\alpha\beta r_{+}^{2}+\left(  \beta^{2}-1\right)  r_{+}\right)
,\label{15}%
\end{equation}

which also yields the mass of the second BWBHSCP solution when $\beta=0$ is set. Namely, we have
\begin{equation}
M_{\left(  2\right)  }\left(  r_{+}\right)  =-\frac{r_{+}}{2}\left(
\alpha^{2}r_{+}^{2}-1\right). \label{16}%
\end{equation}

\subsection{GUP MODIFIED THERMODYNAMICS OF BWBHSCP}

The common feature of all promising theories in quantum gravity is that they contain the minimum observability of the Planck length $(L_{p})$. In this context, it is useful to remind the definition of the GUP \cite{N4}:
\begin{equation}
\delta p\geq\frac{1}{\delta x}\left(  1+\eta L_{p}^{2}\delta p^{2}\right)
, \label{17}%
\end{equation}

where coefficient $\eta$  is a dimensionless physical parameter that represents different quantum gravity proposals. In fact, $\eta$ is not depend on $\delta x$ and $\delta p$ but generally depends on the expectation values of $x$ and $p$ \cite{GERG}. For the energy scales much lower than Planckian scale, we can ignore the extra term, in which the usual uncertainty principle is recovered. If we re-substitute $\delta p$ into the  $\delta p$ seen in the bracket of Eq. \eqref{17}, we get%
\begin{equation}
\delta p\geq\frac{1}{\delta x}\left[  1+\frac{\alpha L_{p}^{2}}{\delta
x^{2}}\left(  1+\eta L_{p}^{2}\delta p^{2}\right)  ^{2}\right]  .\label{18}%
\end{equation}

Neglecting the higher order terms of $L_{p}$, one can have
\begin{equation}
\delta p\geq\frac{1}{\delta x}\left(  1+\frac{\eta L_{p}^{2}}{\delta x^{2}%
}\right)  . \label{19}%
\end{equation}

Recalling the invariant dispersion relation $E$ (energy) $\sim$ $P$ (momentum), Eq. \eqref{19} can be rewritten as%
\begin{equation}
\delta E\geq\frac{1}{\delta x}\left(  1+\frac{\eta L_{p}^{2}}{\delta x^{2}%
}\right). \label{20}%
\end{equation}

Thus, the energy can be defined in a more convenient form:
\begin{equation}
E\geq\frac{1}{\delta x}+\frac{\eta L_{p}^{2}}{\delta x^{3}}+O\left(
\frac{L_{p}^{3}}{\left(  \delta x\right)  ^{4}}\right)  . \label{21}%
\end{equation}

Adding higher order terms that would elaborate  Eq. \eqref{21} would of course reveal more GUP effects. Therefore, we can expand Eq. \eqref{21} as follows
\begin{equation}
E\delta x\geq1+\frac{\eta L_{p}^{2}}{\delta x^{2}}+\frac{\eta_{1}L_{P}^{3}}{\delta x^{3}}+\frac{\eta_{2}L_{P}^{4}}{\delta x^{4}}+\frac{\eta_{3}L_{P}^{5}}{\delta x^{5}},
\label{22}%
\end{equation}

where the subscript numbers are the order of derivatives of $\eta$ with respect to its argument. Now, let us consider a particle with the length $l$ and energy $E$, which is swallowed by a black hole. In such a case, the black hole involves a minimum rise area as $\Delta A\geq4(\ln2)L_{p}^{2}E\delta x$ in which we consider
$\delta x\sim l$ and $\ln2$ represents the minimum rise of entropy. By
substituting Eq. (\ref{22}) into the minimum rise area formula, we then have
\begin{equation}
\Delta A\geq4(\ln2)L_{p}^{2}\left[  1+\frac{\eta L_{p}^{2}}{\delta x^{2}}+\frac{\eta_{1}L_{p}^{3}}{\delta x^{3}}+\frac{\eta_{2}L_{p}^{4}}{\delta x^{4}}+\frac{\eta_{3}L_{p}^{5}}{\delta x^{5}}\right].
\label{23}%
\end{equation}

To compute the microcanonical entropy of the BWBHSCP, one can simply follow the methodology given in \cite{GERG} and get
\begin{multline}
\frac{dS}{dA}\approx\frac{\Delta S_{\min}}{\Delta A_{\min}}\simeq\\
\frac{1}{4L_{p}^{2}}\left[  1-\eta L_{p}^{2}\frac{1}{\delta x^{2}}-\eta_{1}L_{p}^{3}\frac{1}{\delta x^{3}}+\left(  \eta^{2}-\eta_{2}\right)\frac{L_{p}^{4}}{\delta x^{4}}+\left(  2\eta\eta_{1}-\eta_{3}
\right)  \frac{L_{p}^{5}}{\delta x^{5}}\right]  .\label{24}%
\end{multline}

By integrating the above expression, one can find the entropy as follows:
\begin{multline}
S\approx\frac{A}{4L_{p}^{2}}-\\
\pi\eta\ln\frac{A}{L_{p}^{2}}+\frac{4\pi^{3/2}\eta_{1}
L_{p}}{\sqrt{A}}-\frac{\left(  \eta^{2}-\eta_{2}
\right)  L_{p}^{2}4\pi^{2}}{A}-\frac{16L_{p}^{3}\pi^{5/2}\left(  2\eta\eta_{1}
-\eta_{3}\right)  }{A\sqrt{A}}.\label{S25}%
\end{multline}

It is worth noting that to have Eq. \eqref{S25}, the terms with order higher than $O\left(
\frac{L_{p}^{5}}{\delta x^{5}}\right)$ are neglected. By using $A=4 \pi R^{2} \simeq 4 \pi \delta x^{2}$ where $R$ is the event horizon: $R=r_{+}$. Besides, we assume that the particle acquires  $\delta x \sim R$ \cite{m25,m26} position uncertainty as it falls into the black hole. Furthermore, in the loop quantum gravity and STH, the entropy-area relationship of black holes (for $\left.A \gg L_{P}^{2}\right)$ is given by
\begin{equation}
S=\frac{A}{4 L_{P}^{2}}+\rho \ln \frac{A}{L_{P}^{2}}+\beta \frac{L_{P}^{2}}{A}, \label{S25n}
\end{equation}

where $\beta$ and $\rho$ can take various values in the content of STH and the loop quantum gravity \cite{N4}. Based on the assumption that the entropy expression given in Eq. \eqref{S25n} is more accurate and if Eqs. \eqref{S25} and \eqref{S25n} are compared, one finds out that $\eta_{1}=\eta_{3}=0$. Thus, in Eq. \eqref{22}, all terms with even power of $\frac{1}{\delta x}$ should be terminated. Namely, only even powers of Planck length could exist in the GUP. Thus, the GUP modified BWBHSCP entropy is represented as
\begin{equation}
S\approx\frac{A}{4L_{p}^{2}}-\pi\eta\ln\frac{A}{L_{p}^{2}}-\frac{\left(
\eta^{2}-\eta_{2}\right)  L_{p}^{2}4\pi^{2}}{A}.\label{27}%
\end{equation}

Applying $A=16\pi M^{2}$ in Eq. (\ref{27}), one can define the GUP assisted entropy of the BWBHSCP of first kind as follows:
\begin{multline}
S_{\left(  1\right)  }\approx\frac{\pi}{L_{p}^{2}}\left(  \alpha^{2}r_{+}%
^{3}+2\alpha\beta r_{+}^{2}+\left(  \beta^{2}-1\right)  r_{+}\right)  ^{2}-\\
\pi\eta\ln\frac{4\pi\left(  \alpha^{2}r_{+}^{3}+2\alpha\beta r_{+}^{2}+\left(
\beta^{2}-1\right)  r_{+}\right)  ^{2}}{L_{p}^{2}}-\frac{\left(  \eta^{2}-\eta_{2}\right)  L_{p}^{2}\pi}{\left(  \alpha^{2}r_{+}^{3}+2\alpha\beta r_{+}%
^{2}+\left(  \beta^{2}-1\right)  r_{+}\right)  ^{2}}.\label{N28}%
\end{multline}

In Eq. (\ref{N28}), if the GUP parameter tends to zero ($\eta\rightarrow0$) only the first term representing the non-GUP entropy \eqref{S25n} of BWBHSCP remains. Furthermore, if $\beta\rightarrow0$, then we get the GUP modified entropy of the BWBHSCP of second kind:
\begin{equation}
S_{\left(  2\right)  }\approx\frac{\pi}{L_{p}^{2}}\left(  \alpha^{2}r_{+}%
^{3}-r_{+}\right)  ^{2}-\pi\eta\ln\frac{4\pi\left(  \alpha^{2}r_{+}^{3}%
-r_{+}\right)  ^{2}}{L_{p}^{2}}-\frac{\left(  \eta^{2}-\eta_{2}
\right)  L_{p}^{2}\pi}{\left(  \alpha^{2}r_{+}^{3}-r_{+}\right)  ^{2}%
}.\label{29}%
\end{equation}

\section{GREYBODY FACTORS OF BWBHSCP}

In this section, the GFs of scalar fields radiated from the BWBHSCP are going to be analyzed. To this end, we shall reduce the radial wave equation to a one-dimensional Schr\"{o}dinger-like wave equation in terms of the tortoise coordinate.
The Klein-Gordon equation for perturbation of massless scalar fields around a black hole can be expressed as%

\begin{equation}
\frac{1}{\sqrt{-g}}\partial_{\mu}(\sqrt{-g}g^{\mu\nu}\partial_{\nu}\Psi)=0,
\label{30}%
\end{equation}

where $\sqrt{-g}=r^{2}\sin\theta$. If we apply the above equation to the BWBHSCP line-element \eqref{3}, we get
\begin{equation}
-\frac{1}{f(r)}\partial_{t}^{2}\Psi+\left[  \frac{2f(r)}{r}\partial_{r}+f%
\acute{}%
(r)\partial_{r}+f(r)\partial_{r}^{2}\right]  \Psi+\frac{1}{r^{2}}\left[
\cot\theta\partial_{\theta}+\partial_{\theta}^{2}+\frac{1}{\sin^{2}\theta
}\partial_{\varphi}^{2}\right]  \Psi=0. \label{31}%
\end{equation}

By taking cognizance of the symmetries of the metric, we introduce an ansatz as
\begin{equation}
\Psi=e^{-i\omega t}\frac{R(r)}{r}e^{im\varphi}Y_{lm}(\theta),\label{32}%
\end{equation}

in which $R(r)$ and $Y_{lm}$ represent the radial function and spherical harmonics, respectively, $m$ represents magnetic quantum number, and $\omega$ denotes the energy of the scalar fields. Moreover, using the tortoise coordinate $r_{\ast}=\int\frac{dr}{f(r)}$ with Eq. \eqref{32} in Eq. \eqref{31}, one can obtain
\begin{equation}
\frac{d^{2}R(r)}{dr_{\ast}^{2}}+(\omega^{2}-V_{eff})R(r)=0, \label{33}%
\end{equation}

in which the effective potential can be determined as
\begin{equation}
V_{eff}=f(r)\left[  \frac{f%
\acute{}%
(r)}{r}+\frac{\lambda}{r^{2}}\right]  , \label{34}%
\end{equation}

where a prime symbol denotes the derivative with respect to $r$ and $\lambda=l(l+1)$ (recall that $l$ stands for the orbital quantum number). For the two BWBHSCP solutions, the effective potentials become
\begin{equation}
V_{eff(1)}=\left(  1-\frac{B}{r}-\alpha^{2}r^{2}-2\alpha\beta r-\beta
^{2}\right)  \left[  \frac{B}{r^{3}}-2\alpha^{2}-\frac{2\alpha\beta}%
{r}+\frac{\lambda}{r^{2}}\right]  , \label{35}%
\end{equation}

and
\begin{equation}
V_{eff(2)}=\left(  1-\frac{B}{r}-\alpha^{2}r^{2}\right)  \left[
\frac{B}{r^{3}}-2\alpha^{2}+\frac{\lambda}{r^{2}}\right]  . \label{36}%
\end{equation}

To see the behaviors of the effective potentials, we consider Eqs. \eqref{35} and \eqref{36} and plot $V_{eff}$ versus $r$ graphs for various physical parameters of $\alpha$ and $\beta$: see Figs. \eqref{fig1} and \eqref{fig2}.

\begin{figure}[h]
\centering\includegraphics[width=9cm,height=10cm]{Kanzi1.pdf}\caption{Plots of $V_{eff(1)}$ as a function of $r$ for different values of parameters $\alpha$ and $\beta$. The plots are governed by Eq. \eqref{35}, in which the parameters are chosen as  $B=1$ and $\lambda=2$.} \label{fig1}
\end{figure}

\begin{figure}[h]
\centering\includegraphics[width=9cm,height=10cm]{Kanzi2.pdf}\caption{Plots of $V_{eff(2)}$ as a function of $r$ for different values of parameter $\alpha$. The plots are governed by Eq. \eqref{36}, in which the parameters are chosen as  $B=1$ and $\lambda=2$.} \label{fig2}
\end{figure}

\textcolor{blue}{One of the most important quantities in GR is GF, in which a high value of the GF implies a high probability that Hawking Radiation can reach to spatial infinity.}The GFs are known as the transmission probabilities of the wave modes generating through the relevant effective potential \cite{dd23}. Using the semi-analytical approach \cite{23}, the GFs can be computed as follows
\begin{equation}
\sigma_{l}(\omega)\geq\sec h^{2}\left\{  \int_{-\infty}^{+\infty}\wp dr_{\ast
}\right\}  , \label{37}%
\end{equation}

\textcolor{blue}{where $\sigma_{l}(\omega)$ is dimensionless GF that depends on the angular momentum quantum number $l$ and frequency of the emitted particles $\omega$}. Function $\wp$ is given by
\begin{equation}
\wp=\frac{\sqrt{(h%
\acute{}%
)^{2}+\left[  \omega^{2}-V-h^{2}\right]  ^{2}}}{2h}, \label{38}%
\end{equation}

in which $h$ is a function satisfying the following conditions 1) $h\left(r_{*}\right) > 0$ and 2) $h(-\infty)=h(\infty)=\omega$. Without loss of generality, if we simply set $h=\omega$ and replace the
tortoise coordinate with its standard definition: $r_{\ast}=\int\frac{dr}{f(r)}$, Eq. (\ref{37}) becomes%
\begin{equation}
\sigma_{l}(\omega)\geq\sec h^{2}\left\{  \frac{1}{2\omega}\int_{r_{h}%
}^{+\infty}\frac{V_{eff}}{f(r)}dr\right\}  .\label{39}%
\end{equation}

However, when using Eq. (\ref{39}), the calculations of the GFs for both BWBHSCP solutions are found to be inconclusive. The main reason of this failure is that the integral is set for the lower bound. We realized that the way to eliminate this problem is to change the method. To overcome this issue, at this stage, we employ another method which was prescribed in \cite{N5}. Thus, we first set $h=\sqrt{\omega^{2}-V_{eff}}$ in Eq. (\ref{38}). Since there are no classically forbidden zones in this approach \cite{N5}, one has%
\begin{equation}
\sigma_{l}(\omega)\geq\sec h^{2}\left\{  \frac{1}{2}\int_{-\infty}^{+\infty
}\left\vert \frac{h%
\acute{}%
}{h}\right\vert dr_{\ast}\right\}  .\label{40}%
\end{equation}

As can be seen from Figs. \eqref{fig1} and \eqref{fig2}, the effective potential peaks are related with
$h(+\infty)=h_{peak}=\sqrt{\omega^{2}-V_{peak}}$. Therefore, by setting $h(-\infty)=\omega$, Eq. \eqref{40}  thus recasts in
\begin{equation}
\sigma_{l}(\omega)\geq\sec h^{2}\left\{  \ln\left(  \frac{h_{peak}}{h_{\infty
}}\right)  \right\}  =\sec h^{2}\left\{  \ln\left(  \frac{\sqrt{\omega
^{2}-V_{peak}}}{\omega}\right)  \right\}  . \label{41}%
\end{equation}

We observe that the current bound will be pointless once $\omega^{2}<
V_{peak}$. On the other hand, one can derive the GF with the assist of transmission probability $\bigg(T_{l}(\omega)\bigg)$ via the Miller-Good
transformation method \cite{MGT}. Therefore, Eq. (\ref{41}) can be rewritten as
\begin{equation}
\sigma_{l}\left(  \omega\right)  \equiv T_{l}(\omega)\geq\frac{4\omega^{2}(\omega^{2}-V_{peak})}{(2\omega
^{2}-V_{peak})^{2}}.\label{42}%
\end{equation}
To compute $V_{peak}$, one should first define $r_{peak}$. For instance, in the first kind of solution if we let $B=1, \lambda=2$, and $\alpha=1$, $r_{peak}$ can be computed as

\begin{equation}
r_{peak}=\frac{3\beta^{2}+3\pm\sqrt{9\beta^4-46\beta^2+73}}{8\left(\beta^{2}-1\right)}.\label{dd42}%
\end{equation}
Thus, after substituting  Eq. \eqref{dd42} into Eq. (\ref{35}), the corresponding $V_{peak}$ is obtained. One can repeat the same procedure for the second kind of solution, for different parameters as well. The GFs of BWBHSCP for some fixed parameters and various $\alpha$ and $\beta$ are depicted in \textcolor{blue}{Figs. (\ref{fig3}) and (\ref{fig4})} for the first and second kind solutions, respectively. It is worth noting that the increase in $\alpha$ and $\beta$ values decrease the GFs of the first kind BWBHSCP solution, but in the second kind BWBHSCP solution by increasing $\alpha$ the GFs grow up to $\alpha=2$ then start to decline.

\begin{figure}[h]
\centering\includegraphics[width=9cm,height=10cm]{Kanzi3.pdf}\caption{Plots of
$T_{l(1)}\left(  \omega\right)  $ versus $\omega$ for the first solution of
scalar particles. The physical parameters are chosen as; $B=1$ and
$\lambda=2$.} \label{fig3}
\end{figure}

\begin{figure}[h]
\centering\includegraphics[width=9cm,height=10cm]{Kanzi4.pdf}\caption{Plots of
$T_{l(2)}\left(  \omega\right)  $ versus $\omega$ for the second solution of
scalar particles. The physical parameters are chosen as; $B=1$ and
$\lambda=6$.} \label{fig4}
\end{figure}

\section{QNM\lowercase{s} OF BWBHSCP}

Gravitational waves from black holes possess the ringdown. The resonant frequencies that dominate the ringdown are studied by using the QNMs, which are described as waves propagating between the event horizon and spatial infinity. Namely, the QNMs of a black hole can be regarded as the solutions for the related equations of the perturbation concerned. QNMs also obey the following boundary conditions: i) pure ingoing waves at
horizon and ii) pure outgoing waves at spatial infinity.  A QNM is represented by a complex number with two types of information: the real term indicates the temporal oscillation and the imaginary term presents the exponential decay. These modes  can be detected by several large gravitational wave detectors which are still under developments \cite{sskk11}.

In this section, for the scalar perturbation, we follow the WKB approximation method to compute the frequencies of the QNMs of the BWBHSCP. To this aim, we should simply modify the derived one-dimensional Schr\"{o}dinger- equation \eqref{33} to the following Zerilli type differential equation:%
\begin{equation}
\frac{d^{2}Z}{dr_{\ast}^{2}}+V_{Geff}Z=0,\label{43}%
\end{equation}

where $Z$ supposed to have a time-dependence $e^{i\omega t}$ and
$V_{Geff}$ is the generic effective potential. The WKB approaches can be enlarged from the $3^{rd}$ to the $6^{th}$ order \cite{25} and more \cite{dd25}. The complex frequencies of the QNMs are defined as \cite{25}:
\begin{equation}
\omega^{2}=\left[  V_{0}+\sqrt{-2V^{\prime\prime}
_{0}}\Lambda\left(  n\right)  -i\left(  n+\frac{1}{2}\right)  \sqrt{-2V^{\prime\prime}
_{0}}\left(  1+\Omega\left(  n\right)  \right)  \right]  , \label{44}%
\end{equation}
where%
\begin{equation}
\Lambda\left(  n\right)  =\frac{1}{\sqrt{-2V^{\prime\prime}
_{0}}}\left[  \frac{1}{8}\left(  \frac{V_{0}^{\left(  4\right)  }}{V_{0}^{\prime\prime}
}\right)  \left(  \frac{1}{4}+\alpha^{2}\right)  -\frac{1}{288}\left(
\frac{V_{0}^{\prime\prime\prime}
}{V_{0}^{\prime\prime}
}\right)  ^{2}\left(  4+60\alpha^{2}\right)  \right]  , \label{45}%
\end{equation}

and%
\begin{multline}
\Omega\left(  n\right)  =\frac{1}{-2V_{0}^{\prime\prime}}\left[  \frac{5}{6912}\left(  \frac{V_{0}^{\prime\prime\prime}}{V_{0}^{\prime\prime
}}\right)  ^{4}\left(  77+188\alpha^{2}\right)  -\frac{1}{384}\left(
\frac{V_{0}^{\prime\prime\prime 2}V_{0}^{\left(  4\right)  }}{V_{0}^{\prime\prime3}}\right)  \left(  51+100\alpha^{2}\right)  +\right.  \\
\left.  \frac{1}{2304}\left(  \frac{V_{0}^{\left(  4\right)  }}{V_{0}^{\prime\prime}}\right)  ^{2}\left(  67+68\alpha^{2}\right)  +\frac{1}{288}\left(
\frac{V_{0}^{\prime\prime\prime}V_{0}^{\left(  5\right)  }}{V_{0}^{\prime\prime 2}}\right)  \left(  19+28\alpha^{2}\right)  -\frac{1}{288}\left(  \frac
{V_{0}^{\left(  6\right)  }}{V_{0}^{\prime\prime
}}\right)  \left(  5+4\alpha^{2}\right)  \right]  ,\label{46}%
\end{multline}

In Eqs. (\ref{44})-(\ref{46}), the primes and superscripts ($n=4,5,6;$ for the higher order derivatives) denote the differentiation with respect to $r_{\ast
}$. The value of $r_{\ast}^{0}$ is determined and $%
\alpha=n+\frac{1}{2}.$ Considering the effective potentials \eqref{35} and \eqref{36}, the QNM frequencies are tabulated in Tables \eqref{tab1} and \eqref{tab2} for the first and second kind BWBHSCP solutions, respectively.\\

\begin{minipage}[c]{.40\textwidth}
   \centering
  \begin{tabular}{ |c|c|c|c|c| }
\hline
$l$ & $n$ & $\alpha$ & $\beta$ & $\omega_{solution(1)}$\\
\hline
1 & 0 & 0 & 0.1 & 0.286589623-0.096033341i\\
&  & 0.1 & 0.2 & 0.033656151-0.197605927i\\
&  & 0.2 & 0.3 & 0.033454334-0.280248891i\\
&  & 0.3 & 0.4 & 0.034255997+0.501632599i\\
&  & 0.4 & 0.5 & 0.152033452+0.713727366i\\
&  & 0.5 & 0.6 & 0.311345572+0.918153498i\\
&  & 0.6 & 0.7 & 0.507559367+1.112884744i\\
&  & 0.7 & 0.8 & 0.737220788+1.295439260i\\
& 1 & 0 & 0.1 & 0.258327264-0.301168481i\\
&  & 0.1 & 0.2 & 0.023903202-0.025845636i\\
&  & 0.2 & 0.3 & 0.220700417-0.414178179i\\
&  & 0.3 & 0.4 & 0.387300679-0.818680303i\\
&  & 0.4 & 0.5 & 0.512701323-1.148126858i\\
&  & 0.5 & 0.6 & 0.652993941-1.349528912i\\
&  & 0.6 & 0.7 & 0.873546922-1.356239820i\\
&  & 0.7 & 0.8 & 1.310381508-1.124252140i\\
\hline
\end{tabular}
\captionof{table}{QNMs of scalar waves of the first kind BWBHSCP spacetime.}\label{tab1}
\end{minipage}\qquad

\begin{minipage}[c]{.40\textwidth}
   \centering
  \begin{tabular}{ |c|c|c|c| }
\hline
$l$ & $n$ & $\alpha$ & $\omega_{solution(2)}$\\
\hline
1 & 0 & 0 & 0.291114116-0.098001363i\\
&  & 0.1 & 0.029982323-0.406591230i\\
&  & 0.2 & 0.106971882-0.838143510i\\
&  & 0.3 & 0.217170609-1.295283573i\\
&  & 0.4 & 0.352035324-1.773332950i\\
&  & 0.5 & 0.504836567-2.269166503i\\
&  & 0.6 & 0.670912075-2.781643191i\\
&  & 0.7 & 0.847564070-3.310501544i\\
& 1 & 0 & 0.262211870-0.3074323461i\\
&  & 0.1 & 0.068560465-0.619918791i\\
&  & 0.2 & 0.231082654-1.302481917i\\
&  & 0.3 & 0.455973672-2.038317313i\\
&  & 0.4 & 0.725807111-2.816329955i\\
&  & 0.5 & 1.026894923-3.631446894i\\
&  & 0,6 & 1.351964324-4.482378509i\\
&  & 0.7 & 1.698488478-5.368078250i\\
\hline
\end{tabular}
\captionof{table}{QNMs of scalar waves of the second kind BWBHSCP solution.}\label{tab2}
\end{minipage}\qquad

The results seen in Table \eqref{tab1} reveal the effect of brane-world parameters $\alpha$ and $\beta$ of the first solution on the QNMs. The oscillation frequencies (real parts) first decrease with the increasing $\alpha$ and $\beta$ parameters then start to monotonically rise, this behaviour is also observed for the damping rates (imaginary parts). The QNMs of the second solution exhibit more regular behaviours as  $\alpha$ parameter increases: both real and imaginary parts grow with increasing  $\alpha$ values.

\section{CONCLUSION}
In this paper, the GFs and QNMs of gravitational perturbations throughout the BWBHSCP geometries are investigated. To obtain the corresponding GFs and QNMs, we have perturbed the BWBHSCP backgrounds with the Klein-Gordon equation. Taking the advantage of the symmetry, we decomposed the wave function into radial and angular (with the aid of the spherical harmonics) parts. The derived radial wave equation has been used to obtain the effective potentials \eqref{34}. Using the semi-analytical approach \cite{23}, GFs of the BWBHSCP metrics have been computed and represented in Eq. \eqref{41}. The GFs of BWBHSCP for some fixed parameters and various $\alpha$ and $\beta$ are depicted in Figs. (\ref{fig1}) and (\ref{fig2}) for first \eqref{4} and second \eqref{8} kind BWBHSCP solutions, respectively. We have deduced from those figures that the increase in $\alpha$ value decreases the GFs of the both BWBHSCP solutions.  Then, we have considered the $6^{th}$ order of the WKB approach to compute the QNM frequencies. Additionally, as shown in Tables \eqref{tab1} and \eqref{tab2}, our QNM results reveal that the BWBHSCP refers the classical QNM behaviors of the Schwarzschild black hole for $\alpha \rightarrow 0$ \cite{25}. Besides, as can be observed in the tables, for some $(\alpha,\beta)$ values, the imaginary term of the QNM frequencies are negative. Therefore, our results imply that some modes are found to be unstable. Moreover, we have also studied the effect of the GUP on the BWBHSCP entropies, till the square order of Planck length.

The results of this study are promising and motivate us for
further work in this direction. Therefore, we plan to extend our study to the other type brane world
black holes, such as the rotating ones \cite{rbh1,rbh2}.

\section*{Acknowledgements}
We are thankful to the Editor and anonymous Referee for their constructive suggestions and comments.

redpajama_set_name: RedPajamaArXiv


This cauliflower is an easy, tasty, crunchy treat. The curry spices give off their fragrant aroma and the coconut gets crisp and sweeter when toasted on the outside of the cauliflower.
-Preheat oven to 400 degrees Fahrenheit.
-Pull apart or chop cauliflower into 1 inch pieces (about the size of a large grape).
-Mix together the coconut flakes, curry powder, salt, and cayenne. You can do this in a bowl or an easier way is to use a gallon sized zip-top bag.
-Beat the egg white in a medium bowl just until frothy (~30 seconds).
-Toss the cauliflower in the egg white until evenly coated. Place the egg white coated cauliflower in the bag or bowl with the coconut and spices. Toss again until the cauliflower is coated.
-Empty the bag or bowl onto the greased baking sheet. Gently, to not dislodge too much coconut, spread the cauliflower into a single layer.
-Roast for 15 minutes. Gently turn the cauliflower again leaving it in a single layer. Roast an additional 10 minutes. Check for doneness.
-Remove and eat. Some of the spiced coconut will have fallen off and formed toasty clumps, serve these as a garnish on top.


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Last week, I had the opportunity to attend a fan trip to The Prairie Club in Valentine, Nebraska. While I remembered seeing The Prairie Club's two courses in the top five of GolfWeek's best in-state rankings (Dunes #2, Pines #4), the only golf-related images in my mind of Nebraska were of the pictures I'd seen online of Sand Hills, the country's number one overall rated course in nearby Mullen.
The perceptions of Nebraska in my mind were probably similar to the images of it in many of your minds: Endless farmlands and wide open spaces.
The Prairie Club proved to be the golf trip of all golf trips for us: Fabulous golfing, outstanding food/drinks and service, and very nice lodging in one of the resort's new cabins.
The food and service was world-class. Fresh, meaty bacon and breakfast sausages accompanied the typical continental breakfast staples, and my lunches consisted of Nebraska-raised burgers, pulled pork sandwiches and a French dip. And my dinners… My mouth started salivating again just remembering them… Locally raised prime rib, New York strips, rib eyes and fish. Surprisingly to me, my favorite appetizer of the trip was the local, fresh fried murels, which barely edged out the bull bites.
The owner of The Prairie Club, avid outdoorsman, golfer and businessman, Paul Schock, initially purchased the resort's land for its hunting and fishing resources. One of the area's renowned amateur golfers, Paul enlisted the help of Tom Lehman (course designer of the Dunes) and Graham Marsh (course designer of the Pines) to design and bring to fruition Nebraska and the Sand Hills area's premiere golfing destination.
A minimalist golfer's dream, the Prairie Club is isolated from anything like urban America. While it is located in Valentine, it is a solid 20-minute drive from the town. The only realistic lodging and meal options are found on site, and the quality of the club's offerings leave no reason for visitors to leave the premises.
The club features a beautiful new lodge with hotel rooms, restaurants and bars. Each cabin features a common space that would be perfect for card games, four suites with bedrooms and personal bathrooms, and a back patio that purveys the Snake River Canyon and looks up to a big country sky filled with more stars than I had ever seen.
One thing is for sure: The Prairie Club puts the getaway in golf getaway.
Brian Weis, owner/operator of GolfTrips.com, GolfWisconsin, GolfNebraska and about 40 other golf-related websites, and I left Milwaukee at 5 am last Sunday morning, dividing up our trip with a stop at The Harvester in Rhodes, Iowa, the state's number one and country's 82nd overall rated track.
Following 18 holes, and hundreds of miles of driving, we arrived at The Prairie Club in time for a meal and a couple of the club's most popular drink special: The Moscow Mule. Served in the traditional copper mugs, bar manager Birk also offers an apple version, which was refreshing on a warm afternoon between rounds.
We made our way to the cabin, where we were joined by one of the country's top golf course photographers, Brian Orr, and Darin Bunch of Fairways and Greens and Golf Getaways.
Brian and Darin were a lot of fun to play with – they are true throw-backs in the game of golf, playing hickory stick clubs from the green tees (~ 6000 yards)… And pretty well!
All great golf destinations need to have courses that are different enough that players do not feel like they are playing the same place over and over. The Prairie Club does that very well, with it's Pines and Dunes tracks.
Our first round in Nebraska was on Monday morning on the Pines course. The Pines, tipped out at 7403 yards, is a softer, slightly more picturesque version of sand hills golf, with several holes playing linksy similar to on the Dunes course, but primarily on the outskirts of the property amid Ponderosa pines and beautiful canyons.
The drives to both courses take at least five minutes from the lodge, promoting a feeling of escapism and that lovely disorientation that coincides with losing oneself on a great golf course.
The first three holes on the Pines course have a links-like feel, and are great warm-up holes to start dialing in the driver for what is to come.
Drive down the middle to left side of the fairway on one and take aim at a wide-open green.
The first par five on the course, the driving area on the second hole can be taken on to the left or right of the centrally located fairway bunkers. A back-stop on the right side of the green can be used to filter approaches toward middle and back pin locations.
With an elevated green, a ridge dividing it, and sand traps all around, the third is a fairly straight forward par three for The Prairie Club.
A long par four, the fourth ushers golfers out of the Pines course's first links segment and toward the first Snake River Canyon portion of The Prairie Club.
Part of what makes the Pines course so playable is the mix of woodland and links golf that it provides. The woodlands portion of it emerges on the fifth, with a somewhat blind tee shot that has to carry sand and is best driven with a hard fade on this dogleg right par four.
An excellent par three, the sixth plays to a raised green with a false front and huge ridges that make hitting the right level of the putting surface essential if hoping for a realistic chance at birdie.
One of my favorite holes at The Prairie Club, the seventh is a long par five with a lot of character. The drive can either be drawn long, or else played short to stay within the tree lines. Hit an accurate second shot to set up a reasonable approach downhill and over the right-side tree line.
Heading out of the trees again, the eighth can be missed right to the shared fairway between it and the adjoining ninth.
I love a great drivable par four, and the ninth on the Pines course is an outstanding one! At 300 yards from the white tees, it is next to impossible for big hitters to refrain from going for it. The green of the ninth hole features the biggest false front on the course, and is one of the shortest greens from front to back.
One of the many sand traps that protect the already-difficult green complex on the ninth. Can you believe I actually parred from here? Somewhat of a typical par for me, actually: Drive to the green-side bunker, left the second shot in the bunker, hit the back-left of the green, rolled in a 40-footer… This game's easy!
The green on the par three tenth is quite intimidating. It's obvious from the tee boxes that it breaks hard toward the middle from the left to the right, so a left-side pin location looked pretty daunting. The four of us were all within 20 feet off the tee, though, and I was the only one to birdie it.
Don't get excited – that was the end of my hot putting for the trip.
Eleven is a long, tight par five. Keep everything down the middle on this hole, and the second shot somewhat left to keep a good angle at the green.
An intimidating driving hole, the twelfth is best played with a long draw from the white or green tees, or long fade from the tips, to keep tee shots in the short grass. The hole bends slightly leftward, to a raised green that falls off in all directions to short chipping areas.
Thirteen heads back to the sand hills, with a sharply uphill par four with deep, craggy bunkering everywhere.
Fourteen was tough the first time we played it: Looking at the cart's on-board GPS system, we could tell there was 200 or so yards of fescue to clear, but we didn't know much else. Both courses at The Prairie Club do a good job of off-setting tee boxes so they are rarely straight-ahead – this is a prime example of that on the Pines.
During our second round of the trip on the Pines course, a massive storm was brewing in Valentine – baseball-sized hail took out cars and roofs, and gave us winds that stayed steady in the 35-plus mile per hour range, peaking at gusts well over 60. The wind was directly behind us on this 326-yard uphill par four, so I went for it.
Hitting the back-right of the green, I geared up for a 50-foot eagle putt that I put 20 feet past the pin. I then got about half-way there and really started getting nervous. Fortunately, the next one went in.
While the weather report was telling us we should expect 80% chance of rain, the course was never touched. We lucked out every day with the weather, making the experience even that much better.
A long par five, the fifteenth drives uphill and plays to the right. The fairway in the driving area breaks hard toward the bottom-right, leaving no visibility for the second swing to tee shots that collect near the bottom.
A memorable par four, the sixteenth starts with a demanding tee shot, and an intimidating approach. The Snake River Canyon provides a picturesque natural back-drop to the green complex, and begs golfers to play short of the putting surface.
Probably my favorite par three on the Pines course, the seventeenth is a mid-range one-shotter that plays to a green that is much bigger than it looks, especially from front to back.
If you're looking for a fantastic finishing hole with choose-your-own-adventure features everywhere, the eighteenth is just the hole for you. A big par five, the eighteenth tips out at 595 yards, and plays to 549 from the whites.
The perfect tee shot for big hitters is to the internal bend of the fairway, leaving a shot of 200 yards over the canyon to a raised green that fronts the clubhouse.
The ideal tee shot for anyone who cannot play a 200-yard approach is to the middle or right side of the fairway, where they can then play the fairway that bends around the right side of the wasteland.
Enjoy the look-back on the eighteenth hole and the Nebraska sand hills with a Moscow Mule on the back patio following your round. Grab a bite to eat, too – you'll need the energy for the wild and dramatic golfing experience that is the Dunes course.


Troutdale Volunteer Fire and Rescue recently celebrated the unveiling of their new steps and porch, which will be used to host events held at the rescue squad building for the Troutdale community each year.
The porch construction was the result of a collaborative effort between Troutdale town officials and the fire and rescue squad department members. Replacing the building's old porch took around a month, and was celebrated with a community meal and a ribbon cutting ceremony on Oct. 20.


Working with award-winning Bristol-based app developers, Calvium, Bristol Parkhive (a UWE/Bristol Parks Forum collaboration in support of Bristol's European Green Capital Year 2015) is creating a smartphone app to promote Bristol's parks and green spaces to visitors and serve as a valuable resource for residents.
The app will connect information about parks facilities, walking routes and trails, parks groups activities and events, travel info, and local stories and histories, into a user-friendly, visually appealing digital product which aims to enhance the usability and visibility of ALL of Bristol's parks and green spaces.
We are seeking students to help develop the content for the app, by generating and producing content for specific parks and green spaces, writing copy and doing some simple research.
The role will include: Writing copy for the app (for example, describing the individual parks and green spaces and what they have to offer); Researching and working with community parks groups around the city to collate/generate interesting local stories and information; visiting specific parks and green spaces to collect first-hand information when existing content is unavailable; Organising content and taking notes.
Suited for: This position would be well suited to students studying History, Social Sciences, Journalism, English or Environmental subjects, and offers a great opportunity to develop your skills and experience through a live project which aims to promote Bristol's parks and green spaces and will contribute to Bristol's European Green Capital Year 2015 programme - which has an international reach & audience.


A real estate specialist from Medford Pads can be a tremendous asset throughout the process of purchasing new Medford property. Your agent will do much more than simply showing you houses for sale in Medford MA. They will work with you to assess your financial situation and devise the best purchasing plan for you, as well as making sure that both parties involved in the sale are on the same page throughout the process. Working with a Medford MA real estate agent is the best way to make sure that the personal and financial goals of your Medford purchase are turned into a reality.
Once you've consulted with a Medford agent and made the decision to buy new property, you can start the exciting part of the process: shopping for brand new Medford MA real estate. Finding a new Medford property that meets your needs can be time consuming, but staying committed to the hunt is the only way to guarantee that you'll find the perfect property for you.
The best way to locate new Medford real estate is by attending multiple showings of several different houses for sale in Medford MA. During the search process, your Medford agent will constantly keep you updated with the latest sales listings and information so that you have all the resources you need to make the best decision. Remember, it is important to stick with the goals that you and your Medford agent have determined no matter how long the search process takes. When you finally find the perfect new Medford property, you'll know the time was worth it.
After you've found an ideal new Medford property, your Medford agent will work with you to create a competitive offer for your desired property based on a Comparative Market Analysis. A Comparative Market Analysis helps you determine an offering price by comparing your prospective property to other similar properties that have recently been sold in the Medford MA real estate market. This allows your Medford agent to craft the most effective offer to help get you the Medford property you want.
When negotiating your offer with the seller, it is of key importance to remember that different purchasing terms can have different (and sometimes negative) effects on the value of your new property. Once you have submitted your offer and submitted your deposit to the seller, the offer can be accepted. You and your Medford agent will review several important factors, including property inspection, your financing contingency, a review of any applicable condominium documents, and the drafting of a mutually beneficial Purchase and Sale (P&S) document that will bind the transaction.
Part Four - Closing on Your New Medford Property.
Once the seller has accepted your offer, both you and the seller should expect to begin completing any contingencies about 10-14 days before signing the P&S agreement. At the signing of the P&S, you will submit another deposit to further bind the sale. Typically, it takes 14-45 days from the signing of the P&S agreement to close on your new Medford property.
Note: It is always recommended that buyers work with a Medford MA real estate attorney throughout the purchasing process. They can be an extremely helpful resource in ensuring that your purchase is a success.
Even after the purchase of your new Medford property is complete, your Medford real estate agent can still be a valuable resource. Keeping in contact with your local Medford real estate agent can be beneficial to you as a new property owner. They can assist you with questions about your property, connecting you with local Medford services, and provide you with any additional real estate information you might need.
To speed up your search, sign up below to receive up to date sales listings for houses for sale in Medford MA.


I am an assistant professor in English Education at Brigham Young University, where I have been teaching full-time since 2007. Before that, I taught junior high and high school English courses for eleven years. My research interests include any pedagogical issues connected to English or Language Arts teaching, with a focus on digital literacies and grammar instruction. I am also passionate about young adult literature and its role in the classroom.
At BYU, I teach methods courses to pre-service English teachers and supervise student teachers. Each course has content on this site to allow students to engage in dialog outside of class and to collect resources and materials.
A course in methods for teaching grammar in the secondary schools. In this course, we explore a contextual approach to teaching grammar, advocating that we situate grammar/language instruction in meaningful reading and writing instruction.
This is the capstone course for our English Teaching majors, integrating the content from all of the previous methods courses and providing our majors with a practicum experience in local classrooms.
This literature course (required for English Teaching majors and an elective for English majors) focuses on literature written for young adults. We cover a broad range of young adult titles, from S. E. Hinton's Outsiders to titles that are popular today.


text:
Q: R: Iterate over pairs of columns in dataframe by regex match I need to iterate over pairs of columns in a dataframe.  Every column will have a corresponding column with a "_ans" suffix (and identical prefix).  I need to create new column with the suffix "_score" if the "_ans" column and the comparison column are equal.
Reproducible example:
    set.seed(42)
    df <- as.data.frame(matrix(sample(1:9, 10 * 5, replace = TRUE),
    ncol = 10, dimnames = list(NULL, c("CB1", "LB2", "CW3", "WC1",
    "LW20", "CB1_ans", "LB2_ans", "CW3_ans", "WC1_ans", "LW20_ans"))))

> df
  CB1 LB2 CW3 WC1 LW20 CB1_ans LB2_ans CW3_ans WC1_ans LW20_ans
1   3   9   6   9    1       7       3       2       5        1
2   3   3   4   2    5       1       3       7       4        4
3   7   7   7   1    7       6       4       6       3        4
4   5   8   7   5    2       6       2       7       2        3
5   6   3   3   2    3       1       9       9       1        4

If I would do this manually, it would look like:
df$CB1_score <- df$CB1 == df$CB1_ans
df$LB2_score <- df$LB2 == df$LB2_ans
df$CB3_score <- df$CW3 == df$CW3_ans

Resulting output:
  CB1 LB2 CW3 WC1 LW20 CB1_ans LB2_ans CW3_ans WC1_ans LW20_ans CB1_score LB2_score CB3_score
1   3   9   6   9    1       7       3       2       5        1     FALSE     FALSE     FALSE
2   3   3   4   2    5       1       3       7       4        4     FALSE      TRUE     FALSE
3   7   7   7   1    7       6       4       6       3        4     FALSE     FALSE     FALSE
4   5   8   7   5    2       6       2       7       2        3     FALSE     FALSE      TRUE
5   6   3   3   2    3       1       9       9       1        4     FALSE     FALSE     FALSE

And so on.  I have been working on this for an hour trying to figure out a way to automate this without for loops, but cannot think of the right approach.

A: Here is a tidyverse solution using purrr:map:
map(c("CB1", "LB2", "CW3", "WC1", "LW20"), ~ df %>%
    mutate(
        !!(paste0(.x, "_score", collapse = "")) :=
            UQ(rlang::sym(.x)) == UQ(rlang::sym(paste0(.x, "_ans", collapse = ""))) )) %>%
    reduce(., left_join)
#  CB1 LB2 CW3 WC1 LW20 CB1_ans LB2_ans CW3_ans WC1_ans LW20_ans CB1_score
#1   9   5   5   9    9       5       7       8       4        9     FALSE
#2   9   7   7   9    2       4       8       1       4        8     FALSE
#3   3   2   9   2    9       9       4       2       1        6     FALSE
#4   8   6   3   5    9       5       7       9       9        9     FALSE
#5   6   7   5   6    1       8       1       6       4        6     FALSE
#  LB2_score CW3_score WC1_score LW20_score
#1     FALSE     FALSE     FALSE       TRUE
#2     FALSE     FALSE     FALSE      FALSE
#3     FALSE     FALSE     FALSE      FALSE
#4     FALSE     FALSE     FALSE       TRUE
#5     FALSE     FALSE     FALSE      FALSE

A: One base-R solution:
nms <- colnames(df)
ans <- nms[grepl("_ans$", nms)]
qstn <- gsub("_ans$", "", ans)
# in case there's something wrong with the names??
ans <- ans[ qstn %in% nms ]
qstn <- qstn[ qstn %in% nms ]

scores <- df[qstn] == df[ans]
colnames(scores) <- paste0(qstn, "_score")
cbind(df, scores)
#   CB1 LB2 CW3 WC1 LW20 CB1_ans LB2_ans CW3_ans WC1_ans LW20_ans CB1_score LB2_score CW3_score
# 1   9   5   5   9    9       5       7       8       4        9     FALSE     FALSE     FALSE
# 2   9   7   7   9    2       4       8       1       4        8     FALSE     FALSE     FALSE
# 3   3   2   9   2    9       9       4       2       1        6     FALSE     FALSE     FALSE
# 4   8   6   3   5    9       5       7       9       9        9     FALSE     FALSE     FALSE
# 5   6   7   5   6    1       8       1       6       4        6     FALSE     FALSE     FALSE
#   WC1_score LW20_score
# 1     FALSE       TRUE
# 2     FALSE      FALSE
# 3     FALSE      FALSE
# 4     FALSE       TRUE
# 5     FALSE      FALSE

A: One base R option would be to iterate over all columns in your data frame which don't end in _ans, and then compare them against their _ans counterparts.  We can use grepl and sapply here:
cols <- names(df)[grepl("^(?!.*_ans).*$", names(df), perl=TRUE)]
for (name in cols) {
    df[paste0(name, "_score")] <- df[[name]] == df[[paste0(name, "_ans")]]
}

df

  CB1_score LB2_score CW3_score WC1_score LW20_score
1 FALSE    FALSE     FALSE     FALSE       TRUE
2 FALSE    FALSE     FALSE     FALSE      FALSE
3 FALSE    FALSE     FALSE     FALSE      FALSE
4 FALSE    FALSE     FALSE     FALSE       TRUE
5 FALSE    FALSE     FALSE     FALSE      FALSE

Demo

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text:
The view from Scotland: Still hanging on the telephone
Despite the silence from London, Alex Salmond is getting to grips with his fiefdom.
By Douglas Fraser
The number to dial is 0131 556 8400. That reaches the Scottish Executive, where Alex Salmond, the Scottish First Minister, awaits a call.
Diplomatic protocol requires that the PM offer his congratulations on the election of other government leaders. Tony Blair did so for Nicolas Sarkozy in the passable French that he learned at Fettes College. Just across Scotland's capital from his alma mater, the phone isn't ringing. This isn't protocol, but the politics of the playground. Although Blair met Colonel Gaddafi and brokered peace between Ian Paisley and Martin McGuinness, the Scottish Nationalists are supposed to be content with a call from Douglas Alexander.
Perhaps the Westminster leadership limbo leaves it unclear who has to do the dirty work of dealing with a Nationalist leader whom the PM and his successor loathe. Perhaps they think that if they ignore him, he might go away. But the best guess at the reason for Labour's behaviour is that the party is in denial.
Labour had a better result than most feared, down by only four seats. Yet warning Scots that a vote for the SNP would have consequences akin to biblical famine and pestilence did not stop the Nationalists gaining 20 seats, ending on a knife edge of 47 to Labour's 46. With the Tories and Lib Dems abstaining, a couple of Green votes were enough to ensure that Labour's Jack McConnell was tipped out of office, handing the Nats power for the first time in their 73-year history.
The upside-down world of Lewis Carroll
The twilight of the British Union
The year woke broke: a brief history of a contested word
The evidence of denial was led by Philip Gould, who last month offered NS readers his curious reading of the campaign as "Labour at its best". He came north to repeat this to MSPs, telling them how proud they should be. From Westminster, it may seem that the loss of power on the Celtic fringe, with Welsh Labour holding on to office with little power in Cardiff, is an unfortunate consequence of midterm blues: from Holyrood, it is a calamity. Ten years ago, Labour won 56 out of 72 Scottish seats at Westminster. At Holyrood, 37 Labour constituency MSPs remain and many more have turned marginal. Under a new voting system, the party lost a third of its councillors and now has majority control of just two councils.
Now, disbelievingly, Labour faces four years in opposition and has some hard questions to answer. Why did Scots think they were being taken for granted? What has the party delivered for the bleak town centres it represents, from Brown's Kirkcaldy to McConnell's Wishaw? How did it lose its role as the political vehicle for change, aspiration and Scottish identity?
Lovestruck teenager
Midterm blues can take some of the blame for the loss of power. Brown can blame McConnell. McConnell can blame Brown. Both can blame Blair. Or they could take comfort from how Labour's vote did not collapse and the SNP victory margin was eye-wateringly tight.
Labour's biggest danger is that it will believe its own spin and ignore the need to renew itself and its hollowed-out organisation, or to purge the numpties – the dead wood, underperformers and time-servers who control tiny local party machines – from the ranks of its MSPs and MPs.
The lack of a call from No 10 doesn't look good for Salmond, either. Looking miffed as he waits by the phone, he seems less like a wannabe statesman than a lovestruck teenager. But, for all that he is 18 seats short of a working Holyrood majority, he has set quite a pace for his new administration.
Much of this was set out in mid-March, when a 49-item, "first 100 days" strategy was published, ranging across big-budget commitments for freezing council tax, more police, nurses and teachers and free prescriptions; a start to legislation on waiting-time guarantees; writing off and replacing student debt; and direct elections for health boards. This was coupled with easy bits, from appointing a council of economic advisers to declaring a two-month winter festival from St Andrew's Day to Burns Night. So far there has been a slimmed-down ministerial team, a block on new nuclear power, publication of a long-suppressed report into government spending, a call for Scotland to have its own Olympic team and abolition of Forth Bridge tolls.
Being a canny sort, Salmond is positioning each proposal to make it hard for his opponents to vote against. He is also holding back on the tricky parts. He has not yet set about introducing a local income tax or replacing public-private partnerships with an arm's-length agency issuing bonds. And he has yet to admit to his own party that the Holyrood arithmetic means they won't get their independence referendum any time soon.
He has signalled the fights he wants to pick with Downing Street, including a claim on some welfare budgets and a share of North Sea oil revenue. That is where the Salmondista revolution is being watched with most interest, but it may prove hard to press for more powers or cash if Downing Street won't even speak to him.
Douglas Fraser is Scottish political editor of the Herald
Douglas Fraser
Salmond's audacious leap
Salmond: set England free

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For those that know me, it is no secret that animals are a huge part of my life (okay, basically my whole life!). I always tell my Nana it is her fault that I've come to love animals so much. When I was very young, my Nana and Papa used to take my sister and I to feed the stray cats behind the hospital she worked at. Her and my Papa went faithfully, trekking through the woods to make sure those cats had food. These are memories that have stayed in my heart forever, and my love for animals grew from there (specifically for the homeless ones). I was fortunate to grow up alongside many dogs throughout the course of my childhood. I adopted my first dog right after I graduated college, and he was the light of my life. For several years I lived in an area where there were countless stray animals, and that is when I found my passion for rescue work. My love for animals and my desire to do more led me to my dream job at the SPCA as an Adoption Specialist. Rescue work isn't always easy. We see things that bring us to tears and shatter our hearts; but it is exactly where I am supposed to be. There is nothing more rewarding than seeing the happy endings, but we can only continue to keep saving lives with your help and support! There are so many animals waiting for their happily ever after... would you consider contributing and be a hero to these animals?


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How safe are our reinforced concrete buildings?
Flux-Cored welding an option for South Africa?


text:
When Medicare is the Piggy Bank
September 28, 2009 / 2:54 PM / AP
Medicare is looking like a big fat piggy bank for health care overhaul.
President Barack Obama and the Democrats want to pay for much of their plan to cover the uninsured by cutting hundreds of billions from the Medicare budget over the next 10 years.
From its inception, the health plan for seniors has been kept afloat by taxes out of workers' paychecks. Now, Medicare savings would count toward helping uninsured working-age children and grandchildren afford their own coverage.
Most seniors are willing to help younger generations. But having reached that point in life when you have to spend more time in the doctor's office than you'd prefer to, older Americans worry the cuts will mean lower quality care.
The proposed cuts to hospitals, nursing homes and other providers are bigger than any Congress has imposed since the late 1990s. However, in percentage terms, they're far from the largest ever. And Democrats are also proposing to spend tens of billions to improve Medicare prescription coverage and preventive care.
"Seniors should definitely be paying attention," said Mark McClellan, who ran Medicare under President George W. Bush. "There's some redesign, some improvements, but unquestionably there would be some adverse impacts. It's a mixed bag, but it's not like the sky is falling."
Here are some questions and answers on how the health care overhaul would affect Medicare beneficiaries:
Q: Obama says no one is talking about cutting Medicare benefits, is he mistaken?
A: He might want to add a caveat. Benefits under traditional Medicare won't be cut. But seniors who've signed up for private insurance plans through Medicare Advantage could lose valuable extra benefits, according to the Congressional Budget Office.
For years, the government has been paying the private plans more than it costs traditional Medicare to deliver similar services. The plans used the money to provide extra benefits, mainly lower copayments and deductibles. Seniors on tight budgets responded by signing up, and now nearly one-fourth of Medicare recipients are in private plans.
As Obama and the Democrats wean private plans off their subsidies, beneficiaries will suffer the consequences.
"Some beneficiaries will lose additional benefits they have been fortunate to have been receiving," said Robert Berenson, a physician turned Medicare expert at the Urban Institute public policy center. "They are likely to see higher out-of-pocket costs, and it's likely that some plans will drop out of the program."
On the other hand, everyone on Medicare will save a little on their monthly premiums as payments to private plans are scaled back.
Q: How extensive are these cuts anyway?
In dollar amounts, they're huge. They appear more manageable when viewed as a share of overall Medicare spending.
After accounting for proposed Medicare improvements, the House plan would reduce net spending on the program by $218 billion over 10 years, according to an analysis by the Kaiser Family Foundation. The Senate Finance Committee proposal would decrease net spending by $377 billion over the same period.
Kaiser found that the House cuts amount to 3 percent of projected Medicare spending from 2010-2019, while the Senate reductions are about 5 percent. By comparison, the 1997 balanced budget bill passed by a Republican Congress and signed into law by then-Democratic President Bill Clinton reduced Medicare spending by 12 percent over 10 years.
Research indicates that as much as 30 percent of Medicare spending goes for services that are of questionable value to patients.
Q: With all these cuts, how can Obama claim he's improving benefits?
A: By offering cheaper prescription drugs.
Under a deal with the White House, drugmakers would offer a 50 percent discount on brand-name prescriptions for beneficiaries who fall into the "doughnut hole," the notorious Medicare coverage gap. House Democrats want to eliminate the doughnut hole by 2023, but drug industry opposition may thwart them.
Coverage for preventive care would also get better.
The House and Senate bills eliminate copayments and deductibles for prevention. The House would also increase subsidies to help low-income seniors with copayments and deductibles.
"When you look at the improvements in traditional Medicare filling the doughnut hole, free prevention, help for low-income seniors I think all of those things narrow the gap between what Medicare Advantage has been providing and what traditional Medicare provides," said John Rother, top strategist for AARP. "In effect, they are improving the benefit for everyone."
Q: I keep hearing that Congress wants Medicare to pay for quality, not quantity. What does the legislation say?
A: The bills would launch several experiments to reorganize how doctors and hospitals care for patients, particularly seniors with chronic illnesses. If the tests work, lessons could be rapidly adopted throughout Medicare. Two major ones deal with "medical homes" and "accountable care organizations." Here's the background:
Seniors with several chronic illnesses see many different doctors a year, and juggle dozens of prescriptions. If they had a "medical home," a general practice doctor would take on the role of patient advocate and care coordinator. That could be as basic as ensuring one specialist doesn't recommend medication that reacts against a drug another doctor has prescribed unintentionally sending the patient to the emergency room.
An "accountable care organization" is a network of hospitals, nursing homes, doctors' offices and other providers who work together to provide the best possible care, while trying to operate efficiently and hold down costs. Models include Minnesota's Mayo Clinic and Intermountain Healthcare in Utah.
Lawmakers will be looking carefully to see how beneficiaries and providers in their home states are affected by the proposals.
More changes are in store in coming years. For Baby Boomers, it may not look a whole lot like grandma's Medicare.
First published on September 28, 2009 / 2:54 PM
Ex-Air Force officer at Capitol riot intended "to take hostages"


text:
"We're not coming over here and telling them how to do anything. The guys on the ground in New Zealand already know how to do it."
James Henderson (New Zealand Reseller News)
As far as working cliches go Down Under, it's an all too familiar sight to see those big bad straight-talking Aussies cross the Tasman, march steadfast into the boardroom and attack the jugular of its New Zealand division.
Seen merely as a side-dish amidst an Australian degustation, Kiwis are often considered after thoughts, lost in the bigger picture of business.
But that of course, is a load of baloney, typified by Express Data's recent rebranding in New Zealand, incorporating all things Dicker Data as the distributor moves onto bigger and brighter days in the Kiwi channel.
"To be honest," admits David Dicker, CEO, Dicker Data, "we haven't had to do anything. The guys on the ground in New Zealand already know how to do it.
"We're not coming over here and telling them how to do anything. In fact, this operation is run much more in line with how we run our operations in Australia."
Over a year since confirming the completion of its AU$65.5 million purchase of the competing distributor, on both sides of the Tasman, Dicker admits the Kiwi division of the business has been, to a degree, left to its own devices.
"This was already a good company so we didn't want to come in and make a lot of changes, we didn't see the need," he says. "To be honest New Zealand runs so well that we've been able to leave it alone for a year so we could focus our efforts on the Australian aspect of the acquisition.
"Express Data in Australia was a heavily process driven organisation with a different structure and philosophy to Dicker Data, we were completely different companies. But in New Zealand that's not the case. Just look at their philosophy and aims, they're on the same page as us."
Echoing Dicker's observation of the Kiwi arm of the business, Dicker Data New Zealand chief Phil Presnall says the acquisition and subsequent rebranding has had minimal to zero impact on the company, setting the distributor up for further growth across the country in 2015 and beyond.
"It's been easy," he adds, "when we got acquired we realised we were more like these guys than our original parent company and this came after only a few conversations."
Having recently brought Toshiba on board in New Zealand, Presnall's task in the Kiwi market is clear; recruit more vendors and drive greater revenue.
"Without being specific about numbers, we're looking to bring more vendors across in the volume space so we're expecting large double-digit top line growth in terms of the next 12 months," he forecasts.
"Going forward I'd like to think we'd have at least another two or three significant vendors on board by the end of the year."
Very much on Dicker Data New Zealand's target list is HP, and despite the tech giant being currently locked in across the ditch, Dicker accepts that when it comes to signing up new vendors, patience is very much a virtue.
"Our main function is to get vendors," he adds. "That's how I see it. We don't have HP here and that isn't great given HP is our biggest customer in Australia.
"We should have HP in New Zealand but we don't and that's the politics of the whole thing. We'll have to work on that and it's a long process.
"In Australia it took us nearly 15 years to secure HP printers so it is a difficult and length process. I've been in the business for 37 years so I can be patient. Obviously we want to do it as quick as we can but it is difficult to take it away from the other guy."
Admitting that Dicker Data "got lucky" in Australia following Ingram Micro's well-documented SAP fiasco, Dicker accepts that such circumstances allowed the distributor to make serious inroads into the market which their channel rival has so far struggled to claw back.
"We're operating in a numbers game, if you hit the numbers you'll get the result over time but if you don't then you'll be screwed, it's that simple," he adds.
"The way I see it is our revenue is not too far behind Ingram Micro in the commercial space so I don't see why we can't replicate that here."
In pursuing HP, Dicker naturally faces stiff competition from current distributors Ingram Micro and Exeed in New Zealand, but such is the nature of the channel veteran, he accepts that it won't be easy.
"More vendors equates to more revenue and we are actively trying to bring across existing vendor relationships from Australia to New Zealand, and likewise, vice-versa," he says.
"But even with Toshiba, we're the company's biggest customer in Australia and their longest standing partner but despite all this it still took a year to get the New Zealand deal over the line.
"And let's not forget, they were the ones who threw the balls up in the air so yeah, you have to be patient."
For Dicker the process in New Zealand will be no different to Australia; distribution is a master and slave relationship, and "we are the slaves."
"It has worked like that since 1978 and I figured that out pretty early on when I first started in this game," he says. "They come to us and want things done and we have to provide.
"We have to be better than the other guys and considering they are foreign multinationals in the New Zealand market, we have to respond and stay competitive."
More vendors undoubtedly brings the need for more resellers, with Presnall sending a clear message to the channel that if "anyone wants to transact any of our vendor lineup then we want to do business with you and give you a great experience."
Requiring no specific criteria or expertise, if Dicker Data are representing a brand in New Zealand, then under the leadership of Presnall they will be selling to everyone that sells that brand.
"It's not rocket science," Presnall adds. "Our role in New Zealand as a distributor is to make our number while keeping our vendors, staff and customers happy. Those are the basic requirements of any business.
"We've been very fortunate to have had the freedom to execute on this and do what we believe is the right thing for the business in New Zealand.
"The Dicker Data guys have built up a lot of IP and knowledge over the years and it is a great opportunity for us to leverage that where possible. We are backed with heaps of resource so for New Zealand, everything is upside following this deal.
"Dicker Data is a relatively flat organisation so everything is only a phone call away, we don't have to jump through hoops to get anything done and given the whole industry is undergoing huge change at the moment, being agile gives us a massive advantage."
Presnall, held in the highest regard by his new Australian colleagues, believes the key for Dicker Data moving forward in New Zealand is to maintain a level of flexibility that allows the company to "change before you need to change" while continuing to reinvent itself amidst great change in the Kiwi channel market.
"We've got to stay on top of our game," he adds. "The same is not enough because the competition will leap frog us which is why we play to our strengths.
"The strength of our business evolves around the relationship we have with our customers and we have better relationships that the other guys because we are always there for them.
"If everything is straight forward then fine but nothing ever is in this world and that's why we are available at the other end of the phone, or at your door, to come fix an issue in minutes rather than days."
Such is Presnall's determination to maintain his company's notable high-levels of customer service, that Dicker revealed no plans to keep vendor product managers offshore in Australia, serving as a regional point of contact rather than in-country.
"That wouldn't work," he says. "I've had a house in New Zealand since 1999 and I know that approach wouldn't work. Our operations are on the ground and that's where our support system will stay.
"Technically, we're happy to run New Zealand as an independent operation in that respect. We will allow Phil to go to market how he sees fit as we have complete faith in the Kiwi team.
"Of course we could run it out of Australia but it doesn't make sense too, so we won't."
Capturing the mood of the company across Australia and New Zealand, Presnall believes "vendors want a local presence."
"People in New Zealand like you to turn up on their doorstep and provide the lowdown on latest products and help solve problems, no matter how big or small they are," Presnall adds.
"The face-to-face element is huge for us in terms of how we engage with our channel and that won't change."
As reported by Reseller News' sister publication ARN, Dicker Data is on track to crack AU$1 billion in revenue for the financial year, following two strong first quarters that are expected to continue into Q3 and Q4.
Currently targeting AU$30 million profit in sales, Dicker remains confident that collectively speaking, the company is "going to get it."
"That's our target across the two entities," adds Dicker, banishing the notion that when it comes to New Zealand, he is merely cashing a cheque at the end of each month.
"Of course we have certain revenue targets in mind but as I keep repeating, we're not trying to blend New Zealand into Australia or ask them for monthly reports etc. They know what they need to do so we're happy to let them get on and do it."
With the ribbon now cut and business as usual, Dicker Data in New Zealand looks set to banish the stereotype of Australian interference, and given Presnall's philosophy and go-to-market strategies, it would appear a certain Mr Dicker is right to leave him to it.


text:
Q: height of text compare to an image I can't put the text in the middle height of the image it is in with.
This is what I write in the HTML:

x

This is what I write in the CSS:
.languagesIcons {
   width: 55px;
   margin: 0 10px 0 0;
}

All of that runs in a
 which its CSS is:
#languages {
   display: grid;
   grid-template-columns: repeat(4, 1fr);
   font-size: 22px;
   gap: 30px;
   padding: 20px 0 0 0;
}

A: You should use position:absoluteon the image and the text placed in a span for example and use position:relativeon the container which is a p tag here. Then you can adjust its position with transform:translateY()for example.
See the code below :

p{
position:relative
}

.languagesIcons {
   width: 55px;
   margin: 0 10px 0 0;
   position:absolute
}
div{
   display: grid;
   grid-template-columns: repeat(4, 1fr);
   font-size: 22px;
   gap: 30px;
   padding: 20px 0 0 0;
}
span{
position:absolute;
transform:translateY(50%)
}

x

A: You could just add vertical-align:middle to your languageIcons class:
.languageIcons{
width:55px;
margin: 0 10px 0 0;
vertical-align:middle;
}

A: To vertically align text and image, use :

    x


text:
Proof Of Aliens Life
Alien Encounters
Alien Sightings
Alien Crop Circles
Ancient Astronaut Theory Believes More In Existence Of Aliens Than The Gods
02/09/2016 09/07/2019 Kim Jones
Do Gods exist? This is one question that could divide the whole human population into two with each parties defending their concepts and refuting others' with their own set of logic and evidence. Gods, as per the ancient astronaut theory are nothing but the extraterrestrial aliens who visited the Earth thousands of years ago and taught a number of advanced things to humans to help them get advanced in terms of technology, science, engineering and religions in leaps and bounds.
There are no Gods, there are aliens
Ancient artifacts, religious texts and many other forms of physical specimens do point to the certainty that mankind used to get advised from people who used to descend from the skies in special carriers or chariots. These descendants from the sky had access to heavenly weaponry and were highly advanced in terms of applied science. While the religious people love to believe that these people from the sky were Gods who had supernatural powers, the proponents of the ancient astronaut theory use these texts and artifacts as a reliable proof of the existence of aliens and the fact that the aliens did come to the earth and helped in human advancements.
Evidence that makes the theory strong
Mentioning about gods or such extraterrestrials is found in scriptures and art specimens of almost every civilization of the planet which strengthens the concept of ancient astronauts. The Mayan Chilam Balaam texts mention about men in flying rings, who descended from the sky in flying vessels. The tablets of Anunnaki talk about Enki who came from a planet called Nibiru that circled the sun every 3600 earth years. Various Sumerian artifacts that have been excavated over different periods of time bear imageries of strange creatures that have little resemblance to humans or any other earthly creature.
Prehistoric and ancient Petroglyphs that are found in many parts of the world bear images of creatures that have little resemblance to humans and point more towards the fact that these were images of aliens who had come down from the skies and met the dwellers of the planet.
Some of the great monuments and engineering structures of the ancient world like the Giza Pyramids, the Stonehenge, the submerged cities that are thousands of years old and found in various parts of the world also point towards the intervention of divine powers in their making as it was not possible for humans to erect such monuments with the limited scientific and engineering skills of those times. The divinity can be looked upon as the scientific knowledge of the aliens, the ancient visitors from the planet.
Description of the video
In the video, Giorgio A Tsoukalos, an eminent proponent of the ancient astronaut theory and publisher of 'The Legendary Times' magazine explains about the ancient astronaut theory with various examples and evidence. He refutes the belief of extraterrestrials being the Gods and harps on the fact that there were no Gods and that all the ancient activities carried out by the humans were done with assistance from aliens.
In his agenda to explain and prove the ancient astronaut theory, Tsoukalos mentions about certain creatures like the two-headed dog with six legs or the giant flying turtles and about extraterrestrials who had the resemblance to humans but had elongated craniums. He produces pictures of creatures that he tries to relate to the aliens, the ancient visitors who had landed on the soils of the Earth.
Top 20 Anunnaki Aliens Facts
The Ancient Alien Theory Of Erich Von Daniken's Research
10 Evidences To Prove The Existence Of The Ancient Civilizations Aliens
Top 10 Proof of Anunnaki Aliens Among Us
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Create a raw image which emulates the Hard Drive.
Start the Virtual Machine to boot from the CD.
Connect to the Virtual Machine through VNC (use display number :1) where 10.10.10.1 is the IP address of the host machine.
For partitioning table option select GPT. After installation is over, during the post-installation configuration enable SSH server, IPV4 and DHCP.
Shutdown the Virtual Machine and use the following command to boot from the hard drive.
Perform the following steps for installing and configuring Virtio.
Download the compressed snapshot of the ports collection.
Now extract the snapshot into /usr/ports.
Install virtio modules using the following commands.
Add the following lines to /boot/loader.conf.
Do the other necessary changes needed for the image and shutdown the Virtual Machine.
To make sure the Virtio modules are loaded, we need to boot the Virtual Machine with another hard disk.
Create another disk with 2GB capacity.
Boot the Virtual Machine created by attaching the created disk to it.
To check if the driver is loaded, use the following command.
We need to change the /etc/fstab file as the primary Hard drive is referred to, using a different name in FreeBSD like "/dev/vtbd0p1".
Edit the file /etc/fstab and replace the letters "ada" with "vtbd".
Edit the following lines as below in /etc/ssh/sshd_config, for SSH access as root and to enable password authentication.
Shutdown the Virtual Machine and upload the image to OpenStack using Horizon or Glance commands.
I don't know what about you, but for me installation took around 4 hours. I don't thing it's really good idea to do this for everyone. It's better just to share an image or something… cause this is not funny I'd say.


text:
Saint-Maixant é uma comuna francesa na região administrativa da Nova Aquitânia, no departamento de Creuse. Estende-se por uma área de 13,86 km².

Comunas de Creuse

redpajama_set_name: RedPajamaWikipedia


text:
Southbury distance to Bridgeport
How far is Southbury from Bridgeport?
Shortest distance between Southbury and Bridgeport is 20.92 miles (33.67 km).
Flight distance from Southbury, CT to Bridgeport, CT is 20.92 miles. Estimated flight time is 00 hours 03 minutes.
The driving distance from Southbury, Connecticut to Bridgeport, Connecticut is: 25.33 miles (40.76 km) by car.
Driving from Southbury to Bridgeport will take approximately 00 hours 38 minutes.
#1 Southbury
Town in Connecticut, United States
#2 Bridgeport
County seat city of Fairfield County, Connecticut, United States
Starting point in Southbury: Main Street North (-73.213296,41.481493)
Ending point in Bridgeport: Main Street (-73.189437,41.179239)
Estimated Travel Time Between Southbury and Bridgeport
The distance between Southbury and Bridgeport is 41 km if you choose to drive by road. You can go 00 hours 27 minutes if you drive your car at an average speed of 90 kilometers / hour. For different choices, please review the avg. speed travel time table on the below.
There is no time difference between Southbury and Bridgeport. The current time is 08:47:51.
A car with a fuel efficiency of 8.3 l/100 km will need 3.38 liters (0.89 gallon) of gas to cover the route between Southbury and Bridgeport.
The estimated cost of gas to go from Southbury to Bridgeport is $2.95 (diesel $3.33).
The place names are translated into coordinates to approximate the distance between Southbury and Bridgeport (latitude and longitude). Cities, states, and countries each have their own regional center. The Haversine formula is used to measure the radius.
Driving distance from Danbury, CT to Southbury 17.92 miles (29 km)
East Norwalk, CT
Driving distance from East Norwalk, CT to Southbury 41.2 miles (66 km)
Driving distance from Fairfield, CT to Southbury 30.86 miles (50 km)
Driving distance from Greenwich, CT to Southbury 62.1 miles (100 km)
Driving distance from Hamden, CT to Southbury 28.05 miles (45 km)
Driving distance from Hartford, CT to Southbury 40.26 miles (65 km)
Hungary, CT
Driving distance from Hungary, CT to Southbury 56.84 miles (91 km)
Driving distance from Manchester, CT to Southbury 50.55 miles (81 km)
Driving distance from Meriden, CT to Southbury 25.62 miles (41 km)
Driving distance from Middletown, CT to Southbury 33.92 miles (55 km)
Driving distance from Milford, CT to Southbury 23.83 miles (38 km)
Driving distance from New Britain, CT to Southbury 31.85 miles (51 km)


It's Prematurity Awareness Day and I want to cry and celebrate at the same time.
My tears are for every baby who has ever been born too early, for every parent who has unexpectedly welcomed a baby too soon, and for every NICU nurse fighting for these tiny soldiers.
My joy is from how proud I am of my own two premies for being brave and strong, and being a source of pure happiness and inspiration.
Not only by your papa and me, but by your family, friends, and even strangers you have never met before. They were rooting for you from day one, the minute they expected you to join this world. They sent us support, encourage, well wishes, gifts, and the comfort in knowing we had a loving village right behind us. Someone always has and always will care about you.
You almost arrived incredibly early. At 21 weeks, we learned you could arrive at any moment. The doctors warned us to prepare for the worse. But you both refused. You held on tight and stayed in my belly because you knew it was the safest and best place to be. You fought the 50/50 odds of surviving twin-to-twin transfusion syndrome (TTTS) and miraculously pulled through without a scratch. How you did it, we may never know. We are just eternally grateful.
I wish I could tell you how much I cried. I wish I could tell you how depressed I became, how full of worry I was, and how unsure I felt. At some point or another, I was confused, shocked, helpless, terrified, and numb. But you know is funny about all of those feelings? They are all about ME. The game changer was getting a grip and committing my mind, heart, and whole self into YOU TWO. Yes, I want you to know that my heart felt like it was torn into pieces. But you also need to know how you saved me without even knowing it.
While you were premies, you were actually big premies! You were each near five pounds, which is REALLY GOOD for being born prematurely. But many of your neighbors in the NICU were much smaller and had bigger obstacles to overcome. Some were born 2, even 3 months early. Some were only 1-2 pounds each. Some were in incubators and couldn't be touched, only seen from the outside or held through these gloves that protected them from the outside world. We talked to some of their parents. Some of them had been in the NICU for 100+ days. It was incredibly painful seeing them have to fight much harder. But you were all in it together, sharing many of the same struggles of being born too soon.
While being premies is something that will always be a part of your life, it does not define you. You boys actually caught up pretty quickly! There were the delays in certain milestones and concerns we had to keep an eye on. But it wasn't long before your pediatrician didn't even consider your premature status very much. Aside from gross motor skills, you both passed EVERY developmental area and milestone according to the NICU graduate survey we filled out. I literally cried tears of happiness being able to report your amazing progress to the doctor.
Read more about Prematurity and World Prematurity Day at the March of Dimes.
If you have a premie baby, tell me about him/her! At how many weeks and days was he/she born? Was there a NICU stay? How was your experience having a premie baby?
This entry was posted in baby, the twins and tagged motherhood, prematurity, premies. Bookmark the permalink.
I'm so excited to see so many preemie posts today! Especially so many similar to my experience. My girl was born at 33 weeks 6 days, and was also a big preemie at 4lbs 7oz. Her first birthday is next week, and I am so happy to say that is caught up and you would never know about her rough start. Thanks so much for sharing!
Yes, I'm definitely loving the premie posts as well! Happy early birthday to your little girl! And happy birthday to YOU, Mama! You made it a year – what an accomplishment.
Your boys are so adorable. I can't imagine what having 2 babies in the NICU must have felt like. They look like they are happy, healthy and thriving. And cute as ever!
My boys were born on time, but I remember feeling nervous up until about 37 weeks. I felt like I could sigh a breath of relief because we had reached a major milestone. Stopping by from Mom Bloggers club!
Beautiful! My cousin just had premie twin boys and we are hoping they will be able to come home for Christmas. Your babies are so precious and I love their names!!
Hi, Monica! Thanks for visiting and for your sweet words. I hope your cousin's boys will be home for Christmas, too!!! Do you mind me asking how early they were born?
Birth is a moment in our lives but the memories last forever. I was induced for preeclampsia with my second at 37 weeks. I am thankful it didn't develop sooner. I can imagine the stress for all involved with a premature delivery. I'm happy everything worked out well for your little guys!