text:
\section{Introduction}

The ATLAS and the CMS collaboration have provided compelling evidences which point out the existence of a new heavy resonance \cite{ATLAS:2012ad,ATLAS:2012ac,Chatrchyan:2012twa,Chatrchyan:2012dg}
that resembles  closely  the Higgs boson of the standard model \cite{Ellis:2013lra}. At energies much
below the scale specified by its mass $\approx 125\ \rm GeV$, other scalar and pseudoscalar representations of the Lorentz group are likely to occur as elementary particles, too. In some cases
they arise as an outcome of theories necessary for solving specific problems in the Standard Model. The QCD axion, for instance, is the Nambu-Goldstone boson resulting from the spontaneous
breaking of the Peccei-Quinn symmetry. It enforces the strong CP conservation \cite{Peccei:1977hh,Wilczek:1977pj,Weinberg:1977ma} and constitutes the genuine paradigm of axion-like particles
(ALPs). These are very light and weakly interacting (pseudo)-scalar particles, whose theoretical conception appears connected to some extensions of the Standard Model resulting from string
compactifications   \cite{Witten:1984dg,Svrcek:2006yi}. Although neither axion nor ALPs have been detected so far experimentally, astrophysical and cosmological arguments have allowed
to impose severe constraints on their masses and coupling constants. While the QCD axion might have a mass embedded between $1\;\mu\rm eV-10\;meV$ \cite{Asztalos:2001jk,lamoreaux}, the ALPs
masses are much less constrained \cite{Jaeckel:2010ni,Hewett:2012ns}. Furthermore, the solar monitoring of a plausible axion flux from the sun \cite{CAST} as well as an assessment of its role
in the cooling of stars \cite{Raffelt:1985nk,Raffelt:1999tx,Raffelt:2006cw} are setting the most stringent upper bound on the strength of the ALP-photon coupling $g\lesssim10^{-10}\ \rm GeV^{-1}$.
Despite that, the validity of these limits must be considered with care   due to their dependence on the models from which they are obtained \cite{evading,Gies:2007ua}. This fact represents a strong motivation
for investigating alternative laboratory-based routes, ideally, with enough sensitivity as to compete with the astrophysical constraints.

In order to achieve this goal, many theoretical  researches have been carried out. Most of them rely on the hypothetical photon-ALP oscillations driven by an external magnetic field
\cite{maiani,Raffelt:1987im,Gabrielli:2006im,Gies:2007ua,Biggio:2006im}. This is because, on the one hand, the resulting axion effects manifest in the modification of the optical properties of
the vacuum, i.e., birefringence and dichroism \cite{Affleck:1987gf,Dittrich,adler,shabad4,Shabad:2011hf,VillalbaChavez:2012ea}, whereas, on the other hand, the regeneration process of a
photon from an ALP could also provide some trace of its existence \cite{VanBibber:1987rq,Adler:2008gk,Arias:2010bh,Redondo:2010dp}. Both ideas have been implemented in polarimetry
\cite{Cameron:1993mr,Zavattini:2007ee,BMVreport,Chen:2006cd} and ``Light Shining Through a Wall''  \cite{Ehret:2010mh,Ehret:2009sq,Chou:2007zzc,Steffen:2009sc,Afanasev:2008jt,Afanasev:2006cv,Pugnat:2007nu,Robilliard:2007bq,Fouche:2008jk}
experiments, but the  feeble  coupling between a photon and an ALP remains a big challenge to overcome  in the search of high levels of sensitivity.  There are, however,  hopes to solve
this issue by increasing the magnetic field strength and its spatial extension. Currently, the interaction region can be macroscopically extended up to an effective
distance of the order of kilometers. But, attainable strengths of the magnetic field are of the order of $10^4\text{-}10^5\;\text{G}$, which is not large enough to make the desirable effects
manifest. With the perspectives of achieving soon much stronger field strengths of the order of $10^{11}\text{-}10^{12}\;\text{G}$ in a short linear space-extension of the order of
$10\;\text{$\mu$m}$ \cite{ELI,xcels}, ultrahigh intense lasers can become an alternative tool for investigating ALPs-induced effects \cite{mendonza,Gies:2008wv,Dobrich:2010hi,Dobrich:2010ie}.
These facilities are envisaged to reach the power level of $200\;\text{PW}$ (future prospects  even aim to reach the $1\;\text{EW}$ threshold \cite{xcels}), corresponding to a peak intensity
of the order of $10^{25}\;\text{W/cm$^2$}$ at diffraction limit. Since such intensities are only few orders of magnitudes below the critical one of QED ($I_{cr}=4.6\times 10^{29}\;\text{W/cm$^2$}$),
there are also hopes that nonlinear effects including the production of electron-positron pairs from the vacuum \cite{Hebenstreit:2009km,ruf2009zz,mocken2010}, photon splitting \cite{DiPiazza:2007yx} and
vacuum-polarization effects \cite{DiPiazza:2006pr,BenKing:2009,BenKing:2010,Heinzl1,Heinzl} may soon be detectable for the first time, together with other processes beyond QED as pion \cite{dadi} and
Higgs \cite{sarah} production (see also the recent review \cite{Di_Piazza_2012}).
However, the presence of an ALP would distort and mix with all these other effects, in particular, with those associated to the dispersive phenomena. Hence, it is desirable to find a setup where
vacuum-polarization effects as predicted by QED and mediated by virtual electron-positron pairs, and those elicited by the presence of ALPs could be ideally isolated from each other.

In this work we investigate self-interaction effects of the electromagnetic field mediated by both virtual electron-positron pairs and the ALPs. We put forward a very simple setup, which allows
in principle to isolate polarization-dependent effects stemming only from the self-interaction of the electromagnetic field in vacuum mediated by a scalar or pseudoscalar ALP. In fact, we find that if a
probe plane-wave field counterpropagates with respect to a strong, circularly polarized plane wave, the ALP-mediated interaction between the probe and the strong field depends on the mutual
helicity of the fields, whereas the one resulting at leading order \cite{Mitter,baier,mini} from the polarization of the virtual electron-positron pairs does not distinguish between the two
helicity states of the probe. In particular, we will see that in the investigated regime, due to the conservation of the total angular momentum along the common propagation direction of the fields, a real ALP can be created only if the
probe and the strong field has the same helicity.  Moreover, the ALP-photon coupling is shown to induce modifications in the  birefringence and dichroism of the vacuum of virtual electron-positron
pairs. In addition, we indicate that in the case of an ultra-short strong plane wave, ALP-induced birefringence and dichroic effects also depend on the carrier-envelope phase (CEP) of the  strong field.
The effects calculated here could provide strong constraints on the axion-photon coupling constant if tested at upcoming ultra-intense laser facilities as the Extreme Light
Infrastructure (ELI) and Exawatt Center for Extreme Light Studies (XCELS) but also by means of relatively long laser pulses  of more  moderate intensities.

\section{General considerations \label{GC}}

The interaction of an  axion field $\Phi(x)$  and an electromagnetic field $F^{\mu\nu}(x)=(\bm{E}(x),\bm{B}(x))$ including
nonlinear QED effects is described by the Lagrangian density\footnote{Natural and Gaussian units with $\hbar=c=4\pi\epsilon_0=1$ are employed throughout.}
\begin{equation}
\label{L}
\begin{split}
\mathscr{L}=&-\frac{1}{4\pi}\mathscr{F}+\frac{\alpha}{360\pi^2}\frac{4\mathscr{F}^2+7\mathscr{G}^2}{F_{cr}^2}+\frac{1}{2}[(\partial_{\mu}\Phi)^2-m^2\Phi^2]-\frac{g}{4\pi}\Phi(\delta_{a,s}\mathscr{F}+\delta_{a,p}\mathscr{G}).
\end{split}
\end{equation}
In this equation we have introduced: 1) the fine-structure constant $\alpha=e^2\approx 1/137$, with $e<0$ being the electron charge; 2) the two electromagnetic
invariants $\mathscr{F}(x)=F^{\mu\nu}(x)F_{\mu\nu}(x)/4=-(E^2(x)-B^2(x))/2$ and $\mathscr{G}(x)=\tilde{F}^{\mu\nu}(x)F_{\mu\nu}(x)/4=-\bm{E}(x)\cdot\bm{B}(x)$,
where $\tilde{F}^{\mu\nu}(x)=\epsilon^{\mu\nu\alpha\beta}F_{\alpha\beta}(x)/2$ is the dual tensor of $F^{\mu\nu}(x)$, with $\epsilon^{\mu\nu\alpha\beta}$
being the completely antisymmetric four-rank tensor ($\epsilon^{0123}=+1$); 3) the critical electromagnetic field of QED $F_{cr}=m_e^2/|e|$, with $m_e$ being the
electron mass; 4) the ALP mass and coupling constant $m$ and $g$, respectively; 5) the discrete variable $a$, which can be equal to either $s$ for a scalar ALP
or $p$ for a pseudoscalar ALP.

The terms in eq.~(\ref{L}) proportional to the fine-structure constant are the lowest-order terms of the Euler-Heisenberg Lagrangian
density in the ratios $|\mathscr{F}(x)|/F_{cr}^2$ and $|\mathscr{G}(x)|/F_{cr}^2$, which are assumed here much smaller than unity (we recall that the critical
field of QED corresponds to a laser peak intensity of $I_{cr}=F_{cr}^2/4\pi=4.6\times 10^{29}\;\text{W/cm$^2$}$, which exceeds by about seven orders of magnitude
presently available laser intensities \cite{Yanovsky_2008}). These terms stem from the self interaction of the electromagnetic field mediated by virtual electron-positron pairs and,
strictly speaking, arise only in the case of constant (uniform) background fields, at least at a typical time (space) scale $\lambda_C=1/m_e=1.3\times 10^{-21}\;\text{s}$ ($\lambda_C=1/m_e=3.9\times 10^{-11}\;\text{cm}$) \cite{Mitter,baier,mini}. We assume that the electromagnetic field
here contains only frequencies (wavelengths) such that the above assumption is justified with sufficient accuracy. Concerning the terms proportional to $g$, which
describe the interaction of the electromagnetic field and an ALP, they are also assumed to be small, such that only lowest-order effects in $g$ will be accounted for here.

From the above Lagrangian density the following equations of motion can be derived:
\begin{align}
\label{Eq_Phi}
 &(\square+m^2)\Phi=-\frac{g}{4\pi}(\delta_{a,s}\mathscr{F}+\delta_{a,p}\mathscr{G}),\\
\label{Eq_F}
&\partial_{\mu}F^{\mu\nu}=\frac{\alpha}{45\pi}\frac{4F^{\mu\nu}\partial_{\mu}\mathscr{F}+7\tilde{F}^{\mu\nu}\partial_{\mu}\mathscr{G}}{F_{cr}^2
-g(\delta_{a,s}F^{\mu\nu}+\delta_{a,p}\tilde{F}^{\mu\nu})\partial_{\mu}\Phi.
\end{align}

We first consider a strong, monochromatic electromagnetic field $F_0^{\mu\nu}(x)=(\bm{E}_0(x),\bm{B}_0(x))$ with amplitude $E_0$, wave four-vector
$k_0^{\mu}=(\omega_0,\bm{k}_0)$ (angular frequency $\omega_0=|\bm{k}_0|$) and propagating along the negative $y$ direction. Thus, in this framework
$F_0^{\mu\nu}(x)=F_0^{\mu\nu}(\varphi_0)=(\bm{E}_0(\varphi_0),\bm{B}(\varphi_0))$, with $\varphi_0=(k_0x)=\omega_0(t+y)$ and
\begin{align}
\label{E_0_B_0}
\bm{E}_0(\varphi_0)=E_0\left[\hat{\bm{z}}\cos(\varphi_0)-\sigma_0\hat{\bm{x}}\sin(\varphi_0)\right],\quad
\bm{B}_0(\varphi_0)=-E_0\left[\sigma_0\hat{\bm{z}}\sin(\varphi_0)+\hat{\bm{x}}\cos(\varphi_0)\right],
\end{align}
where $\hat{\bm{x}}$ and $\hat{\bm{z}}$ are unit vectors associated with the $x$- and the $z$-axis, respectively.  Here, the parameter $\sigma_0$ can assume
the discrete values $0$ (linear polarization) and $\pm 1$ (circular polarization with  positive/negative helicity). In addition we consider a probe plane-wave
field $\mathcal{F}^{\mu\nu}(x)=(\bm{\mathcal{E}}(x),\bm{\mathcal{B}}(x))$ counterpropagating with respect to the strong field and with four-wave vector
$k^{\mu}$ (angular frequency $\omega$), i.e., $\mathcal{F}^{\mu\nu}(x)=\mathcal{F}^{\mu\nu}(\varphi)$, with $\varphi=(kx)=\omega t-|\bm{k}|y$. Note that we
implicitly assumed that the probe field is much weaker than the strong one, such that, while the strong plane wave propagates as in vacuum (refractive index
identically equal to unity), the dispersion relation for the probe field is allowed in principle to be affected by nonlinear QED and ALP effects.

\section{Birefringence and dichroism of the vacuum}

It is convenient to Fourier-transform the above eqs.~(\ref{Eq_Phi}) and (\ref{Eq_F}) and to work in the four-momenta space. By expanding the resulting
equations up to linear terms in the probe electromagnetic field, the equation for the axion field is easily solved and one obtains:
\begin{equation}
\label{phi}
\begin{split}
\phi(k)=&-\frac{g}{4\pi}\frac{iE_0}{k^2-m^2}\langle\delta_{a,s}\{(\omega+\omega_0)[\mathcal{A}_z(k+k_0)+i\sigma_0\mathcal{A}_x(k+k_0)]+(\omega-\omega_0)\\ &\times[\mathcal{A}_z(k-k_0)
-i\sigma_0\mathcal{A}_x(k-k_0)]\}-\delta_{a,p}\{(\omega+\omega_0)[\mathcal{A}_x(k+k_0)\\&-i\sigma_0\mathcal{A}_z(k+k_0)]+(\omega-\omega_0)[\mathcal{A}_x(k-k_0)+i\sigma_0\mathcal{A}_z(k-k_0)]\}\rangle.
\end{split}
\end{equation}
In this equation it is understood that the axion field $\Phi(x)$ can be represented as the sum $\Phi_0(x)+\phi(x)$, with $\Phi_0(x)$ being the solution of
the corresponding wave equation in the presence of the strong wave only. Since both the electromagnetic invariants vanish for a plane wave, we have also
assumed that $\Phi_0(x)=0$. Moreover, in eq.~(\ref{phi}) we have introduced the Fourier transform of the four-vector potential $\mathcal{A}^{\mu}(\varphi)$ of the probe field,
which in our case can be conveniently chosen as $\mathcal{A}^{\mu}(\varphi)=(0,\bm{\mathcal{A}}(\varphi))$, with $\bm{\nabla}\cdot\bm{\mathcal{A}}(\varphi)=0$.
Finally, the two poles in the function $(k^2-m^2)^{-1}$ are intended to be shifted such that the retarded ALP propagator is obtained when going back to
configuration space. It is easy to see that by transforming now the equation of the electromagnetic field, we need to compute the ALP field at $k^{\mu}\pm k_0^{\mu}$.
In general, terms like $\bm{\mathcal{A}}(k\pm 2k_0)$ will appear in the equation for $\bm{\mathcal{A}}(k)$. However, since we are interested in the propagation
of the probe electromagnetic wave for a given frequency and since the effects on the propagation of that frequency of the side-band terms shifted by $ \omega_0$
would be high-order with respect to $\alpha$ and/or $g$, we can consistently neglect these terms in our lowest-order analysis. The resulting equation for the
vector potential of the probe reads:
\begin{eqnarray}
\label{A}
&\left(n^2-1\right)\bm{\mathcal{A}}=\frac{2\alpha}{45\pi}\frac{I_0}{I_{cr}}[4(\mathcal{A}_z \hat{\bm{z}}+\sigma_0^2\mathcal{A}_x\hat{\bm{x}})+7(\mathcal{A}_x \hat{\bm{x}}
+\sigma_0^2\mathcal{A}_z\hat{\bm{z}})]\nonumber\ \\ \displaystyle&\qquad\qquad\qquad-g^2I_0\delta_{a,s}\left[\frac{\mathcal{A}_z-i\sigma_0\mathcal{A}_x}{4\omega\omega_0-m^2}(\hat{\bm{z}}+i\sigma_0\hat{\bm{x}})
-\frac{\mathcal{A}_z+i\sigma_0\mathcal{A}_x}{4\omega\omega_0+m^2}(\hat{\bm{z}}-i\sigma_0\hat{\bm{x}})\right]\nonumber\\ \displaystyle&\qquad\qquad\qquad-g^2I_0\delta_{a,p}\left[\frac{\mathcal{A}_x+i\sigma_0\mathcal{A}_z}{4\omega\omega_0-m^2}
(\hat{\bm{x}}-i\sigma_0\hat{\bm{z}})-\frac{\mathcal{A}_x-i\sigma_0\mathcal{A}_z}{4\omega\omega_0+m^2}(\hat{\bm{x}}+i\sigma_0\hat{\bm{z}})\right],
\end{eqnarray}
where $n=\vert\bm{k}\vert/\omega$ denotes the refractive index of the probe and $I_0=E_0^2/4\pi$ is the peak intensity of the strong wave. Note that, for notational
simplicity, the dependence on $k^{\mu}$ of the vector potential has been  omitted.

\subsection{The linearly polarized case}

We first consider the case of a linearly polarized strong wave ($\sigma_0=0$). In this case, we obtain from eq.~(\ref{A}) that the refractive index of the probe depends on
if it is polarized along the $z$ direction, the so-called ``parallel'' configuration, or along the $x$ direction, the so-called ``perpendicular'' configuration (note that
the strong field is polarized along the $z$ direction). The expressions of the two corresponding refractive indexes $n_{\parallel}$ and $n_{\perp}$ are
\begin{align}\label{npa}
n_{\parallel}=&1+\frac{4\alpha}{45\pi}\frac{I_0}{I_{cr}}-\delta_{a,s}\frac{g^2I_0m^2}{16\omega^2\omega_0^2-m^4},\\
n_{\perp}=&1+\frac{7\alpha}{45\pi}\frac{I_0}{I_{cr}}-\delta_{a,p}\frac{g^2I_0m^2}{16\omega^2\omega_0^2-m^4}.\label{npe}
\end{align}
The results in a constant-crossed field can be obtained starting from Eqs. (\ref{Eq_Phi})-(\ref{Eq_F}) and by setting $\omega_0=0$ in Eq. (\ref{E_0_B_0}). As expected,
the corresponding expressions of the refractive indexes can be obtained from Eqs. (\ref{npa})-(\ref{npe}) by setting $\omega_0=0$ and by substituting $I_0\to 2I_0$. The latter
substitution results from the fact that in the case of the oscillating wave we have neglected the side-band terms proportional to $\bm{\mathcal{A}}(k\pm 2k_0)$ and effectively
used the average value of the intensity of the strong wave. In the limit $g=0$ the well-known results of the refractive indexes including vacuum-polarization effects elicited by the virtual electron-positron pairs are recovered
\cite{Affleck:1987gf,Dittrich}. We note that vacuum-polarization effect due to the axion field would affect only one polarization configuration, depending on if the ALP is a scalar or a
pseudo-scalar particle. The pole at
\begin{equation}
 m_0=2\left(\omega\omega_0\right)^{\nicefrac{1}{2}}\label{resonance}
\end{equation}
stems from the fact that one photon from the probe and one from the strong field can create a real axion. In fact, by indicating as $p^{\mu}$ the four-momentum of the created
axion, the mentioned divergence corresponds to the energy-momentum conservation equation $k^{\mu}+k_0^{\mu}=p^{\mu}$. Obviously, whenever the condition (\ref{resonance}) is fulfilled,
the refractive indexes diverge and our perturbative approach is not applicable. However, eqs.~(\ref{npa})-(\ref{npe}) can be still employed to explore the domain close to the
resonance in which $m=m_0\pm\Delta m$, with $\Delta m\ll m_0$, provided that the condition
\begin{equation}
\Delta m \gg \frac{1}{4}\frac{g^2 I_0}{m_0}\label{closeresonace}
\end{equation}
is fulfilled.\footnote{We note, however, that, by assuming that the next higher-order term in $g$ is of the order of the square of the lowest-order term in eqs.~(\ref{npa})-(\ref{npe}),
then the latter equations can be consistently employed only if $(g^2I_0/4m_0\Delta m)^2\ll (4\alpha/45\pi)(I_0/I_{cr})$.} By assuming to work with a high-intensity laser as those available
at the forthcoming ELI facility \cite{ELI} or at XCELS \cite{xcels} and to employ an optical probe, the expression of the resonant mass $m_0$ and the above conditions can be written in
a more transparent way as $m_0[\text{eV}]=2\sqrt{\omega[\text{eV}]\omega_0[\text{eV}]}$
and $ 3.7\,g^2[\text{GeV$^{-1}$}]I_0[10^{25}\;\text{W/cm$^2$}]/m_0^2[\text{eV}]\ll(\Delta m /m_0)\ll 1$, respectively.

We pursue our analysis by shifting the position of the  pole  in eqs.~(\ref{npa}) and (\ref{npe}) as indicated below eq.~(\ref{phi}). Thus, the two refractive indexes acquire
an imaginary part given by
\begin{equation}\label{npara}
\text{Im}(n_{\parallel})=-\delta_{a,s}\frac{\pi}{2}g^2I_0\delta(4\omega\omega_0-m^2),\qquad
\text{Im}(n_{\perp})=-\delta_{a,p}\frac{\pi}{2}g^2I_0\delta(4\omega\omega_0-m^2).
\end{equation}
In this context, the quantities $\kappa_{\parallel/\perp}\equiv 2\,\text{Im}(n_{\parallel/\perp}) \omega$ coincide with the photon attenuation coefficients in the
head-on collision of a probe photon with the strong plane wave in the corresponding mutual polarization configuration (note that here we neglect the axion-photon back conversion, which is an higher-order process in $g$). This means that the intensity $I_{\parallel/\perp}(L)$
of a probe field polarized in the parallel/perpendicular direction, will be $I_{\parallel/\perp}(L)=\exp(-\kappa_{\parallel/\perp}L)I_{\parallel/\perp}(0)$, after
propagating a distance $L$ inside the strong laser field.

It is worth noting that the photon attenuation coefficients $\kappa_{\parallel/\perp}$ are singular as  a consequence of considering a monochromatic strong field.
The divergence, however, disappears for a pulsed strong plane-wave of the form
\begin{equation}
\label{E_p}
\bm{E}_0(\varphi_0)=E_0f(\varphi_0)\cos(\varphi_0+\varphi_{\text{CEP}})\hat{\bm{z}},\quad
\bm{B}_0(\varphi_0)=-E_0f(\varphi_0)\cos(\varphi_0+\varphi_{\text{CEP}})\hat{\bm{x}},
\end{equation}
with $f(\varphi_0)$ being a (non-negative) shape function and with the CEP $\varphi_{\text{CEP}}$. In this case, instead of employing the
optical theorem, one can directly calculate the probability that a photon with four-momentum $k^{\mu}=(\omega,\bm{k})$ and polarization $\lambda=\parallel,\perp$ transforms into an ALP in passing through the strong laser field
in eq.~(\ref{E_p}). By starting from the Lagrangian density in eq.~(\ref{L}), it follows that the probability associated with the conversion process reads
\begin{eqnarray}
\mathcal{P}_{a,\lambda}=\frac{g^2}{16}\frac{I_0}{\omega_0^2}(\delta_{a,s}\delta_{\lambda,\parallel}-\delta_{a,p}\delta_{\lambda,\perp})^2\left\vert e^{i\varphi_{\text{CEP}}}G\left(\frac{m^2}{4\omega\omega_0}+1\right)+e^{-i\varphi_{\text{CEP}}}G\left(\frac{m^2}{4\omega\omega_0}-1\right)\right\vert^2 \label{P_l}
\end{eqnarray}
where $G(\varrho)=\int d\varphi \exp(i\varrho\varphi)f(\varphi)$. We mention that, in deriving this expression of the probability, one has to transform the conserving $\delta$-function $\delta(p^+-k^+-k_0^+)$, where $q^+=\varepsilon_q+q_y$ for a generic on-shell four-momentum $q^{\mu}=(\varepsilon_q,\bm{q})$, into a $\delta$-function of the form $\delta(k_y-K_{y})$, with $K_y$ resulting from the equation $p^+-k^+-k_0^+=0$, before performing the square of the $\delta$-function itself (see also \cite{Ilderton:2012qe}).

We find interesting that for a finite pulse, the probability of ALP production depends on the pulse shape and, in particular, on the CEP of the strong laser field. On the other hand, if $f(\varphi)=1$, the total probability $\mathcal{P}_{a,\lambda}$ coincides with the corresponding photon attenuation coefficient times the interaction
length $L$, once one identifies the total interaction phase $\Phi=2\omega_0 L$ in the case of a photon counterpropagating with respect to the strong laser beam. This fact provides
evidences that the side-band contributions $\bm{\mathcal{A}}(k\pm2 k_0)$ do not play a role as long as one is interested in the leading order term $\sim g^2$.

The above analysis indicates that both for a scalar or pseudoscalar ALP, the effect of the axion can in principle be isolated from that of the virtual electron-positron pairs by
measuring the intensity of the probe after the interaction. In fact, in the former (latter) case the component of the probe field parallel (perpendicular) to the electric field
of the strong wave is expected to be attenuated by a factor $\sim\exp(-\mathcal{P}_{s,\parallel}/2)$ ($\sim\exp(-\mathcal{P}_{p,\perp}/2)$) after crossing the laser pulse. Note that $\mathcal{P}_{s,\parallel}=\mathcal{P}_{p,\perp}=\mathcal{P}_l$, with
\begin{eqnarray}
&&\mathcal{P}_l=\frac{g^2}{16}\frac{I_0}{\omega_0^2}
\left\vert e^{i\varphi_{\text{CEP}}}G\left(\frac{m^2}{4\omega\omega_0}+1\right)+e^{-i\varphi_{\text{CEP}}}G\left(\frac{m^2}{4\omega\omega_0}-1\right)\right\vert^2.
\end{eqnarray}
The reduction of a component of the electric field of the probe induces a rotation
$\delta \vartheta_a$ of the probe polarization for a scalar/pseudoscalar ALP. For a probe initially polarized at an angle $\vartheta$ with respect to the $x$-axis, the rotation $\delta\vartheta_a$ of the probe polarization angle is given by
\begin{equation}
\delta \vartheta_a=\frac{1}{4}(\delta_{a,s}-\delta_{a,p})\mathcal{P}_l\sin(2\vartheta).
\end{equation}
Note that the sign of the rotation induced by the ALP depends on whether it is a scalar or a pseudo-scalar particle. Finally, in the case of a the strong Gaussian wave with
$f(\varphi)=\exp[-\varphi^2/2(\Delta\varphi)^2]$, one obtains
\begin{equation}
\label{G}
G(\varrho)=\sqrt{2\pi}\Delta\varphi e^{-\frac{1}{2}\varrho^2\Delta\varphi^2}.
\end{equation}
We want to conclude this section by pointing out  that for a spatially focused strong field, rotation of the probe polarization
are also expected from pure nonlinear QED effects \cite{DiPiazza:2006pr,BenKing:2009,BenKing:2010}.

\subsection{The circularly  polarized case}

The case of a circularly-polarized strong wave
\begin{align}
\label{E_circ}
\begin{split}
\bm{E}_0(\varphi_0)&=E_0f(\varphi_0)[\hat{\bm{z}}\cos(\varphi_0+\varphi_{\text{CEP}})-\sigma_0\hat{\bm{x}}\sin(\varphi_0+\varphi_{\text{CEP}})],
\end{split}\\
\label{B_circ}
\begin{split}
\bm{B}_0(\varphi_0)&=-E_0f(\varphi_0)[\sigma_0\hat{\bm{z}}\sin(\varphi_0+\varphi_{\text{CEP}})+\hat{\bm{x}}\cos(\varphi_0+\varphi_{\text{CEP}})],
\end{split}
\end{align}
is easily analyzed by considering  a circularly-polarized probe as well with helicity $\sigma$. In this case the refractive  $n_{\sigma}$ is the
same for both a scalar and a pseudoscalar ALP and, for a monochromatic strong field, it reads
\begin{equation}
n_{\sigma}=1+\frac{11\alpha}{45\pi}\frac{I_0}{I_{cr}}-\frac{g^2I_0\sigma\sigma_0}{4\omega\omega_0-\sigma\sigma_0 m^2}.\label{ncircualr}
\end{equation}
In the case where $g=0$ the resulting refractive index coincides with the one obtained in \cite{Affleck:1987gf,baier}. Besides, our expression shows that only
the refractive index of a wave with the same helicity of  the strong field ($\sigma\sigma_0=+1$) acquires an imaginary part connected to the
total production probability $\mathcal{P}_{\sigma}$ of an ALP. This fact is explained via the conservation of the  component $J_y$ of the total
angular momentum along the $y$-axis and the fact that in the monochromatic case all laser photons have helicity $\sigma_0$\footnote{This is statement is no
longer valid in the case where the external laser wave is a pulsed field of the form (\ref{E_circ})-(\ref{B_circ}).}. In fact, since the ALP also propagates along the $y$-direction and since
it is a spin-0 particle, the creation process is allowed only if the helicity of the probe and of the strong-field photon are the same. For the
same reason as for the linear polarization, this probability diverges. This fact  motivates us to investigate the realistic case where the field of the wave is
a circularly polarized laser pulse. In such a  case, the ALP production probability is finite and, both in the scalar and in the pseudoscalar case, it is given by
\begin{equation}
\label{P_sigma}
\begin{split}
\mathcal{P}_{\sigma}=&\frac{g^2}{8}\frac{I_0}{\omega_0^2}\left\vert\delta_{\sigma\sigma_0,-1} e^{i\varphi_{\text{CEP}}}G\left(\frac{m^2}{4\omega\omega_0}+1\right)+\delta_{\sigma\sigma_0,1}e^{-i\varphi_{\text{CEP}}}G\left(\frac{m^2}{4\omega\omega_0}-1\right)\right\vert^2.
\end{split}
\end{equation}
We note that the factor two arising in this expression with respect to eq.~(\ref{P_l}) does not represent an effective enhancement of the probability,
as for producing a circularly polarized wave with a given amplitude, twice the energy is required than for a linearly polarized field with the same amplitude. Also in the present circularly-polarized case, the ALP production probability in general depends on the temporal shape and, in particular, on the CEP of the strong pulse.
Due to ALP production, a linearly-polarized probe field passing through a circularly polarized strong laser beam with $\sigma_0=\pm1$ acquires an ellipticity $\psi$, given by
\begin{equation}\label{psi}
\psi=\frac{1}{4}\vert\mathcal{P}_+-\mathcal{P}_-\vert=\frac{g^2}{16}\frac{I_0}{\omega_0^2}\left\vert G^2\left(\frac{m^2}{4\omega\omega_0}-1\right)-G^2\left(\frac{m^2}{4\omega\omega_0}+1\right)\right\vert,
\end{equation}
which can be exploited as a possible observable indicating the occurrence of ALP photo-production (see also section~\ref{limits}). By employing eq.~(\ref{G}), the expression of
the ellipticity in the case of a Gaussian profile, can be easily obtained.

It is interesting to observe here that higher-order corrections to the refractive index in $\sim\omega\omega_0/m_e^2$ due to
vacuum polarization do also depend on the mutual helicity of the probe and the strong wave \cite{Mitter,mini}. A similar result has been obtained from the general
expression of the vacuum polarization tensor \cite{baier}. However, such corrections are safely negligible at the optical frequencies we have in mind here.

\section{Exclusion limits \label{limits}}

Since the birefringence effects in a strong circularly polarized wave only arise in principle from the photon-ALP interaction, we limit to this case here.

The non-observation of astrophysical and cosmological consequences embed the mass of the QCD axion within a quite limited range $10^{-6}\;\text{eV}<m<10^{-2}\;\text{eV}$
\cite{Asztalos:2001jk,lamoreaux}. It is worth mentioning at this point that the lowest limit has been established from different axion production processes which
arise in different early universe scenarios as such vacuum realignment and string decay \cite{Asztalos:2001jk}. In contrast, the  upper one follows from the absence of
an observational discrepancy--associated with an  energy-loss argument--in the supernova SN1987a \cite{Asztalos:2001jk,lamoreaux}. In order to keep the argument as general
as possible we employ the more general expression of $n_{\sigma}$ in eq. (\ref{ncircualr}). In this framework, the direction of polarization of an initially linearly
polarized probe, after passing through a circularly-polarized strong laser field extending over a length $L$, will be tilted by an angle $\vartheta=(1/2)(n_+-n_-)\omega L$.
In the case under consideration, it is
\begin{equation}
\left.\vartheta\right\vert_{m^2\neq 4\omega\omega_0}\approx -\sigma_0\frac{g^2I_0}{4\omega_0\omega-m^2}\omega L\label{ellipticity},
\end{equation}
where the condition $m^2\neq 4\omega\omega_0$ has to be intended as that we are sufficiently far away from the resonance according to eq. (\ref{closeresonace}).
Since the strong wave is assumed to be monochromatic, it is understood that $\omega_0L=2\pi L/\lambda_0\gg 1$, where we have introduced here the wavelength $\lambda_0$
of the strong field. Eq. (\ref{ellipticity}) indicates that the rotation of the polarization angle depends on the product $I_0\times L$. From this point of view,
at a given strong laser spot radius, the result depends only on the total energy of the laser.

In order to investigate how the presented experimental setup can provide information on the value of the coupling constant $g$, we initially consider the parameters
of the quasi-monochromatic strong pulse as those envisaged for OMEGA EP system  \cite{OMEGA}  at Rochester, USA.  Among its  four consisting  beamlines, there are  two
which could operate in the infrared regime with  $\omega_0\approx1.17\ \rm eV$ ($\lambda_0=1\;\text{$\mu$m}$),  temporal length of about $1 \ \rm ps$ (corresponding to
$L=300\;\text{$\mu$m}$) by delivering, in addition,  intensities $I_0$ of about $2\times10^{20}\ \rm  W/cm^2$. The probe beam, on the other hand, could be one of the
remaining beamlines operating at the same frequency $\omega=\omega_0$. By taking into account that in the optical regime ellipticities of the order of $10^{-10}$
have been already measured \cite{Muroo_2003}, a negative result of such an experiment would exclude coupling constants $g\gtrsim 3.1  \times 10^{-5}\; \mathrm{GeV}^{-1}$.
We point out that the measurement of an ellipticity of the order of $10^{-10}$ requires that at least about $10^{20}$ photons from the probe pass through the
interaction region. This requirement is fulfilled by the OMEGA EP system, as each beamline has an energy of $1\;\text{kJ}$, i.e. about $10^{22}$ photons \cite{OMEGA}.
In addition, since the beams have similar features and they have a relatively long duration, one can expect that, in principle, a good space-time overlapping of the
beams can be achieved. Finally, we note that the mentioned beamlines at OMEGA EP are expected to be focused to a spot radius of $10\;\text{$\mu$m}$ \cite{OMEGA}, i.e.
about ten times the laser wavelength, such that our calculations performed in the plane-wave approximation are expected to apply with sufficient accuracy.

Let us analyze the constraint that arises  when  an ultra-intense laser pulse of duration $15\;\text{fs}$, photon energy $\omega_0\approx1.55\;\text{eV}$ (such that $L=4.5\;\text{$\mu$m}$)
and intensity $I_0\approx10^{25}\;\text{W/cm$^2$}$ is taken into account. We point out that laser systems with such parameters are envisaged to be available at the ELI and at XCELS facilities.
In order to have a precise synchronization between the colliding  waves it will be convenient to chose the probe beam as a fraction of the high-intensity laser wave and to double its frequency
($\omega=2\omega_0$).
Considering the sensitivity given above for polarimetric measurements in the optical regime,  we find that the values of $g\gtrsim 1.3  \times 10^{-6}\; \mathrm{GeV}^{-1}$ are excluded for
ALP masses sufficiently far from and smaller than the resonance value $3.1 \ \rm eV$ (note that ``how far'' also depends on the value of the coupling constant $g$, see eq. (\ref{closeresonace})).
This result is more stringent than those obtained via laboratory-based  experiments, as the ``Light-Shining-Through-a-Wall'' ones \cite{Ehret:2010mh,Ehret:2009sq} for ALP masses above $10\;\text{meV}$.
It is worth observing that the energy of both the ELI and the XCELS facility will largely exceed $1\;\text{kJ}$ \cite{ELI,xcels} such that an adequate choice of the fraction of energy employed
for the probe beam will ensure in principle that more than $10^{20}$ probe photons pass through the interaction region. This would allow, at least in principle, for measuring such small ellipticities as $10^{-10}$
in a single shot, which is particularly important in this case as, according to the present knowledge, a high shot-to-shot repeatability of the laser performances at such intensities is not
guaranteed. Finally, we mention that in order to reach such high intensities, the beams at the ELI and the XCELS facility are expected to be spatially focused to about one wavelength \cite{ELI,xcels}.
Thus, we expect that our numerical results provide an order-of-magnitude estimate, which is enough here as a first investigation of such effects. However, a more realistic spatial shape of the laser
pulse has to be employed for a more quantitative prediction.

\begin{figure}
\begin{center}
\includegraphics[width=3.8 in]{ALP.eps}
\caption{\label{fig:mb001} Exclusion regions in the $(g,m)$-plane obtained from a polarimetric setup assisted with an intense circularly polarized laser field.
While the green and cyan shaded areas were determined from the rotation induced by an ALP on the initial polarization plane eq.~(\ref{ellipticity}), the black and red wedges were found from
the ellipticity eq.~(\ref{final}). The respective resonant peaks occur at $m_\mathrm{0}=2.3\ \rm eV$ (black) and $m_\mathrm{0}=4.4\ \rm eV$ (red).
The inclined yellow band covers the predictions of the axion models with $\vert E/N-1.95\vert=0.07-7$ (the notation of this formula is in accordance with Ref. \cite{CAST}). The constraint resulting from the horizontal branch stars (HB stars (dashed line))
are also shown. Further exclusion regions (shaded areas in the left corner) provided by  different experimental collaborations dealing with Light Shining
Through a Wall mechanism have been included too (see legend). The exclusion limit resulting from the solar monitoring of a plausible ALP flux (CAST experiment)
has been included as well (dotted line). We point out that the upper bound resulting from such an experiment strongly oscillates in the mass region  $0.4 \ \mathrm{eV}\leqslant m\leqslant0.6\ \rm eV$.
Since we cannot reproduce this oscillating pattern, we show a straight dotted line, corresponding to the exclusion limit $g\leqslant2.3\times 10^{-10}\ \rm GeV^{-1}$, established
in \cite{CAST} at $95\% $ confidence level. For the exact picture of the CAST exclusion limits, we refer the reader  to the original publication \cite{CAST} by the CAST collaboration.
 }
 \end{center}
\end{figure}

If one ignores astrophysical ALP-mass bounds, severe constraints can be also found from the ellipticity [eq.~(\ref{psi})], when working close to the resonance for
$\delta=|4\omega\omega_0-m^2|/m^2\ll 1$. For example, in the case of a Gaussian pulse [see eq.~(\ref{G})] with $\Delta\varphi$ larger than unity, the ellipticity in eq. (\ref{psi}) reduces to
\begin{equation}\label{final}
 \left.\psi\right\vert_{\delta\ll 1}\approx\frac{\pi^3}{2}g^2\frac{I_0}{\omega_0^2}\mathcal{N}^2e^{-(2\pi \mathcal{N}\delta)^2},
\end{equation}
where we set $\Delta\varphi=2\pi \mathcal{N}$, with $\mathcal{N}$ being the number of cycles in the pulse. By assuming to work sufficiently close to the resonance that
$2\pi \mathcal{N}\delta\ll 1$, and by considering again the parameters envisaged at ELI and XCELS (for these lasers it is $\mathcal{N}\approx 5.6$), the absence of a trace
of an ALP in an experiment with sensitivity of the order of $10^{-10}$, would imply that values $g\gtrsim 1.8\times 10^{-7}\ \rm GeV^{-1}$ are excluded
at $m\approx 4.4\ \rm eV$. Note that eq. (\ref{final}) also suggests that more stringent exclusion limits can be obtained for very long pulses
at relatively low intensities. However, such exclusion limits will be valid in very narrow regions according to the constraint $2\pi \mathcal{N}\delta\ll 1$.
As an example, we show the numerical results in Fig.~\ref{fig:mb001} (black wedge) for the parameters associated with the OMEGA EP laser: $I_0= 2 \times 10^{20}\ \rm W/cm^2$, $\mathcal{N} = 300$, $\omega_0=1.17\ \rm eV$. We remark that the
constraint $2\pi \mathcal{N}\delta\ll 1$ prevents from taking the monochromatic limit $\mathcal{N}\to \infty$ directly in eq. (\ref{final}). This limit can be obtained by
first reconsidering eq. (\ref{psi}) and by applying the procedure described below eq. (\ref{P_l}).

Our potential discovery are summarized in Fig.~\ref{fig:mb001}, where some experimental results have been included. The prediction covered by the
hadronic models of Dine-Fischler-Srednicki-Zhitnitskii (DFSZ) \cite{Dine:1981rt,zhitnitskii} and Kim-Shifman-Vainshtein-Zakharov (KSVZ) \cite{kim,shifman} axions are also displayed.
Clearly, our results shows that complementary regions in the $(g,m)$-plane, which are not accessible by laboratory investigation based on dipole magnets, can be probed.
Still, it remains excluded by the  upper bound resulting  from the solar search of axions coming from the sun \cite{CAST} and
the constraints associated with the horizontal branch (HB) stars, emerging  as consequence of considerations of stellar energy loss due to
the axion production \cite{Raffelt:2006cw}. However, it is worth mentioning at this point that the bounds resulting from the absence of plausible astrophysical
and cosmological consequences rely on many assumptions which, eventually,  might over estimate the upper limit. Indeed, it has been established that the inclusion
of macroscopic quantities such as the temperature and the density of the star might relax the aforementioned constraints \cite{evading,Gies:2007ua}.

\section{Summary and outlook}

The self interaction of the electromagnetic field, as mediated by the virtual electron-positron pairs and by a (pseudo)scalar ALP field has been analyzed. In particular, the change
in the polarization state of a probe laser field passing through a counterpropagating  strong laser field has been studied by considering the two cases of linearly and circularly polarized strong field.
In both cases a perturbative treatment was implemented to determine the refractive indexes of the probe. In the case of a linearly polarized strong beam, the coupling with the
scalar/pseudoscalar ALP leads to a modification of the already existing birefringence resulting from the polarization of the virtual electron-positron pairs. In contrast,
when the strong field is circularly polarized, the pure QED-vacuum is no longer birefringent. However, the coupling with an ALP does generate a birefringence and dichroism in the vacuum.
The latter is due to the fact that, according to the conservation of angular momentum, only a probe photon and a strong field photon with the same helicity can produce an ALP.

In addition, the photon attenuation coefficients in the case of a plane wave with arbitrary pulse form have been determined (the particular case of a Gaussian profile has been worked
out explicitly).  The resulting ellipticity induced by the photon-axion oscillation in the field of a circularly polarized plane wave has been then calculated. Both in the linearly-
and in the circularly-polarized strong-field case, we have seen that the attenuation coefficients depend on the temporal shape and, in particular, on the CEP of the strong pulse.
Moreover, we have shown that a high-precision measurement of the latter observable could improve the experimental constraints on the photon-axion coupling constant in the region in
which the ALP mass is of the order of $\sim 1 \ \rm eV$. Of course, several questions regarding the ALP-photon oscillation in a strong laser field remain open. It would be interesting,
for instance, to determine how the collision angle between the probe and the strong laser fields could be exploited to analyze the resonant masses below the eV-regime. This and other
issues will be studied in \cite{selym}.

\section*{Acknowledgments}

S. Villalba-Chavez is very grateful to Ben King, Carsten M\"{u}ller and  Hector M. Casta\~neda for helpful discussions.

redpajama_set_name: RedPajamaArXiv


Palm Springs is a perennially sunny vacation destination known for its delightful golf resorts, warm weather, abundant nature, various wildlife, and amusing feel. For people who want to get away from the cold winter, this surely is the perfect getaway for many Americans. Spend your weekend vacation or an extended holiday in various Palm Springs rental homes to choose from. Beyond the golf resorts for hobbyists and enthusiasts, there are plenty of things to do, from dining, shopping, touring museums, to discovering and hiking the surrounding terrains.
Standing on the brink of Palm Springs, Mount San Jacinto rises more than 3,048 meters above the desert ground and can be effortlessly get up with the picturesque Aerial Tramway. This is, in fact, the world's largest rotating aerial tram car. The sight over the desert is whimsical. On hot days, the cool air on top of Mount San Jacinto is surely a refreshing treat for guests.
Observation decks, at least two restaurants, pieces of historical displays, and instructional videos on the construction and history of the tram are all available as the tram ascends to more than 2,600 meters above the ground. From here, a number of hiking trails run through the pine forest, including a hike to the summit of San Jacinto, but guests can either choose to take the hiking trails or walk around the station should they prefer. The temperature is significantly cooler on top even in summer, so guests who visit the place during the winter should be prepared for possible snowfall.
The Palm Springs Air Museum is known for having one of the country's largest collections Second World War fighter planes that are still working up to this day. In spite of this, the museum is quite compact given the vast collection that is stored inside it and can be explored easily in a considerably short period of time. Much of the collection is exhibited in hangars, so it's a good place to visit when the weather outside gets too hot or if you're looking for an escape from the outdoors.
Indian Canyons – situated at the outskirts of Palm Springs – is a well-known area for hiking and exploring some captivating desert scenery. One of the most noteworthy sections in the Indian Canyons are found at Palm Canyon. This 24-kilometer long canyon includes a creek and waterfalls and is lined with huge palm trees that bring color and vibrancy to the otherwise plain shades of the desert surroundings. Visitors can go for a short walk to the creek or choose to continue on for a longer hike, have a picnic, or simply soak up the calmness of the place. From the parking lot, tracks of several spans lead out into the oasis. On the site is a shop selling souvenirs, Indian art, and other memorabilia.
Another oasis which is also worth checking out and a good place to see birds is the Andreas Canyon. In the same area is Murray Canyon, which is seldom hiked but it gives better opportunities for spotting deer and other wildlife.
The Palm Springs Art Museum is a multi-layered museum featuring both artwork and performing arts. It has been in existence since the late 1930s and previously fixated almost completely on the desert. However, the direction has shifted to mid-century, modern and contemporary art over the years, which includes Native American art. The collection boasts and houses work by prominent artists such as Andy Warhol, Pablo Picasso, Marc Chagall, Henry Moore, and Ansel Adams, among others. Also on site are two outdoor sculpture gardens. Their permanent collections include photography, paintings, pottery, glass, architecture and other designs.
Coachella Valley Preserve – situated at the east of Palm Springs – is another delightful natural space to discover in the Palm Springs area. The sanctuary covers more than 5,200 hectares of desert scenery and is home to an assortment of animals, some of which include great horned owls, lynx, hares, kestrels, lizards, snakes, and other small birds. Book a guided hike with volunteers to make your travel easy and explore the preserve with the area's excellent views. If you are just looking to enjoy some peacefulness, you can also tackle the trekking trails on your own.
Moorten Botanical Gardens is a historical landmark features an incredible exhibit of cacti and desert vegetation with tours. Guests can see desert vegetation that ranges from full-grown trees to the smallest of shrubs. The best time to visit the Moorten Botanical Gardens is in the spring because this is the time when the desert is coming into bloom and its trees are starting to turn green again. The garden is open all year-round, however, during the cooler months – from fall of the previous year until spring of the following year – you can book a tour with a guide to the facility that is offered free with admission.
Of course, a visit to the Living Desert Zoo and Gardens is a must-see in your itinerary. It features plants and animals of the Colorado Desert, and guests will gain some insight in the contribution of deserts in the Americas and even around the globe. The zoo offers various animals from North America and Africa, which includes wolves, coyotes, mountain lions, foxes, zebras, badgers, raptors, leopards, giraffes, hyenas, gazelle, and many other species. The best time to visit is usually in the morning while the heat is still tolerable and the animals are still active.
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We've always known fresh air is good.
North Star Reach CEO Doug Armstrong, a former nurse and clinical research director at the University of Michigan Transplant Center, began taking young organ transplant recipients to camp, one week every summer in 1998. Doug and other health care professionals, along with truckloads of hospital equipment, rented a camp about four hours away. Despite its strengths, the rented camp still had large areas of sand and other obstacles that made moving wheelchairs around difficult. The location was also tough if a camper had a medical emergency.
In 2005, Doug learned about the vacant Fresh Air Camp, an abandoned summer camp in Pinckney, MI that The University of Michigan was about to sell. After hearing about the Pinckney property, the dream of North Star Reach was born.
In late 2007, Doug incorporated a new 501(c)(3) organization and with the help of Dr. Robert Kelch, took over leading this new endeavor.
Believing in the power of an outdoor camp experience for children diagnosed with serious health challenges, in 2011, the University of Michigan agreed to lease the land to North Star Reach long-term for $1 a year.
The North Star Reach Board of Directors began to take shape in early 2008 and expanded rapidly in 2010 and 2011. Doug became the CEO of North Star Reach, and began to hire staff.
In April 2012, North Star Reach became a Provisional Member of SeriousFun Children's Network (SFCN), founded by Paul Newman. In November 2016, North Star Reach was accepted as a Full Member Camp of SFCN, becoming just the ninth SFCN Full Member residential camp in the United States.
"This is a tremendous milestone for us," said Doug at the time. "We're grateful to the Network's dedication and sustaining support in our efforts to positively impact the lives of children and their families facing serious health challenges. And while we take great pride in what we've accomplished, today's announcement is also a toast to our promising future, for the most exciting part of our journey lies ahead as we welcome hundreds of campers and families to their new camp home."
For more information about the history of The Fresh Air Camp, see the terrific article in the March 2019 issue of Michigan Today. Enjoy the "100 Years of Camp History" video below.
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Welcome to McLaren Vale Primary School Outside School Hours Care.
The McLaren Vale OSHC staff would like to welcome all families & children to our service, which operates from our Activity Room, situated between the Junior Primary Building and the Madge Sexton Kindergarten.
The service is committed to providing a safe nurturing environment; where children have rich learning opportunities to learn through play, develop life skills and friendships and have fun!
Our OSHC space underwent a transformation during 2106 with a "natural theme", and a range of new spaces for the children to utilise and explore.
Whilst attending OSHC the children have access to the computer room, library, gym, outside play either on the oval, asphalt, Adventure Playground as well as the new Nature Play space.
Homework/quiet time happens at 5:00pm and this has proven to be popular with parents.
Our afternoon tea menu fits with the Australian dietary guidelines and also Element 2.2.1 of the Framework which states, Healthy eating is promoted and food and drinks provided by the service are nutritious and appropriate for each child. We have a strict NO NUTS policy in OSHC.
(Permanent Bookings) Before School - $14 session & After School - $24 session. This is the maximum fee as many families will receive a rebate through the Child Care Benefits Scheme.
A late fee will apply if children are collected after closing time - $1.00 per minute.
Some afternoons are at capacity. Please contact staff on (08) 8323 9217 for further information.


Bloom Road Consulting is happy to announce that Revenue Cycle Analyst Andrea Klick is the newest member of our Payor Contract Management consulting firm. Andrea brings a wealth of experience to the table. She comes to us from The Vancouver Clinic in Washington where she managed a reimbursement team as part of the Epic Resolute Professional Billing implementation team. Her knowledge of report writing, reimbursement, process improvement and software implementation brings an added depth to our Payor Contract Management services. Andrea holds certifications in Epic 2015 Resolute Professional Billing Administration, Epic 2015 Reporting Workbench, Epic 2015 Radar, Epic 2015 Clarity Data Model - Resolute Professional Billing, Epic 2015 Clarity Data Model – EpicCare Ambulatory, Epic 2015 Clarity Data Model – Cadence.
Andrea is a veteran of our armed forces and served as an Automated Logistical Specialist in the US Army from 1997 – 2000. She enjoys spending time with her family, cooking, and exploring the great outdoors.
At BRC, we provide personal service to every client. Our goal is to help you stay in business by improving your monitoring and recovery of third party payments. We help you make sure you are getting paid correctly. Join us in welcoming Andrea to our team. Please contact us to see how BRC and Andrea's expertise can improve your processes and ensure that you are capturing complete and accurate charges in your billing system.
If you have a need, think BRC.
Be sure to Follow us on Linked In, Twitter, and like us on Facebook.


We've been rough on "The X Factor" lately, so in the interest of fairness: Simon Cowell's return to singing competitions turned a big corner tonight with its first live show.
The high production value of the performances — background dancers! — were a refreshing change of pace from "American Idol" fare. The musical assignments are more imaginative, too.
But the person Cowell has most to thank is: Drew Ryniewicz, (unbelievably) 14, whose performance below is haunting, polished, and most importantly, an indication that a huge star — not just a big star — could come out of this show.


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Will & Grace gives back
In its initial eight-season run, Will & Grace contributed strongly to the LGBT community's struggle for equal rights; in fact, just ask then Vice President Joe Biden about the show's impact, as he discussed in 2012 on NBC's Meet the Press.
Now that the show is back, starting tonight, for a historic re-boot, Will & Grace is looking to enact social change even more directly. A few weeks ago, the burger chain Shake Shack announced a partnership with the show, creating four limited-edition "boozy milkshakes" inspired by the show's characters; the treats are available at four of the chain's New York and Los Angeles locations, with proceeds benefitting the Gay and Lesbian Alliance Against Defamation (GLAAD.) And tonight, a viewing-party celebrating the show's return to prime time (NBC, 9 PM Eastern/Pacific) will benefit a cause the Will & Grace creators and cast have long supported, the Human Rights Campaign.
Plus for each week the show has been in production, its cast and crew have worked with different charitable causes to raise funds and awareness. For example, check out this video Sean Hayes made with Maria Shriver, to aid the Women's Alzheimer's Movement. As Sean announces, any fans who donate $10 or more by October 20 via www.crowdwise.com/willandgracewam will be eligible to win two tickets to a taping of the show in Los Angeles.
Finally, here's the most recent announcement of the show's charitable efforts, benefitting the Children's Hospital Los Angeles. Again, via this campaign which started today at 11AM Pacific, for every $10 donated via www.crowdrise.com/will-and-grace-for-chla, fans will get 1 chance to win a pair of tickets to the November 15 taping of Will & Grace at NBC Universal Studios in Los Angeles, a behind-the-scenes tour of the set, and a personal photo opp with Will, Grace, Jack and Karen -- plus airfare for two on Delta Air Lines and accommodations for two at the Sheraton Universal hotel. 100% of the proceeds will directly benefit CHLA.
"Children's Hospital Los Angeles is a place I hold near and dear, and it's my absolute honor to be able to support them in such a fun and unique way," said show co-creator and executive producer, David Kohan. "They are hard at work every day caring for hundreds of thousands of children with some of the rarest and most complex disorders. The research and care they provide impacts children not just in our immediate community—and I know many people whose children have received life-changing and life-saving care at CHLA—but it reaches children around the globe."
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Keep the Will & Grace Party Going
Here's yet another thing that's changed in the eleven years since Will & Grace last aired in prime time: the concept of the "after show" online.
NBC announced today that, on the morning following the Will & Grace revival's premiere tomorrow night (Thurs. Sept. 28 at 9PM Eastern/Pacific), another talent from within the NBC Universal family, E!'s Kristin Dos Santos, will host the Will & Grace After Party. So this Friday morning, September 29, tune in to any of several of the company's platforms -- the NBC app, its YouTube channel, etc. -- to catch Kristin with fun tidbits from each episode, plus exclusives and surprise guests.
Details in NBC's press release below:
NBC LAUNCHES ULTIMATE FAN CELEBRATION WITH "WILL & GRACE AFTER PARTY" HOSTED BY E! NEWS EXECUTIVE EDITOR KRISTIN DOS SANTOS
Digital Exclusive After Show Available Across "Will & Grace" Social Channels, YouTube, NBC app, Hulu, E! Platforms and NBC's Participating Owned and Affiliate Station Sites starting Friday, September 29
"Will & Grace" Fans Keep the Party Going Via Social and Mobile Chats with NBC's Official Show GIF and Gaymoji Collections
Universal City, Ca, September 27, 2017 – The "Will & Grace" hysterics won't end on Thursday nights! NBC is bringing the ultimate fan experience to life with the "Will & Grace After Party," celebrating all of the reasons we love the iconic sitcom.
The after show will be available Friday mornings, the day after the broadcast airing, of the first six episodes of the season, and can be found across the NBC app, the "Will & Grace" social accounts, YouTube channel, E! platforms and NBC's participating owned and affiliate station sites starting September 29.
Set in a New York-style bar, the "Will & Grace After Party" show combines pop-culture maven Kristin Dos Santos (E! News Executive TV Editor) with "Will & Grace" superfans for a viewing party, games, trivia and exclusive behind-the-scenes material—not to mention surprise appearances from the show's creative team and special celebrity guests. Over the course of the show's first six episodes, "After Party" will provide an all-encompassing fan-centric journey through current and past episodes of Will & Grace and its influence on pop-culture since its initial debut in 1998. Burning questions will be covered like who had better boyfriends - Will or Grace? What were some of Jack's best and worst side hustles? How does Karen manage to drink so much and stay alive? The "After Party" will cover it all with a wink and a smile with real fans getting to be the stars of the show right up until last call.
"With the 'Will & Grace After Party,' we set out to create a true fan experience celebrating the return of one of the most iconic shows on television," said Rob Hayes, Executive Vice President , Digital, NBC Entertainment. "Rather than just focusing on individual episodes, we're going to dive into the series as a whole, discussing its place in pop-culture, and what it means to fans. I can't think of a more appropriate promotional partner than E! News and Kristin Dos Santos as our host. She's not only a TV expert, but a bonafide 'Will & Grace' fan."
"Will & Grace After Party" host and E! News Executive Editor, Kristin Dos Santos says of the project, "I'm truly honored to be a part of this very cool experience for fellow fans of 'Will & Grace.' It's going to be so much fun celebrating this iconic show that has meant so much to so many people."
Additionally, fans can keep the party going all week long with the official "Will & Grace" GIF collection and liven up their group chats with the official show Gaymojis.
The hit comedy series "Will & Grace" features actors Debra Messing as Grace Adler, Megan Mullally as Karen Walker, Eric McCormack as Will Truman and Sean Hayes as Jack McFarland. The series follows best friends Will and Grace as they navigate living together, while they deal with their eccentric friends Karen and Jack. The show originally aired on NBC starting in 1998, with the season eight finale coming in 2006. "Will & Grace" rejoins the NBC lineup with all new episodes Thursday, September 28 at 9 PM.
Labels: After Party, E!, gaymoji, Kristin Dos Santos, NBC, online, Will & Grace, YouTube
Hulu Beefs Up Its Classic Comedy Roster
Hulu, you had me at The Golden Girls. Yes, on February 13, Hulu added the Girls to its service -- and I was hooked. But then just a few weeks back, Hulu also became the exclusive streaming home of Will & Grace, just in time for us to catch up on the show's eight seasons in time for tomorrow night's historic "season 9" re-booted premiere.
Now, Hulu has announced a partnership with Universal television which means lots of good stuff coming our way -- including a streaming home for yet another of the most brilliant comedies of the last few decades, NBC's 30 Rock (beginning October 1.) Check out Hulu's press announcement below for details, which include the addition of other popular titles like Parenthood, as well as original programming like Paul Reiser's new comedy There's Johnny.
Hulu Inks Deal with NBCUniversal for Hundreds of Episodes of TV Favorites Including 30 Rock, Parenthood and More
New Licensing Agreement to Mark Premiere of Paul Reiser's Comedy Series, There's Johnny and SVOD Premiere of Syfy's Face Off, as well as the U.S. Streaming Debut of the complete Made in Chelsea Library
SANTA MONICA, CA (September 27, 2017) – Following a groundbreaking licensing agreement that marked the streaming debut of iconic series Will & Grace, Hulu and NBCUniversal Television and New Media Distribution today announced a new agreement that will make Hulu the exclusive SVOD home to all episodes of Emmy Award winning comedy series, 30 Rock, beginning October 1st, as well as add hundreds of episodes of shows for the whole family to Hulu.
In addition to bringing the complete library of the critically acclaimed and Emmy Award-winning comedy series from creator and star Tina Fey - 30 Rock - to a new streaming home, the new deal includes a full suite of premium programming that will become available to stream on Hulu:
30 Rock. A three-time Emmy Award winner for Outstanding Comedy Series as well as a critical darling,30 Rock comes from the brilliant mind of creator and star Tina Fey, whose character Liz Lemon is asked by her ultra corporate boss Jack Donaghy (Alec Baldwin) to somehow make the fictional program "TGS with Tracy Jordan" a success. Working with an oddball staff, no budget and no sleep, Liz keeps up the good fight against long odds. Also starring Tracy Morgan, Jack McBrayer, Scott Adsit, Judah Friedlander and Jane Krakowski, 30 Rock aired for seven seasons and arrives in its entirety on Hulu on October 1st.
Parenthood. The family favorite, hit drama series will stream in its entirety in early 2018 on Hulu. The critically-acclaimed series, which aired for six seasons, has remained popular with viewers since its finale. Parenthood is a one-hour drama from Award-winning executive producers Jason Katims, Ron Howard and Brian Grazer. It follows the trials and tribulations of the very large, colorful and imperfect Braverman family and features stars including Peter Krause, Lauren Graham, Craig T. Nelson, Bonnie Bedelia, Dax Shepard, Erika Christensen, Monica Potter, Sam Jaeger and Joy Bryant.
There's Johnny. Paul Reiser's highly-anticipated series, There's Johnny, will make its debut on Hulu. The deal marks the premiere for the NBCUniversal period comedy, set in the world of "The Tonight Show Starring Johnny Carson" circa 1972, starring Tony Danza.
Made in Chelsea. The first 13 seasons of the BAFTA award-winning, reality television series from the UK will make their US SVOD debut on Hulu. Since its premiere, the hit series has captivated audiences in the UK and resulted in many spin-offs. Through the deal, the complete series will be made available to stream in the US on Hulu later this year.
Face Off. The first 10 seasons of SYFY's hit reality competition series, Face Off, will become available to stream on Hulu. The series will make its SVOD debut in early 2018. Face Off follows special effects make-up artists as they participate in elaborate challenges for a grand prize and the honor of being Hollywood's next great effects artist.
The new deal expands Hulu's growing library of premium programming with even more hit series from the NBCUniversal Television library. Earlier this month, Hulu and NBCUniversal announced a joint agreement that made all episodes of the Emmy-winning, iconic series Will & Grace available to stream for the first time ever. Hulu is also home to top series from NBC including This Is Us, Blindspot, and the Emmy-winning Saturday Night Live.
About Hulu
Hulu is a leading premium streaming service that offers instant access to live and on demand channels, original series and films, and a premium library of TV and movies to millions of subscribers in the U.S. Since its launch in 2008, Hulu has consistently been at the forefront of entertainment and technology. Hulu is the only streaming service that offers both ad-supported and commercial-free current season shows from the largest U.S. broadcast networks; libraries of hit TV series and films; and acclaimed original series including Emmy Award-winning series The Handmaid's Tale, The Mindy Project, The Path, 11.22.63, the Golden Globe® nominated comedy series Casual, as well as the upcoming Future Man, Castle Rock, Marvel's Runaways and The Looming Tower. In 2017, Hulu added live news, entertainment and sports from 21st Century Fox, The Walt Disney Company, NBCUniversal, CBS Corporation, The CW, Turner Networks, A+E Networks and Scripps Networks Interactive to its offering – making it the only TV service that brings together live, on-demand, originals, and library content all in one place, across living room and mobile devices.
About NBCUniversal Television and New Media Distribution
NBCUniversal Television and New Media Distribution is responsible for the sales and distribution of NBCUniversal product to all forms of television within the U.S. and Canada. This includes current television and film product as well as content from NBCUniversal's vast library (Universal Pictures, Focus Features, Universal Television, Universal Cable Productions, NBC Late Night properties, etc.) distributed in basic cable, pay cable and subscription video-on-demand (SVOD) markets. The division is also responsible for the sales of NBCUniversal content to non-theatrical markets including airlines worldwide.
Labels: 30 Rock, Hulu, Parenthood, Paul Reiser, The Golden Girls, There's Johnny, Will & Grace
40 Years Old, Yet Exciting and New
The Love Boat seasons 1-3
are available on DVD.
clockwise from upper left:
Fred Grandy, Ted Lange,
Bernie Kopell, Jill Whelan,
Gavin MacLeod, Lauren Tewes
Today, September 24, marks the 40th anniversary of the beloved ABC series The Love Boat, which set sail as a regular series in the fall of 1977. Earlier this year, in May, the show's cast reunited on the Today Show, celebrating the 40th anniversary of the airing of the TV movie that launched the series.
Actually, that was the third Love Boat TV movie, the other two having aired in the previous season. After optioning author Jeraldine Saunders' book about her pioneering career as the industry's first female cruise director, producer Douglas S. Cramer knew he had the makings of a great series, a version of his previous hit, Love, American Style, on the seas. But it took three tries, and the addition of legendary producer Aaron Spelling, to get the casting and chemistry just right.
I've been spending the past year, and will spend the months ahead, amassing interviews and never-before-seen photos and other materials for my upcoming book Love Boat Forever. When the book is released, it will be one of many celebrations that continue, as the show continues to air on Me TV and Cosi TV, and memes such as the "Love Boat Generator" proliferate on the web. And this fall, look for the Love Boat cast to reunite at least once more, for a special ceremony involving the Hollywood Walk of Fame.
Posted by Jim Colucci at 9:00 AM 0 comments Links to this post
Labels: 40th anniversary, Aaron Spelling, ABC, Bernie Kopell, Cosi TV, Douglas Cramer, Fred Grandy, Gavin MacLeod, Jeraldine Saunders, Jill Whelan, Lauren Tewes, Love Boat, Love Boat Forever, Me TV, Ted Lange, Walk of Fame
Saturday Night (Truly) Live
After a successful experiment late last season, airing Saturday Night Live truly live in all U.S. time zones for the first time ever, NBC has announced that the adjusted time slots are here to stay.
Starting with the season 43 opener on September 30 -- with host Ryan Gosling and musical guest Jay-Z -- each episode will air as always on the East Coast (live at 11:30 PM), and simultaneously in each of the other time zones -- meaning at 10:30 PM Central, 9:30 PM Mountain and 8:30 PM Pacific. Then, to fill up the remainder of the Mountain and Pacific markets' Saturday nights, SNL will be repeated at 11:30.
For us on the West Coast, it means the chance to see the live version, warts and all. So if something slips getting bleeped, now we'll all get to see, rather than just the lucky folks back East!
Below, the NBC press release from earlier today:
'SATURDAY NIGHT LIVE' IS STAYING LIVE FROM COAST TO COAST
NEW YORK — Sept. 19, 2017 — NBC's Emmy Award-winning "Saturday Night Live" will once again air live simultaneously around the country beginning with the highly anticipated season 43 premiere on Sept. 30 with host Ryan Gosling and musical guest Jay-Z.
Each episode will air live at:
11:30 p.m. Eastern
10:30 p.m. Central
9:30 p.m. Mountain
8:30 p.m. Pacific
For the Mountain and Pacific time zones, "SNL" will be repeated at 11:30 p.m.
The live coast-to-coast airings that began in April grew 11% in "live plus same day" viewership versus what "SNL" was averaging earlier in the season (8.3 million vs. 7.5 million, according to Nielsen Media Research), indicating strong interest in the formerly tape-delayed markets to see the show live.
"Saturday Night Live" is produced in association with Broadway Video. The creator and executive producer is Lorne Michaels.
Labels: Jay-Z, NBC, Ryan Gosling, Saturday Night Live, season 43, time zones
Need a Refresher Before Will & Grace next Thursday?
For those of us dying to see the return, after 11 years off the air, of Will & Grace on Thursday, Sept. 28, here's a little taste to keep us going, and to remind us of the eight great seasons we had.
This afternoon, the Human Rights Campaign, an organization the W&G creators and cast have long supported, circulated the video below, featuring interview snippets about how the show came to be.
And for even more behind-the-scenes stories and clips, check out tonight's Paley Center for Media-produced tribute to Will & Grace, airing at 10PM Eastern/Pacific on NBC.
Labels: David Kohan, Debra Messing, Eric McCormack, Human Rights Campaign, Jimmy Burrows, Max Mutchnick, Megan Mullally, Paley Center for Media, Sean Hayes, Will and Grace
I'm So Glad We'll Have More Time Together
When The Carol Burnett Show first aired on CBS fifty years ago today, on September 11, 1967, few of us probably could imagine a date in 2017, way into the 21st Century, or the show's long-lasting impact.
Even Carol herself was just initially thinking of the show on a short-term basis -- because the show was actually an unintended result of a little-noticed clause in Burnett's contract for The Garry Moore Show wherein CBS promised the musical comedy actress her own program. But from such inauspicious beginnings, Burnett and her talented ensemble cast of Harvey Korman, Tim Conway, Vicki Lawrence and Lyle Waggoner soon became a hit, averaging 30 million viewers per week and ultimately winning 25 Emmy Awards.
And now, even though The Carol Burnett Show has been off the air for several generations, Burnett told me in a 2012 interview that she still gets mail "from teenagers -- even 11-year-olds -- who write me because they've seen individual sketches on YouTube. They're the sweetest letters, saying 'We heard about this show from our parents' or 'our grandparents. We wish we could have been there at the beginning.'"
The timing of the 50th Anniversary celebration is part of a perfect Carol Burnett storm happening in 2017, reminiscent of the big year another then-octogenarian icon, Betty White, experienced in 2010. In July, Netflix announced a new unscripted series, A Little Help with Carol Burnett, in which the comedy legend joins a panel of 4- to 8-year old kids to give life advice. And this past spring, Carol shot the pilot for Household Name, a multi-camera sitcom in which she plays a deliciously haughty 92-year-old movie queen living with a non-showbiz family in her Los Angeles manse; having attended the May pilot taping, I can attest that the show was hilarious, which is why it was surprising when ABC did not pick it up to series at the time of its May upfront presentation. Still, the show is currently being redeveloped by its creator, Michael Saltzman, and the network, which was thrilled with Carol's work, hopes to pick it up in the future.
There have been studies in the past showing that in bad economic times, comedy flourishes; and someday, I'm sure, sociologists will study 2017, and see how the anxiety of the Trump era drove us all towards the comfort of safe, nostalgic programming. Netflix already has had several seasons of success with its Fuller House, and now this season on the broadcast networks we have upcoming reboots of '90s sitcoms Roseanne and Will & Grace. Just the other day, ABC picked up a pilot for a new version of its 1981 show Greatest American Hero -- which wasn't even a hit in its day, but remains beloved by its fans nonetheless -- this time with a female, Indian-American lead. Suddenly, everything old is new again.
And so this December 3, CBS is celebrating the Golden Anniversary of The Carol Burnett Show -- a little late, but perfectly timed to catch us in a nostalgic, holiday mood. The star-studded tribute will tape next month in Los Angeles. Below, CBS' press announcement about the special honoring their comedy icon.
CBS CELEBRATES THE 50TH ANNIVERSARY OF THE CLASSIC, AWARD-WINNING COMEDY PROGRAM "THE CAROL BURNETT SHOW"
WITH A NEW STAR-STUDDED TWO-HOUR SPECIAL
"The Carol Burnett 50th Anniversary Special" to Air Sunday, Dec. 3
Carol Burnett, Original Cast Members Vicki Lawrence and Lyle Waggoner, Costume Designer Bob Mackie, along with Celebrities Jim Carrey, Kristin Chenoweth, Stephen Colbert, Harry Connick Jr., Bill Hader, Jay Leno, Jane Lynch, Bernadette Peters, Maya Rudolph, Martin Short and More Will Commemorate the Groundbreaking Show
CBS will celebrate the 50th anniversary of Carol Burnett's classic, award-winning comedy series with THE CAROL BURNETT 50TH ANNIVERSARY SPECIAL, a new two-hour star-studded event featuring Burnett, original cast members and special guests, on Sunday, Dec. 3 (8:00-10:00 PM, ET/PT) on the CBS Television Network.
Filming on Stage 33 at CBS Television City in Los Angeles, the show's original soundstage, Burnett will reminisce about her favorite sketches, Q&As with the studio audience, guest stars, her memorable wardrobe and bloopers, as well as the tremendous effect the show continues to have on television today as a true pioneer of sketch comedy.
"I can't believe how fast the time went, and what makes me the happiest is that so much of the funny stuff we did still holds up today, and we can share it with generations to come," said Carol Burnett. "What a great ride!"
"'The Carol Burnett Show' was a comedy showcase that was years ahead of its time. If social media existed then, clips from the broadcast would have quickly gone viral," said Leslie Moonves, Chairman and CEO, CBS Corporation. "We are very proud of the show's significant place in CBS' legacy, as well as in television history, and we look forward to this primetime celebration of incredible talent, led by the incomparable Carol Burnett."
The special will also feature original cast members Vicki Lawrence and Lyle Waggoner, costume designer Bob Mackie, as well as other comedians, comic actors and friends, including Jim Carrey, Kristin Chenoweth, Stephen Colbert, Harry Connick Jr., Bill Hader, Jay Leno, Jane Lynch, Bernadette Peters, Maya Rudolph and Martin Short, among others, who will join Burnett to discuss how the revolutionary series paved the way for them and impacted their careers.
"The Carol Burnett Show" premiered on Sept. 11, 1967 and starred Carol Burnett, Harvey Korman, Vicki Lawrence, Lyle Waggoner and Tim Conway. Airing for 11 seasons and a total of 276 episodes, the show earned a total of 25 Primetime Emmy Awards, including three for Outstanding Variety-Music/Comedy Series. In addition, the show earned eight Golden Globe Awards, including one for Best Television Show – Comedy or Musical, and Burnett received four for Best Actress – Comedy or Musical.
THE CAROL BURNETT 50TH ANNIVERSARY SPECIAL will be produced for television by dick clark productions. Carol Burnett, Steve Sauer, Allen Shapiro, Mike Mahan, Mark Bracco, Paul Miller and Leslie Kolins Small are executive producers. Paul Miller directs.
CHEAT TWEET: Celebrate the 50th anniversary of #TheCarolBurnettShow! 2-hour star studded special event on Dec. 3! #CarolBurnett50
Labels: 50th anniversary, A Little Help, Betty White, Carol Burnett, CBS, Harvey Korman, Household Name, Lyle Waggoner, Michael Saltzman, Netflix, Tim Conway, Vicki Lawrence


Different recipes call for different cuts of Welsh beef. Knowing which cuts can be slow-cooked or flash-fried can make all the difference to the flavour and texture of the meat.
For instance, the round making up the top part of the back leg is made up of 3 cuts: topside, silverside and top rump. These are all lean cuts ideal for roasting. The silverside, in particular, is excellent for a roast cooked slowly with wine or stock.
Meanwhile, the fillet is cut from the inside of the loin. Being an under-utilised muscle, the meat is quite tender compared to other parts. This makes it perfect for both a Sunday roast and beef wellington.
You can prepare all of these cuts and more when you order our 10kg Local Black Mountain Welsh Beef Box.
All are freshly cut, vacuum packed and labelled ready for the freezer.


A weekend of fun, family friendly events are guaranteed at SeaFest in Cork between the 7th and 9th of June 2019.
Discover all about our oceans, including the creatures that live beneath, how we explore our seas, the ships that transport us and the fascinating tales from the deep.
SeaFest showcases Ireland's abundant maritime resources – raising awareness of the value and opportunities provided by the sea and celebrates our proud maritime heritage. It incorporates a series of marine-related business and research events, the annual Our Ocean Wealth Summit, as well as a maritime festival.
All events and activities are free; however, a small number of events may require pre-booking. The full line of events for 2019 has not been announced yet, keep an eye on this link, to see the schedule as it is announced.
To book your stay with us during SeaFest 2019, click here.


MMSA provided structural engineering design and construction administration services as part of the $200 million Charleston International Airport (CHS) Terminal Redevelopment and Improvement Program (TRIP) and Central Energy Plant design. Completed in 2016, significant areas of the airport received new additions and renovation, including Concourses A and B, the ticket lobby, baggage claim, concession areas, security screening and passenger processing areas.
The in-depth Airport Improvement article, highlighting the airport's recent additions and renovation, is available for further reading here.


text:
Books for Post Divorce
Books for Post Divorceadmin2017-09-12T12:50:35+00:00
The Co-Parents' Handbook: Raising Well-Adjusted, Resilient, and Resourceful Kids in a Two-Home Family from Little Ones to Young Adults
Starting From Scratch When You're Single Again: 23 Women Share Stories, Encouragement, Recipes, and Lessons Learned When Starting Over Was All They Could Do
How to Sleep Alone in a King-Size Bed: A Memoir of Starting Over
Conscious Uncoupling: 5 Steps to Living Happily Even After
Befriending Your Ex after Divorce: Making Life Better for You, Your Kids, and, Yes, Your Ex
julia@holisticdivorce.com
Boston: 75 Arlington Street, Suite 500, Boston, MA 02116
San Francisco: 350 Rhode Island Street, Suite 240, San Francisco, CA 94103
Los Angeles: 10880 Wulshire Blvd., Suite 1101, Los Angeles, CA 90024
Santa Barbara: 7 W. Figueroa Street, Suite 200, Santa Barbara, CA 93101
Boston: (617) 826-6680
New York: (212) 401-8697
San Francisco: (510) 903-2018
Los Angeles: (310) 954-1594
Santa Barbara: (805) 318-3161
Copyright © 2017 Holistic Divorce, LLC. All Rights Reserved. Privacy Policy | Terms of Use
Disclaimer: It is important to note that this list is not updated on a regular basis. If you do not see a court that you are looking for, or you are unable to get in touch with any of the courts listed here, you may consider calling an authority in your state to confirm the proper phone number and address.


text:
R.C. Olmstead Re-Signs One-Fourth of Roster
R.C. Olmstead said it has signed long-term renewal contracts with 27 of its core processing clients in the past 12 months, about one-fourth of its total client list.
By Marc Rapport | Updated on June 14, 2009
Twenty of the renewals were with Ohio credit unions, with two in West Virginia and one each in Indiana, Kansas, Colorado, Maryland and Michigan. The company provides core processing and related services to about 115 credit unions.
Texas Credit Union Released From 22-Month Conservatorship
Peter Strozniak | January 27, 2023
Edinburg Teachers CU returned to members following a $2.5 million loss, lawsuits and the ousting of a highly compensated CEO.
SECU & Foundation Give $5 Million to Urban Park Development
Michael Ogden | January 27, 2023
It's the largest combined gift to one organization in the history of the CU and Foundation.


text:
Die Engineer-Inseln sind eine Inselgruppe in der Salomonensee und gehören zur Bwanabwana Rural LLG (Local Level Government) Ara im Distrikt Samarai-Murua der Provinz Milne Bay im südöstlichen Teil Papua-Neuguineas.
Die Engineer-Inseln befinden sich am westlichen Rand des Louisiade-Archipels, östlich der Insel Basilaki und südlich von Normanby. Die Inseln bilden eine ungewöhnliche Gruppe, bestehend aus hohen Inseln, niedrige Koralleninseln, Atollen und Unterwasserriffen, die in einem Umkreis von etwa 24 km bis 14 km angeordnet sind.

John Moresby benannte die Inselgruppe 1873 nach den Maschinisten (englisch engineers) seines Dampfschiffes HMS Basilisk. Die Inseln wurden nach den einzelnen Besatzungsmitgliedern aus dem Maschinenraum benannt: Slade, Skelton, Watts, Butchart, Bright u. a.
Den südwestlichen Teil der Gruppe bilden die drei größten Inseln Tubetube (Slade-Insel), Naruaruari oder Naluwaluwali  (Skelton-Insel) und Kwaraiwa oder Kwalaiwa (Watts-Insel), die jeweils 3 bis 4 km lang  und 0,5 bis 1 km breit sind.

Die riffgesäumten Inseln sind hügelig mit Erhebungen von bis zu 150 m wie auf der Slade-Insel. Die östliche Grenze der Engineer-Gruppe ist geprägt von einem halbmondförmig geformten Riff, auf dem sich die vier niedrigen Inseln Hummock (im Südosten), Haszard (im Norden) und die beiden kleinen Inseln Button und Flat befinden.
Im Zentrum der Inselgruppe formen Inseln und Riffe eine halb geschlossene Lagune. Die Inseln Powell und Pender liegen auf dem größeren, westlichen Riff, während die Messum-Insel sich auf dem kleineren östlichen Riff befindet.

Die Shortland-Insel und die Byron-Insel bilden den nordwestlichen Teil der Gruppe. Weitere Inseln der Engineer-Gruppe sind die Bright-Insel, die Good-Insel, die Butchart-Insel und die Deedes-Insel. Die Insel Anagusa (Bentley-Insel) liegt südlich, Koyagaugau (Dawson-Insel) nordöstlich der Engineer-Gruppe.

Die Einwohner der Inselgruppe sprechen Bwanabwana.

Zur Volkszählung 2000 gab es vier Dörfer auf vier gleichbenannten Inseln, mit einer Gesamtbevölkerung von 903, von West nach Ost: Tubetube (Slade Island) (184), Naruaruari (Skelton, auch Falschschreibung Skeleton) (282), Kwaraiwa (Watts Island) (359) und Tewatewa (Hummock Island) (78).

Die wichtigsten Inseln im Überblick:

Alternative Flächenangaben existiere für die Inseln Slade (2,40 km²), Skelton (2,84 km²) und Watts (1,88 km²).

Weblinks
 (engl.)

Einzelnachweise

Inselgruppe (Papua-Neuguinea)
Inselgruppe (Australien und Ozeanien)
Inselgruppe (Salomonensee)
Inselgruppe (Louisiade-Archipel)

redpajama_set_name: RedPajamaWikipedia


text:
Ken Warren draws on 30 years of environmental law experience to provide insightful counsel to his clients. His practice includes regulatory, litigation, and transactional matters involving environmental compliance, permitting, environmental aspects of real estate and corporate transactions, site remediations, sustainability and climate change, and alternative energy issues.
Many of the large and small companies that Ken has counseled have benefited from his practical insight and creativity in addressing regulatory and enforcement challenges. Fortune 500 companies have retained Ken to navigate complex federal and state environmental permitting programs. Ken is also a seasoned environmental litigator and has tried numerous cases to verdict. He served as lead trial and appellate counsel for a Fortune 100 company in a multiparty environmental case in which he obtained a favorable final judgment following a lengthy district court trial and successfully defended the judgment on appeal to the Third Circuit. He has also negotiated and helped to administer consent decrees with novel provisions protecting both the companies and the environment.
Ken employs his extensive experience in the field of water resources to advise clients on water supply and allocation, stormwater and wastewater permitting, total maximum daily loads, and safe drinking water compliance. He negotiated a Safe Drinking Water Act Administrative Order on Consent for a Fortune 500 company and assisted the company in implementing the Site remedy through a CERCLA consent decree. He also serves as general counsel for a multistate water resources agency, the Delaware River Basin Commission. This is a rare achievement for an individual in the private sector.
Ken is widely recognized as a leader in environmental law. He is a member of the American College of Environmental Lawyers and is listed in leading national and international guides of lawyers for environmental law. He served as Chair of the American Bar Association's Section of Environment, Energy, and Resources from 2003 to 2004, during which time he led the section's 10,000 lawyers. He also served as a member of the ABA Standing Committee on Environmental Law and was the initial chair of the ABA's Homeland Security Task Force. Ken writes a regular column for The Legal Intelligencer on environmental law and has authored numerous articles on environmental issues. He also wrote a chapter in The Law of Environmental Justice. Ken is a frequent speaker on environmental matters before sections of the American Bar Association and other groups.
Ken was appointed by the U.S. Environmental Protection Agency Administrator to serve as an industry stakeholder representative on the EPA's National Environmental Justice Advisory Council and served on the Council from 2000 to 2006. He currently serves on the Board of Trustees of the Academy of Natural Sciences in Philadelphia, the oldest natural science museum in the Americas.
University of Pennsylvania Law School, Philadelphia, Pennsylvania, 1979, JD, magna cum laude, Order of the Coif
Brown University, Providence, Rhode Island, 1975, BA, magna cum laude, with Honors
The Honorable Joseph L. McGlynn, Jr., United States District Court for the Eastern District of Pennsylvania, 1979 – 1980
Honors/Awards
University of Pennsylvania Law School
Trial Association Award
Keedy Cup Moot Court Winning Team
Who's Who Legal (Environmental Law)
Named a Leader in Environmental Law by Chambers USA: America's Leading Lawyers for Business
Best Lawyers in America, selected as a Best Lawyer in America in Environmental Law
Best Lawyers in America, selected as Philadelphia's 2017 Environmental Law "Lawyer of the Year"
Protecting Endangered Species: Plight of Right Whale Puts Spotlight on Issue
The Legal Intelligencer, December 9, 2021
The Biden Administration's Climate Change and Environmental Justice Agenda
The Legal Intelligencer, October 7, 2021
Permits for Discharges of Pollutants to Groundwater
The Legal Intelligencer, August 05, 2021
Resolving Interstate Water Disputes: Litigation May Not Be the Answer
The Legal Intelligencer, June 10, 2021
A Setback for Climate Litigation
The Legal Intelligencer, April 8, 2021
President Biden's First Day of Environmental Initiatives
The Legal Intelligencer, January 28, 2021
A New Climate Change Paradigm
The Legal Intelligencer, December 10, 2020
The Coronavirus Pandemic and Environmental Compliance
Pa.'s Climate Change Initiative: Important Step in Collaborative Journey
The Legal Intelligencer, October 10, 2019
Green New Deal Shines Light on Environmental, Economic and Social Issues
The Legal Intelligencer, April 11, 2019
"Management of Fill in Pa.: Environmental Considerations for Developers," The Legal Intelligencer, December 13, 2018
"Proposed Changes to Endangered Species Act Regulations," The Legal Intelligencer, August 10, 2018
"Resolving Environmental Problems Through Collaborative Decision-Making," The Legal Intelligencer, April 12, 2018
"Clear, Science-Based Regulatory Standards for Emerging Contaminants Are Needed," The Legal Intelligencer, December 14, 2017
"Future Efforts to Combat Climate Change," The Legal Intelligencer, August 11, 2017
"Suits To Compel EPA Action Likely To Increase," The Legal Intelligencer, April 14, 2017
"EPA Promotes Partnerships to Improve Drinking Water Safety," The Legal Intelligencer, December 8, 2016
"Presidential Politics and the Environment," The Legal Intelligencer, October 14, 2016
"Lead in Drinking Water: Sharing Responsibility," The Legal Intelligencer, August 12, 2016
"Justices Consider if Jurisdictional Determinations Are Appealable," The Legal Intelligencer, April 8, 2016
"Pennsylvania Supreme Court to Revisit Public Trust Doctrine," The Legal Intelligencer, December 11, 2015
"Pope Francis Calls for Environmental Stewardship in Letter," The Legal Intelligencer, August 14, 2015
"Reach of Citizen Suits Brought Under RCRA Uncertain," The Legal Intelligencer, April 10, 2015
"Revisions on Regulated Medical and Chemotherapeutic Waste," The Legal Intelligencer, December 12, 2014
"Seventh Circuit Case Examines the Ambiguities of CERCLA," The Legal Intelligencer, October 10, 2014
"Legislation Protecting the Habitat of Endangered Species," The Legal Intelligencer, June 13, 2014
"Proposed Revisions to EPA Water Quality Standards Regulation," The Legal Intelligencer, February 14, 2014
"Resolving Air Pollution Disputes Among Neighboring States," The Legal Intelligencer, August 9, 2013
"Recycling Secondary Manufacturing Materials,"The Legal Intelligencer, April 12, 2012
"Hurricane Sandy and Environmental Stewardship," The Legal Intelligencer, November 9, 2012
"Aggregating Air Emissions from Multiple Locations," The Legal Intelligencer, September 14, 2012
"Third Circuit OKs Project to Deepen the Delaware River," The Legal Intelligencer, July 13, 2012
"Controlling Nutrient Pollution: Difficulties in Establishing Criteria," The Legal Intelligencer, March 9, 2012
"Environmental Hearing Board Protects Private and Public Rights," The Legal Intelligencer, January 13, 2012
"Commission Publishes Revised Natural Gas Regulations," The Legal Intelligencer, November 11, 2011 (with Pamela M. Bush)
"EPA Proposes Revised Rules to Regulate Hazardous Waste Recycling," The Legal Intelligencer, September 16, 2011
"Protecting Polar Bears Under the Endangered Species Act," The Legal Intelligencer, July 8, 2011
"EPA Issues Draft Guidance on Clean Water Act Jurisdiction," The Legal Intelligencer, May 18, 2011
"Timing is Critical in Appeals of Agency Action," The Legal Intelligencer, March 11, 2011
"EPA Establishes Chesapeake Bay Total Maximum Daily Load," The Legal Intelligencer, January 13, 2011
"Climate Change Adaptation Gaining Increased Attention," The Legal Intelligencer, November 18, 2010
"Pennsylvania's Regulation of Total Dissolved Solids," The Legal Intelligencer, September 16, 2010
"Judicial Review Under NEPA: A Look at Two Recent Decisions," The Legal Intelligencer, July 15, 2010
"The Federal Strategy to Restore the Chesapeake Bay Watershed," The Legal Intelligencer, May 21, 2010
"Proposed Amendments to State Stormwater Rules," The Legal Intelligencer, September 17, 2009
"Supreme Court's Riverkeeper Decision and Cost-Benefit Analysis," The Legal Intelligencer, July 16, 2009
"Democrats' Clean Energy Bill Could Have Far-Reaching Effects," The Legal Intelligencer, May 21, 2009
"EPA Proposes Mandatory Reporting of Greenhouse Gases," The Legal Intelligencer, March 19, 2009
"Pennsylvania's Energy Efficiency and Conservation Program," The Legal Intelligencer, January 22, 2009
"Protecting Natural Resources Under the Public Trust Doctrine," The Legal Intelligencer, September 18, 2008
"New York Plan Could Inspire Sustainable Philadelphia Programs," The Legal Intelligencer, July 17, 2008
Author of a chapter in The Law of Environmental Justice
Author of numerous environmental program materials for the American and the Pennsylvania Bar Associations
American College of Environmental Lawyers
American Bar Association, Standing Committee on Environmental Law
Past Chair, American Bar Association; Section of Environment, Energy, and Resources
Pennsylvania Bar Association
Delaware Valley Environmental Inn of Court
Board of Trustees, The Academy of Natural Sciences
Board Member, The Pinchot Institute for Conservation
Teaching/Lecturing
Speaker, "Flowing into the Future: Evolving Water Law Issues," Pennsylvania Bar Institute, June 2011
[/wptabcontent][/wptabs]


text:
Q: Converting formula/equation in docx to html using docx4j I'm trying to convert docx containing equations to on Android. I came across docx4j which is great and tested the following sample (HtmlExporterNonXSTL):
https://github.com/plutext/docx4j/blob/android/src/main/java/org/docx4j/convert/out/html/HtmlExporterNonXSLT.java
However I noticed that it doesn't handler equations well - if some symbol or number has some power and/or indices their position is alway in the middle e.g.
k_{n+1}^2 (latex format)
is displayed as:
kn+12 (with 'n+12' having correct smaller font but they are both vertically aligned)

Is there any way to adjust CSS to handle powers and indices? (full formula conversion would be better but I guess it is not so easy). I'm new to docx4j but looks like somehow
handlePPr()
method will need to be modified in HtmlExporterNonXSLT example. Before I would dive into it I thought about asking is it even possible to accomplish it (any way to obtain the offset property of a run?

A: Disclosure: I'm docx4j project lead
You're welcome to modify HtmlExporterNonXSLT in order to fix your particular example, but as you say, full formula conversion would be better.
Here are links to three prior posts on that subject (newest first):

*

*math-equations-and-docx-to-html-conversion-not-working

*need-to-handle-latex-equation

*math-expression-issue

redpajama_set_name: RedPajamaStackExchange


GOAL: To study the rate at which Helicobacter pylori infection is treated in an immigrant cohort after diagnosis by esophagogastroduodenoscopy (EGD). BACKGROUND: Gastric cancer is the second leading cause of cancer death worldwide, and is especially prevalent in East Asia; immigrants from this part of the world remain at higher risk. Infection with H. pylori is a known risk factor for gastric cancer. There have been no studies of completion of H. pylori treatment in immigrant populations. STUDY: Prospective cohort study of East Asian immigrants diagnosed with H. pylori infection who underwent EGD in a gastric cancer screening protocol. Our primary outcome was self-report or chart evidence of completion of treatment of H. pylori. RESULTS: Sixty-eight of the 126 participants (54%) tested positive for H. pylori infection on EGD. Forty-nine (72%) were seen for a follow-up visit at one of the clinics involved in the study. According to clinic records, 39 of these 49 participants (57% of all H. pylori-positive participants) were prescribed treatment. Only 31 participants (46%) completed treatment. Of possible explanatory factors, only having a "regular doctor" was significantly associated with treatment completion (odds ratio=5.6; 95% confidence interval, 1.2-25.0). CONCLUSIONS: In a sample of Asian immigrants, the rate of treatment of H. pylori infection, a potentially modifiable risk factor, was lower than expected. Having a "regular doctor" appeared to increase the likelihood of receiving appropriate follow-up care.


A look at the best, most silent insignificant character in literature, and his connections to one of England's best bands.
Alastic rediscoveres the old 80s text adventure games and gives them a go… at his own peril.
Alastic takes on the age-old argument of whether to add two spaces instead of one after a period when typing.
When US president Donald Trump boasted of having a bigger nuclear button than North Korean leader Kim Jong-un, I thought it'd be fun to try a political cartoon. Several months later, here's a modest attempt.
Friday, October the 13th, 2017 was a unique one, as it occurred exactly 710 years after another Friday, October the 13th, probably the first unlucky one. Resultingly, alastic has a fun romp through his bookshelves to explore the Knights Templar and the conspiracy theories that surround them.


Lahore (Friday, 15 August 2014):- The Directorate of National Savings of Pakistan Prize bond Rs.1500 draw is going to be held at Lahore city on Friday 15, August 2014. This is draw No.59 till so far or rupee 1500 prize bond by National savings of Pakistan. The complete Rs 1500 Prize bond List 2014 August will be uploaded here by Prizebondlist.pk today. The complete Prize bond list of rupees One Thousand And Five Hundred will be held today at Lahore.
This Prize bond 1500 Lucky draw Qura andazi at Big city Lahore of Pakistan organized by savings.gov.pk in month of August is in serial no. 59 can make you winner of the first or second prize of this Rs. 1500 denomination. The rupee 1500 prize bond complete list of draw #59 will be updated here at 5:00 pm on this page. The Rs. 1500 59th draw number full result dated 15-Aug-14 can be view and download here.
You can check out Prize bond Rs.1500 draw full list held on 15-08-2014 at Lahore city (15 th August, 2014) here online.