text:
\section{Introduction}
Solar quiet gamma-ray astronomy started playing a significant role in the early 90's thanks to the EGRET mission. \citet{hudson} pointed out the importance of gamma-ray emission from the quiet Sun as an interesting possibility for highly sensitive instruments such as EGRET.
\citet{seckel} estimated that the flux of gamma rays produced by cosmic-ray interactions on the solar surface would be detectable by EGRET. This emission is the result of particle cascades initiated in the solar atmosphere by Galactic cosmic rays. Meanwhile \citet{thompson97} detected in the EGRET data the gamma rays produced by cosmic ray interactions with the lunar surface. Although they expected similar interactions on the Sun, the EGRET data they analyzed did not show any excess of gamma rays consistent with the position of the Sun. They obtained an upper limit of the flux above 100 MeV of 2 $\times$ 10$^{-7}$cm$^{-2}$s$^{-1}$ . \citet{fairbairn}, analyzing the EGRET data of the solar occultation of 3C279 in 1991, found a photon flux of about 6 $\times$ 10$^{-7}$ cm$^{-2}$s$^{-1}$ above 100 MeV in the direction of the occulted source, which they used to put limits on axion models; however they did not consider the extended solar emission.

Inverse Compton scattering of cosmic-ray electrons on the solar photon halo around the Sun has been estimated to be an important source of gamma-ray emission  \citep{orlando,moskalenko} \footnote{The same process from nearby stars has been studied in \citet{orlando} and \citet{orlandoc}}. In our previous work, we predicted this to be comparable to the diffuse background even at large angular distance from the Sun. The formalism has now been improved and more accurate estimates have been obtained. The anisotropic scattering formulation and the solar modulation have been implemented, in order to give a more precise model for the EGRET data. In this work we explain in detail our model of the extended emission produced via inverse Compton scattering of cosmic-ray electrons on the solar radiation field.

A first report of our detection with EGRET data was given in \citet{orlandob}. Here we describe the full analysis including the spectrum of disk and extended components.  Our result is very promising for the forthcoming GLAST mission which certainly will be able to detect the emission even at larger angular separation from the Sun. Moreover, the extended emission from the Sun has to be taken into account since it can be strong enough to be a confusing background for Galactic and extragalactic diffuse emission studies.

\section{Theoretical model}
Inverse-Compton scattering of solar optical photons by $\sim$ GeV cosmic-ray electrons produces $\gamma$-radiation with energies of 100 MeV and above.
Improving on the approximate estimates given in \citet{orlando}, in this paper the anisotropic formulation of the Klein-Nishina cross section has been introduced, taking into account the radial distribution of the photons propagating outward from the Sun. Our elegant analytical formulation has been replaced by a numerical solution depending on  the angle between the momenta of the cosmic ray electrons and the incoming photons. As pointed out in  \citet{orlando} this will affect the results at about the 10$\%$ level.  Moreover, while in our previous work we used the modulated cosmic-ray electron spectrum as observed at earth, here a formulation of the solar modulation as a function of the distance from the Sun has been taking into account.

The gamma-ray intensity spectrum is:
\begin{equation}
\label{eq1}
I(E_{\gamma})=\frac{1}{4\pi}\int\epsilon(E_{\gamma})dx
\end{equation}
where the emissivity $\epsilon$ is given by:
\begin{eqnarray}
\epsilon(E_{\gamma})=\int dE_{e} \times
\nonumber\\
\times \int \sigma_{K-N}(\gamma,E_{ph},E_{\gamma})~ n_{ph}(E_{ph},r)~c~N(E_{e},r)~dE_{ph}
\label{eq2}
\end{eqnarray}
$N(E_{e},r)$ is the electron density, with $E_{e}$ electron energy, $n_{ph}(E_{ph},r)$ the solar photon density as function of the distance from the Sun $r$ and the solar photon field $E_{ph}$, $\sigma$ is the Klein-Nishina cross section and $\gamma=E_{e}/m_{e}$.
The cosmic-ray electrons have been assumed isotropically distributed everywhere in the heliosphere.
In \citet{orlando}, an elegant analytical formulation in eq (\ref{eq3}) was obtained for the isotropic case, assuming a simple inverse square law for the photon density for all distances from the Sun and a cosmic ray electron spectrum considered constant for all distances and determined from experimental data (see Fig.(\ref{fig4})) for 1 AU.
In order to obtain the inverse Compton radiation over a line of sight at an angle $\alpha$ from the Sun, the photon field variation over the line of sight has to be known.
\begin{figure}[!t
	\includegraphics[width=9cm, angle=0]{8817fig1.ps}
	\caption{Definition of variables for eq.(\ref{eq3}) describing the geometry of the solar inverse Compton emission.}
	\label{fig1}

\end{figure}
As shown in Fig.(\ref{fig1}), for a given point $x$ on the line of sight, the surface photon density is proportional to $1/r^{2}$, where $r^{2}=x^{2}+d^{2}-2$~$x$~$d$ $\cdot$ $cos~\alpha$, with $d$ distance from the Sun. Integrating the photon density over the line of sight from $x=0$ to $x=\infty$ one obtains:
{\setlength\arraycolsep{2pt}
\begin{eqnarray}
n_{ph}(E_{ph})~R^{2}\int_{0}^{\infty}\frac{dx}{x^{2}+d^{2}-2~x~d \cdot cos~\alpha}=
\nonumber\\
=-n_{ph}(E_{ph})~R^{2}~arctan\left( \frac{d \cdot cos~\alpha-x}{d \cdot sin~\alpha}\right) /(d \cdot sin~\alpha~)=
\nonumber\\
=n_{ph}(E_{ph})~R^{2}\left( \frac{ \pi/2+arctan(cot~\alpha)}{d \cdot sin~\alpha} \right)
\label{eq3}
\end{eqnarray}}
which depends only on the angle $\alpha$, where $R$ is the solar radius and $n_{ph}(E_{ph})$ is the solar photon density. For large distance from the source $n_{ph}(E_{ph})$=1/4 $n_{BB}(E_{ph})$, where $n_{BB}(E_{ph})$ is the black-body density of the Sun.
Integrating over solid angle and using eq.(\ref{eq1}) and eq.(\ref{eq2}) with the Klein-Nishina cross section, the total photon flux produced by inverse Compton scattering within an angle $\alpha$ becomes:
{\setlength\arraycolsep{2pt}
\begin{eqnarray}
I(E_{\gamma})=\frac{1}{4\pi} \int_{0}^{2\pi} d\varphi \int_{0}^{\alpha} sin~\alpha~ d \alpha \int dE_{ph} {}
\nonumber\\
{}\times \int \sigma_{K-N}(\gamma,E_{ph}, E_{\gamma})~c~N(E_{e})~dE_{e}~ n_{ph}(E_{ph})~R^{2} \times {}
\nonumber\\
{}\int_{0}^{\infty}\frac{dx}{x^{2}+d^{2}-2~x~d \cdot cos~\alpha}= {}
\nonumber\\
{}=\frac{R^{2}}{16~d}\left( \pi \alpha + (\frac{\pi}{2})^{2}-arctan^{2}~(cot~\alpha)\right) {}
\nonumber\\
{} \times \int dE_{ph} \int \sigma_{KN}~c~N(E_{e})~n_{BB}(E_{ph})~dE_{e} {}
\label{eq4}
\end{eqnarray}
which for small $\alpha$ is proportional to $\alpha/d$ and the intensity $I$ (per solid angle) is proportional to 1/($\alpha d$).
For the case of the anisotropic formulation of the Klein-Nishina cross section and for the electron modulation along the line of sight, we have to use numerical computations, already adopted in \citet{orlandob}.

\subsection{Solar photon field}
\subsubsection{Basic relations}
The Sun is treated as black body where the energy density is characterized by the effective temperature on the surface (T=5777 K) following the Stephan-Boltzmann equation.
For the photon density close to the Sun, the simple inverse square law is inappropriate. In this work the emission from an extended source has been evaluated.
The distribution of photon density from the Sun, as extended source, is given by integrating over the solid angle with the variables shown in Fig.(\ref{fig2})
\begin{figure}[!h
 \centering
	\includegraphics[width=.5\textwidth, angle=0]{8817fig2.ps}
	\caption{ Variables involved in eq.(\ref{eq7}) for the calculation of the photon density around the Sun, where R is the solar radius and r is shown also in Fig. (\ref{fig1})}
	 \label{fig2}

\end{figure}
{\setlength\arraycolsep{2pt}
\begin{eqnarray}
n_{ph}(E_{ph},r)=n_{BB}(E_{ph})\int_{0}^{\phi_{MAX}} \frac{2\pi~R^{2}~sin~\phi ~cos~\beta ~d\phi}{4\pi~s^{2}}
\nonumber\\
=0.5 ~n_{BB}(E_{ph}) \left[ 1-\sqrt{1-(R/r)^{2}}\right]
\label{eq5}
\end{eqnarray}
with $cos~\beta$=$(r~cos~\phi~-~R)/s$ and $cos~\phi_{MAX}~=~R$/$r$.
For large distances from the Sun it reduces to the inverse square law.

\subsubsection{Deviations of solar spectrum from black body}
We checked the effect of deviations of the solar spectrum from a black body.
We used the black-body approximation with the AM0 solar spectrum \footnote{taken from http://www.spacewx.com/}, referring to 2007, period of solar minimum, extrapolated back to the Sun. Since the estimated inverse Compton emission from the Sun is not affected significantly ($<$1$\%$) considering the actual spectrum, we decided to keep the black body approximation for simplicity.
We also verify that the EUV and XUV range of the solar spectrum do not affect the inverse-Compton emission. The irradiance at the shortest wavelengths varies significantly with solar conditions and the range of variability spans a few percent at the longest wavelengths, from 40\% to more than 500\% across the EUV and XUV , from solar minimum to solar maximum.
Moreover, during solar flare, XUV increases, reaching factors of eight or more, and EUV increases on the order of 10-40\% \citep{eparvier}. However, \citet{oncica} found that the X-ray flares cannot contribute to the total solar irradiance fluctuations and even the most energetic X-ray flares cannot account for more than 1 mW/$m^{2}$.
We found that the estimated inverse-Compton emission from the Sun is not affected significantly by the XUV/EUV flux and its variability.

\subsection{Comparison of isotropic/anisotropic formulations}
In \citet{orlando} the isotropic formulation for the Klein-Nishina cross section given in \citet{moskalenkoa}
 was used in the analytical formulation for estimating the IC gamma-ray emission .
In the present analysis we used the following anisotropic Klein-Nishina cross section in a more convenient form than in \citet{moskalenkoa}:

{\setlength\arraycolsep{2pt}
\begin{eqnarray}
\sigma_{K-N}(\gamma,E_{ph}, E_{\gamma}) =
\frac{ \pi r_{e}^{2}m_{e}^{2}}{E_{ph} E_{e}^{2}}\times
\nonumber\\
  \left[ \left(  \frac{m_{e}}{E'_{ph}}\right) ^{2} (\frac{v}{1-v})^{2} {} -2 \frac{m_{e}}{E'_{ph}} \frac{v}{(1-v)}+(1-v)+\frac{1}{1-v} \right]
\label{eq6}
\end{eqnarray}
where
$v=E_{\gamma}/E_{e}$ and
$\gamma$=$E_{e}/m_{e}$, with $m_{e}$ electron mass
and
\begin{equation}
E'_{ph}=\gamma E_{ph}(1+cos~ \eta)
\label{eq7}
\end{equation}
where $\eta$ is the scattering angle for the relativistic case, with $\eta=0$ for a head-on collision.
In Fig.(\ref{fig3}) is shown the contribution to the flux as a function of distance along the line-of-sight for the isotropic and anisotropic cross-sections.
\begin{figure}[!h]
\centering
\includegraphics[width=.35\textwidth, angle=270]{8817fig3.ps}
\caption{ Relative contribution (arbitrary units) of the isotropic (gray lines)
and anisotropic (black lines) cross sections, multiplied by the photon
density along the line of sight for E$_{e}$=10$^{4}$ MeV and E$_{\gamma}$=100 MeV. $x$ and $d$
are defined in Fig 1. The lines represent different angles from the Sun,
from 1$^{\circ}$ to 6$^{\circ}$ (right to left).}.
\label{fig3}
\end{figure}

The integrated inverse-Compton emission was compared for isotropic and anisotropic cross sections; the maximum difference of the intensity for the two Klein-Nishina cross sections is of about 15$\%$ around 300 MeV and for 0.5$^{\circ}$ angular distances from the Sun.

\subsection{Electron spectrum}
The solar modulation of cosmic ray electrons has been widely studied, but is still not completely understood.
\citet{mueller} analyzed the data of Helios-1 from 1974 to 1975, a period that corresponds to the approach to solar minimum,  and reported the measurements of proton and helium cosmic ray intensities for the 20-50 MeV/n energy interval between 0.3 and 1 AU. The proton gradients they obtained were small and generally consistent with zero, while the helium gradients were positive but small. On the basis of Helios-1 data, \citep{kunow} stated: `The radial variation seems to be very small for all particles and all energy ranges'.  The study of \citep{seckel} was based on this hypothesis. Since that time, the modulation theories have been developed including effects like drifts and current sheet tilt variations \citep{thomas} and short time variations. In this work we care only about long period modulations for solar maximum and minimum and we assume that the longitude gradient is negligible.
\citet{mcdonald}, analyzing cycle 20 and 22 of solar minimum between 15 and 72 AU, found that most of the modulation in this period occurs near the termination shock (assumed to be at 100 AU). On the other hand, from solar minimum to solar maximum the modulation increases mainly inside the termination shock. Recently \citet{morales}, investigating the radial intensity gradients of cosmic rays from 1 AU to the distant heliosphere and interpreting the data from IMP8, Voyagers 1 and 2, Pioneer 10 and BESS for Cycles 21, 22 and 23, found different radial gradients in the inner heliosphere compared to \citet{mcdonald}. In this region they obtained an average radial gradient of $\simeq$ 3\% /AU for 175 MeV H and $\simeq$ 2.2\% /AU for 265MeV/n He, that, at 1AU, give an intensity smaller than \citet{mcdonald} for H and higher for He. \citet{gieseler} analyzed the data from Ulysses from 1997 to 2006 at 5AU. They found a radial gradient of 4.5\%/AU for $\alpha$ particles with energies from 125 to 200 MeV/n, which is consistent with previous measurements.

In this work, our model of the modulation of cosmic rays uses the formulation given in \citet{gleeson}, using the studies
regarding the radial distribution of cosmic rays in the heliosphere at solar minimum and maximum.
The cosmic ray electron spectrum is given by the well known force field approximation of cosmic ray nuclei used to obtain the modulated differential intensity J(r,E) at energy E and distance r from the Sun \citep{gleeson}. As demonstrated by  \citet{caballero} it is a good approximation for Galactic cosmic rays in the inner heliosphere. The differential intensity of the modulated spectrum is given by:
\begin{equation}
J(r, E)=~J ( \infty, ~E+ ~\Phi(r) ) ~ \frac{E(E+2E_{0})}{(E+~\Phi(r)+2E_{0})(E+\Phi(r))}
\label{eq8}
\end{equation}
where E is kinetic energy in MeV and $E_{0}$ is the electron rest mass.
We use the local interstellar electron spectrum $J ( \infty, ~E+ ~\Phi(r))$.
$\Phi(r)=(Ze/A)\phi$ where $\phi$ is the modulation potential, Z the charge number and A the mass number.
In order to compute the modulation potential in the inner heliosphere, we used the parameterization found by \citet{fujii} for Cycle 21 from 100 AU to 1 AU, neglecting the time dependence and normalizing at 1 AU for 500 MV (solar minimum) and 1000 MV (solar maximum). As \citet{moskalenko} we find:
\begin{equation}
\Phi(r)=\Phi_{0}(r^{-0.1}-r_{b}^{-0.1})/(1-r_{b}^{0.1})
\label{eq9}
\end{equation}
where $\Phi_{0}$ is the modulation potential at 1 AU, of 500 and 1000 MV for solar minimum and maximum respectively;  $r_{b} =100 AU$ and $r$ is the distance from the Sun in AU.
Figure (\ref{fig4}) shows the local interstellar electron spectrum \citep{strong} and the modulated spectrum at 1 AU, compared with the data.
\begin{figure}[!h
 \centering
	\includegraphics[width=.35\textwidth, angle=270]{8817fig4.ps}

	\caption{ Local interstellar electron spectrum (blue line) as in \citet{strong} and the modulated at 1 AU of 500 MV (red line) and 1000 MV (black line) compared with the data. See \citet{strong} for data reference. }
	 \label{fig4}

\end{figure}
The electron intensity as a function of distance from the Sun is given in Fig.(\ref{fig5}) for different energies and for modulation potential 500 MV.
\begin{figure}[!h
 \centering
	\includegraphics[width=.45\textwidth, angle=0]{8817fig5.ps}

	\caption{ Electron intensity as a function of distance from the Sun in AU, where 0 corresponds to the Sun, for different energies and for modulation potential $\Phi_{0}=500 MV$. }
	\label{fig5}

\end{figure}

\begin{figure}[!h
 \centering
	\includegraphics[width=.36\textwidth, angle=270]{8817fig6.ps}

	\caption{ Contribution to the IC emission for different electron energy ranges, left to right: $100-10^{3}$ MeV, $(1-3) \times 10^{3}$ MeV, $(3-5) \times 10^{3}$ MeV, $(0.5-1) \times 10^{4}$ MeV,$(1-5) \times 10^{4}$ MeV, $(0.5-1) \times 10^{5}$ MeV, $1 \times 10^{5}- 5 \times 10^{7}$ MeV.  }
	 \label{fig6}

\end{figure}
The major contribution to the energy range 100-500 MeV we are interested in comes from electrons with energy between 1 and 10 GeV, as shown in Fig. (\ref{fig6}), obtained for the local interstellar electron spectrum, with no modulation.
To compute the inverse-Compton extended emission from the heliosphere and compare it with the EGRET data, details of the solar atmosphere, the non-isotropic solar wind and the asymmetries of the magnetic field have been neglected, considering the limited sensitivity of EGRET.
Since the biggest uncertaintes in the gamma-ray emission come from the cosmic-ray electron spectrum close to the Sun, in our model we considered two possible configurations of the solar modulation within 1 AU. The "naive" approximation is to assume that the cosmic-ray flux towards the Sun equals the observed flux at Earth, since there is evidence that modulation by the solar wind does not significantly alter the spectrum once cosmic rays have penetrated as far as Earth. Moreover, high energy electrons are less sensitive to the modulation. This approximation gives an upper limit of the modelled flux.  The other approach is to assume that the electron spectrum varies due to solar wind effects within 1 AU. With this "nominal" approximation we assume that the formulation for solar modulation from 100 AU to 1AU can be extrapolated also below 1 AU, using eq. (\ref{eq8}). This gives an approximate lower limit in our model.

\subsection{Calculated extended solar emission}
Figure (\ref{fig7}) shows the spectrum of the emission for two different angular distances from the Sun, without modulation and for two levels of solar modulation ($\Phi$=500, 1000 MV, respectively for solar minimum and solar maximum) and for the cases of upper and lower limits described above.

\begin{figure}[!h]
 \centering
	\includegraphics[width=.45\textwidth, angle=0]{8817fig7.ps}
	\caption{ Spectrum of the emission for (top to bottom) 0.5$^{\circ}$ and 5$^{\circ}$ angular distances from the Sun and for different conditions of solar modulation. Solid lines: no modulation, pink lines: $\Phi_{0}$=500MV, blue lines:$\Phi_{0}$=1000MV, dashed lines: naive model, dotted lines: nominal model. EGB is the extragalactic background as in \citet{stronga}}
	 \label{fig7}

\end{figure}
The angular profile of the emission is shown in Fig.(\ref{fig8}) above 100 MeV without modulation, for two levels of solar modulation ($\Phi$=500, 1000 MV) and for the cases naive and nominal. The emission is extended and is important compared to the extragalactic background (around 10$^{-5}$cm$^{-2}$s$^{-1}$sr$^{-1}$) even at very large angles from the Sun. Even around 10$^{\circ}$ it is still about 10$\%$ of the extragalactic background and with the senstivity of GLAST should be included in the whole sky diffuse emission.
\begin{figure}[!h]
 \centering
	\includegraphics[width=.45\textwidth, angle=0]{8817fig8.ps}
	\caption{ Angular profile of the emission as a function of the angular distance from the Sun above 100 MeV. Blue line: no modulation, pink lines: $\Phi_{0}$=500MV, green lines: $\Phi_{0}$=1000MV, solid lines: naive model, dashed lines: nominal model.}
	 \label{fig8}

\end{figure}
An example of the intensity of the inverse-Compton emission predicted in a region of 10$^{\circ}$ from the Sun is shown in Fig.(\ref{fig9}) for 300-500 MeV.
\begin{figure}[h!]
    \centering
\includegraphics[width=.3\textwidth, angle=0]{8817fig9.ps}

    \caption{Inverse-Compton emission modelled for a region of 10$^{\circ}$ from the Sun for 300-500 MeV and for the naive model of 1000 MV modulation. Intensity is given in cm$^{-2}$s$^{-1}$sr$^{-1}$. In the figure, the minimum value of the intensity is 1.2 $\times$ 10$^{-7}$ cm$^{-2}$s$^{-1}$sr$^{-1}$.}
\label{fig9}
\end{figure}
While the inverse Compton emission is expected to be readily detectable in future by GLAST, the situation for available EGRET data is more challenging. In the following section we present our study with the EGRET database.

\section{EGRET data preparation and selection}
We analyzed the EGRET data using the code developed for the moving target such as Earth \citep{petry}. The software permits us to produce images centred on a moving source and traces of other sources around with respect to the centred source.
To perform the analysis for the Sun, we analyzed the data in a Sun-centred system.
In order to have a better sensitivity and hence detection of our emission component, the diffuse background was reduced by excluding the Galactic plane within 15$^{\circ}$ latitude. Otherwise all available exposure from October 1991 to June 1995 was used (viewing periods 1, 11, 12, 19, 26, 209, 221, 320, 325, 410, 420), excluding the big solar flare in June 1991. When the Sun passed by other gamma-ray sources (moon, 3C 279 and several quasars), these sources were included in the analysis. In order to obtain the flux of the moon to be fitted, the same method performed for the Sun has been made with all data moon centred. Details will be given in \citet{petrya}.

\section{EGRET analysis}
We fitted the EGRET data in the Sun-centred system using a multi-parameter likelihood fitting technique (see Appendix).  The region used for fitting is a circle of radius 10$^{\circ}$ around
the Sun.
The total number of counts predicted includes inverse Compton and solar disk flux, the moon, QSO 3C279, other background sources and the background. We left as free
parameters the solar extended inverse-Compton flux from the model, the solar disk flux (treated as point source since the solar disk is not resolvable by EGRET), a
uniform background, and the flux of 3C279 - the dominant background point source. The moon flux was determined
from moon-centred fits and the 3EG source fluxes were fixed at their catalogue values. All components were
convolved with the energy-dependent EGRET PSF.
\subsection{Model of extended solar emission}
The solar extended inverse-Compton emission was modelled within 10$^{\circ}$ radius from the Sun and with a pixel size of 0.5$^{\circ}$. The model was convolved with the energy-dependent EGRET PSF and implemented in the fit, with a scale factor as free parameter. We took into account the different approximations to the modulation described above, since the data we used cover a period from October 1991 when there was a solar maximum to June 1995 close to the solar minimum. Since the emission we are looking for is very close to the EGRET sensitivity limit, we had to take as much exposure as possible and it was not possible to perform an analysis splitting the data according to solar modulation.
\subsection{3C279}
Since 3C 279 is the brightest source that passes close to the Sun, we decided to leave its flux as free parameter in the fit. We fixed the spectral index at 1.96, the value given in the EGRET catalogue. The flux obtained was then compared to that in the EGRET catalogue.
\subsection{{\bf Other background sources}}
Many sources passing within 10$^{\circ}$ from the Sun were included in the analysis. We decided to implement their fluxes as fixed parameters. With the code \citep{petry} it was possible to know the exact viewing period of any source and hence to determine its flux from the 3rd EGRET catalogue \citep{hartmann}. Hence, we took the flux value in the EGRET catalogue corresponding to the period we used, when this was listed. Since the catalogue does not contain the flux values corresponding to all the periods in which the sources were close to the Sun, in case of incertainty we decided to use the first entry in the catalogue, which is the one from which the source position was derived. In almost all cases, this is the detection with the highest statistical significance, which in most cases corresponds to the maximum value of the flux. We also took the spectral index from the EGRET catalogue. The values adopted for the sources are listed in Table (\ref{table1}).
Since the spectral index of J2321-0328 is not known, the fit was performed without this source above 300 MeV, since in the literature there is no evidence of its detection above this energy. In order to verify that this choice does not affect significantly the fit result, we tested also a typical spectral index of 2. Both fitting results  will be reported in the following results section. The traces of the background quasars were added together in the same data file, rescaled according to their fluxes.

\begin{table}
\begin{minipage}[t]{\columnwidth}
\caption{Parameters of the background sources used for the analysis.}
\label{table1}
\centering
\renewcommand{\footnoterule}{}
\begin{tabular}{l l l }
\hline \hline
Source& Flux ($>$100 MeV)\footnote{Units 10$^{-7}$ cm$^{-2}$s$^{-1}$}     &  spectral index     \\

\hline
 J0204+1458   &2.36  &     2.23   \\
 J0215+123   &1.80&     2.03  \\
 J1230-0204   &1.13  &     2.85   \\
 J1235+0233   &1.24  &     2.39   \\
 J1246-0651   &1.29  &     2.73   \\
 J1310-0517   &1.04  &     2.34   \\
 J1409-0745  &2.74  &     2.29   \\
 J2321-0328    &3.82 &     - \footnote{The choice of the spectral index we used is explained in the text} \\
\hline
\end{tabular}
\end{minipage}
\end{table}

\subsection{Diffuse background}
Since the count maps used for our analysis include only data above $\mid$b$\mid$ $>$15$^{\circ}$ latitude, and the Galactic plane is excluded, the Galactic emission can be well approximated by an isotropic background. We left its intensity as a free parameter in the fitting analysis.
\subsection{Moon}
The flux of the moon was determined from moon-centred data, fitting the flux and an isotropic background. Since the moon moves quickly across the sky, all other sources moving by are taken into account as a constant component included in the isotropic background.  The fit was performed for 2 energy ranges: 100-300 MeV and $>$300 MeV. The value of flux of the moon for the different energy ranges was obtained by maximum likelihood.
The maximum likelihood ratio statistic used for this analysis is described in the appendix.
The values of the best fit fluxes and 1$\sigma$ errors are given in Table (\ref{table2}).
\begin{table}
\caption{Fitting results for the moon}
\label{table2}
\centering
\begin{tabular}{l l l l }
\hline\hline
Energy (MeV)& Moon flux ($cm^{-2}s^{-1}$) & Background ($cm^{-2}s^{-1}sr^{-1}$)  \\
\hline
   $> 100$ & (5.55~$\pm$~0.65)~ $\times 10^{-7}$ & 3.47 $\times 10^{-5}$ \\
   $> 300$ & (5.76~$\pm$~1.66)~ $\times 10^{-8}$ & 1.01 $\times 10^{-5}$ \\
   $100-300$ & (4.98~$\pm$~0.57)~ $\times 10^{-7}$ & 2.13 $\times 10^{-5}$ \\
\hline
\end{tabular}
\end{table}
Previous studies of the EGRET data (Thompson et al.) gave a flux of ($5.4 \pm 0.7) \times 10^{-7}$ cm$^{-2}$s$^{-1}$ above 100 MeV in agreement with our analysis.
\begin{figure}[!h]
 \centering
	\includegraphics[width=.45\textwidth, angle=0]{8817fig10.ps}

	\caption{Spectrum of the moon obtained by the fitting analysis of the EGRET data between October '91 to June '95 (dashed region). Thickness of the line shows the error bars. Black bars are obtained by \citet{thompson97} for different solar conditions, while lines are the theoretical model of \citet{moskalenkob}, for solar maximum (red line) and solar minimum (green line).}
	 \label{fig10}

\end{figure}
The spectrum of the moon shown in Fig.(\ref{fig10}) has been obtained imposing a constant spectral index $\gamma$,
extrapolated up to 2 GeV.

The lunar spectral index was determined as $3.05^{+0.38}_{-0.29}$. Errors are calculated from the uncertainties on the integrated fluxes.
Since the EGRET data we used to analyze the emission from the Sun extend from solar maximum to minimum, in this analysis we estimated an average lunar flux between the two periods of solar modulation. Comparing our spectrum with the model of \citet{moskalenkob} for different solar conditions, we find a good agreement at 100 MeV, while at higher energies the model is about a factor of two higher. More extensive analysis will be given in \citet{petrya}.

\section{Solar analysis results}

The analysis was performed for 2 energy ranges : 100-300 MeV and above 300 MeV as well as the combination to improve the detection statistics. This choice was determined by the limitations of the EGRET data.  Fig.\ref{fig11} shows  the smoothed count maps, centred on the Sun, for those energy ranges and for a region of 20$^{\circ}$ side. The fitting region has a radius of 10$^{\circ}$ centred on the Sun. Since the interesting parameters are solar disk source and extended emission, the likelihood is maximized over the other components.  The analysis was performed for four different estimates of the solar modulation.

\begin{figure}[!h]
 \centering
	\includegraphics[width=.25\textwidth, angle=0]{8817fig11a.ps}\\%Log_100_500sup.eps
	\includegraphics[width=.25\textwidth, angle=0]{8817fig11b.ps}\\
	\includegraphics[width=.25\textwidth, angle=0]{8817fig11c.ps}
\caption{EGRET Sun-centred counts maps (top to bottom)$>$100 MeV, $>$300 MeV and 100-300 MeV. The colorbar shows the counts per pixel. The area is 20$^{\circ}$ on a side and the maps are Gaussian smoothed to 3$^{\circ}$.}
	 \label{fig11}
\end{figure}

\begin{table*}
\caption{Results for different energy ranges and for the naive model of 1000 MV solar modulation. Fluxes are given in cm$^{-2}$s$^{-1}$ and intensities in cm$^{-2}$s$^{-1}$sr$^{-1}$. For details see text. }
\label{table3}
\centering
\begin{tabular}{l l l l l l }
\hline\hline

Model& &  $>$100 MeV & $>$300 MeV with J2321-0328 & $>$300 MeV no J2321-0328 &100-300 MeV\\
\hline\hline
   Source flux&best fit&  4.68$^{+4.17}_{-3.82}$ $\times 10^{-8}$ &  3.38$^{+1.80}_{-1.81}$ $\times 10^{-8}$& 3.38$^{+1.88}_{-1.84}$ $\times 10^{-8}$ &14.04  $\times 10^{-8}$  \\
 &mean&  (5.42$\pm$3.20)$\times 10^{-8}$ &  (3.03$\pm$1.10)$\times 10^{-8}$& (3.65$\pm$1.71)$\times 10^{-8}$ &(14.2$\pm$9.1)$\times 10^{-8}$ \\
  &counts & 28 & 20 & 20 &39\\
\hline
   Extended flux&best fit & 3.83$^{+2.78}_{-2.80}$ $\times 10^{-7}$& 1.54$^{+1.06}_{-1.18}$ $\times 10^{-7}$&1.75$^{+1.08}_{-1.13}$ $\times 10^{-7}$&1.15 $\times 10^{-7}$\\
&mean & (3.89$\pm$2.16)$\times 10^{-7}$& (1.49$\pm$0.67)$\times 10^{-7}$&(1.70$\pm$0.87)$\times 10^{-7}$&(2.07$\pm$1.34)$\times 10^{-7}$\\
&   counts & 273&116&132& 83\\
\hline
Extended solar model&flux &2.18 $\times 10^{-7}$& 0.90 $\times 10^{-7}$&0.90 $\times 10^{-7}$&1.28 $\times 10^{-7}$\\
\hline
Background& intensity & 3.50$\times 10^{-5}$&1.13$\times 10^{-5}$&1.12$\times 10^{-5}$&2.48$\times 10^{-5}$\\
&counts & 2220&750&741&1603\\
\hline
3C279& flux & 4.88$\times 10^{-7}$&1.30$\times 10^{-7}$&1.30$\times 10^{-7}$&5.85$\times 10^{-7}$\\
&counts & 103&29&29&79\\
\hline
Prob. (flux=0)&& 6.4$\times 10^{-3}$&2.3$\times 10^{-4}$& 9.7$\times 10^{-5}$&0.24\\
\hline
Strongest bkg source &flux& 3.82$\times 10^{-7}$ & 1.28$\times 10^{-7}$    & 0.63$\times 10^{-7}$ & 2.54$\times 10^{-7}$\\
Total bkg sources & counts   &113 & 27     & 21 & 66\\
\hline
Moon& flux& 5.55$\times 10^{-7}$ & 0.57  $\times 10^{-7}$  & 0.57$\times 10^{-7}$ & 4.98$\times 10^{-7}$\\
 & counts& 37 & 4     & 4 & 29\\
\hline
\end{tabular}
\end{table*}
For the different models of solar modulation, the expected values of inverse Compton emission are in agreement with the data within 1$\sigma$, with rather big errors bars. This also means that, because of the limited sensitivity of EGRET, it is not possible to prove which model better describes the data. We found probabilities corresponding to 2.7, 3.6/4 and 1$\sigma$ above 100 MeV, above 300 MeV (including/excluding J2321-0328) and for 100-300 MeV respectively for the significance of the detection.
However, we chose the naive model of 1000 MV solar modulation in order to derive the spectra of the extended and disk emission. This is for two reasons: first this model produces the highest value of the likelihood; second it should be the most realistic for the period '91-'95, since the data cover the total period of solar maximum and the upcoming solar minimum.
{\it Hence, we report only the results for the naive case of 1000 MV solar modulation.}
\begin{figure*}[!h]
 \centering
	\includegraphics[width=.45\textwidth, angle=0]{8817fig12a.ps}
	\includegraphics[width=.45\textwidth, angle=0]{8817fig12b.ps}
	\includegraphics[width=.45\textwidth, angle=0]{8817fig12c.ps}
	\caption{Logarithm of the likelihood ratio (ln~$(L/L_{0})$) as a function of the solar disk flux and an extended component for (top to bottom) $>$100 MeV, $>$300 MeV and 100-300 MeV . Color contours are different values of the ratio, as explained in the colorbar. Contours are obtained by allowing the background and the QSO 3C279 component to vary to maximize the likelihood for each value of disk flux and extended component. Contour lines define  1, 2 and 3$\sigma$  intervals for the 2 separate parameters.}
	 \label{fig12}

\end{figure*}
We used both frequentist and Bayesian approaches to analyze the results. The statistical methods are described in the appendix.

Values of the best fit fluxes, 1$\sigma$ errors, counts and mean values with errors are given in Table \ref{table3}.
 Best fit values are calculated from the log-likelihood ratio statistic, while mean values are from the Bayesian method.
 Counts are for the maximum likelihood values, as are the background, the 3C279 fluxes and the probability of the null hypothesis. Values in the first column were used to have more statistics for detection, while separate energies are best for the analysis. For 100-300 MeV range error bars can not be determined by the frequentist method.
 We also give the probability of the null hypothesis (i.e. zero flux from disk and extended emission) using the likelihood ratio statistic. The table contains two cases above 300 MeV with different fluxes of the background sources. The first is obtained including the source J2321-0328 whose spectral index was fixed at a typical value of 2, since it is not given in the 3EG catalogue. The second case does not include that source, since it has not been detected at energy above 300 MeV. We took the second case for the following analysis. These two cases give also an estimate of the uncertainty of our results.
\begin{figure*}[!h]
 \centering
	\includegraphics[width=.32\textwidth, angle=0]{8817fig13a.ps}
	\includegraphics[width=.32\textwidth, angle=0]{8817fig13b.ps}
	\includegraphics[width=.32\textwidth, angle=0]{8817fig13c.ps}
	\includegraphics[width=.32\textwidth, angle=0]{8817fig13d.ps}
	\includegraphics[width=.32\textwidth, angle=0]{8817fig13e.ps}
	\includegraphics[width=.32\textwidth, angle=0]{8817fig13f.ps}
	\caption{Marginal probability of the two components calculated from eq.\ref{eqA4} and cumulative probability as function of the extended (upper panel) and disk (lower panel) fluxes for different energy ranges, (left to right) above 100 MeV, above 300 MeV and for 100-300 MeV}
	 \label{fig13}

\end{figure*}

The log-likelihood ratio for the three energy ranges we analyzed are displayed in Fig.\ref{fig12} as a function of solar disk flux and extended flux.  Colors show different values of the ratio, obtained by allowing the background and the QSO 3C279 component to vary to maximize the likelihood for each value of disk flux and extended component, while contour lines define  1, 2 and 3$\sigma$  confidence intervals for the two separate parameters.
Marginal probabilities of the two components calculated with the Bayesian method and cumulative probability as function of the disk and extended fluxes are shown in Fig. \ref{fig13}.
The sum of the two components, disk and extended, is given in Table \ref{table4}.
\begin{table}
\caption{{\it Sum} of disk and extended components of solar emission for different energies. Values are from the Bayesian method.}
\label{table4}
\centering
\begin{tabular}{l l  }
\hline\hline
Energy (MeV)& Total flux ($10^{-7}$ cm$^{-2}$s$^{-1}$)  \\
\hline
   $> 100$ & (4.44$\pm$2.03) \\

   $> 300$ &  (2.07$\pm$0.79)   \\

 $100-300$ &   (3.49$\pm$1.35) \\

\hline
\end{tabular}
\end{table}
Counts of the source components centred on  the Sun resulting from the fitting technique above 300 MeV are shown in Fig.\ref{fig14}.
\begin{figure*}[!h]
 \centering
	\includegraphics[width=1.\textwidth, angle=0]{8817fig14.ps}

	\caption{Counts of the source components resulting from the fitting technique above 300 MeV. Left to right: solar disk, inverse Compton, QSO 3C279, moon and background sources. Colorbars show counts per pixel.}
	 \label{fig14}

\end{figure*}
A summary of the main results is given in Table \ref{table5}.
\begin{table}
\caption{Fluxes used to produce the plotted solar spectra. Fluxes are in  10$^{-7}$ cm$^{-2}$s$^{-1}$}
\label{table5}
\centering
\begin{tabular}{l l   l}
\hline\hline
Source  & 100-300 MeV &$>$300MeV  \\
\hline

\hline
Extended&2.1$\pm$1.3  & 1.7$\pm$0.9\\
Model extended & 1.3 & 0.9\\
Disk  & 1.4$\pm$0.9 &0.4$\pm$0.2 \\
Seckel's disk model &0-1.1 &0.1-0.5\\
\hline
\end{tabular}
\end{table}
The solar disk spectral index we found is 2.4$^{+0.9}_{-0.8}$. Errors are calculated from the uncertainties on the integrated fluxes. Figure (\ref{fig15}) shows the solar disk spectrum obtained imposing a constant spectral index of 2.4, its mean value, and following a simple power law up to 2 GeV.
For the extended emission, we found a spectral index of 1.7$^{+0.8}_{-0.5}$.  The extended spectrum is shown in Fig. (\ref{fig16}). As for the disk spectrum, the spectral index has been fixed at the mean value. The spectrum is compared with the modelled spectrum for "naive" cases of 500 MV and 1000 MV solar modulation.

\begin{figure}[!h]
 \centering
	\includegraphics[width=.5\textwidth, angle=0]{8817fig15.ps}

	\caption{Solar disk spectrum. The orange regions defines the possible values obtained by varying the mean flux within 1$\sigma$ errors and for $\gamma$=2.4, the mean value of the spectral index.}
	 \label{fig15}

\end{figure}
\begin{figure}[!h]
 \centering
	\includegraphics[width=.5\textwidth, angle=0]{8817fig16.ps}

	\caption{Solar extended spectrum. Gray regions define the possible values obtained by varying the mean flux within 1$\sigma$ errors and for $\gamma$=1.7, the mean value of the spectral index. Black line is the model for the naive case of 1000 MV modulation. For comparison, the pink line shows the model for the naive case of 500 MV modulation. }
	 \label{fig16}

\end{figure}

\section{Tests of analysis procedure}
In order to perform a test of the solar detection, we divided the total exposure which we used for the analysis described above, into two periods with about the same exposure time. Then, we analyzed the data with the same fitting technique explained above.
Both these time periods contain about 3.6$\times$10$^{8}$ cm$^{2}$s of exposure on the Sun.  Assuming equal periods and a constant flux from the Sun, the two periods should give compatible fit results.
As an example, the analysis was performed above 300 MeV, where the detection was most significant and for the naive case and solar modulation 1000 MV.
The first period contains only 3C279, J1409-0745 and the moon, while in the second one there are only the other background sources and the moon; 3C279 is not present.
The total emission from the Sun was then detected at a level of 2.6$\sigma$ and 3.4$\sigma$ for first and second period respectively. The values obtained for the different emission components are consistent within 1$\sigma$. Moreover, they are also in agreement with those obtained for the total period. This confirms the validity of our method and the solar detection.

In order to exclude possible contamination of some faint solar flares detected by CGRO/COMPTEL during the same period, we performed the fitting method also with solar flares times excluded. Values will not be reported since, as expected, we did not find any change in the results.

\section{Discussion}

For the extended solar emission, Fig. (\ref{fig16}) shows that our model is fully consistent with the measured spectrum.
The main uncertainty in the model is the electron spectrum (the solar radiation field and the physics of the inverse Compton are precisely known). The electron spectrum at the relevant energies has about a factor 2 experimental uncertainty. In fact the measured extended fluxes are higher by a factor $\sim$2 (although not very significant) which suggests our electron spectrum could be too low.

Regarding the solar disk flux, the flux in all cases is in agreement with the theoretical value for pion-decay obtained by \citet{seckel}.
The Galactic background obtained with the fitting technique is compatible with the expected Galactic emission (GALPROP) \citep{stronga}. The flux of 3C~279 of 7.2~$\times 10^{-7} cm^{-2}s^{-1}$, sum of the flux for 100-300 MeV and above 300 MeV, is in agreement with the EGRET catalogue. In the catalogue for period 11 used for this analysis the flux is ($7.94 \pm 0.75) \times 10^{-7} cm^{-2}s^{-1}$ above 100 MeV, while for period 12 (the other viewing period used in the analysis) there is hardly any contribution.

With respect to the analysis of EGRET data performed by \citet{thompson97}, our study has some improvements which explain why we succeeded in detection. Instead of excluding data near the sources 3C279 and the moon, they are included in our analysis. This leads to more exposure using contributions from all observing periods. The special dedicated analysis software for moving targets and the inclusion of  the extended emission from the Sun produced a more realistic prediction of the total data and hence a more sensitive analysis.

\section{Conclusions}
In this paper the theory of gamma-ray emission from IC scattering of solar radiation field by Galactic CR electrons has been given in detail. Analyzing the EGRET database, we find evidence for emission from the Sun and its vicinity.
For all models the expected values are in good agreement with the data, with rather big errors bars. This also means that, because of the limited sensitivity of EGRET, it is not possible to prove which model better describes the data.
The spectrum of the moon has also been derived.

Since the inverse Compton emission from the heliosphere is extended, it contributes to the whole sky foreground and has to be taken into account for diffuse background studies. Moreover, since the emission depends on the electron spectrum and its modulation in the heliosphere, observations in different directions from the Sun can be used to determine the electron spectrum at different position, even very close to the Sun. To distinguish the modulation models (eg. with GLAST) an accuracy of $\sim$10$\%$ would be required. With the point source sensitivity of GLAST around 10$^{-7}$cm$^{-2}$s$^{-1}$ per day above 100 MeV, it will be possible to detect daily this emission, when the Sun is not close to the Galactic plane. In additional a precise model of the extended emission, such as that presented here, would be required in searches for exotic effects such as in \citet{fairbairn}

\begin{acknowledgements}

We thank Dirk Petry for providing counts maps, exposure and sources traces of the EGRET data and for useful discussions. We are also grateful to Berndt Klecker for useful discussions and drawing our attention to the Helios results. Thanks are due to the referee David Thompson for helpful suggestions which
significantly improved the presentation and analysis.
\end{acknowledgements}
\bibliographystyle{aa}

redpajama_set_name: RedPajamaArXiv


text:
Posted inEducation
New NEISD Leader Sean Maika: Deliberate, But Quick to Lend a Hand
by Emily Donaldson June 19, 2019 June 18, 2019
NEISD interim Superintendent Sean Maika sits in his corner office filled with personal photographs and items. Credit: Scott Ball / San Antonio Report
After less than two months on the job, Sean Maika already has made the North East Independent School District superintendent's office his own, filling the shelves with personal belongings. A stuffed Mountie toy sits on a shelf next to other trinkets from Canada, Maika's home country. Books fill a large section of shelves, and antlers and license plates from the year he was born are hung on the wall.
Related: North East ISD Names Successor for Retiring Superintendent Brian Gottardy
The personal items scattered throughout his office show more of the new superintendent's personality than one would gather from a typical school board meeting, where for the past several years Maika has sat just off the dais as a member of the central office leadership team.
Up until now, he's been a quiet and contemplative presence in district meetings, describing himself as a "strong observer" who likes to sit quietly and think before making an assumption or comment.
"I think there is so much that we can learn, and I believe wholeheartedly in listening to understand before I need to respond," Maika said.
The new NEISD chief said district officials must listen now more than ever in order to respond to the district's No. 1 challenge: competition from charter schools. In 2018-19, about 7,600 students zoned to attend NEISD schools enrolled elsewhere; most chose to attend IDEA Public Schools, Basis Texas, and Great Hearts Texas.
To address the growing array of educational choices families have, Maika told the Rivard Report that NEISD must do a better job of explaining what options NEISD can offer and showing parents the benefits of existing options. It isn't about adding a menu of new programs, but about focusing on the ones that are already working well for district families, he said.
"Being relevant and being nimble in a competitive environment, not just for us but for most districts, is going to be something that we all have to take on," Maika said.
It's a challenge Maika is eager to take up as he takes the reins from Brian Gottardy, who led the district for eight years before announcing his retirement in January.
Although he holds an interim title, the permanent job is likely to be his, and NEISD trustees can choose to make Maika's title permanent in December.
Sean Maika shakes the hand of outgoing Superintendent Brian Gottardy following being named Interim-Superintendent over Northeast Independent School District Credit: Scott Ball / San Antonio Report
A vision for NEISD's future
Maika prioritizes recognizing individuals and using his abilities and resources to solve problems. This emphasis comes from his experience as an administrator at elementary and middle schools and at the central office level.
"I've never forgotten where I came from," said Maika, who has spent close to a quarter-century working in education. "I never forgot what it is like to be a teacher. We are here to support the 68 schools in NEISD. Because that's my background, I understand to some extent and can connect with our campuses and the people and the struggles that they deal with."
After spending 11 years in the district, Maika thinks he has a good idea of the district's current standing and where it needs to go.
While districts like South San, Edgewood, and San Antonio ISDs look to add more innovative programs or schools to keep competition at bay, Maika emphasizes that NEISD has well-established educational choices for students who don't want to attend the neighborhood school.
Related: Charter-School District Conflict at City Council Reflects Tension in Public Education
With acclaimed programs like International School of the Americas and North East School of the Arts that opened years before many open-enrollment charter schools came to San Antonio, NEISD offers what Maika calls "the original school choice." With the proliferation of charter schools, he wants to make sure families understand the options available within the district.
NEISD offers year-round elementary at Castle Hills Elementary, will open a pre-K academy at the former West Avenue Elementary campus this fall, and provides a range of magnet programs in areas including agriscience, design and technology, engineering, and aviation mechanics.
Related: NEISD to Close West Avenue Elementary, Open Pre-K Academy in Its Place
"We've done business a certain way for a long time, but [the question is] is it working?" Maika said. "Is it reaching the people in the manner that we need it to? We are in the business of dealing with people from 4 years old to 100 years old, and they all want their information in different ways."
This is one of the priorities Maika plans to address in his new role.
It's all about telling the story of NEISD, district spokeswoman Aubrey Chancellor added. Programs like ISA and NESA have been around for many years, but sometimes district officials take it for granted that community members are aware of all the programs and initiatives, she said.
Maika, who has been described as more technologically savvy than his predecessor, wants to try new things to try to reach different audiences. Several weeks ago, he held a virtual town hall on Facebook Live, taking questions and comments from community members. He weighed in on clear backpacks, problems specific to individual campuses, and social-emotional learning, another priority area of his.
Students wear clear backpacks through the halls of LEE High School when the district made them mandatory in high schools and middle schools in 2018. Credit: Scott Ball / San Antonio Report
For Maika, another part of remaining competitive is ensuring his district hires and retains the best staff. The Texas Legislature's new $11.6 billion school finance bill, which includes a requirement that districts use a portion of new funds toward compensation increases, may make that task easier.
However, at NEISD's most recent budget workshop, Maika relied on his experience from close to two-and-a-half decades in education to caution trustees against spending all the additional revenue being sent to school districts as part of the legislation. Referencing previous instances in which the State has told districts to lower property tax rates and then failed to kick in additional revenue to sustain district operations, Maika urged trustees to pay close attention to the future sustainability of increased school funding.
Related: North East ISD Exercises Caution in Budgeting, Considers 3 Percent Pay Increase
Going forward, Maika said the district should be watchful for future state action to protect the interests of NEISD students.
"This job for me is not just professional, it is very personal," Maika said. "I have kids in our schools, so when I am making these decisions, I'm making it in the best interest of the 65,000 students, but also my two. I want the best for all of them."
A leader who 'walks the walk'
Becoming a district superintendent was always Maika's goal. The day he stepped through the doors of Lakeland Elementary in Lewisville ISD for his first day of teaching, he knew he would one day want to lead a district. He soon became an elementary assistant principal, and later a principal before moving to the middle school level.
Donna Newman, NEISD's associate superintendent for instruction and campus administration, remembers Maika when he was an NEISD teacher in the early 2000s. Then the principal of El Dorado Elementary, Newman recalls an ambitious young educator, already eager to take on more responsibilities.
"He has always been just a natural-born leader and he likes to be able to influence what is happening with the kids," Newman said. "He has very, very high expectations of himself and others and he is very collaborative."
Recent NEISD graduate Megan Pursley said she witnessed first-hand Maika's personal investment in students when she encountered bullying at Harris Middle School, where Maika was the principal.
When some students decided to copy the animated TV series South Park and have a "Kick a Ginger Day," Maika got wind of the plan and stood in the hallway, making his presence known, so red-headed students like Pursley felt safe.
"He was fast on it and would not put up with anyone's crap," Pursley said. "He took immediate action, and he was always like that, just getting involved right away."
Churchill High School Principal Todd Bloomer benefited from Maika's hands-on approach to leadership. When Bloomer was starting his first year as principal at Bradley Middle School, he was matched with Maika for a mentorship.
The two forged a close bond that would impact Bloomer's future with the district, Bloomer said. Describing Maika as a can-do leader with no task beneath him, Bloomer tells stories about Maika jumping in on problems without hesitation to find a solution.
On one occasion, Bloomer said Maika asked him who he couldn't live without at Churchill. Bloomer immediately thought of his secretary, who makes sure he has lunch, arrives at appointments on time, and communicates with everyone who needs a response.
"He went back to his office and wrote a thank-you note to my secretary with all the things I said about her," Bloomer said. "He really walks the walk."
Tagged: Brian Gottardy, Comal ISD, Harris Middle School, North East ISD, Sean Maika, type:feature, wc 1000-1500
Emily Donaldson reports on education for the San Antonio Report. More by Emily Donaldson

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text:
The Phelps Hatheway House and Garden
The Phelps Hatheway House and Garden tells the fascinating tale of two very wealthy colonial men, the style they lived in and their boom to bust stories. Located in the Main Street Historic District of Suffield, CT, this 18th century home is a renowned architectural masterpiece of the Connecticut River Valley.
Fort Griswold
Add a touch of reality to your Revolutionary War history lesson with a visit to Fort Griswold Battlefield State Park, site of the 1781 massacre led by the traitorous Benedict Arnold.
Mark Twain House & Museum
The Mark Twain House & Museum is the Hartford, Connecticut home, where the author and his family lived from 1874 to 1891. Twain wrote his most important works during the years he lived there, including Adventures of Huckleberry Finn, The Adventures of Tom Sawyer, and A Connecticut Yankee in King Arthur's Court.
Connecticut's Beardsley Zoo
In 1878, James W. Beardsley donated 100 acres of land to the city of Bridgeport based on the promise that the city would always use the land as a park. In 1920, the city embarked on a campaign to create a zoo and officially opened its doors two years later. The Beardsley Zoo celebrated its […]
Downtown New Haven and Yale University
Yale University is a private Ivy League research university located in New Haven, Connecticut. Founded in 1701 in the Colony of Connecticut, the university is the third-oldest institution of higher education in the United States.


text:
Paboosar is a village located in Khinvsar Tehsil, in the Nagaur district of the Indian state of Rajasthan.

Paboosar is 55 km away from the sub-district's headquarters of Khinvsar and 80 km away from district's headquarters of Nagaur. Paboosar  is administered by an elected Sarpanch (Head of Village).

The village occupies 3,689 hectares. As per 2009 stats, Pabusar is the gram panchayat of Paboosar village.

Population
The population of 2,956 is divided into 521 households, including 1551 males and 1405 females as per Population Census 2011. The population of children with age 0-6 is 578 or 19.55%. The sex ratio is 906 which is lower than Rajasthan state average of 928 whereas the Child Sex Ratio is 1007, higher than Rajasthan average of 888.

In 2011, the literacy rate was 54.42% compared to 66.11% of Rajasthan. Male literacy stands at 67.85% while female literacy rate was 39.19%. 32.95% of the population consists of Scheduled Caste(SCs).

References

Villages in Nagaur district

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text:
Twin Tiers Natives Prepare for Dorian
Monday, September 2nd 2019, 6:43 PM EDT by Alex Bielfeld
HORSEHEADS, NY (WENY) -- On Sunday, Hurricane Dorian wrote itself in the record books with sustained winds of 185 MPH, now tied second all-time for strongest Atlantic hurricanes based off winds. Dorian has caused mass destruction in the Bahamas with gusts measuring greater than 200 miles per hour. Although Hurricane Dorian is not likely to Have any impact to our region, former Twin Tiers residents who live on the eastern seaboard are bracing for the storm. We spoke with former Twin Tiers that live in the potential path of Dorian on how they are preparing.
"The end of last week, I would say like Wednesday through Friday we saw a lot of scrambling of people to get to the grocery store to get things like, batteries and water and people like to stock up on food in case the power goes out. We don't know how long you'll be waiting it out. There's a lot of lines at gas stations because a lot of people out here have generators for when the power does go out," said Lindsay Greer who currently resides in Melbourne,
Fl and is from Athens, PA.
Brevard county in Florida, where Lindsay lives, has issued a mandatory evacuation for the barrier islands that began Monday morning.
Greer also said, This weekend, a lot of people have been starting to board up their houses, board up the windows, bring stuff in from inside, trying to get as prepared as possible. Evacuations started, I believe this morning for beach side around 8 am so a lot of people have been getting their final preparations over there."
Another former resident is in North Carolina and although Dorian is not expected to be as strong as it is now residents from the Carolinas are still recovering from Hurricane Florence.
"It's almost like we are not prepared, we're still kind of regathering from Hurricane Florence. You still have people getting roofs on their house so, I think we are all really nervous about what's going to happen," said Mackenzie Moor who lives in Wilmington, NC and is from Watkins Glen, NY.
Even though these are tough times along the Eastern seaboard, many residents are coming together to help fellow neighbors out.
Christopher Cross who is originally from Corning, NY and now lives in West Palm Beach said, "We all got together and went over what we have stocked up, water, food, and everything. There's some people that live on the ground floor units, we told them if the flooding gets bad, we live on an upper unit on the third floor and said you are more than welcome to come up here if the flooding gets bad."


Qaraite and Rabbanite calendars: origins, interaction, and polemic (2018–2021) is headed by Prof. Sacha Stern (UCL) and Prof. Ronny Vollandt (LMU Munich), with Dr. Nadia Vidro (UCL) as a postdoctoral research associate and is funded by the Fritz Thyssen Foundation.
The Qaraites broke off from mainstream Rabbanite Judaism in 9th-century Iraq, and became a powerful Jewish movement in subsequent centuries, in the Near East, Byzantine Empire, and other Jewish-populated regions. Their main tenet was to reject the authority of the Talmud and rabbinic tradition, and to rely instead on a fresh reading of biblical scriptures, which led to substantially different interpretations and practices in many areas.
Among the most conspicuous differences between Qaraites and Rabbanites was how they reckoned the calendar. Whereas mainstream Rabbanite Jews followed a fixed calendar based on calculation, medieval Qaraites in Muslim lands determined the calendar by empirical factors, such as new moon sightings and the state of ripeness of the crops. These fundamental differences often led to festivals being celebrated on different dates, and hence, to considerable polemic and controversies.
This project investigates the origins of the Qaraite and the fixed Rabbanite calendars, which arose in the 8th-9th centuries and which, in our hypothesis, were closely intertwined. It studies the calendar disagreement between Qaraites and Rabbanites, its significances on each side of the debate, and its polemical uses. This research also reflects on how people run their lives with different timeframes and calendars, and on the impact this exerts upon the sense of social belonging and identity.
Image: New Moon crescent. Photo by Mauro Perani.


it is a clear account of dystonia, however it remains very challenging treating cp with dystonia. @Birkdale neuro rehab centre we are always looking, how we improve postural behaviour resulting from dystonia and how to improve quality of movements. it remains always challnaging.


A year ago today I was sitting in Charles De Gaulle airport in France. I'd just spent a week climbing in the forests surrounding Fontainebleau and I was waiting with one of my friends for our flight back to England. I was tired, suntanned and looking forward to getting back and washing all my kit. Then I got a text message from my brother.
It said: "You'll never believe what's happened".
He said: "Terrorism in America on a massive scale".
Him: "They flew a plane into the World Trade Centre. It's incredible".
Then our flight call came, I switched my phone off and thought nothing more of it. My brother and I joke around over text messages so I just assumed he was winding me up. But as soon as our plane landed and we were waiting to get off I saw a girl switch her phone on and get a text message. She read it and said "Oh that's not funny". At which point I realised that my brother wasn't joking.
My friend went to get the car from the car park and when he picked me up he had the radio and said something like "the world's gone mad". And we listened in silence to people being interviewed about what was happening. The shock, fear and madness in their voices was quite terrible to hear.
When I got home 20 minutes later I put Sky News on and was presented with the picture of the Twin Towers on fire and the endless replays of the planes hitting them. It was, as you know, a terrible atrocity and many people just couldn't believe that sort of thing could happen for real. It's okay to see it on a film. After all, it's just a film. It's not real life. But if I'm honest about it I wasn't that surprised that something on that scale could happen. If I look inside my own heart I know that deep down there is darkness. There is nothing blacker than the heart of man and any person – no matter how good natured – is capable of evil. If you don't have darkness how do you recognise the light?
But there's no argument. It was a terrible crime and innocent people paid with their lives. There can be no excuse to kill and in a modern civilised society it is inexcusable. So 12 months on, what's changed? I'm not sure that a lot has on a world stage. Certainly a lot of Americans have realised that there is a world outside the USA and that their government's foreign policy can have dire consequences when it goes wrong. A lot of people who used to feel safe in a civilised world realise that it just takes a handful of fanatics to break down those walls of protection, and they'll never feel the same way again. But on a world stage it was small potatoes. It sounds callous, but I'm afraid it's true.
A great many more people have died from the actions of evil men in recent years. I could mention Chechnya, Rwanda and Bosnia to name but a few. There are millions of people dying from AIDS, famine and war throughout the Third World and their suffering continues. But modern civilised people have a short attention span and once something's been on the news for a few days they lose interest in it. For example, had President Bush decided to invade Iraq 12 months ago I'm pretty sure he'd have had great public and international support for the move in the wake of the WTC. But a year on the American public are not so keen. And I'm not keen either. We're fickle creatures. I think that sometimes people forget that outside of CNN broadcasts, Fox News specials and BBC reports there is a real world out there with real people who are suffering terribly.
Maybe by going and looking at ground zero people can realise that things they see on TV are real. Terrible things do happen to good people. And maybe the next time people are put out of their homes by dictators, or genocide is committed on innocents and we see it on the news, then maybe we'll take a bit more interest in their plight rather than changing the channel to something more palatable. It's a big nasty world out there. And you can't change it by closing your eyes and pretending it's not there. If September 11th 2001 has done anything, it's opened people's eyes.
Just for the record, I think attacking Iraq is a bad move. I was just using it as an example of the fickle-ness of public opinion!
Good article. Public interest is indeed fickle, but then so is interest at governmental level. Rather than governments ignoring international situations, these things should be delt with politically & diplomatically AS EARLY AS POSSIBLE. Whilst this would not resolve ALL issues, it could help prevent many wars and terrorist activity. Ignoring problems doesnt make them go away, it just makes them fester, and encourages extremist activity whether by the state or the individual. On another note, I was fully in favour of taking military action to reduce the effectiveness of Al-Quaida, but even with Afghanistan, I was very dubious when one of the stated war aims was "to remove the existing regime". Whilst it is easy to condemn "bad" governments for specific actions, I find it difficult to agree with replacing a government with one chosen by outside parties, particularly when those parties are one or two countries. This is what it looks like the US & UK are heading towards with Iraq. Who is so above reproach that they can decide who is fit to govern another country? Nobody really. If action IS taken to remove the Iraqi regime, the ONLY way that this should even be considered is with the full support of the international community. Every country, just as every individual has different ideas about what is right and wrong, that's why each country has it's own laws. It is no more right for one country to dictate to another how it should behave than it is for one person to tell another how to behave. Individuals (generally) behave in the way that is set out in law as the right way to behave by the wider society of that country. Nations should abide the rules set out by the wider society of the international community, and not behave as only they see fit.
The only way to deal with global terrorism is through justice. We need international institutions such as a fully empowered and credible world criminal court to define terrorism and dispense justice. There should be a distinction made between freedom struggles based on human rights and self-determination, and terrorism (this should also include state terrorism as is the case with Isreal).
That was my point manxlennie – one man's terrorist is another mans freedom fighter. I'm as shocked and horrified by 9/11 as the next man, especially when I was looking into Ground Zero this April. I was saying to John yesterday that if the west pulled all support for Israel, then that would calm things in the middle east, and maybe we'd save a few lives by not invading Iraq. But I guess it's all gone a little bit too far now, though it's quite reassuring to see that public support for the war is wavering. We live in interesing times….
I remember people cheering and partying in Times square in New York When Bagdad was bieng bombed by America in 91′ They termed it "Fireworks over Bagdad". So do you blame other people cheering at America.
There are some americans that don't get it: http://www.coffeecup.com/attack/letter1.txt I was shocked when I received that letter in my e-mail last year. That's just as mad as terrorist attacks, IMHO. I'm glad not everybody feels that way, I mean, you may "feel" it if it happened to close people, but you don't really want it, or do you?
manxlennie – you're absolutely right, it's so much easier to create prejudice than it is to dispell it.
It just goes to show that governments don't always represent the best interests or opinions of their people. The UK is exactly the same.
What concerns me will be the years to follow. Iraq are certainly no match for the US and allies, but Hussein isn't the biggest problem. This action will further flame the fires of anti-western hatred. I hate to see what will happen next.


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Worcester in National Arena league final
December 18, 2018 - Breaking News, Leagues, Uncategorized
Worcester Swimming Club secured a place in the prestigious National Arena League finals for the second year running.
The West Midlands regional final at Rugby saw Worcester finish second with 199 points behind City of Derby A on 208.
Boldmere A scored 179, Leamington 169, Sutton-in-Ashfield 147 and Abingdon Vale 141.
After the previous two rounds Worcester topped the league on gala points with Derby second and Leamington third.
They started well as Olivia Fletcher won the women's open 200m individual medley in two minutes 21.16 seconds.
Sam Hall, back from Cardiff University, added second in the men's open 200m IM (2.12.23).
Megan Annis, racing in the girls' 15/u section, picked up a second spot before Harry Chandler won the boys' 10/11 50m butterfly (32.66).
David Annis was first in the boys' 13/u 100m backstroke (1.09.23) as was Will Gearey in the 15/u 100m butterfly (1.00.91).
Jennifer Gearey finished second in the women's open 100m backstroke (1.06.91) and newcomer Max Murray did likewise in the boys' 13/u 100m butterfly (1.07.69).
Will Gearey was second in the boys' 15/u 100m freestyle (54.63) while Tabitha Monkhouse stormed to victory in the women's open 100m breaststroke (1.12.99).
Chandler won again in the boys' 10/11 50m freestyle (30.63) and Aimee Monks claimed the girls' 13/u 100m freestyle (1.02.93).
Murray was second in the boys' 13/u 100m freestyle (1.01.52) while Fletcher finished runner-up in the women's open 100m freestyle (58.77).
In the relays, the boys' 15/u medley quartet of Louis Doyle, George Glover, Will Gearey and Daniel Day won easily.
There were close second places for other relay teams including the boys' 10/11 4x50m medley, boys' 13/u 4x50m freestyle, girls' 13/u 4x50m freestyle and men's open 6x50m freestyle.
The women's open 6x50m freestyle team of Charlotte Hall, Fletcher, Madeleine Hoare, Jennifer Gearey, Josie Armstrong and Monkhouse added another success. The B final will be at Cardiff in March.
Worcester head coach Mark Stowe said: "It was a wonderful team performance.
"Without exception, every single swimmer stepped up, swam superbly and contributed to a thrilling result. I was delighted.
"Making the national finals last year was brilliant but as is so often the case in sport it's sometimes harder to stay at the top than get there in the first place.
"Therefore to repeat that achievement again this year is really pleasing. Huge congratulations to all the swimmers, it's reward for all their hard work and dedication!"
Meghan Higgs, Amelie Forsyth-Ball, Grace Earp, Jessica Day, Jacob Cutler, William Pridden, William Thomas, Emily Clacher, Jessica Dobson, Emma McKay, Adam Rutter, Sam Hawes, Madeleine Fox-Haskins, Lauren Annis, Natasha Dobson, Naomi Marsden, Antony Redfern, Milly Hemming, Ciara Mahanta, Matthew Thomas, Bethan Stokes, Alex Farmer, Bryony Lowe, Kai Gooden-Morris, Libby Gooden-Morris and Beau Vaughan-Hawkins were also in the squad.


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Premier League clubs face disappointment in chase for Inter star Sneijder
January 9, 2013 May 15, 2015 Andrew Tuft
Wesley Sneijder is in talks with Turkish side Galatasaray over a move from Inter, potentially bringing an end to any chance of the Netherlands international moving to the Premier League despite reported interest from Tottenham Hotspur, Liverpool and Manchester United, according to ESPN.
Sneijder has fallen out of favour under Inter coach Andrea Stramaccioni, failing to make an appearance for the club since September. Sneijder's wife recently let slip that she expected to leave Milan in the near future, only to claim she was misquoted, but Galatasaray this week released a statement on their official website announcing they were in negotiations with Inter over the signing of Sneijder.
ESPN adds there was interest in Sneijder from a number of English clubs, including Tottenham and Liverpool, while United are said to have held a long-standing interest in the 28-year-old.
Sneijder, a title winner in Holland with Ajax, Spain with Real Madrid and Italy with Inter, has played more than 100 times for the Milan club, winning the Champions League in 2010.
Liverpool captain Gerrard targets increased goal return
Beckham unlikely to join West Ham or QPR
August 28, 2020 James Hill
Premier League champions Liverpool and FA Cup holders Arsenal will be going head-to-head this weekend at...
Arsenal Europe Liverpool
What Can New Boy Kostas Tsimikas Bring to Jurgen Klopp's Liverpool Side?
Liverpool finally got their hands on the Premier League trophy last season but they are already...
Featured Column Liverpool Premier League
June 8, 2020 James Hill
What We Learned From the Premier League Teams' Friendlies
As we edge closer to the official return of the Premier League, the players and coaching...
Arsenal Chelsea Liverpool Manchester United Newcastle United Premier League


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John Deere, UAW reach tentative agreement
Updated: 9:56 PM CDT Oct 30, 2021
THE CAUSE OF HIS DEATH HAS NOT BEEN RELEASED. UNITED AUTO WORKERS UNION TENTATIVEL REAYCHED AN AGREEMENT WITH JOHN DEERE. THE UNION WILL REMAIN ON STRIKE ASHEY T WORK ON THE RATIFICATION PROCESS. THE UAW VICE PRESIDENT SAYS THE AGREEMENT INCLUDES BETTER PAY. THEY WILL NOT RELEASE SPECIFICS UNTIL MEMBERS AT ALL OF THE JOHN DEERE LOCATIONS HAVE HAD THE OPPORTUNITY TO MEET AND REVIEW THE TERMS OF THE PROPOSED CONTRACT. THE UNION SAYS WE WANT TO THANK THE UAW MEMBERS AND THEIR FAMILI
The United Automobile, Aerospace and Agricultural Implement Workers (UAW) announced Saturday it reached a tentative agreement with John Deere. UAW said the John Deere bargaining team reached a tentative agreement, but the strike will continue while they finish the process of verifying the agreement. "Our UAW John Deere national bargaining team went back to our local members after the previous tentative agreement and canvassed the concerns and priorities of membership," said UAW President Ray Curry. "We want to thank the UAW bargaining team and striking UAW members and their families for the sacrifices they have made to achieve these gains. Our members have enjoyed the support of our communities and the entire labor movement nationwide as they have stood together in support and solidarity these past few weeks."UAW leadership said the agreement has "enhanced economic gains and continues to provide the highest quality health care benefits in the industry." More details will be released when the union members have time to meet and review the proposed contract. On Oct. 14, more than 10,000 John Deere union workers went on strike across the country. A majority of the union had rejected a contract offered by John Deere earlier that week. The workers at the Ankeny plant asked for raises and better retirement benefits. It was the first strike since 1986, which lasted five months.
MOLINE, Ill. —
The United Automobile, Aerospace and Agricultural Implement Workers (UAW) announced Saturday it reached a tentative agreement with John Deere.
UAW said the John Deere bargaining team reached a tentative agreement, but the strike will continue while they finish the process of verifying the agreement.
"Our UAW John Deere national bargaining team went back to our local members after the previous tentative agreement and canvassed the concerns and priorities of membership," said UAW President Ray Curry. "We want to thank the UAW bargaining team and striking UAW members and their families for the sacrifices they have made to achieve these gains. Our members have enjoyed the support of our communities and the entire labor movement nationwide as they have stood together in support and solidarity these past few weeks."
UAW leadership said the agreement has "enhanced economic gains and continues to provide the highest quality health care benefits in the industry."
More details will be released when the union members have time to meet and review the proposed contract.
On Oct. 14, more than 10,000 John Deere union workers went on strike across the country. A majority of the union had rejected a contract offered by John Deere earlier that week.
The workers at the Ankeny plant asked for raises and better retirement benefits.
It was the first strike since 1986, which lasted five months.
UAW member hit, killed by vehicle near Illinois John Deere plant
Agriculture Secretary Tom Vilsack lends support to John Deere strikers
Donations pour in from community for John Deere union workers on strike in Ankeny
Judge denies John Deere's request to limit picketers


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Posted on May 22, 2018 April 14, 2022 by
Circles of Separation (Book 3 of Waldmeer): Choose Again
Amira took every opportunity that crisp, glorious day to be outside. She walked down to the beach and returned via the shops and up the hill taking the longer route past Verloren's holiday house. There was a For Sale sign in the front garden. She stopped to look at it and wondered why Verloren would be selling.
In the five years since Farkas sold this house to Verloren, thought Amira, he has lived at Charlie's property in the back hills and in Ide's bungalow, bought a house, started a relationship, had a baby, ended a relationship, and, hopefully, is now resurrecting that same relationship.
What Amira didn't recall was Farkas's two inter-dimensional trips to the North Country; one to the wolf pack for a whole winter and one to the Head Gardener's house in the Garden of Garourinn. Verloren had also been given the privilege of an inter-dimensional visit to the Garden of Garourinn in her earliest Waldmeer days. Its value seemed to lie dormant for the many years since. Verloren did occasionally dream of the Head Gardener. She didn't know who it was other than a wise man giving advice. Generally, she couldn't recall what the advice had been.
"Hello," said Verloren as she came from the side walkway and saw Amira standing in front of her sign. "As you see, we are selling. I am sick of the small-minded mentality in this town."
"Oh, that's a pity," said Amira. She wanted Verloren to grow, not go.
"Is it a pity?" said Verloren. "For years, I have tried to get these people," she waved down the hill as if she was waving at the peasants below, "to accept and appreciate me. They can't see anything except their own petty lives."
Now that Verloren had virtually no contact with Farkas, her previous attitude to Amira had improved. Every now and again, Amira thought that she even saw a tiny, budding desire for friendship. A different friendship to what Verloren was accustomed to; not to boost her ego, support her gripes and dramas, or further any cause she had in mind, but friendship for its own sake.
Changing her tone, Verloren said, "Since I have put my house up for sale, I have had several dreams that a man keeps telling me, 'Don't change your location. Change your approach.'"
"Really?" said Amira. "That's interesting. In what way?"
"He says something like, 'Don't feed the drama monster. It's insatiable and has no friends.' I don't understand it," said Verloren, "because I don't look for drama. It looks for me!"
"Hmm," said Amira. "It's a spectacular afternoon, so maybe just enjoy it."
Verloren looked at the sky with its vast, endless blue and said, "It is spectacular, isn't it?"
"I have to go now," said Amira. "I'm going into Darnall, this evening, to help Gabriel with a group of dementia patients."
"That's nice of you," said Verloren.
"I don't know how nice it is," smiled Amira. "We are supposed to be teaching them dancing and neither of us knows what we are doing. It may not be nice at all."
Not Well or Sick
That evening, Thomas was sitting in his lounge room admiring the majestic rug Herat had recently given him. He wondered where the intentional fault was that Herat had spoken of. He wondered why Herat had given him a gift that had "undying love and healing" in it. Amidst his wonderings, his phone rang. It was Kathleen.
That's strange, thought Thomas, Kathleen rarely rings me. She waits for me to ring her because she doesn't know my schedule.
"How are you?" asked Thomas with concern.
"Hi, Thomas," said Kathleen. "I'm fine but there's a little issue."
"Yes?" said Thomas with growing concern. If it was "little" she wouldn't concern me with it all, thought Thomas.
"You know that I don't take much notice of medical opinions," said Kathleen. "I suppose that's peculiar because I was involved with the medical field for so long." Kathleen's deceased husband was a doctor. "The people with the worst health seem to be the ones most concerned about their health and the ones with the best health seem to be the ones least concerned about their health."
"Maybe, the well ones are not concerned with their health because they are well," said Thomas half-heartedly. His mind was racing with scenarios about Kathleen.
"Perhaps," said Kathleen, "but I have a feeling it's the other way around. Anyway, so as to not cause a fuss, I do all those annoying tests women over fifty are supposed to keep doing." Kathleen's voice faltered. "You are the only person I am telling this to. I have received a troubling test result today and I need to see a specialist in the next few weeks."
Thomas was still. When something really mattered, Thomas became a different person. Not completely different, but a higher version of himself. It had happened to him numerous times in his life, but he didn't understand what he was doing. It was the healing gift.
"I see," said Thomas after a lengthy pause. "Kathleen, you are not to worry about this because you are going to be well and happy. Nothing is going to hurt you. Further, I think that it may be a fortuitous opportunity for us to go on a holiday for a few weeks.
"What about work?" asked Kathleen.
"My deputy can take over. I have years of leave accrued. So, where would you like to go? On a cruise?"
"No, Thomas," said Kathleen emphatically. "I can't think of anything worse than being stuck in a confined space with indulgent people, indulging in massive amounts of food and indulgent, endless entertainment. No."
"Okay," laughed Thomas. He loved cruises. "It's not a busy time of year for tourists. It's cold. Why don't we just set out in the car and make up our mind what to do as we travel? We are old enough to trust that life will show us where to go and how to get there."
"Agreed," said Kathleen. "There is one other person that I have told."
"Who?" asked Thomas.
"My brother, Aishi," said Kathleen.
Aishi was a monk and worked in a retreat centre in the hills outside of the city.
"Oh, yes," said Thomas. "Of course. What did he say?"
"He said, 'When the body is in its rightful mode, it is silent. We feel neither well nor sick, healthy nor unhealthy. The body becomes the quiet, perfectly functioning tool by which God uses us in this life. Your body can be well just as easily as sick. Your life can be harmonious and glad just as easily as it can be tormented and dramatic. Choose carefully. And if you have chosen unfortunately then choose again.'"
"I will pick you up after work this Friday," said Thomas
Kathleen said softly, "Thank you, Thomas."
Don't Tell Me
In Darnall:
"You look so much younger without any facial hair," said Teresa to Bryan, that same evening, in one of the Darnall restaurants. They had driven there separately as it was easier for Bryan to drive straight to Darnall from the farm rather than to drive via Waldmeer. Bryan had dressed up and shaved. It was their first outing since breaking up. Teresa looked at Bryan's fresh, young face and the ten-year age gap seemed more obvious than it ever did before.
"You are not allowed to say that I look so much older when I do certain things," laughed Teresa.
Bryan laughed too but decided it was best not to say anything, even in jest, in their current circumstances.
After the meal, Bryan wanted to say something else before the evening ended.
"I want to be upfront with you," said Bryan.
"Aren't we always?" said Teresa.
Bryan frowned a bit and looked at Teresa as if to say, You were not upfront with me about not wanting to get married. He said, "I've been on a date with one of my old school friends."
As Teresa and Bryan were both locals of Waldmeer, Teresa probably knew the woman. Her mind checked through all the women from Bryan's year level who would be now in their early thirties and who were still single or single again. She couldn't remember who was in his year level. It was too far below her. She was out of high school when he was still running around the primary school playground getting grazed knees and plotting to steal the treasures from the girls' stick cubbies.
"If that is what you want," said Teresa, "that is what you must do."
"It's not what I want," said Bryan a little condescendingly. "I want love, but not everyone wants that."
"Do you think you love more because you are hurt?" said Teresa. She reached down to get her bag. "Talk to me about love when you know what it's like to get up to someone, night after night, even though you are exhausted; when you know what it's like to take the blame for someone else's weaknesses because they can't carry it themselves; when you know what it's like to protect someone even though you will become the target of someone else's hatred; when you know what it's like to never stop praying for someone until the day that they are safe." She stood up, put money on the table, kissed him on the cheek, and said, "Don't tell me what love is, Bryan."
The project coordinator from the Psychology Department handed Gabriel instructions and said, "This is from the dance instructor. I will be in the room with you but I will be a non-participating observer. We want to see if the dancing program has any observable effect on the patients' memories."
Gabriel read the instructions to Amira.
Tonight is Rumba. Introduce the side basic step. Weight on left leg, side step to right, bring left leg in, transfer weight onto left leg, and then transfer weight onto right again. Repeat other side. Introduce hip action at elementary level. Music is being arranged by the Dementia Unit. Thank you for your assistance. We will be taking over, as arranged, next week.
"Let's just begin and see what happens," said Amira.
Gabriel started reading from the notes and showing the class what to do. No one moved or even listened. He put the paper on a nearby chair.
"Can anyone dance?" he asked the class.
"We can," said an elegant gentleman in his mid-eighties. "My name is Wolfgang and this is my wife, Madeline. My wife has been here in the Dementia Unit for the past year."
"Wonderful," said Gabriel. Oops, I hope he doesn't think I'm saying wonderful to his wife having dementia, thought Gabriel.
Full of the gift of the gab, Wolfgang continued without missing a beat, "We danced competitively decades ago and went to Blackpool many times. It was the most important international competition of the year. I presume it still is."
Some of the class members were now listening.
"Would you and Madeline like to demonstrate?" said Gabriel turning on the music.
Gabriel may not have been a dance teacher but he was an art teacher and could read a class.
"We would love to," said Wolfgang. He took hold of his wife's hand and, as they danced, he seemed to be regaining part of Madeline. "We were quite a duo back then. I remember that my white jacket caused a big stir amongst all the conventional black ones. It upset the apple cart, alright. Some of the judges loved it and some hated it. We didn't care. Who cares about judges when you have each other and you are creating something together? Winning only matters when you don't have what dancing really is."
"I think I'd still want to win," said Gabriel. Amira laughed.
As Wolfgang and Madeline danced, Gabriel and Amira went around the class dancing with each participant. Shuffling would be more accurate, but it was enthusiastic shuffling.
"I remember," said Wolfgang to anyone who wanted to listen, "the first time I danced with Madeline. We were having a tryout. Neither of us was very good at that stage. We did Cha Cha and it went okay. Then came Rumba; the dance of love. A few steps into the dance, Madeline held her hand on my stomach. I was a little surprised because she was a shy and proper young lady. It seemed a little forward. Not that I minded. Oh, no. You see, it was the way she touched me. I felt electricity in my body. I didn't know if other people felt it when they danced with her or only me. Either way, I wanted her."
Wolfgang smiled at Madeline and she smiled back, although it wasn't clear if she understood anything he was saying.
"When my wife was much younger," said Wolfgang, "she would often say, 'You gotta know when to hold 'em and when to fold 'em.'"
"Did she?" asked Madeline who suddenly found her voice but not her memory. "What a wise thing to say. I hope you held onto her."
"I did," smiled Wolfgang.
Later, while walking down the hall, Amira said to Gabriel, "That was easy."
"How is Lan-Lan?" asked Gabriel.
"Cute as ever," said Amira. "It looks like Farkas may be back home, at least for the weekends, so I won't have Lan-Lan quite as much."
At that moment, Wolfgang walked past and stopped to kiss Amira's hand and shake Gabriel's. "Thank you, young man," said Wolfgang. "You reminded me of how love makes life light up." He walked off briskly, calling behind him, "See you next week. Before we know it, we will all be at Blackpool."
CategoriesCircles of Separation Tagsauthors, donna goddard, fantasy, fantasy books, fantasy fiction, healing and spirituality, love, relationships and love, spiritual authors, spiritual books, spirituality, Waldmeer, writing
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Nikolai Alexandrovich Berdyaev (1874–1948) was born in Kiev into an aristocratic family. He was educated in a military school and later entered the University of Kiev, from which he was expelled for embracing Marxism and taking part in political agitation. At twenty-five he was exiled from Kiev to the north of Russia and narrowly escaped a second period of exile shortly before the Revolution. Previously, however, he had broken with Marxism in company with Sergius Bulgakov, and in 1909 he contributed to a symposium that reaffirmed the values of Orthodox Christianity. After the October Revolution, he was appointed by the Bolshevists to a chair of philosophy in the University of Moscow, but soon fell into disfavor for his independent political opinions. He was twice imprisoned and in 1922 was expelled from the country. He settled first in Berlin, where he opened a Russian Academy of Philosophy and Religion, then moved to Clamart near Paris, where he lectured in a similar institution. In 1939, he was invited to lecture at the Sorbonne and lived through the German occupation without harm. After the liberation, he announced his adhesion to the Soviet government, but later, in an article he published in a Paris, Russian-language newspaper, he criticized the return to a policy of repression. He died in Clamart.
Books by Nikolai Berdyaev :
The Russian Idea
Translated by R. M. French
Introduction by Christopher Bamford
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Chandra K. Zender
Mrs. Zender
Chandra K. Zender, 40, of TH 10, Sycamore, Ohio, died at 1 p.m. Tuesday, May 7, 2019, in the emergency room at Wyandot Memorial Hospital, Upper Sandusky, Ohio.
She was born on July 14, 1978, in Upper Sandusky, to Ben H. and Chris Martin. Ben survives in Sycamore, and Chris and companion, David Lyons, reside in rural Sycamore. Chandra lived over 20 years with her companion, Randy A. Luman.
Surviving are a daughter, Kaylah Luman of New London, Ohio, and three grandchildren, Brayden, Grayson and April. Also surviving are two brothers, Jason (Gina) Zender of Sycamore and Joshua (Cori) Zender of Sycamore.
She had worked for many years helping her dad with masonry work as Zender Construction. She attended Mohawk High School. For hobbies, she enjoyed doing arts and crafts, loved to work in her garden, loved to go mushroom hunting, loved her cats, and loved to go to flea markets, listen to music and watch movies.
Funeral services for Chandra will begin at 3 p.m. Wednesday, May 15, 2019, at the Walton-Moore Funeral Home, Sycamore, with Pastor Terry Robinson officiating. Burial will follow at Pleasant View Cemetery, Sycamore. Visitation will be 1-3 p.m. Wednesday, prior to the funeral service.
Memorial contributions can be made to the donor's choice in care of Walton-Moore Funeral Home, P.O. Box 350, Sycamore, OH 44882. Online expressions of sympathy can be made at waltonmoorefuneralhome.com.