text:
\section{Introduction}

Radio halos in galaxy clusters are extended sources with a low surface brightness permeating the
central cluster regions. They show an approximately regular shape, resembling the cluster X-ray halo,
a steep radio spectrum $J_{\nu} \propto \nu^{-\alpha_R}$ with spectral index $\alpha_R$ typically
$\simgt 1$, and little or no polarization (see, e.g., Feretti 2003 for an observational review).
Cluster radio halos are generally quite extended with radii $R_h \simgt 1 $ Mpc, even though smaller
halos (with $R_h \simlt 0.5$ Mpc radii) have also been detected. The one in the Coma cluster, which is
usually considered the archetype of this population of radio sources, has $R_h \approx 0.9
h_{70}^{-1}$ Mpc.

The spectral slopes fall in the range $0.7 \simlt\alpha_R \simlt 2$ (as obtained from WENSS and NVSS
observations at 327 and 1400 GHz, respectively; see, e.g., the data compilation in Kempner \& Sarazin
2001). In a few well studied cases, with a wider frequency coverage, the spectral shape is known with
a better accuracy. In particular, the Coma radio-halo spectrum has been studied from $\sim 30$ MHz to
$\sim 5$ GHz, and can be fitted by a single power-law with $\alpha_R \approx 1.35$ in the frequency
range $30-1400$ MHz (Deiss et al. 1997). More recent data indicate a steepening at $\nu > 1.4$ GHz
(Thierbach et al. 2003). Some evidence has been also reported (Giovannini et al. 1993) that the
spectral index $\alpha_R$ between $\nu = 326$ MHz and $1.4$ GHz changes from $\approx 0.8$ at an
angular distance $\theta \approx 3$ arcmin from the Coma cluster center up to $\approx 1.4$ at $\theta
\approx 12$ arcmin.
In this respect, however, Deiss et al. (1997) pointed out that the emission at 1.4 GHz is much more
extended than found by Giovannini et al. (1993), thus indicating that the radial increase of
$\alpha_R$ might be in fact weaker than claimed.

The widely accepted view is that the radio halos (see, e.g., Brunetti 2003 for a theoretical review)
are produced by synchrotron emission from a population of relativistic electrons with energies $E_e
\approx 7.9 B^{-1/2}_{\mu} (\nu/GHz)^{1/2} {\rm GeV}$ diffusing in the intra-cluster magnetic field
$B$. The electron energy must be $E_e\simgt 1.37 B^{-1/2}_{\mu}$ GeV in order to emit at frequencies
$\nu \simgt 30$ MHz. Here $B_{\mu}$ is the value of the intra-cluster magnetic field in the
synchrotron emission formulae (see, e.g., Longair 1994), given in $\mu$G units.

The radio flux due to a population of relativistic electrons, whose radial density distribution $\eta
(r)$ and energy spectrum is given by
 \begin{equation}
 n_{rel}(E,r) = n_{rel,0} E^{-x} \eta(r)
 \label{eq.el.spectrum}
 \end{equation}
can be written as
 \begin{equation}
 F_{\nu,S} \propto n_{rel,0}  \nu^{- \alpha_R} \int dr r^2 \eta (r) [B_{\bot}(r)]^{\alpha_R + 1} \,,
 \label{eq.radioflux}
 \end{equation}
with $\alpha_R = (x-1)/2$. It clearly depends, in a degenerate way, on the combination of two
quantities: the spectrum and the spatial distribution of the relativistic electron density,
$n_{rel}(E,r)$, and the strength and structure of the transverse magnetic field $B_{\bot}(r)$. In
order to resolve this degeneracy, an independent estimate of one of the two quantities is therefore
needed.

As noted long ago (Perola \& Reinhardt 1972, Harris \& Grindlay 1979, Rephaeli 1979), a direct probe
would consist in measuring the emission inevitably produced by the Inverse Compton Scattering (ICS) of
the same relativistic electrons on the Cosmic Microwave Background (CMB) photons. In particular,
relativistic electrons with energies $E_e \simgt$ a few GeV would scatter the CMB photons up to the
X-ray and gamma-ray energy range. The ICS, on the CMB photons, due to the synchrotron emitting
electrons inevitably produces a power-law emission spectrum
 \begin{equation}
 F_{E,ICS} \propto n_{rel,0} E^{- \alpha_x} \int dr r^2 \eta(r) \,
 \label{eq.hxrflux}
 \end{equation}
with $\alpha_x \equiv \alpha_R$. Thus a measure of this quantity would yield the number of electrons
involved.

By using Coma cluster as a case-study, the goal of this paper is, in the first place, to predict the
brightness distribution of the ICS in the Hard X-Rays (HXR, specifically in the band 20--80 keV) for
different choices on the radial dependence, on the large scale, of the magnetic field, $B(r)$, using
as the only constraint the available information on the (azimuthally averaged) radio brightness
distribution. Such predictions are not based on the theoretical issues concerning the origin of
non-thermal phenomena in galaxy clusters (for a review of this topic see, e.g., Brunetti 2003), hence
in this respect can be considered as model-independent. We have particularly in mind that our
predictions might be useful to assess the potential of HXR imaging devices in this field. In this
context, the consequences on the ICS emission related to the small scale structure of the magnetic
field, both in direction and strength, will be emphasized.

In the second place, and to its natural extent for what concerns the small scale structures of the
magnetic field just mentioned, the information available on its longitudinal strength, as it can be
obtained, and has been inferred already, from Faraday Rotation (FR) measurements, will be used to make
what at present can be regarded as our ``best'' prediction on the spatially integrated ICS HXR
emission. The latter will then be confronted with observational results, which claim that this
component has been already detected (Fusco-Femiano et al. 1999, 2004, Rephaeli et al. 1999).

The plan of the paper is the following. In Sect.2 the radio brightness profile in Coma is used to
constrain, in a parametric form, the radial dependence of the relativistic electron density and that
of the magnetic field, and the relationships between the two. Sect. 3 is devoted to the impact of both
scalar and vectorial fluctuations in the magnetic field on the synchrotron emissivity. In Sect. 4 the
relativistic electron density as a function of radius is derived for a set of representative values of
the central magnetic field, $B_0$, and three different radial profiles for $B(r)$. Correspondingly, in
Sect. 5 the predicted ICS brightness profiles are illustrated. In Sect. 6 the results are confronted
with the measurement of a HXR candidate ICS spectral tail in Coma, and discussed also in the light of
the available information on the strength of $B$ from Faraday Rotation measurements. Sect. 7 contains
summary and conclusions.  We use $H_0=70 km\, s^{-1} Mpc^{-1}$ and a flat, vacuum-dominated cosmology
($\Omega_{\Lambda}=0.7, \Omega_m \approx 0.3$) throughout the paper.

\section{The radio-halo surface brightness in Coma}

We derive here the constraints on the spatial structure of the magnetic field $B(r)$ and of the
relativistic electrons density, $n_{rel}(E,r)$, in the Coma cluster from the analysis of its
radio-halo surface brightness. Since the radio halo emission depends on both the magnetic field
amplitude and the relativistic electron density in a degenerate way (see eq. \ref{eq.radioflux}), the
magnetic field spatial structure will be inferred from the radio halo surface brightness observations
by assuming parametric models for the spatial distribution of the relativistic electrons.

First of all, we fit the azimuthally averaged radio brightness profile of Coma observed at $\nu= 1.4$
GHz (Deiss et al. 1997) assuming initially the profile
\begin{equation}
S_\nu(\theta)=S_{\nu,0} \bigg[1+ \bigg({\theta \over \theta_c} \bigg)^2 \bigg]^{-q_R'}
 \label{bril.inf}
\end{equation}
and using the same core radius which fits the cluster X-ray brightness, with $\theta_c=10.5'$ (Briel
et al. 1992). In this case, we find a best fit parameter $q_R'=1.63 \pm 0.09$ with a reduced $\chi^2$,
$\chi^2_{red}=2.13$ with 6 d.o.f. (we give hereafter $1 \sigma$ uncertainties).

Because this fit is not sufficiently accurate, as can be judged in Fig.\ref{fig.fitbril}, it was
repeated letting this time both $q_R'$ and $\theta_{c,R}$ as free parameters. In this case a much
better fit is obtained ($\chi^2_{red}=0.40$ with 5 d.o.f., see Fig.\ref{fig.fitbril}), with $q_R'=
3.9\pm1.2$ and $\theta_{c,R}= 23.8\pm6.2$ arcmin. In the following, the parameter values from the
second fit will be used.
\begin{figure}[htbp]
\begin{center}
 \epsfig{file=fit_brillanza3.ps,height=8.cm,width=9.cm,angle=0.0}
  \caption{\footnotesize{The spatial distribution of the radio-halo brightness
  of the Coma cluster fitted with the functional form in eq. (\ref{bril.inf}): the dashed curve represents
the fit with $\theta_{c}$ fixed at 10.5 arcmin form the X-ray profile, the solid curve with the best
fit value of $\theta_{c,R}=23.8$ arcmin. Data are from Deiss et al. (1997).
  }}\label{fig.fitbril}
\end{center}
\end{figure}

By adopting these values, along with a value of the spectral index independent from $\theta$, we are
implicitely assuming that they apply also to the emission at frequencies lower than $\nu=1.4$ GHz. At
this frequency the electron energy is related to the field strength as $E_e \approx 9.35
B^{-1/2}_{\mu}$ GeV. Electrons with this energy emit via ICS photons with energy $E_X\sim 700
B_\mu^{-1}$ keV. Therefore, for $B<8.75\, \mu$G, the 20-80 keV ICS emission is due to electrons which
emit in radio at frequencies $\nu \simlt (350-1400)$ MHz. Since we shall confine ourselves to $B$
values smaller than the limit above, the spectral steepening observed at $\nu > 1400$ MHz (Thierbach
et al. 2003) has no effects on our predictions.

On the other hand, in order to emit via ICS in the 20--80 keV band, the electrons must have energies
$E_e \approx 0.35 GeV (E/keV)^{1/2}$ $ \approx 1.6-3.2$ GeV. The radio frequency at which these
electrons emit via synchrotron is in the range $\nu \approx (40-60) B_{\mu}$ MHz. For a value of $B$
as small as $B$ = 0.2 $\mu$G, their radio emission would fall in the range $\approx 8-32$ MHz, which
lies completely outside the frequency span of the observations available (see, e.g., Deiss et al.
1997). Therefore, one must be aware that any ICS prediction for values of $B_{\mu}$ less than unity
relies, to an extent which increases when $B$ decreases, upon a simple extrapolation of the observed
spectrum.

The radial dependence of the synchrotron emissivity, which corresponds to the brightness profile
assuming spherical symmetry, is given by
\begin{equation}
J(r) \propto [1+(r/r_{c,R})^2]^{-q_R}
 \label{eq.radiobrightnessprofile}
\end{equation}
with best-fit parameters $q_R = q_R'+1/2 = 4.4$ and $r_{c,R} = 0.67h_{70}^{-1}$ Mpc.

To convert this dependence into constraints on $B(r)$ and $n_{rel}(r)$, we adopt a simple functional
form, namely $n_{rel}(E,r)= n_{rel,0} E^{-x} \eta(r)$ (as in eq.\ref{eq.el.spectrum}) $B(r) = B_0
g(r)$, where
\begin{eqnarray}
\eta(r) &=& [1+(r/r_{c,R})^2]^{-q_e}\\
   g(r) &=& [1+(r/r_{c,R})^2]^{-q_B},
   \label{eq.radialprofiles}
\end{eqnarray}
with the same core radius $r_{c,R}$. It follows that
\begin{equation}
 J(r) \propto \eta(r) g(r)^{\beta_R}
 \label{eq.radiobrightnessprofile2}
 \end{equation}
with $\beta_R=\alpha_R+1=2.35$ (with the adopted value $\alpha_R = 1.35$). In order to reproduce the
observed brightness profile, the following relationship must be obeyed:
\begin{equation}
 q_e+\beta_R q_B = q_R
 \label{eq.qvalues}
 \end{equation}

We shall consider, for illustration of the HXR brightness profile to be expected, three cases: {\it
i)} a uniform distribution of the relativistic electrons, $q_e=0$, with the corresponding slope
$q_B=q_R/\beta_R=1.87$; {\it ii)} the case of a constant pressure ratio between the magnetic field and
relativistic electrons, $q_e=2q_B$, hence $q_B=1.01$ and $q_e=2.02$; {\it iii)} a uniform magnetic
field, $q_B=0$, with the corresponding slope $q_e=4.4$.

The first and the last should be regarded as limiting cases. We are fully aware of the fact that
according to hydrodynamical simulations (see, e.g., Gon\c{c}alves \& Fria\c{c}a 1999, Dolag et al.
2001, 2002) the magnetic field strength is likely to decrease radially. It is also important to stress
that these simulations indicate, in addition, that the $B$ field fluctuates on a wide range of scale.
These fluctuations can be very relevant when it comes to infer the amount of radio-emitting electrons,
hence of their ICS emission, as we shall see in the next Section.

Here it is worth stressing that a result from hydrodynamical simulations, which seems to be partly
supported by observational results on Faraday Rotation (Dolag et al. 2002) -- namely that $B(r)$ goes
approximately like the density of the thermal gas -- if assumed to hold for Coma, implies what is
shown in Fig. \ref{fig.dolag}: this figure shows, in fact, that the density of the relativistic
electrons, in order to reproduce the radio brightness profile, would have to increase from the center
outward up to a maximum at about 0.8R$_h$. We regard this as a rather unlikely situation, a
consequence which seems, to our knowledge, to have been disregarded so far. We shall however return to
this situation in Sect. 6.
\begin{figure}[htbp]
\begin{center}
 \epsfig{file=profel_z.ps,height=8.cm,width=9.cm,angle=0.0}
  \caption{\footnotesize{The radial distribution of the relatvistic electrons,
if $B(r)$ is assumed to go like the density of the thermal intracluster gas, as from hydrodynamical
simulations by Dolag et al. (2002).
  }}\label{fig.dolag}
\end{center}
\end{figure}

\section{The role of magnetic field structure: radial profile and  fluctuations}

The intra-cluster magnetic field is likely consisting of a smooth component on top of which there are
scalar (amplitude) and vectorial (directional) fluctuations.

Because the synchrotron emissivity depends non-linearly on the amplitude of the transverse component
$B_\bot$ of the magnetic field, $J_\nu \propto B_{\bot}^{\alpha_R+1}$, a radial dependence in the
smooth component of $B$, as well as the fluctuations, do have an impact on the number of relativistic
electrons responsible for the same radio-halo flux.

Concerning the smooth component with profile $B(r)=B_0 g(r)$, one can introduce its volume-averaged
value:
\begin{equation}
 <B> = {\int dV B(r) \over \int dV}= 3 B_0 \left(\frac{r_{c,R}}{ R}\right)^3 I \, ,
 \label{eq.averageb}
 \end{equation}
where $I = \int_0^p dx x^2 g(x)$, $x \equiv (r/r_{c,R})$ in terms of the typical core radius $r_{c,R}$
of the magnetic field, and of the maximum radial extension of the magnetic field $R=p r_{c,R}$. For
the same volume-averaged value of the magnetic field, we have verified that the volume integrated
number of relativistic electrons is larger when $q_B = 0$ than for any other value in the interval
$0-1.87$ selected in the previous Section.

To obtain a quantitative estimate of the impact of scalar fluctuations, we adopt a simple treatment.
Let us assume that, on scales smaller than $l(r)$
\begin{equation}
l(r) \ll {dr \over dB } B(r)
\end{equation}
where $B$ can be considered independent of $r$, the strength is subject to fluctuations $\delta B$,
such that
\begin{equation}
\langle B + \delta B \rangle = B
\end{equation}
Hence within $l(r)$
\begin{equation}
\langle (B+\delta B)^2 \rangle = B^2 + \langle (\delta B)^2 \rangle
\label{eq.fluct}
\end{equation}

Upon substitution of eq.(\ref{eq.fluct}) in the synchrotron formula, one obtains
\begin{equation}
J(r) \propto n_{rel}(r) B(r)^{\alpha_R+1} \bigg[ 1+ {\langle (\delta B)^2 \rangle  \over B^2}
\bigg]^{(\alpha_R+1)/2} \label{eq.emissivityfluct}
\end{equation}

The factor containing the second order effect of the fluctuations in eq.(\ref{eq.emissivityfluct}) is
always $\geq 1$, and can itself be a function of $r$. If we assume, for the sake of simplicity, that
it is independent of $r$, then one can immediately compute the factor, after integrating over the
volume to obtain the flux $F_{\nu}$, by which the quantity $n_{0,rel}$ is overestimated with respect
to the case of zero fluctuations. For example, with the value of $\alpha_R$ adopted for Coma, this
factor is equal to $1.12, 1.6, 2.26$  for $\langle (\delta B)^2 \rangle / B^2 = 0.1, 0.5$ and $1$,
respectively.

Vectorial fluctuations are of great importance in the interpretation of Faraday Rotation measurements,
yielding
\begin{equation}
RM=\int n_{th} \vec{B} \cdot d\vec{\ell}
\end{equation}
where $n_{th}$ is the density of thermal electrons inferred from X-ray observations.

These measurements, given the independent constraint on $n_{th}$, are in principle a very good tool to
estimate the strength of the $B$ field parallel to the line of sight, along with the coherence scale
of the field direction. We shall return on this issue in Sect. 6. Here it is sufficient to recall that
the average value of this scale is very much smaller than the cluster radius. To quantify the effects
of the directional fluctuations on the emissivity, we shall assume a random and isotropic
distribution. The emissivity formula will therefore contain the term
\begin{equation}
\langle B_\bot^{\alpha_R + 1}\rangle = f(\alpha_R)B^{\alpha_R +1} = 0.5 \bigg(\int_0^\pi (\sin
\theta)^{2+\alpha_R}d\theta \bigg) B^{\alpha_R +1} \label{eq.random}
\end{equation}

\section{Constraints on the relativistic electron density}

If we use the smooth radial distribution of the intra-cluster magnetic field as given by
eq.(\ref{eq.radialprofiles}), the normalization of the relativistic electron distribution in
eq.(\ref{eq.el.spectrum}) which reproduces the radio-halo flux at 1.4 GHz, $J_{1.4}= 0.64$ Jy (Deiss
et al. 1997), can be written as
 \begin{equation}
 n_{rel,0} = K_{\alpha_R} I_R^{-1} f^{-1}(\alpha_R)\bigg( \frac{B_{0}}{\mu G} \bigg)^{-(\alpha_R+1)} \,
 cm^{-3} GeV^{-1}
 \label{eq.nrel0}
 \end{equation}
where $I_R = \int_0^1 dx x^2  [ 1 + (R_h/r_{c,R})^2 x^2]^{-q_R}$, $f^{-1}(\alpha_R)$ is given by
eq.(\ref{eq.random}), and, we remind, $q_R = q_e + \beta_R q_B$. For the choice $\alpha_R$ = 1.35, the
normalization factor $K\cdot f^{-1}$ in eq.(\ref{eq.nrel0}) is equal to 8.64$\cdot 10^{-14}$.

For the predictive purposes declared in Sect. 1, we have adopted the following values of the central
magnetic field strength, $B_{0}$ = 0.1, 0.2, 0.5, 1, 3, 5 $\mu$G. For the three combination of $q_e$
and $q_B$ anticipated in Sect. 2, and $\alpha_R=1.35$, the quantity  $n_{rel,0}$ is given in
Tab.\ref{tab.parametri}, Col. 5, along with, in Col. 4, the volume average of $B$ calculated,
according to eq. (\ref{eq.averageb}), {\it within the observed value $R_h$ of the radio--halo}.

For all the combinations of the selected values of $B_0$, $q_e$ and $q_B$, we show in
Figs.\ref{fig.pressionia}-\ref{fig.pressionic}, as a function of the radial distance from the center,
the pressures contributed by the relativistic electrons, $P_{rel}$, by the magnetic field, $P_B$, and
by the thermal gas, $P_{thermal}$. The relativistic electron pressure was evaluated assuming
$E_{min}=1$ GeV. The pressure profiles in these figures are extrapolated out to $R_{vir}$, which is
approximately equal to 3 Mpc (Lokas \& Mamon 2003).

The pressure of the relativistic electrons needed to fit the radio-halo brightness of Coma strongly
decreases with increasing values of the central magnetic field $B_0$, consistently with
eq.(\ref{eq.nrel0}). More important, it is apparent that the pressure provided by the relativistic
electrons is always smaller than the pressure of the thermal gas. Whithin $R_h$ this holds in all
cases also when the magnetic pressure is added to that of the electrons.

To be kept in mind, as emphasized in Sect. 3, the presence of scalar fluctuations in the magnetic
field $B$ would decrease the values of $n_{rel}$, given in Table 1, by the factor $[ 1+ {\langle
(\delta B)^2 \rangle / B^2}]^{(\alpha_R+1)/2}$.

\begin{figure}[tbp]
\begin{center}
\vbox{
 \epsfig{file=pressioni_a1_coma.ps,height=8.cm,width=9.cm,angle=0.0}
 \epsfig{file=pressioni_a2_coma.ps,height=8.cm,width=9.cm,angle=0.0}
}
  \caption{\footnotesize{The radial distribution of the pressure of
  the relativistic electrons (dashed) and the magnetic field (dotted) which fit the Coma radio-halo
  brightness. We show the predictions for models with $q_e=0$ and $q_B = 1.87$ for values $B_{ 0} = 0.1, 0.2$
  and $0.5$ $\mu$G (upper panel) and for $B_{0} = 1, 3$ and $5$ $\mu$G (lower panel).
  We also show the pressure of the thermal intra-cluster gas (solid) for comparison. The
  vertical dashed line is placed at $R_h$ = 0.9 Mpc.
  }}\label{fig.pressionia}
\end{center}
\end{figure}
\begin{figure}[tbp]
\begin{center}
\vbox{
 \epsfig{file=pressioni_b1_coma.ps,height=8.cm,width=9.cm,angle=0.0}
 \epsfig{file=pressioni_b2_coma.ps,height=8.cm,width=9.cm,angle=0.0}
}
  \caption{\footnotesize{Same as Fig.\ref{fig.pressionia} but for models with $q_e=2.02$ and
  $q_B = 1.01$.
  }}\label{fig.pressionib}
\end{center}
\end{figure}
\begin{figure}[tbp]
\begin{center}
\vbox{
 \epsfig{file=pressioni_c1_coma.ps,height=8.cm,width=9.cm,angle=0.0}
 \epsfig{file=pressioni_c2_coma.ps,height=8.cm,width=9.cm,angle=0.0}
}
  \caption{\footnotesize{Same as Fig.\ref{fig.pressionia} but for models with $q_e=4.4$ and $q_B = 0$.
  }}\label{fig.pressionic}
\end{center}
\end{figure}

\section{Inverse Compton Scattering emission}

In this Section we use the radial profiles of the relativistic electrons and of the magnetic field, in
any of the abovementioned combinations which fit the radio halo brightness distribution, to predict
the brightness distribution of the HXR emission produced by ICS of the relativistic electrons on the
CMB photons.

For the general case of a relativistic electrons distribution as in eq. (\ref{eq.el.spectrum}), it is
imperative, in spherical symmetry, to introduce a maximum radius out to which it is assumed to hold,
and beyond which it goes to zero. This is so because the density of CMB photons is a constant, unlike
the strength of the magnetic field, which is constrained, for any choice of $q_e$, by the radio
brightness profile. Here we assume this radius equal to $R_{vir}$ = 3 Mpc, corresponding to a maximum
value of the angular distance from the centre $\Theta = 105$ arcmin.

Among the cases selected, it is evident from Figures \ref{fig.pressionia}, \ref{fig.pressionib} and \ref{fig.pressionic}
 that for some values of $B_0$, when either
$q_e$ or $q_B$ are equal to zero, the non-thermal pressure does not always remain below the thermal
one when one moves beyond $R_h$, and this need to be kept in mind. For simplicity we shall provide the
ICS brightness predictions {\it in all cases} using the same value of $\Theta$.

The HXR ICS surface brightness at the energy $E_X$ and at the angular distance $\theta$ from the
cluster center writes as
\begin{eqnarray}
S_X(E_X,\theta) & = & S_{X,0} \left [1+(\theta/\theta_{c,R})^2 \right]^{-q_e+1/2}
\label{eq.brilhxr}\\
                & \cdot & [{\cal B}(q_e-1/2,1/2)-{\cal B}_m(q_e-1/2,1/2)]
                \nonumber
\end{eqnarray}
where ${\cal B}$ and ${\cal B}_m$ are the Beta and incomplete Beta functions, respectively  (Abramowitz \&
Stegun 1972)
\begin{eqnarray}
 {\cal B}(a,b)&\equiv &\int_0^1 t^{a-1} (1-t)^{b-1} dt \\
 {\cal B}_m(a,b)&\equiv &\int_0^m t^{a-1} (1-t)^{b-1} dt
\end{eqnarray}
with
\begin{equation}
m= \frac {1+ (\theta/\theta_{c,R})^2}{1+(\Theta/\theta_{c,R})^2}.
\end{equation}
Here
\begin{eqnarray}
S_{X,0} & = & 4.17\times10^{-4} \times (8)^{\alpha_R-1} \left( \frac{E_X}{\mbox{keV}}
\right)^{-\alpha_R} \left( \frac{r_{c,R}} {\mbox{Mpc}}\right) \label{eq.sx0}\\
        & \cdot & \left(\frac{n_{rel,0}}{\mbox{cm}^{-3}\mbox{GeV}^{-1}}\right) \mbox{ erg s}^{-1} \mbox{ cm}^{-2}
        \mbox{ keV}^{-1} \mbox{ arcmin}^{-2},
        \nonumber
\end{eqnarray}
Specifically for Coma, the HXR surface brightness, in the 20--80 keV band, was calculated according to
the choice of parameters described in Sect. 2 and 4, and reported in Tab. \ref{tab.parametri}. To be
noted that $n_{rel,0}$ depends of course only on the value of the central radio emissivity, while
$\langle B \rangle$ represents the volume average out to $R_h=0.9h_{70}^{-1}$ Mpc. The brightness
profiles, as a function of the angular distance from the center, are given in Figs.
\ref{fig.brilhxr2}-\ref{fig.brilhxr05}, which contain, for comparison, the brightness in the same
spectral band of the thermal gas emission. It is evident that, within $\Theta = 32'$ corresponding to
$R_h$, the non-thermal HXR brightness, for appropriate values of $q_e$, can be comparable to, or
greater than the thermal one only for values of $B_0$ less than 0.5 $\mu G$. Beyond $\Theta = 32'$ the
brightness is based upon pure extrapolations outside the maximum extent of the radio-halo, $R_h$, as
measured so far. Spatially resolved HXR observation would shed light on the true distribution of the
relativistic electrons (together with that of the magnetic field) not only within but also outside
$R_h$. It is appealing that the necessary technical capabilities might be available with the next
coming dedicated experiments like, e.g., NeXT (e.g., Takahashi et al. 2004).
\begin{table}[tbp]
\begin{center}
\begin{tabular}{ccccc}
 \hline \hline
 $ q_e $ & $q_b$ & $B_0$     & $<B> $    & $n_{rel,0}$   \\
         &       & $(\mu G)$ & $(\mu G)$ & $(cm^{-3} GeV^{-1})$  \\
 \hline
 0 & 1.87 & 0.1  & 0.03 & $6.46\times10^{-10}$  \\
 2.02 & 1.01 & 0.1 & 0.051 & $6.46\times10^{-10}$ \\
 4.4 & 0 & 0.1 & 0.1 & $6.46\times10^{-10}$ \\
  0 & 1.87 & 0.2  & 0.06 & $1.26\times10^{-10}$ \\
 2.02 & 1.01 & 0.2 & 0.1 & $1.26\times10^{-10}$ \\
 4.4 & 0 & 0.2 & 0.2 & $1.26\times10^{-10}$ \\
  0 & 1.87 & 0.5  & 0.15 & $1.48\times10^{-11}$ \\
 2.02 & 1.01 & 0.5 & 0.255 & $1.48\times10^{-11}$  \\
 4.4 & 0 & 0.5 & 0.5 & $1.48\times10^{-11}$ \\
 0 & 1.87 & 1  & 0.3 & $2.89\times10^{-12}$ \\
 2.02 & 1.01 & 1 & 0.51 & $2.89\times10^{-12}$  \\
 4.4 & 0 & 1 & 1 & $2.89\times10^{-12}$ \\
 0 & 1.87 & 3  & 0.9 & $2.19\times10^{-13}$ \\
 2.02 & 1.01 & 3 & 1.5 & $2.19\times10^{-13}$ \\
 4.4 & 0 & 3 & 3 & $2.19\times10^{-13}$ \\
 0 & 1.87 & 5  & 1.5 & $6.58\times10^{-14}$ \\
 2.02 & 1.01 & 5 & 2.55 & $6.58\times10^{-14}$ \\
 4.4 & 0 & 5 & 5 & $6.58\times10^{-14}$  \\
 \hline
 \end{tabular}
\end{center}
 \caption{\footnotesize{The list of parameters used for the calculation of the Coma HXR brightness.}}
 \label{tab.parametri}
 \end{table}

\begin{figure}[tbp]
\begin{center}
 \epsfig{file=brilex_1_coma.ps,height=8.cm,width=9.cm,angle=0.0}
  \caption{\footnotesize{The spatial distribution of the HXR brightness of the Coma cluster in the 20-80 keV
  energy band as produced by ICS of relativistic electrons reproducing the radio halo flux.
  We show the predictions for different models:
  $q_e=0$ (dot-dashed curve), $q_e=2.02$ (dashed curve) and $q_e=4.4$ (dotted curve)
  for a value $B_{0}=1$ $\mu$G ~. The thermal bremsstrahlung brightness of Coma integrated in the same energy band
  (solid curve) is also shown for comparison.
  }}\label{fig.brilhxr2}
\end{center}
\end{figure}
\begin{figure}[tbp]
\begin{center}
 \epsfig{file=brilex_3_coma.ps,height=8.cm,width=9.cm,angle=0.0}

  \caption{\footnotesize{Same as Fig. \ref{fig.brilhxr2} but for $B_{0}=3$ $\mu$G ~.
  }}\label{fig.brilhxr3}
\end{center}
\end{figure}
\begin{figure}[tbp]
\begin{center}
 \epsfig{file=brilex_5_coma.ps,height=8.cm,width=9.cm,angle=0.0}
  \caption{\footnotesize{Same as Fig. \ref{fig.brilhxr2} but for $B_{0}=5$ $\mu$G ~.
  }}\label{fig.brilhxr4}
\end{center}
\end{figure}
\begin{figure}[tbp]
\begin{center}
 \epsfig{file=brilex_01_coma.ps,height=8.cm,width=9.cm,angle=0.0}
  \caption{\footnotesize{Same as Fig. \ref{fig.brilhxr2} but for $B_{0}=0.1$ $\mu$G ~.
  }}\label{fig.brilhxr01}
\end{center}
\end{figure}
\begin{figure}[tbp]
\begin{center}
 \epsfig{file=brilex_02_coma.ps,height=8.cm,width=9.cm,angle=0.0}
  \caption{\footnotesize{Same as Fig. \ref{fig.brilhxr2} but for $B_{0}=0.2$ $\mu$G ~.
  }}\label{fig.brilhxr02}
\end{center}
\end{figure}
\begin{figure}[tbp]
\begin{center}
 \epsfig{file=brilex_05_coma.ps,height=8.cm,width=9.cm,angle=0.0}
  \caption{\footnotesize{Same as Fig. \ref{fig.brilhxr2} but for $B_{0}=0.5$ $\mu$G ~.
  }}\label{fig.brilhxr05}
\end{center}
\end{figure}

We wish to conclude this Section with a note on how the volume averaged magnetic field strength should
be computed when using integral values of the radio and the HXR (ICS) flux. Cospatial radio and ICS
flux values can be used to estimate the quantity $(B_{ICS})^{\alpha_R+1} \propto F_{ICS}/F_{radio}$
(e.g. Carilli \& Taylor 2002). In general, except for the case $B$ = constant, the inequality\\
$\langle B^{\alpha_R +1} \rangle \neq  \langle B \rangle^{\alpha_R +1}$.\\
holds, and the use of the right hand side of the inequality to estimate the average value of $B$ (as
in, e.g., Henriksen 1998, Fusco-Femiano et al. 1999, 2004), is formally incorrect, although
quantitatively only by a modest factor. In addition, it must be noted that the value of this quantity
differs from the actual value of $ \langle B \rangle$, which obtains from eq. (\ref{eq.averageb}) and
depends on $q_B$, as it will be shown numerically in the next Section.

\section{Discussion}

This Section will first address the conclusions on $\langle B \rangle$, that follows from available
integral measurements. Then, it will concentrate on the further constraints, that can be derived from
FR measurements.

The integrated HXR flux from Coma has been measured with BeppoSAX and RossiXTE (Fusco-Femiano et al.
1999, 2004, Rephaeli et al. 1999). Both measurements found an excess on top of the thermal emission,
which amounts to $F_{20-80}=(1.5\pm0.5)\cdot10^{-11}$ erg s$^{-1}$ cm$^{-2}$ (Fusco-Femiano et al.
2004), and has been interpreted as ICS emission from the radio--halo. It must be mentioned that the
BeppoSAX result is still controversial (see Rossetti \& Molendi 2004), however, for the purpose of
this discussion, it could at worst be regarded as an upper limit.

\begin{figure}[tbp]
\begin{center}
 \epsfig{file=brilex_last1_coma.ps,height=8.cm,width=9.cm,angle=0.0}
  \caption{\footnotesize{The 20-80 keV brightness distributions in the Coma cluster,
as produced by ICS of relativistic electrons within a sperical volume corresponding to the radio halo
($\Theta$ = 32 arcmin): the normalizations are chosen to provide an integral value equal to the flux
measured by Fusco-Femiano (2004). The three curves correspond to  $q_e=0$ (dot-dashed), $q_e=2.02$
(dashed) and $q_e=4.4$ (dotted).
 The thermal bremsstrahlung brightness of Coma integrated in the same energy band
  (solid curve) is also shown for comparison.
  }}\label{fig.fusco}
\end{center}
\end{figure}

\begin{figure}[tbp]
\begin{center}
 \epsfig{file=brilex_z_coma.ps,height=8.cm,width=9.cm,angle=0.0}
  \caption{\footnotesize{Same as Fig. \ref{fig.fusco}, for the relativistic
electron distribution given in Fig. \ref{fig.dolag}.
  }}\label{fig.fuscodolag}
\end{center}
\end{figure}

First we consider the case, discussed in Fusco-Femiano et al. (1999, 2004), that this flux is ICS from
within the spherical volume of the radio-halo. Thus we use eq. (\ref{eq.brilhxr}) with $\Theta$ = 32
arcmin, corresponding to $R_h$, and the accordingly different normalization of eq. (\ref{eq.sx0}). By
equating the measured flux to the integral of $S_X$ out to $\Theta$, we obtain the results on $B_0$,
$\langle B \rangle$ and $n_{rel,0}$ given in Table 2, for the three different combinations of $q_e$
and $q_b$, used throughout this paper. The corresponding brightness profiles are shown in Fig.
\ref{fig.fusco}. To be noted that, as anticipated in the previous Section, the three values of
$\langle B \rangle$ are not identical, and that we recover the one obtained by Fusco-Femiano et al.
(2004), namely 0.2 $\mu$G, only if the magnetic field is constant, i.e. $q_B$ = 0.

Within the two extremes for $q_e$, 0 and 4.4, the central value $B_0$ decreases from 0.55 to 0.20
$\mu$G. The intermediate value, $B_0$ = 0.32 $\mu$G is probably the most ``realistic'', in that it
corresponds to a radial decrease in both the relativistic electron density and in the magnetic field
strength.

Furthermore, referring to the considerations devoted, in Sect. 3, to the effects of scalar
fluctuations in the magnetic field, this estimate should, in principle, be considered as an upper
limit: by how much it might differ from reality is hard to tell objectively, it could be evaluated on
the grounds of specific models, a goal beyond the scope of this paper.

On the other hand, some information on the strength of the field, along with the scale of its
vectorial fluctuations, can and have been inferred from Faraday Rotation (FR) measurements, hence we
now turn to their implications.

These measurements have been carried out in several Clusters (see, e.g., Clarke et al. 1999, 2001,
Dolag et al. 2001, 2002) and various papers have been devoted to the uncertainties on the derivation
of values for $B_\parallel$, which are related to the limited statistics on the number of independent
measurements for the same cluster (Newman, Newman \& Rephaeli 2002) or the approximations adopted for
the spectrum of the fluctuations as a function of their scale-length (En\ss lin \& Vogt 2003, Murgia
et al. 2004). When the FR measurements are made using embedded radio sources, the typical central
field strength is found to be $\sim 10-30\mu$G (Eilek 1999), but in general terms FR measurements on
background sources are considered more reliable. For Coma in particular, using data on background
sources, Kim et al. (1991) found a value of $B_\parallel$ for the region within the X-ray core radius
equal to $1.7\pm0.9 \mu$G. Furthermore, Feretti et al. (1995) found that fluctuations probably occur
on all scales down to $\approx 1$ kpc.  For a random vectorial distribution, the previous estimate on
$B_\parallel$ can be translated into an estimate of $B_0$ equal to $3.8\pm2.0 \mu$G.

Taken at face value, this quantity is significantly larger than $B_0$ given in Table 2, even in the
most favourable assumption of $q_e$ = 0. In other words, the interpretation of the excess 20--80 keV
flux, referred to above, in terms of ICS emission from the radio--halo, is hard to reconcile with
these further constraints. The more so if the possible presence of scalar fluctuations, which would
reduce $B_0$ below the strength given in Table 2, is not neglected.

One must however take into account that, for the time being, the excess HXR flux has been detected
only with non-imaging instruments, thus it cannot be excluded that the ICS emission extends outside
$R_h$. The FWHM  of the BeppoSAX PDS instrument used by Fusco-Femiano et al. (2004) covers the Coma
Cluster out to an angular distance from the center $\theta$ = 42 arcmin. If we integrate out to this
radius the predicted ICS profiles, the ones given this time by eq.  (\ref{eq.brilhxr}) and eq.
(\ref{eq.sx0}), we recover the excess HXR flux for values of $B_0$ = 1.37, 0.40, 0.20 $\mu$G for $q_e$
= 0, 2.02 and 4.4 respectively. However, even if we do so, we come close to the central $B$ value
estimated through the FR measurements only with $q_e$ = 0, a rather unlikely hypothesis, although, as
can be judged from Fig. \ref{fig.pressionia}, the non-thermal pressure remains well below the thermal
one out to $R_{vir}$, and therefore cannot be discarded on this ground.

If one accepts this hypothesis, it follows that  most of the HXR emission should be produced by
relativistic electrons located in the outer regions of the cluster. Conversely, the radio-halo
emission is dominated by relativistic electrons located in the central part of Coma and certainly at
distances smaller than $R_h$. The electrons which produce the bulk of the HXR emission are thus
different from those producing the bulk of the radio-halo emission. This is a consequence of the
assumption of an extended, diffuse HXR emission originating from ICS of CMB photons off relativistic
electrons. We note here that the different spatial location of the radio-halo emission and of the bulk
of the HXR emission is also a prediction of various models invoked to reproduce the formation of the
Coma radio-halo (see, e.g., Brunetti et al. 2001, Kuo et al. 2003).

Finally we have considered also the relativistic electrons distribution illustrated in Fig.
\ref{fig.dolag}, which follows from assuming $B(r)$ proportional to $n_{th}(r)$, as from
hydrodynamical simulations (Dolag et al. 2002). The HXR brightness profile is shown in Fig.
\ref{fig.fuscodolag}. Most of the electrons being confined in the outer regions of the radio-halo,
with a density peacking at about 0.8$R_h$, it turns out (upon integration over a spherical volume with
radius $R_h$, last and separate line in Table 2) that $B_0$ = 1.1 $\mu$G, two times larger than for
$q_e$ = 0, and much closer to the estimate from FR measurements. Evidently the same comment applied to
the previous hypothesis remains valid, namely that most of the electrons responsible for the ICS
emission are other than those responsible for most of the radio emission, albeit both are fully
confined within $R_h$.

These considerations make it very clear that in order to properly address the whole issue we badly
need spatially resolved observations in the HXR band, where new generation telescopes are being
designed to operate. Obviously the success will depend more on sensitivity and particle background
than on angular resolution, which could be in the order of one arcmin for this special purpose.

To conclude the discussion, we must remark that the EUV emission excess found in the Coma Cluster, in
the energy band 65-200 eV (see, e.g., Lieu et al. 1996, Bowyer et al. 1999, 2004) does not have any
implication on our results. In fact, relativistic electrons which emit in the mentioned EUV band by
ICS, emit by synchrotron in the frequency range $\nu \sim (0.13-0.4)\,B_\mu$ MHz. Thus, these
electrons should emit synchrotron in the observed radio band ($\nu \geq 30$ MHz) only for magnetic
field $B \geq 75$ $\mu$G, a situation that can be excluded on several grounds, the most obvious being
that the magnetic pressure would largely exceed the thermal pressure. This is not to exclude that the
EUV emission excess might itself be due to IC emission, as proposed for instance by Bowyer et al.
(2004). This is another, open problem, to which we are going to devote an independent paper
(Marchegiani et al., in preparation).

\begin{table}[tbp]
\begin{center}
\begin{tabular}{ccccc}
\hline \hline
 $ q_e $ & $q_b$ & $B_0$         &    $<B>$         & $n_{rel,0}$       \\
         &       & $(\mu G)$     &  $(\mu G)$       & $(cm^{-3} GeV^{-1})$ \\
 \hline
  0      & 1.87  & 0.55          &  0.17        & $1.16\times10^{-11}$  \\
 2.02    & 1.01  & 0.32          &  0.16        & $4.20\times10^{-11}$\\
 4.4    & 0     & 0.20          &  0.20        & $1.29\times10^{-10}$\\
\hline
 - & -          & 1.10          & 0.18         & $2.37\times10^{-12}$\\
 \hline
 \end{tabular}
 \end{center}
 \caption{\footnotesize{The parameters reported in this table are evaluated from the requirement that
 the ICS HXR emission from the radio-halo of Coma, assumed spherical, equals the flux observed by BeppoSAX. We
 report here the central value of the magnetic field $B_0$, the volume-averaged value $<B>$ and the central density
of the relativistic electrons $n_{rel,0}$, for
 the three sets, used throughout this paper, of parameters on the relativistic electron and magnetic
field distributions, which
 reproduce the Coma radio-halo brightness. The separate last line is devoted to the case where the electron distribution
 given in Fig. \ref{fig.dolag} is used.
}} \label{tab.parametri2}
 \end{table}

\section{Summary and conclusions}

Radio halos, that is diffuse synchrotron emission in Clusters of Galaxies, is a rather common
phenomenon which implies the presence of a non-thermal intracluster component, in addition to the
thermal component that gives rise to the diffuse X-ray emission. Unlike the latter, whose density and
temperature distributions can be directly inferred from X-ray measurements, the former is a
combination of relativistic electrons and magnetic fields, whose relative weight in the radio
emissivity cannot be deduced on the basis of the observed radio properties alone. In order to resolve
the degeneracy between these two parameters, an independent estimate of either one or the other is
required.

For the relativistic electrons this estimate can be obtained by measuring their unavoidable emission
through Inverse Compton Scattering on the photons of the Cosmic Microwave Background. It turns out
that, for astrophysically reasonable values of the magnetic field, the ICS emission by the same
electrons responsible for the radio emission should fall in the HXR, roughly in the range 10-100 keV,
and could therefore be easily separated, given adequate sensitivity in that range, from the thermal
emission on spectral grounds.

Alternatively, Faraday Rotation measurements on background radio sources, seen through the cluster,
can provide an absolute estimate of the magnetic field, given the available constraints on the
contribution to the rotation by the thermal electrons.

This paper, using the radio-halo in Coma as a case-study, and its brightness radial distribution as
the only constraint, concentrates on predicting the HXR (20-80 keV) brightness distribution of the ICS
emission, for different, model-independent, central values and radial behaviours of the magnetic field
(or, equivalently, of the density of the relativistic electrons). We had in mind that such predictions
could be valuable to establish requirements on sensitivity for the next generation of hard X-ray
imaging telescopes. Spatially resolved observations would tell us directly the density distribution of
the relativistic electrons, and consequently of the $B$ field. We wish to stress that such
measurements would give us information not only on the smooth radial dependence of $B$, but also of
its scalar fluctuations on small scales. These fluctuations, because of the non-linear dependence of
the radio emissivity on the field strength, imply systematically a smaller number of electrons for the
same radio flux, and consequently they reduce the HXR brightness for the same value of the locally
averaged value of $B$.

The Coma Cluster is a case where detection of a HXR tail on top of the thermal emission has already
been claimed (Fusco-Femiano et al. 2004, Rephaeli et al. 1999). We use the value of this excess flux
to estimate the central value of the field, $B_0$, for three different forms of the radial
distribution of its smooth component, and a random, isotropic distribution of its direction on scales
much smaller than the size of the radio-halo. We do this either assuming that the electrons and
magnetic fields are completely confined within the borders of the radio-halo, as determined so far, or
assuming that the distrutions adopted in our predictions extend out to the virial radius, $R_{vir}$,
of Coma. In the first case we find values of $B_0$ between 0.2 and 0.55 $\mu$G, with the largest value
corresponding to an electron density constant with radius (the volume averaged value of $B$ is exactly
equal to the value of 0.2 $\mu$G obtained by Fusco-Femiano et al. (2004) only if $B$ is assumed
constant). In the second case, taking into account the field of view of the instrument used by
Fusco-Femiano et al. (2004), we find values between 0.2 and 1.4 $\mu$G. Again, the largest value
obtains if the relativistic electron density is assumed constant with radius, a rather unlikely
possibility, which however we cannot exclude simply on dynamical grounds, because their pressure
remains below that of the thermal gas extrapolated out to $R_{vir}$. The intermediate form of the
radial distribution of $B$, yields $B_0$ = 0.4 $\mu$G.

As a third case, we consider the possibility, supported by hydrodynamical simulations (Dolag et al.
2002), that $B(r)$ is proportional to $n_{th}(r)$. This implies a rather peculiar relativistic
electron density distribution, which has its minimum value at the center, and peaks at about 0.8$R_h$.
Upon integration over the spherical volume within $R_h$, the HXR flux measured by Fusco-Femiano et al.
(2004) is recovered with $B_0$ = 1.1 $\mu$G.

A comparison with estimates from FR measurements is then made. Although such estimates are still
controversial, a value of $B_0$ equal to 1-2 $\mu$G seems rather acceptable. Consistency with the
estimates from the HXR excess is at best marginal. The more so if one considers that the latter were
obtained ignoring the (admittedly hard to quantify in a model-independent way) scalar fluctuations,
whose presence would decrease the value of $B_0$. Moreover, if the claimed HXR excess emission is
really there, and it is due to ICS, it would follow that the electrons responsible for the bulk of
this emission are mostly distributed outside the region where the electrons responsible for the bulk
of the radio emission reside. It is then quite evident that measurements of the HXR brightness
distribution, whose prediction is the main scope of this paper, are a necessary step to clarify this
important issue.

\acknowledgements{The authors thank the Referees for useful comments which helped to improve the
paper. S.C. is supported by PRIN-MIUR under contract No.2004027755$\_$003.}

redpajama_set_name: RedPajamaArXiv


text:
Using legal background to aid statutory interpretation - R (English Bridge Union Ltd) v The English Sports Council
It has been reported in the media that, in R (English Bridge Union Ltd) v The English Sports Council, the Administrative Court determined the question of whether or not bridge should properly be classified as a sport. Nowhere in the judgement is that question addressed. What the court did was determine whether (for the purpose of fulfilling its functions) the English Sports Council (the 'Council') could lawfully adopt a definition of sport which required physical activity, given the Council's Royal Charter and the relevant legislation.
In finding that it was entitled to adopt such a definition, the court held that repealed parts of an Act can legitimately be used to assist in understanding the proper interpretation of the parts of the Act which remain in force.
Established by Royal Charter in 1996, one of the Council's key functions is the distribution of funding for sporting activities, including funding provided under the National Lottery etc Act 1993 and under the Physical Training and Recreation Act 1937 (the '1937 Act'). Neither the relevant legislation nor the 1996 Charter defined sporting activities for these purposes and, in its recognition policy, the Council adopted the definition of "sport" from the European Sports Charter; which defined sport as including specified forms of "physical activity".
This meant that so-called "mind sports" (such as bridge) did not qualify as a sport and could not benefit from the Council's funding or obtain any other benefit that might have followed from being classified by it as a sport. Other recognised definitions of sport include "mind sports". For example, bridge is recognised as a sport by the International Olympic Committee.
The Council's rationale for adopting the definition in the European Sports Charter was that the definition aligned with the underlying legal framework for its activities. In particular, the 1996 Charter referred to "sport and physical recreation". Tracing the background of the Council's predecessor bodies led back to the 1937 Act, also relevant because the Council distributes funds under powers contained in that Act. The 1937 Act referred to the provision of "physical training and recreation".
A background memorandum to the 1937 Act suggested that it was intended to encompass only physical activities. In addition, provisions in the 1937 Act at the time of commencement (now repealed) supported this as its intention. For example, a predecessor body of the Council was given functions relating to "the maintenance and improvement of the physical well-being of the people by means of exercise and recreation".
The Council submitted that its engagement with sport related only to sport which involved physical activity and that this was supported by the proper interpretation of the legal framework.
English Bridge Union (the 'EBU'), the representative body for bridge in England, brought judicial review proceedings against the Council's adoption of a recognition policy using a definition of sport which was limited to physical activity. The challenge was brought on the following key grounds:
The Council had misconstrued the 1996 Charter in adopting a policy where physical activity was required for an activity to be recognised as a sport. The reference to "sport and physical recreation" in the 1996 Charter should not limit sport to physical activities as this would be against the ordinary natural meaning of the word. There was also no necessity to confine the definition of objects of the 1996 Charter to those set out in the 1937 Act (as the 1937 Act did not impose a duty on the Council).
In any case, the Council had misconstrued the phrase "physical training and recreation" in the 1937 Act. This was in part because the proper interpretation of the statute has moved on with the passage of time, such that "mind sports" should now fall within such a phrase (even if they did not when the legislation was passed). But this was also because the Council was seeking to use wording in the 1937 Act which had been repealed to understand its proper meaning and this was an impermissible approach to statutory interpretation.
The claim failed on all grounds. In summary Dove J held that:
It is "entirely permissible to have regard to any relevant parts of the Act which were part of the Act as originally passed but were subsequently repealed in seeking to understand the intention of Parliament". When taking into account the repealed provisions and the background memorandum, the court was not persuaded that the Council had fallen into error.
The court did not agree with the EBU that the meaning of the phrase "physical training and recreation" has moved on since 1937. There may be good policy reasons for the 1937 Act to promote mind sports, but this does not alter the meaning of the legislation; the inclusion of mind sports would require the Act to be amended by Parliament.
The meaning of the 1996 Charter could only properly be derived from examination of the text of the Charter alongside the background. While not determinative, it was quite proper for the Council to use the 1937 Act as a starting point. The 1937 Act (properly interpreted) and the other background to the 1996 Charter provided sufficient support for the conclusion that the Council's (and its predecessors') work was confined to physical activity.
For these reasons, it was appropriate for the Council to have adopted the definition of "sport" from the European Sports Charter.
In this case, the court was required to apply three different rules of statutory interpretation:
First, a statute is 'always speaking' - the meaning of a provision cannot change over time, but the context or application of a statutory expression may change (R (Quintavalle) v Secretary of State for Health). For example, an Act passed several decades ago which applies to dogs could not properly be interpreted to apply to cats, but it could properly be held to apply to animals which were not regarded as dogs when the Act was passed, but are so regarded now. Dove J did not consider that this rule assisted the EBU.
Second, it is often permissible to consider the background materials to a statutory provision to aid in interpretation, although there are limitations to this (such as the rule set out in Pepper (Inspector of Taxes) v Hart for when recourse may be had to Hansard materials).
Third, it is permissible to have regard to parts of an Act which have been repealed in seeking to interpret parts of the Act which remain in force.
The third of these rules is the least established. Dove J considered that the authorities relied on by the EBU did not assist them in arguing that the repealed provisions could not be considered, because the authorities related to the cessation of substantive effect of a provision on its repeal. Dove J considered that whether or not a repealed provision has substantive effect is a different question from whether or not a repealed provision can be used to assist in understanding Parliament's intention in relation to other provisions which are still in force.
It is entirely logical that, in interpreting a provision which is not completely clear, the court should be able to look at the entire background, including repealed provisions. Repealed provisions can clearly be of value in assisting a court to understand legislative intention (as they were in this case).
Nonetheless, where a provision has been repealed, one might be forgiven for assuming that it can be consigned to history. On the basis of this rule of interpretation, that assumption would be incorrect.
It should be noted that the courts have, in a number of cases, considered repealed provisions in a much broader way, where the repealed provision is not in the same piece of legislation as that under scrutiny, but where there is some other reason why Parliamentary intention from one Act might (at least in part) be gleaned from another. Use of repealed provisions in this way will necessarily be context specific.
There seems to be no reason in principle why the principle of having regard to parts of legislation which have been repealed (in order properly to interpret parts which are still in force) should apply any differently to primary legislation than to secondary legislation or any other legislative document (such as a byelaw or licence condition).
Anyone seeking to construe the meaning of ambiguous or unclear provisions should be prepared to review repealed provisions which are related. In addition, from the other end of the telescope, this rule of interpretation should be in the mind of those drafting amendments to such provisions since it may, in certain cases, impact on how repeals should be enacted.
We note that the EBU has applied for permission to appeal.
Related Public Law & Regulation
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John P Cooper Partner - Birmingham
john.cooper@gowlingwlg.com
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redpajama_set_name: RedPajamaCommonCrawl


The First Great Awakening in the American colonies is often dated 1740-43. Like other great revivals, the spiritual climate of the churches had reached a low point. Practices like the Half-Way Covenant brought many into church membership without requiring any indication of saving faith. Consequently, churches were a mixture of believers and unbelievers. The vitality of the Christian testimony was watered down by its mixture with the world.
Far Reaching Results. Traveling evangelists like George Whitefield and Gilbert Tennent were used by God to quicken the spirits of His people. Through their preaching many church members and even preachers came under the conviction of the Holy Spirit and realized that they had never been converted. They were greatly distressed until they had made their salvation sure. Historians estimate that 25, 000 to 50,000 persons were added to the churches in New England alone. New churches were started in record numbers, and colleges like Dartmouth and Princeton began to train missionaries and ministers to carry the gospel to the lost world. This revival also laid the foundation of cooperative relationships between denominations. The religious liberties guaranteed in the new republic had their birth in this revival.
Revival at Northampton. Sometime around 1734 revival began to occur in several locations in New England. God used these early revivals and awakenings to prepare the soil of New England for the sowing of the gospel that would follow. Northampton, Massachusetts, was the site of a citywide awakening in 1734-35. Jonathan Edwards was pastor of the Congregational Church. Prior to the revival the town experienced a "degenerate time" with a "dullness of religion." According to Edwards, the young people were addicted to tavern drinking, lewd practices, and frolics among the sexes the greater part of the night.
In a nearby village two young people died in the spring of 1734. People began to think soberly about spiritual and eternal matters. In answer to the prayers of His people, God began to move. In the fall Edwards preached on justification by faith alone. In December of 1734, five or six persons were converted. One of them was a young woman who was "one of the greatest company keepers in the whole town." Her life was so radically changed that everyone could tell it was a work of God's grace. During the following six months, 300 people were hopefully converted in this town of 1,100.
Would you like to see God sweep our city and church like that? Would you be willing to pray: "God whatever it takes for you to bring revival to your people, please do it"?
This account has been adapted from "Narrative of Surprising Conversion" by Jonathan Edwards in The Works of President Edwards, New York: Levitt & Allen, 1857 (pp.231-272); and The History of American Revivals by Frank Granville Beardsley, 1912 (pp. 20-83).
• Pray that you and your family will seek first His Kingdom in every area of life (Mark 6;33).
During his time in Houston, Texas, Charles Parham was impressed to open a short-term Bible school on January 1, 1906. The most important person to be touched by Parham at this school was a son of slaves, a black Holiness preacher named William Joseph Seymour (1870-1922).
After the school, Seymour left Houston to accept a call to pastor a newly formed Holiness congregation on Sante Fe Street in Los Angeles. His first sermon was from Acts 2:4, which earned for him a padlocked door on the meeting place.
"As though hit by a bolt of lightning, the entire company was knocked from their chairs to the floor. Seven began to speak in tongues and magnify God….Soon it was noised over the city that God was pouring out His Spirit".
Soon large crowds gathered at the Asberry home. Only after part of the floor collapsed were the meetings moved to an abandoned A.M.E. Church building at 312 Azusa Street in mid-April of 1906. Vinson Synan calls the meetings at Azusa Street among "the most far-reaching religious meetings of the twentieth century." Synan continues: "No sooner had Seymour began preaching in the Azusa location than a monumental revival began. Scores of people began to 'fall under the power' and arise speaking in other tongues." Services continued daily for 1000 days.
O Father, do it again! Pour out your Pentecostal power upon your Church, that the overflow might renew a parched and desolate land! In Jesus' awesome Name! Amen.
• Pray for our elected officials to receive the "fear of the Lord" as they lead.
Please join regional saints at the Lincoln Memorial, Saturday, Nov 1, 2014.
Following a regional prayer event Washington Prayer Gathering, Oct 13, many believed that further prayer, celebration, and declaration should follow. So, A Word for America was born!
Add your voice to the choir by your presence or prayer!
In Matthew 24 and 25 Jesus exhorts His disciples to be watchful in prayer. The End-Time Church must be awake to pray. Informed intercession helps us to be motivated to lift our prayers above our personal needs to the matters that concern our Father. His house, you and I, is a House of Prayer for ALL nations.


Caponata is a Sicilian Vegetable Stew based on vegetables, above all aubergines. Serve it with our delicious rosemary focaccia bread.
BLANCH the chopped celery in lightly salted water for a few minutes, then drain.
by the oil. – you may need to add another spoon of oil.
WHEN the aubergines are golden on each side remove from the pan and drain on some kitchen paper.
INTO the same used pan put a little oil and add your blanched celery, onion, and crushed garlic.
FRY for a few minutes and then add the tomato paste, vinegar, sugar, olives, capers and water.
REDUCE the heat to low and cook covered for 10 mins.


Through the generations of life we celebrate the ordinary and extraordinary moments of each person's life. These celebrations are based upon the three values of mutual respect, self-determination and faith in God.
Tri- Generations is a leading provider of services and supports to individuals with developmental disabilities in the state of Kentucky. Each location of Tri-Generations controls its growth and retains its size so we can remain connected and committed to make a difference in the lives of those supported. Through proven history, experience, reputation and our values base, Tri-Generations customizes services & supports to fulfill each individual's unique journey in life, recognizing ever-changing needs.
Tri-Generations believes that people with intellectual/developmental disabilities and their families are the primary decision makers in the management of their lives. Tri-Generations supports and facilities the use of person centered processes. Tri-Generations will support individuals and their families to make informed decisions, which will empower them to direct their supports to the extent they desire while providing effective individualized supports to ensure health and safety.
Tri-Generations promotes the full inclusion of people with intellectual/developmental disabilities into their communities. Tri-Generations also believes in promoting quality of life, health and safety by enhancing natural relationships with friends, families, neighbors and fellow citizens, as these relationships occur in the community.
Tri-Generations believes every person's life is grounded in flexible, individualized support, and an understanding of the life stages experienced by all people from birth, through childhood, adulthood, and old age. Tri-Generations recognizes that the journey through life includes continual transition and adaptation. While a person's goals and needs change throughout their lifetime, all people rely on their families and the larger community for their sense of belonging and identity.
Tri-Generations recognizes the strengths of all people with intellectual/developmental disabilities and their families, from all races, ethnicities, cultures, and socioeconomic circumstances. Tri-Generations' goal of diversity is to support individuals and their families in a culturally respectful manner, which is responsive to their beliefs, personal life styles, attitudes, language and behaviors, as we strive to provide meaningful opportunities for full participation in their communities.


Brits who plan to relocate to a new house within the UK should prepare for higher costs, which now amount to £7,381 on average, according to a study. The research showed that the average fees have increased to its highest level in the last seven years, even when adjusted for inflation.
Higher stamp duty also contributed to more expensive fees for relocation. The study noted that it accounted for 27% of expenses, which amounted to £2,019 based on the medium home price in 2017. A decade ago, Britons paid £1,814 in taxes for a medium-priced property acquisition.
The economic crisis in 2009 primarily led to an increase in basic stamp duty. The government raised it to £175,000 that year. Solicitors conveyancing fees also accounted for a portion of the expenses. The UK government recently supported the Competition and Markets Authority's (CMA) proposal, which aims to make property conveyancing services more transparent and competitive.
High stamp duties may have forced homeowners to reduce their asking prices, particularly on Stockton-On-Tees where most sellers have discounted their listings by £13,350 or 8% on average. Experts said that the move reflected the desire to offload properties in a sluggish market in November.
In London, only 39% of listings had discounted prices during the month. However, asking prices fell by £53,251 or 7.4% on average. Those who bought homes in Kensington and Chelsea noticed the biggest markdown at £129,559 on average, which equated to a 7.9% discount.
A home purchase does not end by simply signing the deal and paying the asking price, so be prepared to cover all expenses up until you move into your new house. Learn about the market before you sign the sale agreement.


The OC Center for Facial Plastic Surgery offers a variety of top-of-the-line skin care products that can revitalize your skin and reduce the appearance of sun damage, acne, and other blemishes. As an extensively trained facial plastic surgeon, Dr. Ali Sepehr can help you make your skin smoother and healthier with customized skin treatment plan designed just for you. The product lines we carry are medical-grade and are made to help you replenish healthy skin on a cellular level, improving tone, texture, and strength. With prescription-strength skin care products, you improve the look and feel of your skin and attain a healthy, youthful sheen.
Please contact The OC Center for Facial Plastic Surgery for more information on skin care products available at our practice.
A medically-supervised skin care program gives patients access to products that are stronger and have more effective ingredients than are available over-the-counter.
Photodamage and premature signs of age such as wrinkles and brown spots can be remarkably improved with Firm and Fade cream. This advanced skin care solution penetrates deep into the skin to provide a tighter and smoother texture. Firm and Fade also balances and evens skin tone while accelerating the growth of healthier skin layers. With Firm and Fade as part of your regular skin care regimen, you can help your skin to achieve a more youthful and radiant complexion.
SkinMedica®contains a number of restorative ingredients that have proven to renew the skin and reduce the signs of a number of common skin conditions. This advanced product line can diminish the appearance of fine lines, discoloration, and ages spots while working to enhance the skin's texture, elasticity, and tone.
Essential Defense Mineral Shield SPF 35 – this hypoallergenic sunscreen provides the highest level of defense against UVA rays available. It also offers vital UVB ray coverage for comprehensive skin protection without clogging pores. Oil-free and fragrance-free, the serum can be excellent for use on sensitive skin types.
Essential Defense Mineral Shield Broad Spectrum SPF 32 (Tinted) – this slightly tinted formulation often works well for individuals with darker skin tones and provides the same level of intensive UVA and UVB ray protection as the SPF 35 sunscreen. Offering all of the benefits characteristic of SkinMedica®'s Essential Defense products, this advanced sunscreen is hypoallergenic, oil-free, paraben-free, fragrance-free, and should not clog pores.
Post-Procedure System – many of SkinMedica®'s products can be beneficial for patients who are undergoing laser skin resurfacing or other skin rejuvenation treatments. The Post-Procedure System includes a number of creams that can help the healing process and even enhance the results of a cosmetic enhancement procedure.
Lytera® 2.0 Pigment Correcting Serum – this versatile serum can correct hyperpigmentation, diminish the appearance of dark spots and blotches, and create a more even skin tone for individuals of all skin types. The formulation works well alone, or for the purpose of optimizing adjunctive treatment results, such as chemical peels, microdermabrasion, and more.
SkinMedica® Rejuvenative Moisturizer – composed of a derivative of hyaluronic acid, this moisturizer can effectively rejuvenate, replenish, and nourish facial hydration for normal to dry skin types. The formulation works to optimize skin health when used alone, or as part of a wider skincare regimen.


text:
using System;
using System.Collections.Generic;
using System.Linq;
using System.Text;
using System.Drawing;

namespace BB.Common.WinForms
{
    public abstract class BaseTheme
    {
        public Dictionary<string, Color> Colors { get; protected set; }
        public Dictionary<string, Brush> Brushes { get; protected set; }
        public Dictionary<string, Pen> Pens { get; protected set; }
        public Dictionary<string, int> Units { get; protected set; }
        public abstract string Name { get; }

        public BaseTheme()
        {
            Colors = new Dictionary<string, Color>();
            Brushes = new Dictionary<string, Brush>();
            Pens = new Dictionary<string, Pen>();
            Units = new Dictionary<string, int>();

            LoadProperties();
        }

        protected abstract void LoadProperties();

        public void AddColor(string name, Color color)
        {
            Colors[name] = color;
        }

        public void AddBrush(string name, Brush brush)
        {
            Brushes[name] = brush;
        }

        public void AddPen(string name, Pen pen)
        {
            Pens[name] = pen;
        }

        public void AddUnit(string name, int unit)
        {
            Units[name] = unit;
        }
    }
}

redpajama_set_name: RedPajamaGithub


Curvy bottle shaped porcelain table lamp in a glossy textured stained ivory crackle finish with matching sphere finial. Topped with tall putty colored fabric shade with light gray cotton lining. 3-way switch.


text:
Speakers and Events
Daily Trojan Editorial Board
Expansion of LGBT education beneficial
By ELENA KADVANY
October 23, 2011 7 Comments/in Columns, Featured, Opinion
LGBT rights are slowly but surely advancing in America on the national and local levels. "Don't ask, don't tell" was officially repealed in September. California passed a law last week that requires public schools to teach students — from kindergarteners to high schoolers — about LGBT Americans as a part of U.S. history courses. San Diego State University created California's first LGBT major, to be offered in spring 2012.
Rita Yeung | Daily Trojan
California's new law and SDSU's groundbreaking new major underscore the importance of education in generating progress in LGBT rights. Legislature is necessary for change, but perhaps what this fight for rights really needs is a shift from the courts to the classroom.
There's still much progress to be made. Parents have withdrawn children from school in response to the recently passed law. Same-sex marriage is legal in six states — New York, Massachusetts, Connecticut, Iowa, Vermont and New Hampshire — but not in California. Proposition 8 was overturned last August, but it is currently under stay, which prevents any new same-sex marriages.
When it comes to higher education, LGBT education is complex; and really is the most critical place for the movement to grow.
LGBT education is different at each level of schooling. For elementary school students, educators say it's more appropriate to stick to lessons on family diversity and anti-bullying, rather than sex or LGBT figures' roles in history.
For middle- and high school-age students, sex education becomes more important as it fills in the gaps where the LGBT community has previously been left out in history lessons.
Without LGBT studies there can be no increase in knowledge, or research. Without further research, textbooks or information for younger students to learn about, LGBT issues cannot be improved. And without it, there is a lack of support for the community.
Gender studies exists at many universities, but there's a distinct lack of LGBT-specific education. SDSU is one of only two schools in the nation, along with Hobart and William Smith Colleges in upstate New York, to offer such a major. City College of San Francisco is also waiting for approval to offer an associates degree in LGBT studies.
The creation of such a major is a sign of increasing acceptance and equality for LGBT students.
It's understandable that parents take children out of school because of California's new law — whether for religious or personal reasons — but at the university level, it's different. Students who don't agree with LGBT education are unaffected. They can choose not to participate.
By doing so, however, they would miss out on educational and professional benefits. Non-LGBT students stand to gain from the expansion of LGBT education.
According to a study published by the Stanford School of Medicine in September, American medical schools are falling behind in LGBT-health-related curriculum. The study surveyed deans from medical schools on time colleges spend on LGBT issues and found one-third of the colleges surveyed had zero exposure to LGBT issues in the clinical years.
For current pre-med students, applying to medical school armed with a major or a minor and foundational knowledge of LGBT issues could provide a real edge to fill this educational gap.
Employers are always looking for candidates with not just a diverse educational background, but an understanding of diversity, a critical skill for pretty much any career today.
The increasing attention on LGBT rights also has exciting potential to create entire new fields of study across disciplines: from history and literature to medicine and law.
USC offers a gender studies major and minor as well as an entire LGBT resource center. Why not be a pioneering university and expand USC's resources even further by offering education on LGBT topics?
Elena Kadvany is a senior majoring in Spanish. Her column "Beyond the Classroom" runs Mondays.
Tags: gender studies, lgbt, SDSU, stanford school of medicine
Chick-fil-A protests do more harm than good
This group of Trojans has shot at postseason
LGBT groups push to alter applications
USC to host LGBT Pride and Prep Day
Panel says Greeks, LGBT still at odds
Marky Mark says:
Chinese Student: I am studying physics and calculus.
American Student: I am studying LGBT history and Harvey Milk.
Chinese Student: That's great, now can I have extra fries with my order?
USCLGBT says:
Also, check out a discussion about SB 48: http://sait.usc.edu/lgbt/about/upcoming-events/ally-discussion-sb48-fair-education-act-moving-forward.aspx
Just to mention that the USC medical program does sponsor LGBT health discussions with LGBT leaders from around Los Angeles and it's an opportunity for each class to learn about working with LGBT patients; there also is a transgender educational panel that is frequently sponsored by the medical program. Although there can be more; this is a positive step in the right direction at USC.
Marshall Wilson says:
The Queer and Ally Student Assembly (QuASA) will be holding a discussion which touches upon issues raised in this article. Below is a link with information related to the event.
Ally Discussion: SB48-FAIR Education Act Moving Forward
11/3/2011, 12:00 – 1:00 PM TCC 350/351
http://sait.usc.edu/lgbt/about/upcoming-events/ally-discussion-sb48-fair-education-act-moving-forward.aspx
Rev Kit Tobin says:
Excellent article and in complete agreement that all colleges and universities should at the very least have courses on LGBTQ issues, and preferably majors. There should also be, as in California, state wide mandated age appropriate education in all our public school systems.
The first undergraduate major in LGBT Studies was established at Hobart and William Smith Colleges in Generva NY. Graduates with LGBT Majors have gone on to work in areas as diverse as the Peace Corps and Rochester Institute of Technology. Hobart was founded by Bishop Henry Hobart in 1822, and is still an associate college of the Episcopal Church.
Expansion of LGBT education beneficial | Daily Trojan says:
[…] is a senior majoring in Spanish. Her column "Beyond the Classroom" runs Mondays. Email This ArticleRelated Articles:TagsThis article is tagged: gender studies, lgbt, SDSU, stanford school of […]
Expansion of LGBT education beneficial – Daily Trojan Online | Live Newsline says:
[…] Daily Trojan Online […]
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Option to set subscribers is pretty confusing as it is not sorted properly. It is requred to sort displayed users but also groups of users.
Users are grouped by company, and sorted by name.
In my Feng Office 1.6.2. that is not the case. Companies are random ordered. They are not sorted neither by name nor by creation order.
I could not easily reproduce it, but we'll take a deeper look.
Any more information will be valuable.


text:
Als Bombenanschläge von Berlin wird eine Serie von Sprengstoffanschlägen gegen Verkehrseinrichtungen in Berlin bezeichnet, die 1943 von der Polnischen Heimatarmee verübt wurde. In Stettin und Breslau kam es zu ähnlichen Anschlägen.

Hintergrund
In der Zeit des Nationalsozialismus opponierte der Bund der Polen in Deutschland mit seiner Zentrale in Berlin gegen die nationalsozialistische Gesetzgebung, wirtschaftliche Benachteiligung und individuelle Schikanen, wobei er sich juristischer und publizistischer Mittel bediente. Kurz nach Ausbruch des Zweiten Weltkriegs wurden Führungsgruppen des Bundes sowie anderer polnischer Organisationen verhaftet und in Konzentrationslager verbracht. Das Vermögen der Organisationen wurde eingezogen und jede weitere Aktivität untersagt.

Widerstand gegen den Nationalsozialismus unter den Polen Berlins fand zunächst in Einzelaktionen statt und beschränkte sich auf Kriegsdienstverweigerung, Unterstützung von Fremdarbeitern oder Hilfe für die verfolgten Juden der Stadt. Größere zusammenhängende Aktionen, die von Spionage bis hin zu Attentaten reichten, ergaben sich erst in Zusammenarbeit mit verschiedenen Stellen des Geheimdienstes der Polnischen Heimatarmee. Daneben wurde Propaganda unter Zwangsarbeitern und der deutschen Bevölkerung betrieben.

Im Mai 1942 stellte die Polnische Heimatarmee eine Spezialeinheit für Sabotage und Diversion zur Durchführung von Sonderaktionen auf. Diese Einheit mit dem Codenamen "Zagra-Lin" unterstand der Warschauer Organisation "Osa-Kosa" und bestand aus 18 Personen, die von Hauptmann Bernard Drzyzga (Deckname "Jarosław") kommandiert wurden. Sein Stellvertreter war der aus Bromberg stammende Józef Artur Lewandowski ("Jur"). Sie wurde im Dezember 1942 durch die Hauptabteilung für Sabotage "Kedyw" gegründet mit dem Ziel, Sabotageakte auf dem Gebiet des Deutschen Reiches und der besetzten Gebiete durchzuführen. Die Angehörigen der Gruppe verfügten über eine gute Ausbildung und ausgezeichnete Deutschkenntnisse.

Ein am Umbau des Bahnhofs Friedrichstraße beteiligtes Unternehmen warnte bereits am 18. Januar 1941 den Bahnhofsvorsteher, "dass polnische Arbeiter […] ein Attentat vorhaben." Die Polizei veranlasste daraufhin den Abzug aller polnischer Arbeiter von der Baustelle.

Anschläge der "Zagra-Lin"
In den Abendstunden des 13. Februar 1943 explodierte im unterirdischen S-Bahnhof Friedrichstraße eine Bombe, als dort gerade zwei Züge hielten. Nach Polizeiermittlungen war ein mit Sprengstoff und Metallsplittern gefüllter Pappkoffer unter einer Sitzbank deponiert und gezündet worden. Der Bericht der Gestapo nannte den Sprengkörper eine "Höllenmaschine". Bei dem Anschlag gab es vier Tote und 60 Verletzte.

Am 24. Februar kam es zu einem erneuten Anschlag auf die Berliner S-Bahn, bei dem 36 Menschen starben und 78 verletzt wurden. Am 10. April explodierte eine Bombe im Lehrter Stadtbahnhof, wobei 14 Personen zu Tode kamen; 60 erlitten Verletzungen. Nach diesem Vorfall ordnete Adolf Hitler an, dass sich der Reichsführer SS Heinrich Himmler persönlich der Untersuchung annahm. 10.000 Reichsmark wurden als Belohnung für die Ergreifung von beteiligten Saboteuren ausgesetzt, jedoch konnte keiner der Attentäter festgesetzt werden.

Ein weiterer Anschlag auf den Schlesischen Bahnhof kostete am 10. Mai 1943 das Leben von 14 Betroffenen, 27 wurden hierbei verletzt. Andere Anschläge trafen bereits 1942 und in den folgenden Kriegsjahren unter anderen neben dem Stettiner Nordbahnhof auch den Bahnhof Berlin Alexanderplatz und den U-Bahnhof Berlin Zoologischer Garten. Bei einem ähnlichen Angriff in Breslau starben am 23. April 1943 vier Menschen. Neben den Sprengstoffattentaten sind aus spärlichem Aktenbestand noch Anschläge mit Schusswaffen auf S- und U-Bahn-Züge in Berlin überliefert, deren Urheberschaft jedoch nicht geklärt werden konnte.

Gemäß einer schriftlichen Erklärung der Gruppe "Zagra-Lin" waren ihre Attentate "eine Reaktion auf den deutschen Terror auf polnischem Boden". Die Anschläge wurden kaum bekannt, da die Gestapo die Verletzten noch am Krankenbett sowie die Angehörigen der Getöteten zum Schweigen verpflichtete. Über die Vorkommnisse wurde die strengste Nachrichtensperre verhängt, um die Moral der Bevölkerung nicht zu untergraben. Tatsächlich drangen kaum Informationen an die Öffentlichkeit.

Am 5. Juni 1943 nahm die Gestapo in der Kirche des Heiligen Alexander am Plac Trzech Krzyży in Warschau bei der Trauung eines Mitglieds der "Osa-Kosa" etwa 90 Gäste fest. Obwohl von den Verhaftungen keine Mitglieder der "Zagra-Lin" betroffen waren, löste sich die Einheit jedoch in der Folge auf.

Rezeption
1995 wurde neben dem Eingang zum Hauptbahnhof Breslau eine Gedenktafel für die Kampfgruppe "Zagra-lin" durch eine Initiative des Weltverbandes der Soldaten der Heimatarmee Polens angebracht.

Literatur
 Michael Braun: Nordsüd-S-Bahn Berlin. 75 Jahre Eisenbahn im Untergrund. Berliner S-Bahn Museum (Hrsg.), GVE-Verlag, Berlin 2008. ISBN 978-3-89218-112-5. 288 S.
 Wolfgang Jacobmeyer: Heimat und Exil. Die Anfänge der polnischen Untergrundbewegung im Zweiten Weltkrieg. Göttingen 1973. 369 S.
 Juliusz Pollack: Wywiad, sabotaż, dywersja. Polski ruch oporu w Berlinie 1939–1945. Ludowa Spółdzielnia Wydawnicza, 1991. ISBN 8-32054-345-2. 166 S.
 Aleksander Czerwiński: Dywersja w Berlinie. In: "Komandos", Ausgabe 10, 1996. S. 32–34.

Einzelnachweise

Anmerkungen

Berlin in der Zeit des Nationalsozialismus
Terroristischer Sprengstoffanschlag
S-Bahn Berlin
Polnische Heimatarmee
Deutschland im Zweiten Weltkrieg
Konflikt 1943
Deutsch-polnische Beziehungen
Aktion des Widerstands im Zweiten Weltkrieg

redpajama_set_name: RedPajamaWikipedia


text:
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hmwSite.controllers = angular.module('controllers', []);

hmwSite.controllers.controller('NavbarLinksCtrl', ['$scope', '$http',
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		$http.get('json/navbar-links.json').success(function (data) {

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// angular.module('myApp.controllers', [])
//   .controller('MyCtrl1', [function() {
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//   }])
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//   }]);


text:
Lady Gaga Just Released A New Music Video And It Will Make You Want To Cry
The singer strips it all back. - by Shahbaz Malik
Lady Gaga has well and truly dropped her "Bad Romance" days with her video for latest single, "Million Reasons".
In the new clip, we see her break down in tears in a makeup chair before channelling her inner country girl.
There is even a sweet little moment that highlights the bond she shares with her sister.
ladygaga View Profile
likes - View Post on Instagram
Love you sis ❤
The video serves as a continuation to the first high-energy single, "Perfect Illusion" from her latest album Joanne.
RELATED: Lady Gaga Reveals She Lives With PTSD After Being Raped
Fans have speculated as to whether on not the song is an ode to her ex, Taylor Kinney after recently discussing details of their breakup.
Gaga opened up about the relationship in an emotional interview with CBS, "I think women love very hard," she said. "We love men. We just love with everything we have. And sometimes I don't know that that love is met with the type of dignity that we wish it would be met with".
Watch the touching music video below.


Jake looked up at the king and gave a light smile. " That you." He said before standing and leaving the huge room. Jake let out a heavy sigh as he headed down the endless stairs to the dungen. Jake stopped at the bottem stair hear a scream from what sounded like a child. This ripped his heart out.
Being who he was Jake hated to be down here. And he had only came down three times before. The smell of the dark place made him gag. But he went on down the rest of the steps and looked around. See one of the guards Jake asked them where the girl was and he was lead to the cage like cell where she was being kept. At least she hadn't been here for days, only a few hours.
Jake asked the guard to let the girl out. Letting him know that the king gave the orders. Once the door was open Jake looked at the girl and shook his head. " I'm so sorry." Jake whispered before leading the girl out of the room and up the never ending case of stairs. Once they were to the top Jake lead her out the nearest door. Where Red was waiting. Looking the girl in the eyes Jake shook his head. " I'm so so sorry, I didn't think giving you the money would get you into the kind of mess. How can I repay you for what I have caused you."
This girl didn't need this to happen. What id jake would have found out to late, and she would have been killed. he had no clue what he would do then. To know that he kill some one for what he thought was a good deed. Jake sighed and dropped his eyes to the grassy spot where they stood. He would do anything to help this girl. " Anything you need." Jake said looking back up to her.
He grinned. "Ah, Princess, I fear if I wanted to break that promise it would be off with my head," he teased. He then leaned in and whispered into her ear, "Sweet Princess, I can give you my word as a knight I would never think to break a promise to you."
Tommy let out a soft chuckle. "Oh Princess, you fail to realize every word that escapes your rosy pink lips is important. Besides, when you talk on and on about things it's easy to tell you are a passionate young woman. Passion is important in a lady," he informed her with a nod.
Tommy was glad to know she liked surprises, because Tommy always liked to surprise people. He loved it when a surprise was utterly unexpected and he could see the looks on the face of who he surprised. The joy that flushes through their face is impossible repeat. It only happens once.
"Oh, dear Princess, the training field is not a place suitable for a Princess. I am also quite sure your beauty would catch the eyes of our knights and they would not be able to pay attention," he told her honestly with a chuckle about how the young recruits always eyeballed passing women. Part of the reason people even became knights was to impress ladies and have a better chance at getting the hands of maidens of high rank.
Tommy remembered when he first became a knight. He had admired his older brother, a knight of brave and daring. Once his brother was vanquished in one of many wars Tommy promised to avenge him and take his place as knight. Fortunately, Tommy did a much better job than his brother at fighting.
She was a bit surprised when Jake came back for her, and she decided ultimately he was alright. "No, I'm quite alright, there is nothing I want from you, sorry to be a burden," she said quietly and hurriedly. Now that she was out of that horrid place all of her plans were right back on track. She had to keep away from this knight or she would not be able to go through with her plan as flawlessly as she wanted.
If she befriended the knight he would be pulled into the entire mess. If he got in the way of her plans, he could turn her in and have her arrested. Ally knew if she was going to be able to pull off her scheme she would have to remain under the radar. With all these rumors of her thievery she may be watched a bit more closely and then she would not be able to even pickpocket a noble.
Ally was definitely not going to back down from her plans though. She was not going to stand around and let her father die. Speaking of her father, she needed to hurry home and see how he was doing. She had only been in the dungeon for overnight, so he had to be alright...right? Her doubtful thinking made Ally panic. She had been shaking slightly from the fright of being in the dungeon, but her shaking increased a bit now, fueled by her worry about her father.
"I really need to be going," Ally mumbled, deep in thought about her father and plans to rob the nobles. She was thinking about waiting a little longer to preform the theft so people had forgotten about her arresting. But too much time could prove fatal for her father. He needed that medicine soon; he had been sick for almost 7 months now. The medicine costed 50,000 gold pieces and in two days would have her father doing much better. Ally had saved up 6,482 gold and she knew there was no way she could get the rest of the money in time without stealing. She had worked all she could, sold all she had, done everything she could think of. Without that medicine her father had maybe a week or two left to live.
The fourth day. That was when she would do it. The fourth day of tournaments was the feasting day. It was the middle day of the tournaments and the day of feast and dance. It was the day where the competitors tried to woo whomever they were fighting for. All of the nobles would be at the feast and ball, no one ever missed it. That was when Ally could ransack their houses for the money she needed for her father. She would make the trip to the next town over on horseback to get the medicine for her father. Once he was cured Ally would need to lay low for a while assuming she wasn't caught in action. If she was, then she would need to escape and leave her father to tend to himself. There was no way she would risk him coming with her, he could be framed as an accomplice.
Ally took a step back from Jake, her eyes darting from side to side. She always feared someone would know what she was thinking and what she was planning and arrest her for it. Theft was one of the worst crimes one could commit, especially against a high ranking person.
Claire: "Well, maybe you can put me in one of the armors you men wear? And attract less attention to myself?" giggling slightly I moved my hair from the front-to the back. So it didnt make my skin any itchyer from the strands that happened to brush my skin. "Im sure my father might be mad for wearing one but its just to watch. I get really interested in what the recruits learn and what the teacher teaches." learning what the recruits learn would be a great experience for me. Also it would be a great idea to learn for self defence if needed. Cause sometimes, Dimitri isnt around and is putting up papers around town about the tornaments for my sisters hands, as well as mine. "Dimitri tends to show me some things of what he gets to see. But they are some moves I know already."
Personality: Vivian is over-all quite quiet. She keeps to herself unless she feels the need to speak out to another commener. She is the oldest of her the two siblings, therefore usually managing the family, as her mother finds it easier to sit in a chair all day and watch Vivian work (Well..thats how Viv see's it) You wont see Vivian out at nights, you know.. like hanging with the dukes or other wealthy commoners. She finds it more fun and way less dramatic to be by herself.
Personality: Now with the title of a princess most commoners think, stuck up-spoiled-and sick wealthy. Fraelah's family may be all that but sure isnt. Fraeah has a total wild spirit and a rebel at heart. Her mother always tells her that being a princess comes with responsibilities, things to act mature about. But Fraelah knows this isnt what she wants- its what her mother wants for her. If she could have it her way it would be chaps and her brothers old dress shirt that he grew out of years ago every day. But because its not her way, it goes- corset gown and heels everyday. Oh except when you know, she finds a way out of the ball rehearsals and dinner meetings.
The birds were chirping outside of Frae's window when she sat up and stretch out her arms, yawning at the desire to curl back up in the layers of ruffles sprawled around her queen sized mattress. But her mother was calling for the kitchen down the 3 flights of steps. She groaned and stood up "Coming mother!" She quickly grabbed the dress from her maid and slipped it on refusing the frail womens help.
The dining table seated her mother, father, brother, and one of her sisters. She sat down smiling and nodding at the butler who had politely pulled the chair from under the table. Taking the fork, Fraelah poked at the food taking a couple bites of the eggs and cinnamon bread toast. After picking at the plate she looked up and smiled at her mother "I should be on my way, the garden needs tending to.." Obviousley trying to get out of a conversation she didnt want in to.
She pulled her crimson yellow hood over her head and looked around. The town was filled with commeners selling and trading many objects, from fresh daily kill- to rare and valuable glass objects. For Fraelah the truffle stand was her favorite, as for when she was a child her father would take her and her older brother out and buy them each a piece of the carmel covered chocolate morsels. Fraelah found the town to be a quite delightful place to hang around, and the town was where she spent most of her time when she could slip away from being in the kingdoms castle.
Carrying a small woven basket she followed on the edge of the stands catching the objects in her sights. She was careful to keep her head down and the hood on. If a guard were to find her she would be dragged back to her mother, where she would then be scolded with her mothers words "The town is no place for a princess! There is so much for you to do around here--" and it went on. Fraeh ducked under a string of flowers and quickly paced over to the fountain where most town dancing and singing was held. There was only a band of three violin players with a hat placed out in front of them for coins. She dropped some silver into the hats pocket smiling and heading on her way. Even though she didnt really know where she was going, Frae new anywhere was better then the castle, where she would find herself under her mothers commands knitting or weaving on the spin-wheel.
He let out another chuckle at her insistancy. Tommy wasn't quite sure it would be alright to bring such a lady out into the barbaric ways of war. He had always admired the innocence in women and their fragility, providing him with a good reason to be near; protection. He paused to ponder for a moment. She did seem quite set on coming into the field, yet for him to put her directly in the face of danger was absurd. It was not unheard of for recruits to be injured or even killed in training accidents; a reason for the training field being several miles from Alevania. It took about twenty minutes to reach it by horseback.
"Well, my sweet Princess, you do seem quite firm on your stance of accompanying me to the field, but I too remain firmly against your wishes, I beg your parden. You must understand training grounds are no safe place to be. I do believe you are best off remaining away from evil such as that of war and fighting," he explained to her. She was so beautiful that even if a single strand of her hair were to be cut short the deepest sadness inside Sir Thomas would be awakened.
"I do hope you consider my opinion but I cannot deny you the right to visit the grounds. I could always explain the way I train recruits if you truly are so interested," he offered as a sort of compromise. Tommy gazed deep into her eyes, perhaps even into her soul. His lips parted and he spoke without thinking.
"The way your eyes shine in the light is spectacular," he spoke, almost a whisper. A light blush coated his cheeks as his eyes flicked to the ground with embarrassment. Tommy looked back to the Princess and spoke again, returning to the previous subject.
"Of course if you seek a fight you can find me training each and every night just past the orchard field. I shall be on horseback practicing my javelin for the tournament for your hand," he announced proudly. By saying this it meant that Tommy knew his paperwork would be approved and he would be set to fight in the tournament. Normally when tournaments were hosted the ladies were housed in a tent covered on all sides as not to witness horrors of fighting; though there would always be some exceptions. The front of the tent would be lifted to reveal the victor to the ladies and then dropped back down while the tournament progressed. The tent would be lifted in the less voilent chalanges such as horse riding and javelin throwing.
Claire: I nodded listening to him go on about how dangerous it would be for me..he had a point. I nodded once again "Alright, it would be nice if you could explain to me,thank you." a smile spreaded on my lips and it began to grow due to his beautiful comment, I lifted my hand and felt hit hot face. Aww, he was blushing, now that was a real man for you! "Oh, alrighty then. I shall appreciate your jousting for my hand." I felt so small compared to him, oh boy, I wonder how it would work out. "Well.. I shouldnt keep you from your duties. By the time you get back here, I should be up in my room, you are more then welcome to go inside, but be sure to knock." I giggled softly "I know you will, you are just tht kind of a man. Thats what I look for."


Diurnal instability and moist southerly flow ahead of a front will result in afternoon thunderstorms today. A front will cross the region early Saturday followed by upper ridging Sunday and Monday. Another frontal system will move across the region early part of next week.


text:
Mount Afton är ett berg i Kanada.   Det ligger i provinsen British Columbia, i den centrala delen av landet,  km väster om huvudstaden Ottawa. Toppen på Mount Afton är  meter över havet.

Terrängen runt Mount Afton är bergig. Den högsta punkten i närheten är  meter över havet,  km söder om Mount Afton. Trakten runt Mount Afton är nära nog obefolkad, med mindre än två invånare per kvadratkilometer..

Trakten runt Mount Afton består i huvudsak av gräsmarker.  Trakten ingår i den hemiboreala klimatzonen. Årsmedeltemperaturen i trakten är  °C. Den varmaste månaden är augusti, då medeltemperaturen är  °C, och den kallaste är februari, med  °C.

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Berg i British Columbia
Berg i Kanada 1000 meter över havet eller högre