text:
\section{INTRODUCTION} \label{sec:intro}

The Abell cluster A4059 is compact and
dominated by a central cD galaxy ESO~349-G010.
The cluster is classified as richness~1
and is at a redshift of 0.0487
(Abell, Corwin, \& Olowin 1989;
Green, Godwin, \& Peach 1990, hereafter GGP;
Schwartz et al.\ 1991).
The cluster is not well studied in optical.
Of the 284 galaxies which have been identified as candidates
for membership in the cluster,
only 11 galaxies have known redshifts
(Green et al.\ 1988, 1990).
The redshift of the cD galaxy appears to be
consistent with the cluster mean velocity
within the measurement errors (Green et al.\ 1990),
which may indicate that the cluster has achieved a
somewhat relaxed state.

The central cD galaxy hosts the radio galaxy PKS2354-35,
with a total radio power of
$1.5\times10^{42}$ ergs s$^{-1}$
(Schwartz et al.\ 1991; Taylor et al.\ 1994).
A VLA A-array observation at 8.4 GHz (Taylor et al.\ 1994)
showed that the radio galaxy has a double-lobe structure
extending along the major axis of the host galaxy.
The alignment of the radio structure, cD major axis,
and the overall cluster elongation is an intriguing
feature, which may help us understand the formation
and evolution of cD galaxies and the radio sources
associated with these galaxies (West 1994).

Observations with $HEAO~1$ and {\it EXOSAT}
(Edge \& Stewart 1991;
Schwartz et al.\ 1991;
Edge, Stewart, \& Fabian 1992)
have established that the cluster is a bright X-ray source with
strong cooling flow around the central cD galaxy.
Recent {\it ASCA} observation also revealed a possible chemical
abundance gradient around the central cD galaxy
(Ohashi 1995).
A similar feature has been seen in a few other clusters,
such as the Centaurus, AWM7 (Ohashi 1995),
and Virgo clusters (Matsumoto 1994).

Excess soft X-ray absorption has been seen in the
X-ray spectra of the central regions in a number of
cooling flow clusters of galaxies.
A4059 is near the southern galactic pole
(galactic latitude of $-75.9^{\circ}$)
with a low galactic neutral hydrogen column density of
$1.45\times10^{20}$ cm$^{-3}$
(Stark et al.\ 1992).
This makes A4059 a good case for studying
intrinsic X-ray absorptions.

In this paper, we will first analyze the
spatial properties of the global X-ray emission of the cluster
(\S~\ref{sec:spatial}).
We then investigate the X-ray spectral properties of the gas,
such as the gas temperature distribution
and the intrinsic absorption in the center of the cluster,
using ROSAT PSPC archival data (\S~\ref{sec:spectral}).
The detailed X-ray structure near the cD galaxy will be
compared to the radio emission from the cD galaxy in
\S~\ref{sec:central}.
Finally, we summarize the main results
(\S~\ref{sec:summary}).
Throughout the paper, we have assumed
a Hubble constant of 50 km s$^{-1}$ Mpc$^{-1}$ and $q_0$ = 0.5.

\section{OBSERVATIONS AND DATA REDUCTION} \label{sec:observ}

The cluster A4059 was observed with the ROSAT HRI
(High Resolution Imager) on 6 October, 1993,
for 6263 seconds in four observation intervals (OBIs).
The observation was centered at the cD galaxy PKS2354-35.
The data reduction was done using the standard PROS package.
The data was first examined for periods of high background,
and about 140 seconds was removed.
Vignetting and background corrections were applied.
A4059 has a relatively small angular size
(see Fig.~\ref{fig:xray_galaxies};
Green et al.\ 1990).
The X-ray emission from the cluster is well confined within
the ROSAT HRI FOV ($\sim 40'$ in diameter).
Thus, we can determine the X-ray emission background from
within the HRI field;
the background region is chosen to be an annulus
centered at the cD galaxy PKS2354-35
with the inner and outer radii being 700$''$ to 900$''$,
respectively.

\begin{figure*}[htb]
\vskip3.8truein
\special{psfile=fig1.ps angle=0 voffset=-100
        hoffset=60 hscale=60 vscale=60}
\caption{
A contour map of the ROSAT HRI image of Abell~4059
superposed on an optical map from the Digitized Sky Survey.
The X-ray image was adaptively smoothed with a signal-to-noise
ratio of 5, and was corrected for background, vignetting, and exposure.
The X-ray contour levels are:
(0.000926, 0.00155, 0.00256, 0.00426, 0.00706, 0.0117, 0.0194, 0.0322,
 0.0534, 0.0886)
cnts arcmin$^{-2}$ s$^{-1}$.}
\label{fig:xray_dss_whole}
\end{figure*}

In order to provide spectral information to complement the
HRI spatial data, we retrieved the ROSAT PSPC observation of A4059.
The cluster was observed for 5514 seconds on 21-22 November, 1991
(observation WP800175; PI: R. Schwarz).
We first removed periods of high background from this data
(Master Veto rate $MV > 170$).
This resulted in a rejection of 107 seconds of exposure time.
The spectral fitting of the data was done using the XSPEC package.

The pointing accuracy of the ROSAT HRI is important
to our discussion of the central X-ray and radio structures
in the cluster (\S~\ref{sec:central_radio}).
Unfortunately, there are no ideal X-ray reference sources
with accurate optical or radio positions in the HRI field
to calibrate the X-ray pointing accuracy.
The SB galaxy, ESO 349-G009
(about $5'$ to the north of the cD galaxy)
may be associated with an X-ray source,
but the X-ray emission is extended,
which makes the position measurement of the X-ray source and the
correct optical correspondence uncertain.
There are several other galaxies
to the southeast of the cD galaxy
(Fig.~\ref{fig:xray_galaxies})
which may also have X-ray emission,
but these X-ray sources are too weak for their positions
to be determined accurately.
Thus, we rely on the absolute positions provided by the aspect
solution of the star camera on ROSAT.
Based on previous experience,
the HRI X-ray images presented in this paper could have
an absolute position error of up to about $10''$.
We discuss the relative alignment of the optical, radio, and
X-ray images in more detail in \S~\ref{sec:central_xray}.

\begin{figure*}[htb]
\vskip4.0truein
\special{psfile=fig2.ps angle=0 voffset=-100
        hoffset=+45 hscale=60 vscale=60}
\caption{
A contour map of the ROSAT HRI emission of Abell~4059
superposed on a grey scale map of the smoothed galaxy $b$-band
optical surface brightness distribution.
The X-ray contour levels are the same as those in
Figure~\protect\ref{fig:xray_dss_whole}.
The grey scale of the galaxy optical surface brightness
is logarithmically spaced,
with the lowest and highest levels at
$6.85\times10^{-10}$ and $1.24\times10^{-7}$
ergs cm$^{-2}$ s$^{-1}$ arcmin$^{-2}$, respectively.}
\label{fig:xray_galaxies}
\end{figure*}

\section{GLOBAL X-RAY SPATIAL ANALYSIS} \label{sec:spatial}

\subsection{Global X-Ray Structure} \label{sec:global_struct}

As reported by {\it EXOSAT} (Schwartz et al.\ 1991)
and {\it ASCA} (Ohashi 1995),
the X-ray emission from the cluster is concentrated near
the cD galaxy, PKS2354-35.
Figure~\ref{fig:xray_dss_whole} shows the ROSAT HRI image
of the entire cluster superposed on an optical image
from the Digitized Sky Survey.
The X-ray image was corrected for background and vignetting,
and was adaptively smoothed with a signal-to-noise ratio of 5
per smoothing beam using our
adaptive kernel image smoothing routine
(AKIS; Huang \& Sarazin 1996).

To better compare the global X-ray and optical properties of the cluster,
we also produced a smoothed galaxy optical surface brightness image
of the cluster, which is shown superposed on the contours
of the X-ray emission in Figure~\ref{fig:xray_galaxies}.
In the smoothed optical surface brightness image, each galaxy was
weighted by its $b$-band optical luminosity, and
the image was then adaptively smoothed with at least 25 average
galaxy luminosities per smoothing beam.
The galaxy positions and luminosities are from GGP.
We note that of the total of 284 galaxies listed as cluster members
by GGP, only 11 galaxies have the measured redshifts.
Therefore, some of the galaxies in the GGP sample
may be nonmember galaxies seen in projection against the cluster.

Although the large scale X-ray image of A4059 is elongated with
NNW to SSE, there also is some evidence for a concentration in the
emission directly north of the central cD galaxy PKS2354-35.
In Figure~\ref{fig:xray_dss_whole}, this secondary peak appears
in the general direction of the SB galaxy ESO 349-G009.
With a blue magnitude of 14.6 (GGP),
this is the second brightest galaxy in the cluster.
In the HRI image, there is a broad peak in this region.
The feature is stronger in the ROSAT PSPC image, but the
X-ray centroid lies about $30''$ to the south of the galaxy.
ESO~349-G009 was classified by Buta (1995) as a ring-type
galaxy, which may indicate an interaction with another galaxy and/or
strong star formation.
In fact, the galaxy is a powerful IRAS source (IRAS~23544-3457)
with a luminosity from 40 to 120 $\mu$m of
$7.5\times10^{10}$ L$_{\odot}$
(IRAS Point Source Catalog 1988).
The galaxy is also a radio source
with a flux density of $10.8\pm0.2$ mJy
at the 1.4 GHz band from the NVSS
(Condon et al.\ 1993),
which corresponds to $8.41 \times 10^{22}$ W Hz$^{-1}$
at the galaxy redshift ($z = 0.04207$).
The infrared and radio fluxes are consistent with the general correlation
found for starburst galaxies
(Condon 1992).
If ESO 349-G009 is the source of the extra X-ray emission to the north
of the cluster center, then its X-ray luminosity is approximately
$10^{42}$ ergs s$^{-1}$.
All of these properties are consistent with a strong starburst in
ESO 349-G009.
This galaxy may be similar to NGC~6045 in the Hercules cluster
(Huang \& Sarazin 1996).
This may indicate that there exist a class of spiral galaxies
in galaxy clusters
which are currently undergoing strong star formation at a rate
$\sim$10 times that of M~82.

Alternatively, Figure~\ref{fig:xray_galaxies} suggests that there is
a peak in the galaxy distribution to the north of the cluster center.
Because the grey scale image in this Figure gives the optical surface
brightness, part of this peak is due to ESO 349-G009.
However, there may be a subcluster in this region, which provides the
extra X-ray emission.

Figures~\ref{fig:xray_dss_whole} and \ref{fig:xray_galaxies}
show that the global X-ray emission
is elliptical and elongated along the major axis of the
galaxy luminosity distribution.
The major axis of the cD galaxy is also
aligned in the same general direction.

To quantify elongation of the cluster,
we have used the ellipse fitting routine in STSDAS
(Jedrzejewski 1987)
to fit elliptical isophotes to the X-ray emission, to the
cD galaxy optical surface brightness, and to the cluster
galaxy optical luminosity distribution.
The position angles ($PA$) and ellipticities are shown in
Figures~\ref{fig:ellipse_pa}
and \ref{fig:ellipse_e}.
The $PA$ is measured counter-clock-wise from the north.
The optical image of the cD is from the Digitized Sky Survey.
Figure~\ref{fig:ellipse_pa} shows that
the major axis of the cD galaxy is in
$PA \approx 160^{\circ}$.
In the outer regions ($r \ga 50''$), the X-ray emission seems to have
the same orientation as the cD within the fitting errors.
A similar result was found from a wavelet analysis
of the ROSAT PSPC image (Slezak et al.\ 1994).
The outer X-ray orientation also agrees reasonably well with that
of the smooth galaxy optical surface brightness, and the X-ray
surface brightness and galaxy distribution give similar values for
the ellipticity, as well.
The galaxy distribution is at a slightly smaller position angle
than either the X-ray emission or cD galaxy (at smaller radii).
Our result for the orientation of the galaxy distribution
are consistent with those of GGP.

\begin{figure*}[htb]
\vskip3.5truein
\special{psfile=fig3.ps angle=0 voffset=-210
        hoffset=+50 hscale=60 vscale=60}
\caption{
The position angles ($PA$) from elliptical fits to the X-ray surface
brightness, optical surface brightness of the cD galaxy PKS2354-35,
and the cluster galaxy optical surface brightness as a function of the
semimajor axis.
$PA$ is measured counter-clockwise from the north.
The rapid change in the orientation of the X-ray emission at 40$''$
is due to the X-ray bar structure at smaller radii.}
\label{fig:ellipse_pa}

\vskip3.5truein
\special{psfile=fig4.ps angle=0 voffset=-210
        hoffset=+50 hscale=60 vscale=60}
\caption{
The ellipticity of the X-ray emission, optical surface brightness of
the cD galaxy PKS2354-35, and the cluster galaxy luminosity distribution
as a function of the semimajor axis for elliptical fits.
The ellipticity is defined as $1-b/a$,
where $a$ and $b$ are the semimajor and semiminor axes of the ellipse,
respectively.}
\label{fig:ellipse_e}
\end{figure*}

However, in the inner part ($r \la 50''$) of the X-ray image,
the elongation of the X-ray surface brightness is
is rotated by about 90 degrees with respect to the major axis of
the cD galaxy.
The X-ray image is also significantly more elliptical in the innermost
regions.
The sudden change in the $PA$ is
due to the X-ray bar structure in the central area.
We will discuss this feature in detail in \S~\ref{sec:central}.

\subsection{X-ray Surface Brightness and Gas Density Profiles}
\label{sec:spatial_profile}

To derive the X-ray surface brightness profile,
the X-ray emission was accumulated in circular annuli.
Tests have shown that the results for circular annuli are
consistent with the results for elliptical annuli
for moderate values of the ellipticity
(White et al.\ 1994).
The X-ray counts in these bins were corrected for vignetting,
exposure, and background.
The count rate was then converted into a physical flux in
the ROSAT X-ray band $0.1-2.4$ keV,
assuming a Raymond-Smith thermal spectrum
with a temperature of 3.43 keV
(\S~\ref{sec:spectral_temp}),
the total (galactic and intrinsic) absorption column density
$N_H = 1.40\times10^{20}$ cm$^{-2}$
(\S~\ref{sec:spectral_cool}),
and the abundances from the {\it ASCA} spectrum
(Ohashi 1995).

The azimuthally averaged X-ray surface brightness profile
is plotted in Figure~\ref{fig:xray_surf_whole}
(upper curve).
The errors for each data point follow
directly from Poisson counting statistics including the
background subtraction.
 From the X-ray surface brightness,
one can derive the electron density distribution
by de-projection (Fabian et al.\ 1981).
Spherical symmetry was assumed,
and the same thermal spectrum was adopted as used in the conversion to
the physical flux.
The resulting electron density profile is shown as the lower set of
filled squares in Figure~\ref{fig:xray_surf_whole}.
The errors on the electron density are 68\% confidence ranges
derived from Monte Carlo simulations of 100 statistical realizations
of the data.

\begin{figure*}[htb]
\vskip4truein
\special{psfile=fig5.ps angle=-0 voffset=-170
        hoffset=+60 hscale=60 vscale=60}
\caption{
The ROSAT HRI X-ray surface brightness and de-projected electron
density for A4059.
The upper data (open circles) give the X-ray surface brightness in
the photon energy band 0.1$-$2.4 keV
(vertical scale on the left).
The solid curve is the best-fit $\beta$-model
for the surface brightness with all 23 data points,
while the dotted line is the fit with the first 4 data points removed.
Both fits show that these is an excess X-ray emission
in the center of the cluster.
The lower data points (filled squares)
are the de-projected electron density distribution
(scale on the right).
The error bars show the 1-$\sigma$ errors for the surface brightness
or the electron density.
For the X-ray surface brightness,
the errors are derived directly from Poisson counting statistics;
the errors for the electron density are from 100 Monte Carlo
simulations.}
\label{fig:xray_surf_whole}
\end{figure*}

In Figure~\ref{fig:xray_surf_whole},
the X-ray surface brightness is strongly peaked
toward the center of the cluster.
We tried to fit the data using the
conventional isothermal $\beta$-model,
$I_X (r) = I_0 \ [1 + ( r / r_X )^2]^{-3\beta + 1/2}$.
Here, $I_0$ is the central surface brightness,
$r$ is the projected radius,
and $r_X$ is the core radius of the X-ray emission.
The model was convolved with the Point Response Function (PRF)
of the ROSAT HRI.
The best $\chi^2$ fit for all 23 data points
gave $\beta = 0.55^{+0.03}_{-0.03}$
and $r_X = 66^{+10}_{-9}$ kpc
(uncertainties are 90\% confidence limits for
one interesting parameter).
The value of $\chi^2$ was 27.8 for 20 degrees of freedom (d.o.f.),
which is not an acceptable fit.
The model surface brightness (solid line) is plotted in
Figure~\ref{fig:xray_surf_whole}.
Clearly, there is a central excess of X-ray emission
compared to the model for the first four data points.
To test the significance of this excess,
we removed the four innermost data points
from the fit.
The resultant $\chi^2$ value was significantly reduced
by 17.5 to 10.3 for 16 d.o.f.,
which is a dramatic reduction for the removal of four data points.
The improved fit, which gives
$\beta = 0.58^{+0.03}_{-0.04}$ and
$r_X = 77^{+11}_{-12}$ kpc (90\% confidence level),
is plotted as the dotted line in Figure~\ref{fig:xray_surf_whole}.
Ohashi (1995) fitted a $\beta$-model
to his {\it ASCA} data on the X-ray
surface brightness, and found larger values of
$\beta$ (0.65) and $r_X$ (100$''$).
The difference may be due in part to the larger PRF
or harder spectral band of {\it ASCA}.

\subsection{Cooling Flow} \label{sec:global_cflow}

The excess central X-ray surface brightness suggests that A4059
has a cooling flow, as was previously found by
Schwartz et al.\ (1991) and
Edge et al.\ (1992).
We find that the average electron density
within the central $4''$ is
$n_e \approx 0.046\pm0.035$ cm$^{-3}$,
which implies that the gas cooling time for this region is about
$3.1^{+17.2}_{-1.8} \times 10^8$ years
at a temperature of $1.93^{+0.76}_{-0.33}$ keV
(90\% confidence level).

 From the electron density profile, we find that the
cooling radius, defined as the point where the cooling time
equals $10^{10}$ yr, is
$r_c = 120^{+14}_{-9}$ arcsec = $156^{+18}_{-12}$ kpc
(90\% confidence level).
The total cooling rate within this radius is
$\dot{M} = 184^{+22}_{-25}$ $M_{\odot}$ yr$^{-1}$
(90\% confidence level).
This cooling rate is intermediate between the value of
$\dot{M} = 124^{+53}_{-44} \ M_{\odot}$ yr$^{-1}$
from Edge et al.\ (1992) and the estimate of
320 $M_{\odot}$ yr$^{-1}$ by Schwartz et al.\ (1991),
both based on {\it EXOSAT} data.

\section{SPECTRAL ANALYSIS OF THE X-RAY EMISSION} \label{sec:spectral}

\subsection{ Gas Temperature Distribution }
\label{sec:spectral_temp}

We used the ROSAT PSPC observation of A4059 from the archive
(see \S~\ref{sec:observ}) to determine the (projected) X-ray
spectra in circular annuli centered on the cD galaxy PKS2354-35.
The results of the spectral fitting are summarized in
Table~\ref{tab:spectral}.
Because of the limited spatial resolution of the ROSAT PSPC,
the width of each annular bin was set at least 1 arcmin.
The radii are given in the first row of
Table~\ref{tab:spectral}.
For outer bins, the width was increased so that each bin had
enough ($>$ 1000) net photons in the spectral fitting.
The spectra were corrected for particle and X-ray background;
the average Master Veto rate was $MV = 79.88$.
The number of net photons in the spectrum after background subtraction
are listed in the second row of Table~\ref{tab:spectral}.
The spectra were limited to the energy channels
from 0.2 to 2.04 keV.

\begin{table*}[ht]
\caption[Spectral Fits of the ROSAT PSPC Archive of A4059]{}
\label{tab:spectral}
\begin{center}
\begin{tabular}{lcccccc}
\multicolumn{7}{c}{\sc ROSAT PSPC Spectral Fits} \cr
\tableline
\tableline
Radius ($''$)     &  0 -- 60 & 60 -- 120 & 120 -- 180 & 180 -- 260
                  &   260 -- 410 & 410 -- 800                        \cr
Net Photons       & 1914 & 2283 & 1628 & 1460 & 1707 & 1531          \cr
Abundance         & 0.63 & 0.56 & 0.53 & 0.49 & 0.43 & 0.29          \cr
Temperature (keV) & 1.93$^{+0.76}_{-0.33}$ & 2.93$^{+1.32}_{-0.73}$
                  & 4.64$^{+3.16}_{-1.64}$ & 2.76$^{+1.75}_{-0.89}$
                  & $> 3.03$ & $> 2.60$                              \cr
$\chi^2$/d.o.f.   & 51.5/67 & 80.9/77 & 54.4/60 & 55.5/54 & 62.8/62
                  & 65.8/56                                          \cr
\tableline
\end{tabular}
\end{center}
\end{table*}

A Raymond-Smith thermal spectrum was assumed
with a Galactic neutral hydrogen column density of
$N_H = 1.28^{+0.18}_{-0.20}\times10^{20}$ cm$^{-2}$
(90\% confidence level; see \S~\ref{sec:spectral_cool}).
Because the ROSAT PSPC data did not provide strong constraints
on the abundances in the gas, we have fixed the
abundances at different radii to values interpolated from the
{\it ASCA} measurements (Ohashi 1995).
These abundance values are listed in the third row of
Table~\ref{tab:spectral}.
The best-fit temperature values are given in row 4 of the Table;
the upper and lower limits of the gas temperatures
are at the 90\% confidence level.
Because of the large fitting errors,
only lower limits are given for temperatures in bin 5 and 6.
The last row in the Table gives the total $\chi^2$ value
for the fit and the number of degrees of freedom
for each annular bin.

\begin{figure*}[htb]
\vskip3.5truein
\special{psfile=fig6.ps angle=-0 voffset=-200
        hoffset=+60 hscale=60 vscale=60}
\caption{
The azimuthally averaged temperature distribution for the X-ray gas
in A4059.
The temperatures are derived from the ROSAT PSPC data
assuming Raymond-Smith thermal spectrum for the X-ray gas
(Table~\protect\ref{tab:spectral}).
The dotted line is the best single temperature fit
for the entire cluster (3.43 keV).
The errors give the 90\% confidence intervals for the
temperatures.}
\label{fig:pspc_temperature}
\end{figure*}

The temperature distribution of the gas is plotted
in Figure~\ref{fig:pspc_temperature}.
Also plotted in the Figure is the result (dotted line)
of a single temperature fit of the entire cluster
within a radius of 800$''$.
This single temperature fit gives a
total $\chi^2$ of 175.3 for 162 degrees of freedom.
It gives the gas temperature and metal abundance of
$3.43^{+1.06}_{-0.73}$ keV and
$0.28^{+0.32}_{-0.24}$ solar (90\% confidence), respectively.
It also gives the best fit value for the absorption column of
$N_H = 1.40^{+0.20}_{-0.20}\times10^{20}$ cm$^{-2}$,
which is consistent with the value from Stark et al.\ (1992).
This result is in agreement with
the results from other instruments:
$3.7^{+0.7}_{-0.7}$ keV (1~$\sigma$ confidence;
$EXOSAT$; Schwartz et al.\ 1991;  Edge \& Stewart 1991),
$3.5^{+0.3}_{-0.4}$ keV
(1~$\sigma$ confidence; $Einstein$; David et al.\ 1993),
and 3.9 keV ({\it ASCA}; Ohashi 1995).

Figure~\ref{fig:pspc_temperature} shows that,
except the central annular bin,
the single temperature fit is a fairly good representation of the
gas temperature distribution in the cluster.
The central bin seems to suggest a gas temperature drop in the
center of the cluster.
To test this hypothesis, we have divided the entire cluster
into two sets of spectral data:
the central bin and the rest of the cluster.
We then fit the two spectra simultaneously, either
requiring that the temperature of the central bin equal that of
the rest of the cluster, or allowing the central bin to have a
different temperature.
Allowing the central bin to have a separate temperature
resulted in a reduction of the total $\chi^2$ value by 7.9
(from 218.3 to 210.4)
with the decrease of 1 degree of freedom
(from 222 to 221).
 From the $F$-test, the hypothesis that the central temperature
is the same as that of the rest of the cluster can be rejected at the
95\% probability level.

\subsection{Gas Cooling and Intrinsic X-ray Absorption}
\label{sec:spectral_cool}

The spatial analysis of the ROSAT HRI X-ray surface brightness
requires that there be a cooling flow in the central region of A4059
(\S~\ref{sec:spatial}).
The reduction in the central temperature is also consistent with this
(see \S~\ref{sec:spectral_temp}, Figure~\ref{fig:pspc_temperature},
and the preliminary ASCA result by Ohashi [1995]).
However, the ROSAT PSPC spectra do not require any significant
cooling flow component.
For example, within $r < 150''$
(slightly larger than the cooling radius; \S~\ref{sec:spatial}),
a single temperature Raymond-Smith thermal model
gives a reasonably good fit to the spectra:
total $\chi^2$ of 145.6 for 135 degrees of freedom.
The addition of the cooling flow component
to the above model does not improve the fit.
The maximum cooling rate within this radius is
$\dot{M} < 29 \, M_{\odot}$ yr$^{-1}$ at the 90\% confidence level.
For the PSPC spectra of the entire cluster
($ r < 800''$),
the addition of a cooling flow component does not
improve the corresponding single temperature model fit either.
At 90\% confidence level, the cooling rate
is $\dot{M} < 80$ $M_{\odot}$ yr$^{-1}$
with a fitted absorption column density of
$N_H = 1.39^{+0.11}_{-0.13}\times10^{20}$ cm$^{-2}$.
This strong upper limit on the cooling rate is clearly
inconsistent with the result from the spatial data analysis.

One explanation for this inconsistency between the
X-ray surface brightness profile and the X-ray spectrum of
the central region of the cluster
would be if the cooling flow had only begun recently.
In \S~\ref{sec:global_cflow},
we determined the gas cooling time at the center of the cluster.
Because of the large errors in the electron density,
the cooling time of the central gas could be as large as
$2.0 \times 10^9$ years.
This is comparable to the gas relaxation time following
a subcluster merger (Roettiger, Burns, \& Loken 1993).
Thus, if this cluster recently underwent a merger which disrupted any
pre-existing cooling flow, it is possible that cooling of the central gas
might have only begun within the last $\la$2 Gyr.
Then, very little gas may have actually cooled down to low
temperatures ($k T \la 10^7$ K).
On the other hand, A4059 now appears to be a quite relaxed cluster.
The X-ray image is quite regular on large scales
(Fig.~\ref{fig:xray_dss_whole}; Buote \& Tsai 1996),
although Slezak et al.\ (1994) has suggested that there is some evidence
for substructure based on a wavelet analysis of the ROSAT PSPC image.

The spectral fitting also shows
there is very little (if any)
intrinsic, excess soft X-ray absorption toward the center of the cluster.
If we adopt the Galactic neutral hydrogen column density of
$N_H = 1.45\times10^{20}$ cm$^{-2}$
(Stark et al.\ 1992),
the limit on the intrinsic absorption in the center of the cluster
($r \le 60''$)
is
$\Delta N_H < 0.14\times10^{20}$ cm$^{-2}$
at the 90\% confidence level.
Alternatively, we can use the spectrum of the outer cluster
($r = 125'' - 800''$)
to fix the Galactic absorption,
and determine the excess absorption in the center.
The best-fit model gives central excess absorption
$\Delta N_H = 0.088\times10^{20}$ cm$^{-2}$
with a total $\chi^2$/d.o.f. = 192.1/207.
At 90\% confidence level, the central excess intrinsic absorption
has only an upper limit of
$\Delta N_H < 0.40\times10^{20}$ cm$^{-2}$.
This upper limit for A4059 is rather low when compared to
X-ray spectral fits of some other cooling flows clusters
(White et al.\ 1991; Allen et al.\ 1995).
However, this limit only applies to excess absorption which is
in front of the cluster emission.

\section{CENTRAL STRUCTURE OF THE X-RAY AND RADIO EMISSION}
\label{sec:central}

\subsection{Central X-ray Structure} \label{sec:central_xray}

In the center of the cluster, the X-ray emission is
strongly peaked towards the cD galaxy PKS2354-35.
Figure~\ref{fig:xray_central_opt} shows the contours of the
X-ray emission within the central 6$'$
superposed on the corresponding optical field
from the Digitized Sky Survey.
The X-ray emission was adaptively smoothed
with a signal-to-noise ratio of 5 per smoothing beam.
As discussed in \S~\ref{sec:global_struct},
the X-ray emission is elongated in the same direction
as the cD on the scales of $r \ga 50''$.
However, on smaller scales ($r \la 50''$), the X-ray
emission is concentrated to an elongated X-ray bar,
which is nearly perpendicularly to the major axis of the cD.
The centermost part of the X-ray image is shown in grey scale in
Figure~\ref{fig:xray_central_radio},
superposed on the 4.8 GHz radio contour map
(Taylor et al.\ 1994).
The radio source will be discussed in the next section
\S~\ref{sec:central_radio}.
As discussed in \S~\ref{sec:observ},
we have adopted the absolute positions from the aspect solution
for the HRI X-ray data.
The agreement of the radio and optical nucleus with a central position
along the X-ray bar suggests that the X-ray positions are not completely
wrong.
However, the brightest part of the bar extends for about 15$''$, so
this is not a very strong constraint on the accuracy of the X-ray
positions.

\begin{figure*}[htb]
\vskip4truein
\special{psfile=fig7.ps angle=0 voffset=-90
        hoffset=+40 hscale=60 vscale=60}
\caption{
The central structure of the ROSAT HRI X-ray emission in A4059.
The X-ray contours are superposed on the optical image from
the Digitized Sky Survey.
The X-ray image was adaptively smoothed
to a signal-to-noise ratio of 5 per smoothing beam.
The X-ray contour levels are:
(0.0108, 0.0148, 0.0202, 0.0275, 0.0374, 0.0510, 0.0694, 0.0946, 0.129)
cnts arcmin$^{-2}$ s$^{-1}$.
Two features about 1/2 arcmin to the southeast and northwest
of the center of the radio galaxy are actually holes rather
than peaks (see Figure~\protect\ref{fig:xray_central_radio} below).}
\label{fig:xray_central_opt}
\end{figure*}

Figure~\ref{fig:xray_central_radio} also shows
two X-ray emission minima (``X-ray holes'')
above and below the X-ray bar.
Are the two X-ray holes statistically significant?
First, we compare the X-ray surface brightness
in the two X-ray holes with the average surface brightness
at the same radius.
The two X-ray holes are defined as two elliptical regions
with semimajor and semiminor axes of $13''$ and $10''$,
centered at
R.A.\ = $23^{\rm h}57^{\rm m}02{\fs}8$,
Dec.\ = $-34^{\circ}46^{\prime}02{\farcs}5$,
and
R.A.\ = $23^{\rm h}56^{\rm m}59{\fs}7$,
Dec.\ = $-34^{\circ}45^{\prime}02{\farcs}0$
A total of 15 and 12 photons were detected in the
northern and southern holes, respectively.
Based on the counts in an annulus between $24''$ and $50''$,
we expect $29.7 \pm 1.4$ counts in each X-ray hole.
Thus, the Poisson probabilities that the number of photons
in each X-ray hole
could be equal or less than 15 and 12 are about
0.23\% and 0.019\%, respectively.

Alternatively, we can verify the statistical significance
level of the two X-ray holes by
performing the Poisson simulations of the central X-ray image
based on the ellipse fitting model (\S~\ref{sec:spatial}).
Out of 1000 statistical realizations of the image,
we found three instances in that the simulated X-ray count
in the northern X-ray hole was less than or equal to 15, and
no cases where the simulated X-ray count in either hole was
less than or equal to 12.
These tests suggest that the two X-ray holes are real,
and are unlikely to be the results of statistical fluctuations.

\subsection{Radio Lobes and Two X-ray Holes} \label{sec:central_radio}

The central cD galaxy PKS2354-35 is a strong radio source
with two relatively bright radio lobes
(the radio jets  are not pronounced).
A 4.8 GHz B-array VLA radio contour map is shown in
Figure~\ref{fig:xray_central_radio}
(Taylor et al.\ 1994).
The linear size of the radio source is also measured
from a VLA 1.4 GHz map from the NRAO VLA Sky Survey (NVSS),
which shows a slightly larger linear size
(after deconvolution with the radio beam)
of about $63'' \times 22''$ (FWHM).

\begin{figure*}[htb]
\vskip3.3truein
\special{psfile=fig8.ps angle=0 voffset=-130
        hoffset=+40 hscale=60 vscale=60}
\caption{
Contours of the VLA 4.8 GHz radio image (Taylor et al.\ 1994)
are superposed on a grey scale version of the ROSAT HRI X-ray map.
The X-ray grey scale ranges from
0.0133 to 0.136 cnts arcmin$^{-2}$ s$^{-1}$.
The intensities near the centers of the northern and
southern X-ray holes are
0.0265 and 0.0199 cnts arcmin$^{-2}$ s$^{-1}$,
respectively.}
\label{fig:xray_central_radio}
\end{figure*}

It is interesting that the two radio lobes lie
perpendicular to the central X-ray bar
and extend towards the areas of the two X-ray minima.
The radio and X-ray structure in A4059
is similar to that of NGC~1275 in the Perseus cluster
(B\"{o}hringer et al.\ 1993),
it was argued that the two X-ray minima are due
to the displacement of X-ray emitting gas by the radio plasma.
However, in A4059 the radio emission at 1.4 GHz and 4.8 GHz
does not extend into the central areas of the two X-ray holes,
although it is possible that the radio source
extends further at lower frequencies.

In the following, we compare the nonthermal pressure
in the radio lobes with thermal pressure of the
X-ray emitting gas in the region around the radio lobes.
Because we are most interested in the interaction of the radio
plasma and the X-ray emitting gas on the scale of the X-ray
structures seen in Figure~\ref{fig:xray_central_radio},
we will estimate the radio pressure on the largest observed scales
of the radio.
The radio lobes end at about 35$''$ from the center,
where the average electron density is about
$8.6\pm2.5 \times 10^{-3}$ cm$^{-3}$
(90\% confidence level).
The X-ray gas thermal pressure is then
$5.2^{+3.5}_{-2.3}\times 10^{-11}$ ergs cm$^{-3}$ at this radius,
assuming a gas temperature of $1.93^{+0.76}_{-0.33}$keV
(Table~\ref{tab:spectral}).
The largest scale of the radio emission from the
1.4 GHz NVSS radio image
(Condon et al.\ 1993)
is about $63'' \times 22''$ (FWHM).
PKS2354-35 is a 1.27 Jy source at 1.4 GHz,
and has a spectral index of $-1.43$
(Taylor et al.\ 1994).
Assuming that this extended radio flux
comes from a uniform prolate cylindrical region of size
$63'' \times 22''$,
that the ratio of the energy of ions to electrons is unity,
that the volume filling factor is unity,
that the magnetic field is perpendicular to the line of sight,
and that the lower and upper cutoff of the radio frequencies
are 10 MHz and 100 GHz, respectively,
we find a minimum energy magnetic field of 17 $\mu$G,
and a radio pressure
of $9.0\times10^{-12}$ ergs cm$^{-3}$
(e.g., Miley 1980),
which is about a factor of 5.8 smaller than the
gas thermal pressure.
But considering the uncertainties in the estimate of the
minimum-energy radio pressure
(e.g., if the energy ratio of ions to electron is 100,
the radio pressure becomes $8.4 \times10^{-11}$ ergs cm$^{-3}$),
the radio pressure may be comparable to
that of the thermal X-ray gas.

Closer to the center, nonthermal radio pressures
are somewhat higher in the two radio lobes;
the pressures are
$3.1 \times 10^{-11}$ ergs cm$^{-3}$ and
$5.6 \times 10^{-11}$ ergs cm$^{-3}$
for the northern and southern radio lobes, respectively
(Taylor et al.\ 1994).
These pressures are, however, measured at a distance of
$6.8'' - 8.5''$ from the radio core.
On this scale, the X-ray thermal pressure is about
$1.1^{+1.3}_{-1.0} \times 10^{-10}$ ergs cm$^{-3}$.
So, the thermal and nonthermal pressures are again comparable
in the innermost regions,
and it is possible that the radio lobes and the X-ray gas
are in pressure equilibrium.
This would be expected if the radio lobes have displaced, expanded
against, and been confined by the X-ray gas.
This is consistent with the interpretation of the X-ray holes as regions
where the radio source has displaced the X-ray gas.

On the other hand, it is odd that the radio emission in
the available images does not appear to fill the observed
X-ray holes.
One possibility is that the relativistic electrons in the X-ray
hole regions have undergone severe synchrotron losses,
or that the X-ray holes are residuals of
a previous epoch of radio activity.
In a 17 $\mu$G magnetic field, synchrotron losses dominate,
and the lifetime of electrons emitting at a frequency of 1.4 GHz,
the lowest frequency at which the source was observed and detected
with on the largest linear size, is $1.2 \times 10^7$ years.
We can also estimate the age of the radio source from
the variation in the radio spectral indices
(Myers \& Spangler 1985).
Taylor et al.\ (1994) found that the spectral index of the radio
source changed from $-1.1$ at the radio core to $-2.5$ at
the faint, diffuse component to the radio lobes,
which suggests this faint, diffuse radio component
has been around for about $2.6 \times 10^7$ years.
Thus, we are not surprised that much of the
radio emission at 1.4 GHz or higher
has faded beyond the region of the observed radio lobes.
An upper limit to the age of the X-ray holes, assuming they are supported
by nonthermal pressure, is the timescale for their disruption by
Rayleigh-Taylor instabilities and/or by buoyant forces.
Roughly, either of these processes should occur on a timescale which is
$\sim$10 times the sound crossing time of the holes in the
surrounding X-ray gas.
This maximum age is about $10^9$ years, which is
much longer than the lifetime of electrons emitting
at the observed radio frequencies.
Thus, it is possible that
the radio emission from much of the region has faded,
but that the lobes are still supported by the pressure of cosmic ray ion,
low energy cosmic ray electron, and the magnetic field.
In general, in a radio source with a steep spectrum like
PKS2354-35 (Taylor et al.\ 1994),
most of the nonthermal electron pressure is due to electrons
at low energies, which might emit at very
low radio frequencies.

\subsection{Alignment of the X-ray, Optical, and Radio Emission}
\label{sec:central_alignment}

As described in \S~\ref{sec:spatial},
the X-ray isophotes for $r \ga 50''$ are aligned with the
direction of elongation of the optical isophotes of the cD galaxy
PKS2354-35, and the cluster galaxy isopleths.
In addition, the strong radio lobes from the cD galaxy
is also extended along the major axis of the cD potential.
This is consistent with the anisotropic merger model
for the formation cD galaxies and the orientation of their sources
as proposed by West (1994).
West noted that the alignments in A4059 continue to larger scales,
where the two nearest Abell clusters also lie approximately
along the same axis.
In his model, cD galaxies were formed by anisotropic mergers occurring
preferentially along an axis determined by large scale structure.
Gaseous accretion associated with these mergers determined the
axis of rotation of a central black hole, and this is the axis along
which radio jets propagate.
Evidence for the alignment of the X-ray emission, central cD galaxy,
subclusters, host clusters, and surrounding superclusters
have been proposed recently in many other clusters
(e.g., West et al.\ 1995;
Allen et al.\ 1995;
West, Jones, \& Forman 1995).

\subsection{Radio Lobe Inflation or a Rotating Disk?}
\label{sec:central_disk}

The central X-ray structure in the cD galaxy PKS2354-35
is similar to that in NGC~1275 (B\"{o}hringer et al.\ 1993).
In the case of NGC~1275, the regions of X-ray minima
are filled by the radio lobes from the central cD galaxies.
The radio nonthermal pressure in the lobes is comparable to
the X-ray thermal pressure in the surrounding gas,
within the errors.
This is consistent with the idea that the radio lobes have displaced
the X-ray emitting gas, and are expanding against and being confined
by this gas.

The same model may apply to PKS2354-35 in A4059, but the radio emission
does not seem to extend completely into the X-ray holes
in either the 1.4 or 4.85 GHz radio images.
It is possible that the extended radio emission has
a very steep spectral index, and that lower frequency
radio emission fills the X-ray holes.
Alternatively, it may be that the present period of radio activity in
PKS2354-35 is ending,
or that the X-ray holes are relics of a previous
epoch of activity.
This might account for the absence of radio emission from the outer
parts of the X-ray holes.
In either scenario, the holes may still contain cosmic ray ions, low energy
cosmic ray electrons, and magnetic fields with a sufficient pressure
to maintain the X-ray holes against the pressure of the surrounding
X-ray emitting gas.

An alternative interpretation for the central X-ray structure emphasizes
the elongated X-ray bar rather than the X-ray holes.
Perhaps it is not that the X-ray emission from the holes is weak, but
rather that the emission orthogonal to the direction of the holes
(along the bar) is strong.
The X-ray bar might be a disk of X-ray emitting gas seen edge-on.
A disk might be formed from cooling flow gas with angular momentum, which
becomes more rotationally supported as it contacts into the center of the
cluster.
Eventually, part of the gas from this disk might feed an accretion disk
around the central AGN, and the radio jets may emerge perpendicular to
this disk.
Recently, 2-D numerical simulations have shown that
a rotationally supported disk
can be formed under some circumstances in a cooling flow
(Garasi, Loken, \& Burns 1996).
On the other hand, Nulsen, Stewart, \& Fabian (1984) have argued that
turbulent viscosity will effectively transport
the angular momentum of cooling flow gas outward, and that the gas will
not form a rotationally supported disk in the inner regions.
A disk might also be formed due to a merge with a gas rich
dwarf galaxy, although such galaxies are rare in centers
of rich cluster.

In either case, there would be no reason to expect the initial angular
momentum of the gas would be aligned with the major axis of the cluster
and cD galaxy.
However, West (1994) argues that cD galaxies are highly prolate, and
that differential procession will cause accreting gas to settle into
a disk which is perpendicular to the major axis of the galaxy, as
required in A4059.
Hydra A seems to show just such a disk, which is seen prominently
in 21 cm H~I emission
(Dwarakanat et al.\ 1995).
Optical emission line spectra of the disk in Hydra A show that it is
rotating
(Ekers \& Simkin 1983;
Baum et al.\ 1988).
However, there is no similar evidence for a rotating disk
in Abell~4059.

\section{SUMMARY} \label{sec:summary}

In summary, we have analyzed the ROSAT HRI image and PSPC spectra
of Abell~4059.
The most striking feature of the X-ray image is
the two X-ray holes and an orthogonal X-ray bar
in the center of the cluster.
It is likely that the radio plasma from the cD galaxy
may have displaced the X-ray gas and created the X-ray holes,
or we may be seeing a rotationally supported disk of the
X-ray emitting gas.
There may also be a moderate cooling flow
in the center of the cluster,
$\dot{M} = 184^{+22}_{-25}$ $M_{\odot}$ yr$^{-1}$,
as suggested by the X-ray surface brightness profile.
However, such a cooling flow is not needed in
the spectral fitting of the PSPC data.
It may be that the cooling flow has just begun in the
center of the cluster.
In addition, very little intrinsic absorption was found
in the center of the cluster.

\acknowledgments

This research was supported in part by NASA Astrophysical Theory Program
grant NAG 5-3057, NASA ASCA grant NAG 5-2526, and NASA ROSAT grant 5-3308.
The optical images are from the Digitized Sky Survey.
The Palomar Observatory Sky Survey was funded by the National Geographic
Society, and the Oschin Schmidt Telescope
operated by the California Institute of Technology and Palomar Observatory.
The Digitized Sky Survey was produced at the Space Telescope Science
Institute (STScI) under U. S. Government grant NAG W-2166.

redpajama_set_name: RedPajamaArXiv


text:
Q: How do I read CSV file row by row and update Python script? I have the following Python 2.7 script:
import urllib as ul
tracking_id = "abcde=="
encodedtrackingid = ul.quote(tracking_id)
mcid = "123456"

URL = "https://example.com/id?abcd&d_mid="+mcid+"&=124"+encodedtrackingid+"%011"
print URL

from mechanize import Browser
br = Browser()
br.set_handle_robots(False)
response = br.open(URL)
print response.read()

import requests

url = "https://example.net/rest/v1/mbox/4513452615415"

querystring = {"client":"example"}

payload = "{\r\n              \"mbox\" : \"example\",\r\n\"CloudVisitorId\":\""+mcid+"\",\r\n              \"thirdPartyId\": \""+tracking_id+"\",\r\n              \"contentAsJson\": \"true\",\r\n                             \"mboxParameters\": \r\n                             {        \r\n                             \"mboxMCGLH\": \"6\"     \r\n                             }\r\n}\r\n"
headers = {
    'content-type': "application/json",
    'cache-control': "no-cache",
    'postman-token': "289879f645d-1543-e6df-87fb-1cef88f55110c5"
    }

response = requests.request("POST", url, data=payload, headers=headers, params=querystring)

print(response.text)

What I want to do is the following:
a) Repeat this script by updating the tracking_id and the mcid variable from a CSV file.
The CSV file has no headers and has the following columns:
Column: A - tracking_id
Column: B - mcid
I need the script to read the CSV file run the script for row 1, then repeat the same process for row2, row3, row4 etc. Each time the script runs the tracking_id and the mcid variable updates, and the output of the response variable is stored into a CSV file.
The end result would be a CSV file  that would have the following:
Column A - tracking_id
Column B - mcid
Column C - response
Any help is much appreciated.
Thanks

A: First of all, I would wrap the initial script up in a function (myfunction in the code below) taking the tracking_id and the mcid as parameters and returning the value you wish to retrieve.
import csv

# Loading csv
with open("mycsv.csv", 'r') as csv_file:
    reader = csv.reader(csv_file)
    # Reading row by row
    for row in reader:
        tracking_id = row[0]
        mcid = row[1]

        # Getting result
        result = myfunction(tracking_id, mcid)

        # Opening csv result file in append mode
        with open("mycsv_result.csv", "a+") as csv_save:
            writer = csv.writer(csv_save)
            writer.writerow([tracking_id, mcid, result])
            csv_save.close()

Then this script should do the trick.

EDIT :
Here is the function missing. I also suggest you to read this in order to learn how to create basic functions.
def myfunction(tracking_id, mcid):
    import urllib as ul

    encodedtrackingid = ul.quote(tracking_id)

    URL = "https://example.com/id?abcd&d_mid=" + mcid + "&=124" + encodedtrackingid + "%011"
    print
    URL

    from mechanize import Browser

    br = Browser()
    br.set_handle_robots(False)
    response = br.open(URL)
    print
    response.read()

    import requests

    url = "https://example.net/rest/v1/mbox/4513452615415"

    querystring = {"client": "example"}

    payload = "{\r\n              \"mbox\" : \"example\",\r\n\"CloudVisitorId\":\"" + mcid + "\",\r\n              \"thirdPartyId\": \"" + tracking_id + "\",\r\n              \"contentAsJson\": \"true\",\r\n                             \"mboxParameters\": \r\n                             {        \r\n                             \"mboxMCGLH\": \"6\"     \r\n                             }\r\n}\r\n"
    headers = {
        'content-type': "application/json",
        'cache-control': "no-cache",
        'postman-token': "289879f645d-1543-e6df-87fb-1cef88f55110c5"
    }

    response = requests.request("POST", url, data=payload, headers=headers, params=querystring)

    return response

A: import csv

#traceroute
traceroute_output = """
185.86.232.2     0.512 ms    0.453 ms    0.414 ms
188.95.232.58    0.795 ms    0.765 ms    0.731 ms
188.95.232.67    1.493 ms    1.463 ms    1.560 ms
188.1.239.85     1.853 ms    1.827 ms    2.001 ms
"""
reader = csv.reader(traceroute_output.splitlines(), delimiter=' ', skipinitialspace=True)

for row in reader:
    if len(row)< 7:
        #neglecting invalid values
        continue
    key_value = row.pop(0)

Here is some sample code which wrote some time ago to parse the CSV file separated by spaces, You can modify according to your requirements. I hope this will be useful.

redpajama_set_name: RedPajamaStackExchange


Home Bunch recommends not scrimping on lighting. Lights can make a big difference in the entry way of your home, and they help to make the porch more useable in the evenings.
I like the drink station idea. I also like a nap on the porch at night, that swinging mattress is awesome. I don't know if I would get up.
Love the hanging bar… Its a perfect space saver!!!
Very nice ideas… Thanks for sharing.
Do you know where the braided rug is from? In photo 6.
Love the hammock chair. Where did you buy it?
Our family home is a brick Georgian with beautiful wide brick porch with doric columns and nothing looks good on our porch except for matching ferns in black urns or matching flowers in chippendale planters. The space is so formal nothing else seems to fit. I have never seen anyone successfully put furniture on a formal porch.
Love the drink station idea!!!! And the couches. You know what I think makes a beautiful front porch? Having one of those beautiful glass doors like you see in New Orleans and Savannah.
We have a swing bed under our house at the beach, it is awesome. (that I built!) Lots of pillows, use it as the focal point. I have swings and chairs plus a couple of tables on our front porch at home. I have a baby mattress, so I am going to cut down the plans for my swing bed with a twin mattress, and make one for the porch here using the crib mattress. http://www.wooditsreal.com (My bed is the one with the red and white striped bedding.) Thanks for the ideas. I really, really love the idea for the lights. Awesome.


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redpajama_set_name: RedPajamaCommonCrawl


text:
Why Transgender Activism Will Fail: Biological Differences Are Real
CP Current Page: Opinion | Wednesday, October 11, 2017
By Michael Brown, CP Op-Ed Contributor | Wednesday, October 11, 2017
Michael Brown holds a Ph.D. in Near Eastern Languages and Literatures from New York University and has served as a professor at a number of seminaries. He is the author of 25 books and hosts the nationally syndicated, daily talk radio show, the Line of Fire.
Transgender activism will never succeed in reshaping our society for one simple reason: It is not natural. Biological differences are too deeply instilled in the human race. Male-female distinctives are too obvious and real. It is futile to declare war on gender.
It is one thing to be asked to empathize with those who struggle with gender identity confusion. It is another thing to declare that biological categories do not determine reality.
It is one thing to recognize that some people do not fall within the normal, male-female spectrum due to genetic abnormalities. It is another thing to claim that gender is whatever you perceive it to be.
Every time we hear the announcement that someone is having a boy or a girl, we are reminded that transgender activism is failing. Otherwise, shouldn't the parents-to-be say, "We just saw the ultrasound, and we're having a human!"? Or, perhaps, "How exciting! We saw the ultrasound, and the packaging is female!"?
If we really believed the transgender talking points, that's how we would communicate. And yet even liberal celebrities like Kylie Jenner, the daughter of none other than Bruce "Caitlyn" Jenner, announce the sex of their babies when they learn it. (Note this TMZ headline about the baby: "Kylie Jenner, Travis Scott: IT'S A GIRL!")
And how many parents are choosing not to name their children in accordance with their biological sex? How many are choosing gender-neutral names in case the child happens not to line up with the sex they were "assigned" at birth?
Last month, two high-school students complained to their school when their bus driver insisted that they sit on the girls' side of the vehicle. (Apparently, it was his custom to have boys sit on one side and girls on the other.) The problem was that, although biologically female, these girls identify as "neither male nor female," which, we are informed, "is referred to as trans nonbinary."
I know that the school was sympathetic to their plight, pledging to speak to the driver in private. (They got off the bus rather than change their seats.) But are we really to believe that these kids are "neither male nor female"? Is this the new reality? Will society buy it as a whole? Certainly not.
Other schools are already witnessing a pushback.
For example, also last month, "A Florida elementary school teacher who asked students to use gender-neutral pronouns in the classroom is being transferred to an adult education program.
"According to a Tallahassee Democrat report, Leon County Schools officials announced Tuesday that Chloe Bressack would no longer teach fifth grade at Canopy Oaks Elementary School."
"Superintendent Rocky Hanna said Bressack agreed that 'given the complexity of the issue,' a transfer would be best for the teacher's career and the fifth-graders."
Parents were not willing to have their kids call Bressack "Mx." (pronounced "Mix") and refer to her as "they" – for good reason. It's just not natural.
Earlier this month, a new study proposed that, "Schools should make sex education more inclusive of transgenders by not referring to biological body parts with the correct term because it might make transgender people uncomfortable."
Do you really think this will fly? Will the whole world be turned upside down because of the confusion and sensitivities of less than 1 percent of the population?
And what about the all-female college at Cambridge that recently announced it is accepting males who identify as females? I wonder what will happen when the other students discover that these so-called transwoman can still impregnate them.
The statement of Barbara Stocking, president of Cambridge's Murray Edwards College, is ludicrous: "We are a college that is open to all outstanding young women, and so it is absolutely right, both legally and within our set of values, for anyone who identifies as female to be able to apply to study with us."
How long will it be before people look back at these words with incredulity? This new definition of "outstanding young women" will not fly either.
Not surprisingly – and quite sadly – numerous headlines recently reported on "The rise of transgender reversals: Surgeon in sex-change hub of Serbia reports a surge in the rate of patients changing their mind."
But this is hardly breaking news. For several years now, former male-to-female Walt Heyer has devoted his SexChangeRegret.com to these all-too-numerous stories. And Ryan T. Anderson devoted a whole chapter to this in his forthcoming book When Harry Became Sally: Responding to the Transgender Moment.
What is remarkable is that "the United Kingdom's Bath Spa University turned down an application by James Caspian, a psychotherapist who specializes in working with transgender people, to conduct research on gender reassignment reversals. The university deemed the subject 'potentially politically incorrect.'"
This too is creating a backlash, both within and without the university. Political correctness – in this case, fear of offending transgender activists – is devouring itself.
That's why the same parents who changed their views on homosexuality, wanting to be "tolerant" and "inclusive," are not changing their views on gender. After all, it's one thing to say, "Who am I to tell two men or two women they cannot love each other?" It's another thing to say, "I have no problem with 15-year-old Jake sharing the locker room and shower stalls with my daughter Tammy, since he now identifies as a girl and wants to play on the girls' basketball team."
It's not natural, biological differences are too real, and male-female distinctive are too foundational for changes like this to be accepted widescale.
Watch and see. The pushback against transgender activism will continue.
Dr. Michael Brown (www.askdrbrown.org) is the host of the nationally syndicated Line of Fire radio program. His latest book is Saving a Sick America: A Prescription for Moral and Cultural Transformation. Connect with him on Facebook or Twitter.
UK to Ban 'Sex' Question on Census to Not Offend Trans, Nonbinary Citizens; Feminists Outraged
Parents Slam Transgender Push to Remove Gender-Specific Terms 'Penis, Vagina' in School Sex Ed
More Men Regretting Sex Change Surgery, Suffering Crippling Depression: Surgeon
UK Catholic Girls School Tells Students to Use Transgender Pronouns
A personal tribute to Dr. Norman Geisler
We're commanded to pray for presidents but not to give them photo-ops
'The Handmaid's Tale' is more conservative than you think
'Unplanned' movie will cause men to repent for mistreating, abandoning women and shift the culture
Religious freedom is for Muslims too


Get away from it all at Campbell House Bed and Breakfast now celebrating 22 years in Historic Ligonier. Experience uniquely decorated rooms with private-baths. Enjoy life from the porch or take a short stroll to shoppes, restaurants, our beautiful bandstand or visit Fort Ligonier. Near to golfing, fishing, museums, biking and hiking or just relaxing. Perfect for any reason in any season.
So many reasons to Vacation in Ohiopyle!


For courses in Human Physiology. This package includes Pearson Mastering A&P. Move beyond memorization: Prepare students for tomorrow's challenges Human Physiology: An Integrated Approach is the #1 best-selling 1-semester human physiology text world-wide. The 8th Edition engages students in developing a deeper understanding of human physiology by guiding them to think critically and equipping them to solve real-world problems. Updates, such as new Try It activities and detailed teaching suggestions in the new Ready-to-Go Teaching Modules, help students learn and apply mapping skills, graphing skills, and data interpretation skills. The text reflects Dr. Silverthorn's active learning style of instruction and builds upon the thorough integration of "big picture" themes with up-to-date cellular and molecular physiology topics that have always been the foundation of her approach. Pearson Mastering A&P features new Interactive Physiology 2.0 tutorials, new Try It! Coaching Activities, and Phys in Action! Video Tutors, complementing Human Physiology and providing a cohesive learning experience for today's learners. Reach every student by pairing this text with Pearson Mastering A&P Mastering (TM) is the teaching and learning platform that empowers you to reach every student. By combining trusted author content with digital tools and a flexible platform, Mastering personalizes the learning experience and improves results for each student. Pearson Mastering A&P should only be purchased when required by an instructor. Please be sure you have the correct ISBN and Course ID. Instructors, contact your Pearson representative for more information.
Auteur Silverthorn, Dee Unglaub, Ph.D.


The seventh Horncastle Junior Angling match of the year was held at Bainside Coarse Fishery.
A total of 12 boys and girls attended.
This week's format was a pairs match, with the younger anglers matched with the older juniors.
With the winning bag from pegs 10 and eight were Hannah (10lb) and Elsie (5lb) respectively.
Results: Olivia 3lb 2oz, Jake 2lb 12oz, Henry 3lb, James 1lb 4oz, Kerrien 2lb 8oz, Rosie 8lb 6oz, Elsie 5lb, Jasmine 3lb, Hannah 10lb, Callam 2lb, Libby 1lb 12oz, Oscar 1lb 4oz.


Tesco Pharmacy, pharmacy, listed under "Pharmacies" category, is located at Brunton Ln Kingston Park Newcastle Upon Tyne Tyne and Wear, NE3 2FP, United Kingdom and can be reached by (01916) 934447 phone number. Tesco Pharmacy has currently 0 reviews.
Browse all Pharmacies in Newcastle Upon Tyne Tyne and Wear.


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SportsCollege Sports
Michigan beats Loyola (Chicago) in Final Four, advances to title game
By: Ralph D. Russo, AP Sports Writer

LOS ANGELES, CA - MARCH 22: Moritz Wagner #13 and Charles Matthews #1 of the Michigan Wolverines celebrate in the second half while taking on the Texas A&M Aggies in the 2018 NCAA Men's Basketball Tournament West Regional at Staples Center on March 22, 2018 in Los Angeles, California. (Photo by Harry How/Getty Images)

SAN ANTONIO (AP) -- Moe Wagner, Charles Matthews and Michigan erased a 10-point second-half deficit and the Wolverines ended Loyola-Chicago's storybook NCAA Tournament run with a 69-57 victory Saturday night in the Final Four.
The third-seeded Wolverines (33-7) will take a 14-game winning streak into their first national championship game appearance since 2013, and second under coach Jon Beilein.
Michigan will play either Villanova or Kansas for its first NCAA title since 1989 on Monday night at the Alamodome.
Lovable Loyola (32-6), with superfan Sister Jean courtside and their fans behind the bench standing for pretty much the entire game, could not conjure another upset. The Ramblers were the fourth 11th-seeded team to make it this far and like the previous three, the semifinals were the end of the road.
Loyola had no answers for the 6-foot-11 Wagner and its offense, so smooth and efficient on the way to San Antonio, broke down in the second half and finished with 17 turnovers.
Wagner, playing in front of his parents who made the trip from Germany, scored 24 points, had 15 rebounds and was 10 for 16 from the field. Matthews, the Kentucky transfer and Chicago native, added 17 points, including a run-out dunk with 1:33 left that made it 63-53.
As the seconds ticked off, Wagner pumped his fist to the many Michigan fans who made the trek to San Antonio and Loyola's Aundre Jackson, who got the Ramblers rolling with a late game-winning 3 in the first round against Miami, looked toward the roof and shook his head.


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Markt Strategie
Daily comment
Visie van de week
Real-time charts
more Daily Comment items
Monday January 30th
Thursday January 26th
Wednesday January 25th
Tuesday January 24th
Monday January 23rd
Wednesday November 2nd
Thursday December 22nd
Tuesday January 4th
Tuesday November 1st
Stock futures rise as traders try to add to October's strong gains, look to Fed meeting
U.S. stock markets index futures rose Tuesday, the first day of November, as Wall Street tried to build on last month's sharp gains and looked ahead to a key Federal Reserve decision on rates. Futures tied to the Dow Jones Industrial Average were up 230 points, or 0.7%. S&P 500 and Nasdaq 100 futures added 1.1% and 1.4%, respectively. The rise in stock futures came as rates fell ahead of the central bank's rate decision as investors hope for a sign that the Fed will ease its tightening stance in the months ahead. A better-than-feared earnings season, meanwhile, continued with a strong report from Pfizer while Uber shares popped on a revenue beat and strong gross bookings. Some traders also pointed to optimism from unconfirmed reports that China could be moving away from its Zero Covid policy as a source for Tuesday's early gains. "Stocks are trading very well following unconfirmed reports on social media overnight about China formulating a plan to exit its 'zero tolerance' approach to COVID," wrote Adam Crisafulli of Vital Knowledge. "While the consensus narrative has embraced the 'Fed will slow its tightening pace' narrative, China remains among the most hated markets on the planet w/its equity indices at multi-decade lows – there's still a lot more room to rally on the upside in the coming quarters assuming a more realistic COVID approach is implemented," he added. Wall Street on Monday wrapped up a strong month of gains, with the Dow rallying nearly 14% for its biggest monthly advance since January 1976, as investors rotated out of technology and hedged hopes on stalwarts like banks. The S&P 500 and Nasdaq Composite added about 8% and 3.9%, respectively. Tuesday also kicks off the Fed's November meeting, which many expect will result in a 75 basis point interest rate hike. Investors will also monitor the central bank's statement and Fed Chair Jerome Powell's press conference for signs that the Fed may slow its tightening pace. Economic releases for Tuesday include job openings data and construction spending for September. The ISM manufacturing report for October is also due. Stocks in Hong Kong led gains in the Asia-Pacific session after concluding the month of October with a more than 14% loss, hovering around the lowest levels that it's seen since April 2009. The Hang Seng index in Hong Kong rose 5.23% to 15,455.27, with Hang Seng Tech up 7.8% after unconfirmed reports of reopening talks taking place in China. Mainland China's Shanghai Composite gained 2.62% to 2,969.20 and the Shenzhen Component added around 3.24% to 10,734.25 after the Caixin manufacturing PMI for the country came in at 49.2, slightly better than expected. The Nikkei 225 in Japan was 0.33% higher at 27,678.92 while the Topix rose 0.47% to 1,938.50.The Kospi in South Korea also rose 1.81% to 2,335.22. Oil prices rose on Tuesday, paring losses from the previous session, as a weaker U.S. dollar offset widening Covid-19 curbs in China that have stoked fears of slowing fuel demand in the world's second-largest oil consumer. Brent crude for January delivery rose 73 cents, or 0.8%, to $93.54 a barrel at 0406 GMT. The December contract expired on Monday at $94.83 a barrel, down 1%. U.S. West Texas Intermediate (WTI) crude rose 58 cents, or 0.7%, to $87.11 a barrel, after falling 1.6% in the previous session. Gold prices were flat on Tuesday, after touching their lowest levels in more than one week, as the dollar held firm ahead of the U.S. Federal Reserve's policy meeting, where the central bank is likely to deliver another oversized interest rate hike. Spot gold was listless at $1,633.69 per ounce, as of 0059 GMT, having earlier touched its lowest level since Oct. 21. U.S. gold futures fell 0.3% to $1,636.30. The dollar index was steady after rising 0.8% overnight, hurting gold's appeal for overseas buyers.
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Celebrity News November 02, 2022
Haley Lu Richardson & Brett Dier Secretly Called Off Engagement 2 Years Ago
"The White Lotus" Season 2 star Haley Lu Richardson and "Jane the Virgin" alum Brett Dier secretly split in 2020 after eight years together.
The exes posted the news on Instagram Stories this week, revealing they wanted to "share it and move on."
Haley, 27, wrote, "Hey guys. This is me and Brett. We actually separated two years ago. But life goes on and we are both existing and doing pretty well turns out."
The "Five Feet Apart" actress continued, "We shared a deeply special chunk of our lives together. I'm so glad to have had the last couple years to heal and grow without the internet knowing but we kinda just wanted to share it and move on now. Love yourselves! Life is life babies!"
Brett, 32, wrote on his account, "We separated 2 years ago but we saw each other today for the first time. We are happy and so thankful for the time we had together. (For those people who have been dying to know what happened to us). Haley's post is better worded so go read that one! Have a great day!"
Haley and Brett announced their engagement in 2018, and Richardson dished on the proposal during a visit to "Busy Tonight" in 2019.
"I just asked," she said. "Neither of us are, like, crazy-romantic people, so nothing was planned. He was sitting there eating a pizza and he was telling me a joke that Shia LaBeouf had said in an interview, and he was, like, pretending to be Shia LaBeouf explaining this joke and for some reason I just cut him off and was like, 'Wanna marry me?'"
Haley added, "Maybe that got us in the mood, I don't know. But yeah, we're engaged now."
Around that time, she also opened up to Cosmo about taking their time to get married.
"We've been together for seven years. We just want to take our time. We're still not used to the word fiancé," she explained. "It's so pretentious in saying it. Neither of us are used to it. We still call each other boyfriend and girlfriend. We're just engaged. And I love Brett. And we'll get married one day."
She said of proposing, "I was totally in the moment and this gut feeling came up and coerced me to ask him to marry me and I did. And he said yes. I feel like the trick to that was just not thinking about it at all before it happened. I just kind of did it."
Haley also starred in "Five Feet Apart" in 2019 alongside Cole Sprouse. "Extra's" Renee Bargh caught up with the stars to find out more about the tearjerker. Watch!
#CelebrityNews #CouplesNews #TrendingStories
Video! Cole Sprouse & Haley Lu Richardson Surprise Audiences at 'Five Feet Apart' Screenings
Justin Baldoni on What He Hopes Audiences Will Take Away from 'Five Feet Apart'
More in Celebrity News
Annie Wersching of '24,' 'Timeless' Dies at 45
Bella Thorne Turns Heads at Sundance
Tom Verlaine, Frontman of Influential Band Television, Dies at 73
Marc Anthony Marries Nadia Ferreira — Inside the Star-Packed Nuptials!
Claire Danes Says Her Son, 4, Is 'Less Than Thrilled' About Her Pregnancy
Matt Damon Melts Down on Jimmy Kimmel's 20th-Anniversary Show
Sylvia Syms, Esteemed English Actress Seen in 'The Queen,' Dies at 89


6 sets with vector decorative design elements in vintage style with vintage flower illustrations, ornaments, ornate frames, labels, logos, decorative borders, vintage inscription and lettering, dividers, filigree, decor flourish. Format: EPS stock vector clip art and illustrations. Free for download.
Set name: "Decorative design elements set" for Adobe Illustrator.
Theme tags: retro, vintage, decorative.
Posted on 30/05/2012, in Free Vector Graphics | Tags: borders, decorative, elements, floral, frames, labels, ornaments, retro, vintage.


Create a beautiful rug using a jelly roll! Jean will guide you through the steps and pass along tips and tricks. You will need to sew your strips together before class. Once you make one you'll be hooked! One jelly roll will make a rug approximately 30" x 44". Keep going to make it bigger!


Much bigger and easier than the typical form. It's not really clear, where these plants originate. They were grown in the Oxford botanical garden (UK) for decades but apparently nobody still knows, where the mother plants were collected.
Nowadays it's believed that Heliamphora nutans "Giant" is in fach a natural hybrid of Heliamphora nutand and Heliamphora glabra and so, it's no surprse that the offspring oes not fall true from seeds - many seedlings looked different from the mother plants.
We can now offer the real thing!
In contrast to many other Heliamphoras these plants tolerate higher temperatures and as such are ideal beginners plants. The plants can be grown in various peaty mixes, however many growers prefer pure living Shagnum-moss. In recent times dead Sphagnum of very high quality from Chile and New-Zealand became widely available. A mix of such moss with horticultural-grade Perlite, a bit of good quality peat-moss and pinebark-choppings makes an excellent mix. However, when using Sphagnum, it's important to allow for a good drainage as otherwise, Sphagnum has the tendency to rot quickly. Please note, that all Heliamphoras require good illumination. They can, however easily be grown indoors under fluorescent tubes as long as they are close to the lights and temparature requirements can be met. Many growers in fact prefer to grow them in terrariums under fluorescent tubes from cultivatiing Heliamphora in the greenhouse.


Delivery flowers in Rouf Athens | Florist Rouf | Send flowers Rouf | Flower shop Rouf Athens, Greece | Flowers - Milva Flowers!
Florist Rouf Athens. Send flowers in Rouf Athens, Greece online same day from flower shops. Free flower delivery in Rouf Athens Greece from local florist.
Flower shop in Rouf Athens sending gift baskets flowers & fresh bouquet with cut red, white roses and many flowers by hand, delivered same day.
Flower delivery Rouf Athens There are 69 products.


You've been in beautiful Colorado for less than an hour, and you're already getting antsy to get the heck out of your vehicle and onto the slopes of Vail County, the trails of one of Colorado's gorgeous national forests, or just the cozy queen bed waiting for you in the spare bedroom at your family member's house in Colorado Springs. You can't help it. You're ready to finally arrive at your destination, and you hit the gas. That's when you see those tell-tale blue and red lights in your rearview mirror.
We've all been there, waiting with our hands nervously gripping the steering wheel as an officer, deputy, or trooper walks up with a traffic ticket in mind. While some Colorado traffic tickets aren't likely to spoil your entire vacation, some could result in steep penalties, including hefty fines and even time in prison. Keep reading for a brief rundown on traffic tickets in Colorado.
In the State of Colorado, traffic tickets are separated into two main categories: traffic infraction tickets and traffic offense tickets. The type of ticket issued for a traffic violation depends on the severity, circumstances, and results of the violation.
If you are ticketed for a traffic infraction, you will likely be able to simply pay the ticket and be on your way. Class A and Class B driving infraction tickets may result in fines and/or court costs. These traffic violations are typically less severe in nature, including failing to use a turn signal, speeding up to 24 MPH, and failing to obey traffic signals. These infractions are handled civilly, meaning you will probably not require the advice of a criminal defense attorney for a traffic infraction ticket.
Being ticketed with a traffic offense ticket, on the other hand, can result in much harsher penalties. These tickets are typically classified as misdemeanor traffic offenses, meaning they are handled as criminal, not civil, cases. You may be issued a Class 2 misdemeanor traffic offense ticket for reckless or careless driving, and you may be issued a Class 1 misdemeanor traffic offense ticket if an accident that occurred while you were driving carelessly resulted in the injury or death of another. Being charged with a Class 1 misdemeanor may result in more than a year of jail time and hefty fines.
Remember to drive safely while visiting Colorado! If you're facing criminal charges for a traffic offense, don't hesitate to contact our Colorado Springs criminal defense attorney.


There are plenty of ideas that might just work for you and help you finance your franchise business. You are all set to run a franchise business; you have everything what it takes to run it, but you may still be wondering where to get the start-up funds. But, before you go ahead and start reviewing the different options, you are advised to first do the basic calculations. For example, you must have a clear picture about how much money you will need. Make sure you take all necessary factors into account while you are doing this calculation. Some of the important factors to consider here include advertising fees charged by the franchise, royalty payments to the franchisor, the franchise fee to open the business, and other such things. Now, following is a brief rundown on some of the funding sources.


Russian lady with 9 years experience in hospitality search for administrative work in SPA with immediate hiring.
I am hairdresser from Belarus. Searching for work in Sharm el Shaikh.Big experience.All the details in the CV and interview.
I'm an Italian girl who wants to work.


(Newser) – A judge heard a DMX rap song before adding his own lyrics to a court proceeding on Wednesday, ordering the rapper imprisoned for a year in a tax fraud case. Federal Judge Jed Rakoff took requests Wednesday, accommodating DMX's desire to hear his hit "Slippin'" before DMX faced the music over his admission of guilt. The judge called DMX's fraud a "brazen and blatant" crime that could not go unpunished, the AP reports. The 47-year-old rapper, known to law enforcement and the courts as Earl Simmons, has been incarcerated since his bail was revoked in January.
He sobbed during the proceeding as his lawyer, Murray Richman, recalled his nightmarish childhood. Richman said DMX has been a model prisoner. Still, prosecutors sought five years in prison for him, citing a lengthy rap sheet and drugs. Richman wanted him free to support his 15 children and pay back more than $2 million in taxes. As "Slippin'" played in the packed courtroom, DMX nodded his head slightly to the beat while some of his supporters nodded more enthusiastically. Given a chance to speak, he said he knows taxes need to be paid and what he did was wrong. "I wasn't following the rules," he said. "I was in a cloud." The judge said that in the court's view DMX "is a good man." "In many ways," the judge said, "he's his own worst enemy."
Some black folks don't like to pay taxes because it's a slave tax. If he makes more and more money than the average Afro-American, how is it possible he can't pay up the government?
A year in prison to nothing to these sub humans. He'll be a celebrity and live like a king. That's a joke to people like him.


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Q: dimple.js scatterplot duplicating axis lables Using dimple.js, I am rendering a scatter plot with the code below. This works fine, but when i hover the mouse over any point, the x and y values are shown twice, once as decimal and below that as percentage.  How can i simply keep the percentage x,y values in the hover-popup?  Also, is there a way to display additional items in the hover-popup?
Here is the fiddle demonstarting the issue:  http://jsfiddle.net/dizzy0ny/ch2187dd/52/
var svg = dimple.newSvg("#chartContainer", 600,600);
var myChart = new dimple.chart(svg);
myChart.setBounds(90, 35, 480, 400)
xAxis = myChart.addMeasureAxis("x", "x");
yAxis = myChart.addMeasureAxis("y", "y");
xAxis.showGridlines = true;
xAxis.tickFormat = '.1%'
yAxis.tickFormat = '.1%'
s1 = myChart.addSeries(["x","y","group"], dimple.plot.bubble, [xAxis, yAxis]);
s1.data = data_scatter

s2 = myChart.addSeries(["y","group"], dimple.plot.line, [xAxis, yAxis]);
s2.data = data_ser1

myChart.addLegend(90, 480, 330, 20, "left");
myChart.draw();

A: As per the docs here: http://dimplejs.org/adhoc_viewer.html?id=adhoc_bar_custom_tooltips
You can change the default tooltip like so:
s1.getTooltipText = function (e) {
    return [
        "This is a custom tooltip!",
        "X value: %" + (e.aggField[0]*100).toFixed(2),
        "Y value: %" + (e.aggField[1]*100).toFixed(2),
        "Group: " + e.aggField[2]
    ];
};

Check out your updated fiddle here: http://jsfiddle.net/ch2187dd/55/
Also, try not to forget those semi-colons! :)


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CAJ's Work
Accountable Policing and Justice
Equality Coalition
Protecting Human Rights and the Peace Settlement
BrexitLawNI Project
Why Support Human Rights in Northern Ireland?
Promoting Justice /
Protecting Rights
Written Evidence to the House of Lords EU Justice Sub-Committee Inquiry into Rights after Brexit
Committee on the Administration of Justice
Publications, Submissions
Brexit, citizenship rights, good friday agreement, human rights, human rights and brexit, withdrawal agreement
Contained within the Ireland/Northern Ireland protocol of the draft Withdrawal Agreement is a commitment from the UK to ensure that, in the event of Brexit, there will be "no diminution" of key rights set out in the Good Friday Agreement.
This commitment is to be implemented through 'dedicated mechanisms', including new oversight and enforcement powers for the Equality Commission for Northern Ireland (ECNI) and the Northern Ireland Human Rights Commission (NIHRC).
However, even at this late stage there has been no further information from the UK government as to the nature of such powers. Nor any parliamentary or public scrutiny of them.
Because of this, CAJ has provided evidence in relation to these new powers to the House of Lords EU Justice Sub-Committee, which is currently conducting an inquiry into 'Rights after Brexit'.
Our submission urges the Committee to seek clarification over a number of different areas, including the exact nature of the powers and whether the intention is to protect all rights contained within the GFA or only a portion of them (which is what the correct wording appears to suggest).
Additionally, we encourage the Committee to question what will happen in the event of the UK making a 'no deal' exit from the EU.
The submission is available to read here: CAJ-evidence-to-Lords-EU-Justice-Sub-Committee-Inquiry-on-Rights-after-Brexit
Promoting Justice/ Protecting Rights
MI6 unilaterally assumed power to break law on UK soil, tribunal reveals
Committee on the Administration of JusticeNews, Press releases0
CAJ Annual Report 2020
Committee on the Administration of JusticeAnnual Reports, Publications, Reports0
Submission to the Committee of Ministers in relation to the supervision of the cases concerning the action of the security forces in Northern Ireland (October 2020)
Committee on the Administration of JusticePublications, Submissions0
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Campaigner Review
Saige Driver
| Updated
Dekdoyjaidee / Getty Images
> Marketing Solutions
The best email marketing services have extensive tools, such as an easy-to-use email editor, a large library of responsive templates, contact management, analytics and reporting, segmentation, A/B split testing, inbox preview, and automated tools.
The Best Email Marketing Services and Survey Software of 2020
Campaigner is simple email marketing software with all the essential features to create professional and effective email marketing campaigns.
View all our recommendations for email marketing services on our best picks page.
Overall, Campaigner has an impressive list of email marketing tools and a large template library. Its tools make it easy to create professional emails, manage a healthy contact list and create automated customer journeys. While it does offer a free trial, you have to provide a credit card before signing up. It doesn't have a free version.
Competitive Pricing and Terms
Like most other email marketing services, Campaigner's prices are based on the number of subscribers you have. All plans come with an array of helpful features, including chat support, an extensive knowledgebase, media hosting, a drag-and-drop email editor, contact management, segmentation tools, geolocation, exclusion lists, custom footers, A/B split testing, autoresponders, email reports, social media integration, and more than 900 templates.
Campaigner's cheapest plan starts at $19.95 per month for up to 1,000 contacts. The next plan starts at $29.95 per month for up to 3,500 contacts.
The most expensive plan starts at $550 per month for up to 100,000 contacts. This plan also includes workflows, static segment sampling and single opt-in forms.
If you have a list with more than 100,000 subscribers, you need to contact Campaigner for a quote.
If you prepay for a year, you receive an 18 percent discount.
While Campaigner doesn't have a free plan, it does have a 30-day free trial for businesses with up to 1,000 contacts. However, you have to sign up for the trial with a credit card. Most other email marketing services offer a free trial without a credit card.
Campaigner Features
Campaigner has a wide selection of email marketing tools that make creating campaigns a breeze.
A/B split testing: A/B split testing is designed to increase contact engagement, interactions and conversations. It allows you to test slight changes in your email marketing campaigns against different versions. You can test different subject lines and other variables. Once Campaigner determines which version gets the best results, it'll send the better email to the rest of your subscribers.
A/B split testing can also help you determine what day of the week and time of day has the best open rates, what subject line is most effective, and if the time of day affects the overall click rate.
Analytics: You can view open and click rates broken down by device, whether a campaign is marked as spam, bounce rates, and other statistics. It shows who is reading your email campaigns, social media shares and Google Analytics data.
Autoresponders: With Campaigner's autoresponders, you can send the right emails at the right time. You can schedule and send emails on a daily, weekly, monthly or annual basis on the dates you select. You can also send recurring emails such as renewal notices, reminders or monthly promotions. Pinpointe can be set to send out emails on your contacts' birthdays or anniversaries.
Contact lists: Campaigner's contact management tools make it easy to keep your contact lists healthy. Its Custom Fields feature lets you effectively target, segment and track your subscribers. You can include the custom field on signup forms to let contacts select their interests based on the fields you've added, send targets campaigns on their birthdays, and identify premium customers based on their past purchases.
You can quickly import your existing contacts with Gmail, Salesforce or another email program you use. You have the option to place signup forms on your website.
Deliverability: Campaigner has an in-house email delivery team to ensure your email lands in the right inboxes. Other deliverability tools include authentication standards, feedback loop subscription and complaint data analysis, comprehensive unsubscribe management, and CAN-SPAM compliance functionality.
Email editor: Campaigner's full email editor has a variety of features, including tables, personalization options and templates. You can edit and create emails with its editor, in HMTL or with plain text. If you're unsure how to create a professional-looking email, you can watch Campaigner's video tutorials to learn how to use its tools to best effect.
Email templates: Campaigner has more than 900 professionally designed templates that you can personalize with its full email editor. All templates are designed and optimized to be viewed on mobile, tablet or desktop screens.
With these email templates, you can easily create an email that matches the look of your website, create plain text emails, build your own template inside the email editor, or use your own code with the HTML uploader.
Media library: Campaigner's media library is a dedicated storage space where you can upload, organize and manage assets such as images and templates. You can also edit your images within the library.
Segmentation: With Campaigner's segmentation tools, you can deliver targeted messages to the right people. You can segment email campaigns based on age, gender, company size, industry, purchase history, job title and more.
Campaigner's Ease of Use
Campaigner has a drag-and-drop editor and a library of more than 900 templates that you can easily customize with your own colors, images and logos. However, we couldn't try out the editor or other tools such as list management or automation, because you have to provide a credit card to start a free trial.
If you have questions, you can contact Campaigner support by live chat, phone or email. It also has an online search tool to help you find answers, along with a resource center that includes video tutorials, infographics, webinars and case studies.
While Campaigner does offer a free trial, it makes you sign up with your credit card. Your card won't be charged until you agree to a plan, but most email marketing solutions don't require a credit card for free trials. Some email marketing solutions also offer a free version of their services, but Campaigner doesn't.
Saige received her Bachelor's degree in Journalism and Telecommunications from Ball State University. She is the social media strategist for Business.com and Business News Daily. She also writes reviews and articles about social media. She loves reading and her beagle mix, Millie.
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this was intended to be some sort of fun self cartoony drawing but then it turned into shading practice i guess? and then i tied it up into something. was originally black /white/red but I thought the blue was kind of cool and I also don't feel right putting something very colorless in my gullacass galleries tbh lol.


jobopenings for the Posts of Officer, Clerks in United Bank of India.
Jobs Details :- Application are invited for the Posts of Officer, Clerks in United Bank of India.
Officer : 05 posts (Footballer -2, Cricketer -2, Table Tennis player -1).
Application Fee : Rs.400/- for Officer and Rs.200/- for Clerk (Rs.50/- for SC/ST/PWD) to be deposited through CBS at any of the Branches of United Bank of India by means of a Payment challan OR (ii) Through NEFT at any Bank branch.
How to Apply : Application Form complete in all respects should be sent by Registered / Speed post only in a closed envelope superscribed as ' APPLICATION FOR THE POST OF MALE SPORTS PERSON IN UNITED BANK OF INDIA' to The Assistant General Manager (H.R.M),United Bank Of India, Head Office, H.R.M. Department, United Tower,12th Floor,11 Hemanta Basu Sarani, Kolkata-700001 to reach latest by 29/09/2012.


Over 76 RV spaces available at 2 separate locations on Highway 97 East. With all your amenities included (full hookup, trash, and free WiFi), 30/50 amp, an on-site laundromat for your convenience, and monthly and weekly rates available, our RV Park has you covered. Clean and secure RV Park with on-site office and management. RV and Mobile Home rentals are available. Located in Pleasanton, Texas (Atascosa County) and the heart of the Eagle Ford Shale, Highway 97 East RV Park is one of the best places to stay if you have an RV or travel trailer.
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From San Antonio: Follow I-37 towards Corpus Christi and take Exit 109 toward Pleasanton/Floresville/TX-97. Continue west on TX-97 for 2.5 Miles and Hwy 97 RV Park East will be on your right. From Laredo: Follow I-35 towards San Antonio Turn right onto TX-85 East in Dilley. Turn left onto TX-97 E. Use any lane to turn left onto S Main St. Take a slight right onto TX-97 E. Continue for 4 miles and Hwy 97 RV Park East will be on your left.


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