text:
\section{Introduction}
\label{sec:introduction}

The standard picture of thermal plasmas associated with supernova remnants (SNRs) is that the state of the gas appears to be either an ionizing plasma (IP) for young or intermediate aged SNRs (e.g.\ Kepler's SNR, Kinugasa and Tsunemi 1999), or plasma in collisional ionization equilibrium (CIE) for old SNRs (e.g. 30 Dor C, Yamaguchi et al. 2009). However, recent X-ray observations have revealed several SNRs are in recombination-dominated phase (IC 443, Yamaguchi \etal\ 2009; W49B, Ozawa \etal\ 2009; G359.1$-$0.5, Ohnishi \etal\ 2011; W28, Sawada \& Koyama 2012; W44, Uchida \etal\ 2012; G346.6$-$0.2, Yamauchi \etal\ 2013). These recombining plasmas (RPs) have an ionization temperature ($T_{\mathrm{z}}$) higher than the electron temperature ($T_{\mathrm{e}}$); $T_{\mathrm{z}}$ is a useful parameter defined to be the temperature which would be required to ionize the plasma to the same degree assuming that the plasma is in CIE.
The discovery of RPs at SNRs requires us to modify the conventional evolution scenario of SNRs.

3C 391 (G31.9+0.0) is a bright Galactic SNR displaying diffuse X-ray emission close the center of its radio shell and is classified as a mixed-morphology SNR (MM-SNR) (Reynolds \& Moffett 1993).
The radio shell with a radius of \timeform{5'} has the shape of a partial circle in the northwest (NW) part and there is a faint extended structure in the southeast (SE) region.
This suggests a break-out morphology into a lower density region from the main SNR shell.
The detection of two OH maser spots at 1720~MHz from 3C 391 by Frail \etal\ (1996) indicates an interaction with molecular clouds. They also reported a possibly extended OH emission at the edge of the NW shell.
The velocity of two maser spots (105 and 110~km~s$^{-1}$) agrees with a previous study of H\emissiontype{I} absorption velocity (Radhakrishnan \etal\ 1972).
H\emissiontype{I} observations show that the distance to 3C 391 is between 7.2~kpc and 11.4~kpc, assuming a distance to the Galactic center of 8.5~kpc.
The surrounding molecular gas of 3C 391 can be traced by CO (J $=$ 1$\rightarrow$0) emission at velocities from 90 to 110~km~s$^{-1}$ (Wilner \etal\ 1998).
The results of the CO observation support the early expansion of 3C 391 inside a dense molecular cloud and the breakout of the blast wave to the SE region.

Knowledge of the astrophysical environment around SNRs is of great importance in order to reveal the origin of the RPs in the context of the SNR evolution.
Interestingly, most of the RP SNRs are MM-SNRs that interact with molecular clouds and are associated with bright GeV gamma-ray emissions (IC 443, Abdo \etal\ 2010a; W28, Abdo \etal\ 2010b; W49B, Abdo \etal\ 2010c; W44 Abdo \etal\ 2010d). While some young SNRs show bright TeV gamma-rays (RX J1713.7-3946, Aharonian \etal\ 2004), middle-aged SNRs are usually found to be predominantly emitting in the GeV energy band.
A significant excess (13$\sigma$) of GeV gamma-rays at the position of 3C 391 with Fermi-LAT was reported by Castro \& Slane (2010).
The radio rim of the NW region and the closer OH maser spot are \timeform{4'} apart from the GeV emission peak in the test statistic map.
The GeV emission associated with 3C 391 probably arises from accelerated cosmic rays in the shock-heated molecular clouds.
The interaction with the molecular gas and the association of the gamma-ray emission would be the keys for understanding the morphology and spectrum of the thermal plasmas in RP SNRs.

In this paper, we report on an X-ray study of SNR 3C 391, taking advantages of low and stable in-orbit background and high sensitivity of the Suzaku X-ray observatory (Mitsuda \etal\ 2007). We construct a model for the galactic background emission to complement the poor photon statistics, then we fit several plasma models to the X-ray spectrum of 3C 391. Our observation data is a part of the Suzaku Key Project to search for RPs in galactic SNRs. Section 2 describes the observation and data reductions and Section 3 presents the data analysis. Then, we interpret our results in Section 4 and conclude in Section 5.

\section{Observations and Data Reductions}
\label{sec:observation}

We observed SNR 3C 391 for an exposure time of 100 ks with the Suzaku satellite in 2010 October 22--24 during the AO5 cycle.
This observation was performed as one of the Key Project observations aimed at systematic search for RPs.
The pointing position was ($\alpha_{2000}$, $\delta_{2000}$) = (282.3812, $-$0.9417).
The observation instrument we used is the X-ray Imaging Spectrometer (XIS; Koyama \etal\ 2007), X-ray charge coupled device (CCD) cameras on the focal plane of the X-Ray Telescope (XRT; Serlemitsos \etal\ 2007). XIS\,0 and 3 are front-illuminated (FI) CCDs, and XIS\,1 is a back-illuminated (BI) CCD.
The XIS was operated with the normal-clocking, full-frame mode.
Since in-orbit radiation damage has degraded the charge transfer efficiency of the XIS, the spaced-row charge injection technique is applied for the XIS.

We reprocessed the XIS data with the latest calibration results instead of using the cleaned events.
We used the HEADAS software of version 6.13 (Suzaku software of version 20). The calibration database (CALDB) released on 2013 March was used for data processing.
We adopted standard event selection criteria for Suzaku XIS data processing. We excluded events in the intervals of the South Atlantic Anomaly, low-Earth elevation angles less than 5 degrees and the day earth elevation angle less than 20 degrees.
After the data screening, the effective exposure time is about 99.4~ks.
The data of the two editing mode, 3$\times$3 and 5$\times$5 pixel events, were combined, and then we removed flickering and hot pixels of the XIS.

\section{Analysis and Results}
\label{sec:analysis}
\subsection{X-ray Image}
X-ray diffuse emission is clearly detected in the central region of the remnant and is encompassed by the radio rim in the NW.
Figure~\ref{fig:image XIS3} shows an X-ray image of 3C 391 (XIS\,3 only), after correcting the vignetting effect and subtracting the instrumental background (the so-called non X-ray background, or NXB). The NXB was estimated by using xisnxbgen (Tawa \etal\ 2008).
\begin{figure}[htbp]
\begin{center}
\includegraphics[width=7cm]{figure/figure1.eps}
\caption{
NXB-subtracted XIS\,3 image of 3C 391 after the correction of vignetting effect. The energy bands are 0.8--1.7~keV (red), 1.8--3.0~keV (green) and 3.0--5.0~keV (blue). The solid and dashed lines indicate the source regions (NW and SE) and background region, respectively. Contours show a flux map of 1.4~GHz by VLA (Condon et al. 1998). Locations of OH masers are plotted with the magenta crosses (Frail \etal\ 1996). Photons in 8 $\times$ 8 pixels (\timeform{8'.32} $\times$ \timeform{8'.32}) were summed and smoothed with a Gaussian kernel of $\sigma = \timeform{2.6'}$.
}
\label{fig:image XIS3}
\end{center}
\end{figure}

The northwest (NW) region associated with the radio rim has harder X-rays than the southeast (SE) region.
It indicates the difference of the thermal plasma or circumstellar matters between those regions.
We thus divided the image into two regions: the NW and SE region.

\subsection{Background Estimation}

3C 391 is located on the Galactic plane, and hence the major background component is the Galactic ridge X-ray emission (GRXE), whose X-ray flux strongly depends on the position (e.g. Uchiyama \etal\ 2011, 2013). Since the photon statistics of the background region (surrounding region of 3C 391 in the same XIS field) is not good enough due to the limited exposure time and the effective area, subtracting the background data from the source data results in large statistical errors in the SNR spectrum. We therefore constructed a background model for the GRXE.  We extracted the background spectrum from the region excluding 3C 391 in the same field of view, and fitted the GRXE model compiled by Uchiyama \etal\ (2013) to the spectrum.
In this background region, a few percent level of photon contamination from 3C 391, which is due to the leakage of the XRT point spread function into the background region, cannot be neglected.

\subsubsection{Phenomenological Model Fit}
In order to construct the background model, we need to make phenomenological models both for the source and the background regions.
We extracted spectra from the whole 3C 391 region and the background region after subtracting the NXB.
After the vignetting correction, we subtracted the background spectrum from the 3C 391 spectrum.
The redistribution matrix file (RMF) and the ancillary response file (ARF) were created by xisrmfgen and xissimarfgen, respectively (Ishisaki \etal\ 2007).
We used the spectral analysis software XSPEC version 12.8.1 (Arnaud 1996).
We simultaneously fitted all the XIS\,0, 1, and 3 data with a single model. The energy band from 1.7 to 1.8~keV were ignored because of the calibration uncertainty around the Si K edge.

We then modeled the spectra by using a phenomenological model: the continuum X-ray emission is described by bremsstrahlung with temperature of $kT_{\mathrm{b}}$ and line emissions from various ionized atoms are given by Gaussian lines. The interstellar photoelectric absorption was estimated using the cross sections by Morrison and McCammon (1983) with H\emissiontype{I} column density $N_{\mathrm{H}}$.
This phenomenological model successfully reproduces the data ($\chi^2 =$ 404.01/307). Figure~\ref{fig:spec phenom} and table~\ref{tbl:par phenom} show the best-fit spectrum and parameters, respectively.

\begin{figure}[htbp]
\begin{center}
\includegraphics[width=7cm]{figure/figure2.eps}
\caption{X-ray spectrum of 3C 391 with the best-fit phenomenological model (solid line). Only a merged spectrum of
FI CCDs are shown for visibility. The dash line shows bremsstrahlung emission and the dotted lines correspond to atomic line emissions.}
\label{fig:spec phenom}
\end{center}
\end{figure}

\begin{table}[htbp]
\caption{Parameters of the phenomenological model.$^*$}
\label{tbl:par phenom}
\begin{center}
\begin{tabular}{lccc}
\hline

Parameter & \multicolumn{2}{c}{bremsstrahlung} \\ \hline
$N_{\mathrm{H}}$ (10$^{22}$~cm$^{-2}$) & \multicolumn{2}{c}{1.90$\pm$0.05} \\
$kT_{\mathrm{b}}$ (keV) & \multicolumn{2}{c}{0.671$\pm$0.014} \\ \hline
Emission line & energy (keV)$^\dag$ & intensity$^\ddag$  \\ \hline
Ne~\emissiontype{X}~Ly$\alpha$ & 1.022 & 11$\pm$10\\
Ne~\emissiontype{X}~Ly$\beta$ & 1.211 & 23$\pm$8 \\
Mg~\emissiontype{XI}~K$\alpha$ & 1.341$\pm$0.001 & 103$\pm$9 \\
Mg~\emissiontype{XII}~Ly$\alpha$ & 1.472 & 14.7$\pm$2.6 \\
Mg~\emissiontype{XI}~K$\beta$ & 1.579 & 7.1$\pm$1.9 \\
Si~\emissiontype{XIII}~K$\alpha$ & 1.850$\pm$0.002 & 90$\pm$3 \\
Si~\emissiontype{XIV}~Ly$\alpha$ & 2.006 & 3.6$\pm$0.8 \\
Si~\emissiontype{XIII}~K$\beta$ & 2.183 & 3.2$\pm$0.5 \\
S~\emissiontype{XV}~K$\alpha$ & 2.451$\pm$0.002 & 15.9$\pm$0.6 \\
S~\emissiontype{XVI}~Ly$\alpha$ & 2.621 & 1.1$\pm$0.4 \\
S~\emissiontype{XV}~K$\beta$ & 2.877 & 1.3$\pm$0.3 \\
Ar~\emissiontype{XVII}~K$\alpha$ & 3.107 & 1.02$\pm$0.24 \\
Ca~\emissiontype{XIX}~K$\alpha$ & 3.903 & 0.16$\pm$0.13 \\ \hline
$\chi^2$/d.o.f & \multicolumn{2}{c}{404.01/307} \\ \hline

\end{tabular}
\end{center}
$^*$ The uncertainties are the 90\% confidence range. \\
$^\dag$ The centroid energies of strong K$\alpha$ lines are free because they are fundamentally shifted by the contribution of another faint emission lines. \\
$^\ddag$ The units are 10$^{-5}$~photons~cm$^{-2}$~s$^{-1}$.
\end{table}

\subsubsection{Construction of the Background Model}
\label{sec:bgdmodel}

To make the GRXE model in the 3C 391 region, we fitted a composite model consisting of the GRXE, the cosmic X-ray background (CXB) and the contamination of 3C 391 spectrum to the NXB-subtracted background spectrum.
For the CXB, we used a power-law function with a photon index 1.4, which has a flux of 8.2 $\times$ 10$^{-7}$~photons~cm$^{-2}$~s$^{-1}$~arcmin$^{-2}$~keV$^{-1}$ at 1~keV (Kushino \etal\ 2002).  For the contamination spectrum, we used the phenomenological model given in the previous section (table 1) with the normalization as a free parameter.
Uchiyama \etal\ (2013) composed the GRXE with a foreground plasma (FG), a low temperature plasma (LP) and a high temperature plasma (HP). All these models are thin thermal plasmas in CIE, whose temperatures are designated as $kT_{\mathrm FG}$, $kT_{\mathrm LP}$ and $kT_{\mathrm HP}$, respectively.  We used the APEC model by Smith \etal\ (2001).  Metal abundances were taken relative to the solar values (Anders and Grevesse 1989). The GRXE also includes a cold matter (CM) emission with neutral iron line (6.4~keV) of equivalent width $\sim450$~eV. Thus the GRXE model is given by;
\begin{equation}
A_{\mathrm{FG}} \times {\mathrm{FG}} + A_{\mathrm{GRXE}} \times ({\mathrm{LP + HP + CM}}) + A_{\mathrm{CXB}} \times {\mathrm{CXB}},
\end{equation}
where $A_{\mathrm{FG}}$ and $A_{\mathrm{GRXE}}$ are absorptions by the Galactic H\emissiontype{I} with column densities $N_{\mathrm{H}}$ for the foreground plasma and GRXE components, respectively. An interstellar absorption of CXB ($A_{\mathrm{CXB}}$) was taken to be twice of $A_{\mathrm{GRXE}}$.  Following  the result of Uchiyama \etal\ (2013), $A_{\mathrm{FG}}$ and $kT_{\mathrm{FG}}$ were fixed to be $0.56\times10^{22}$~cm$^{-2}$ and 0.59~keV, respectively.  Although the foreground plasma has another CIE component with a temperature of $kT \sim 0.09$~keV, we neglected this component because no significant contribution was expected in our energy range.
Figure~\ref{fig:spec background} shows the background spectrum with the best-fit background model including contamination spectrum. The best-fit parameters of the GRXE are given in table~\ref{tbl:par background}.

\begin{figure}[htbp]
\begin{center}
\includegraphics[width=7cm]{figure/figure3.eps}
\caption{NXB-subtracted spectrum extracted from the background region (black crosses). The best-fit model is shown with the solid line. For visibility, only merged FI data are displayed. The dash lines show the background components of FG (cyan), LP (green), and HP (blue). The magenta and orange lines shows Fe\emissiontype{I}~K$\alpha$ and CXB, respectively. The contamination spectrum from 3C 391 is shown by the red line.}
\label{fig:spec background}
\end{center}
\end{figure}

\begin{table}[htbp]
\caption{Fitting parameters of the background region$^*$}
\begin{center}
\begin{tabular}{ccc}
\hline

Parameter & LP & HP \\ \hline

$N_{\mathrm{H}}$ (10$^{22}$~cm$^{-2}$) & \multicolumn{2}{c}{ 1.13 $\pm$ 0.10 } \\
$kT$ (keV) & $0.87^{+0.05}_{-0.06}$ & $6.7^{+1.5}_{-1.2}$ \\
Abundance (solar) & $0.35^{+0.22}_{-0.13}$ & $0.78^{+0.36}_{-0.21}$ \\ \hline
$f_{6.4}$$^\dag$ & \multicolumn{2}{c}{ 1.5 $\pm$ 1.1 } \\ \hline
$\chi^2$ / d.o.f & \multicolumn{2}{c}{ 458.73/312 } \\ \hline

\end{tabular}
\end{center}
$^*$ The uncertainties are the 90\% confidence range. \\
$^\dag$Observed photon flux of 6.4~keV in units of 10$^5$~photons~cm$^{-2}$~s$^{-1}$.
\label{tbl:par background}
\end{table}

\subsection{Model Fits to the Whole 3C 391 Spectrum}

We fitted several plasma models to the NXB-subtracted spectrum in the entire region of 3C 391. The GRXE model function determined in the previous section was included in the model fitting.
The abundances of Ne, Mg, Al, Si, S, Ar, Ca and Fe were free parameters.
We first tried the APEC model in the XSPEC package, a single-temperature ($kT$) optically thin thermal plasma model in CIE state.
This model is rejected with a large $\chi^2$ / d.o.f value (565.83/315).

One of the most prominent residuals is the excess below  $\sim$1.5~keV. We therefore added another APEC model with metal abundances treated as free parameters. The best-fit metal abundances were all consistent with 1 solar.  We hence fixed all the  abundances at 1 solar.
Then the fit is improved  to $\chi^2$ / d.o.f $=$ 397.51/313 (1.27).

In the atomic database of the current plasma codes, the higher Rydberg series of Fe-L lines ($\sim$1.2~keV) are incomplete (Brickhouse \etal\ 2000). If we add a $\sim$1.2 keV Gaussian line, $\chi^2$ / d.o.f is well improved from $\sim$1.27 to $\sim$1.25. The best-fit spectrum and parameters are given in figure 4 and table 3 (left column).

This two-temperature CIE model still leaves significant residuals at Si\emissiontype{XIV}~Ly$\alpha$ line (2.006~keV), hump-like feature at $\sim2.5$~keV and a hint of excess at 6.4 keV.  The data excess at the 2.5 keV bump above the applied model is $2.6\pm0.7 \times 10^{-3}$~counts~s$^{-1}$ (2.4--2.8~keV).  In the background spectrum, the data excess in the 2.4--2.8~keV band is negative and as small as $0.32\pm0.19 \times 10^{-3}$~counts~s$^{-1}$.
Thus the excess at 2.5 keV in the SNR spectrum, after the background subtraction, is not an artifact due to the background subtraction, but is a real structure. Since the bump energy of $\sim2.5$~keV corresponds to S\emissiontype{XVI}~Ly$\alpha$ line (2.623~keV) and the edge of radiative recombination continuum (RRC) of He-like Si (2.666 keV; Yamaguchi \etal\ 2009), this is likely due to a recombining plasma (e.g. Sawada and Koyama 2012).
We thus applied an NEIJ model in the SPEX version 2.03.03 (Kaastra \etal\ 1996) for the high temperature component.
This model describes a transition plasma that initially in the CIE state with the temperature $kT_1$ then only the electron temperature dropped to $kT$.  The recombination phase is given by the parameter $n_{\mathrm{e}}t$, where $n_{\mathrm{e}}$ and $t$ are the number density of electrons and the elapsed time after the electron cooling, respectively.

The fit is largely improved from the two-temperature CIE model.  As is shown in figure~\ref{fig:spec}, the Si\emissiontype{XIV}~Ly$\alpha$ line (2.006~keV) and hump-like feature at $\sim2.5$~keV have disappeared, even though a hint of excess at 6.4 keV is still remained.
The $\chi^2$ / d.o.f becomes almost acceptable level of 355.14/315 $\sim$ 1.13. The best-fit parameters are summarized in table~\ref{tbl:par all} (right column).

\begin{figure*}[htbp]
\begin{center}
\includegraphics[width=7cm]{figure/figure4a.eps}
\includegraphics[width=7cm]{figure/figure4b.eps}
\caption{NXB subtracted spectra of 3C 391 with the best-fit models and the residuals (lower panel) of the APEC+APEC model (a) and CIE+NEIJ model (b). For visibility, only merged FI spectrum is displayed. The solid and dashed lines correspond to the high and low temperature plasma models. The background model and the Gaussian functions are shown with the dashed and dash-dotted lines, respectively.}
\label{fig:spec}
\end{center}
\end{figure*}

\begin{table}[htbp]
\caption{Best-fit parameters of the whole region$^*$}
\begin{center}
\begin{tabular}{ccccc}
\hline

 & \multicolumn{2}{c}{CIE Plasma}  & \multicolumn{2}{c}{Recombining Plasma} \\ \hline
Parameter & CIE & CIE & CIE & NEIJ \\ \hline
$N_{\mathrm{H}}$ (10$^{22}$~cm$^{-2}$) &  \multicolumn{2}{c}{2.88$\pm$0.08} &  \multicolumn{2}{c}{3.13$^{+0.14}_{-0.12}$} \\

$VEM$$^\dag$ (10$^{60}$~cm$^{-3}$) & 3.2$^{+2.3}_{-0.8}$ & 0.092$^{+0.011}_{-0.015}$ & 2.8$^{+1.4}_{-0.9}$ & 0.18$^{+0.03}_{-0.05}$ \\
$kT_1$ (keV) & -- & -- & -- & 1.8$^{+1.6}_{-0.6}$ \\
$kT$ (keV) & 0.172$^{+0.006}_{-0.017}$ & 0.597$^{+0.011}_{-0.008}$ & 0.170$^{+0.009}_{-0.008}$ & 0.495$\pm$0.015  \\
$n_{\mathrm{e}} t$ (10$^{11}$~cm$^{-3}$~s) & -- & -- & -- & 14.0$^{+1.5}_{-2.2}$  \\ \hline
Abundance (solar) \\ \hline
Ne & & 1.9$^{+1.0}_{-0.7}$ & & 0.7$^{+1.1}_{-0.4}$ \\
Mg & & 0.80$^{+0.18}_{-0.13}$ & & 0.66$^{+0.30}_{-0.12}$ \\
Al & & 0.8$\pm$0.3 & & 0.4$\pm$0.3 \\
Si & & 0.96$^{+0.17}_{-0.11}$ & & 0.82$^{+0.30}_{-0.12}$ \\
S & 1(fix) & 0.85$^{+0.16}_{-0.10}$ & 1(fix) & 0.81$^{+0.31}_{-0.11}$ \\
Ar & & 0.61$^{+0.17}_{-0.14}$ & & 0.65$^{+0.25}_{-0.16}$ \\
Ca & & 1.0$\pm$0.5 & & 1.6$^{+0.8}_{-0.5}$ \\
Fe & & $<$0.13 &  & $<$0.05 \\
others & & 1(fix) & & 1(fix) \\ \hline
$\chi^2$ / d.o.f & \multicolumn{2}{c}{389.68/311} & \multicolumn{2}{c}{355.14/315} \\ \hline
\end{tabular}
\end{center}
$^*$ The uncertainties are the 90\% confidence range. \\
$^\dag$ Volume emission measure $\int n_{\mathrm{e}} n_{\mathrm{p}} \mathrm{d}V$ at the distance of 8~kpc, where $n_{\mathrm{e}}$, $n_{\mathrm{p}}$ and $V$ are the electron and proton number densities (cm$^{-3}$) and the emitting volume (cm$^{3}$), respectively.\\
\label{tbl:par all}
\end{table}

Since the Chandra observation shows that the spectra of 3C 391 has spatial variations with many NEI plasmas (Chen \etal\ 2004), we examine the excess at around 2.5~keV in the context of a composite plasma model. We made a composite model including all NEI plasmas resolved by Chen \etal\ 2004. Their emission measures were fixed to their individual values. The ionization timescales determined by Chen \etal\ 2004 were fixed, and other timescales were free. $N_{\mathrm{H}}$ and abundances were free parameters. We also added the CIE plasma model with a low temperature ($<$0.2~keV).
This composite model gives the best-fit reduced $\chi^2$ of 1.47, leaving the excess of $\sim$2.5~keV of $2.1\pm0.7 \times 10^{-3}$~counts~s$^{-1}$ (2.4--2.8~keV).
Also the excess of 6.4 keV line does not disappear.
If we replace the major 2-NEI plasmas with high emission measures (each $\sim$20\% of the total) with a 1-RP model, the reduced $\chi^2$ value improves to 1.15.  Since the best-fit reduced $\chi^2$ for the multi-NEI+CIE+RP is not smaller than that of the CIE+RP model, we use the CIE+RP model as the best approximation for the SNR spectra, and proceed with the following analysis and discussion.

\subsection{Spatial Distribution of the Recombining Plasma}

In figure~\ref{fig:image XIS3}, we can see significant difference between the NW and SE regions.  We therefore analyzed the NW and SE spectra separately using the same model as was applied to the spectrum of the entire region of 3C 391.

The fit for the NW and SE regions are marginally acceptable with $\chi^2/d.o.f$ of 333/275=1.21, and 306/266=1.15, respectively. However, we find no significant spectral differences except the possible presence of the 6.4 keV line in NW of which the significance level is $\sim 2.4 \sigma$ and a slightly larger $N_{\mathrm{H}}$ in SE.
Figure~\ref{fig:spec dist} (a) and (b) show the results of the NW and SE regions, respectively. The best-fit parameters of each region are shown in table~\ref{tbl:par dist}.

\begin{figure*}[htbp]
\begin{center}
\includegraphics[width=7cm]{figure/figure5a.eps}
\includegraphics[width=7cm]{figure/figure5b.eps}
\caption{NXB subtracted spectra of the SE region (a) and the NW region (b) with the best-fit models and these residuals.
For visibility, only merged FI spectrum is displayed. Solid and dashed lines correspond with NEIJ and CIE model.
The background model and Gaussian functions are shown with the dashed, doted dashed-dotted lines, respectively.}
\label{fig:spec dist}
\end{center}
\end{figure*}

\begin{table}[htbp]
\caption{Best-fit parameters of each regions$^*$}
\begin{center}
\begin{tabular}{ccccc}
\hline

& \multicolumn{2}{c}{SE}  & \multicolumn{2}{c}{NW} \\ \hline
Parameter & CIE & NEIJ & CIE & NEIJ \\ \hline
$N_{\mathrm{H}}$ (10$^{22}$~cm$^{-2}$) &  \multicolumn{2}{c}{3.05$^{+0.12}_{-0.14}$} &  \multicolumn{2}{c}{3.45$^{+0.15}_{-0.16}$} \\

$VEM$$^\dag$ (10$^{60}$~cm$^{-3}$) & 1.5$^{+0.7}_{-0.5}$ & 0.09$^{+0.02}_{-0.03}$ & 2.3$^{+0.4}_{-1.0}$ & 0.08$\pm$0.02 \\
$kT_1$ (keV) & -- & 1.6$^{+1.9}_{-0.5}$ & -- & 2.7$^{+\infty}_{-2.0}$ \\
$kT$ (keV) & 0.184$^{+0.012}_{-0.010}$ & 0.50$\pm$0.02 & 0.159$^{+0.014}_{-0.005}$ & 0.55$\pm$0.02  \\
$n_{\mathrm{e}} t$ (10$^{11}$~cm$^{-3}$~s) & -- & 14$^{+2}_{-3}$ & -- & 15$\pm$2  \\ \hline
Abundance (solar) \\ \hline
Ne & & 1.3$^{+1.9}_{-0.8}$ & & 0.5$^{+1.3}_{-0.4}$ \\
Mg & & 0.85$^{+0.51}_{-0.22}$ & & 0.56$^{+0.31}_{-0.17}$ \\
Al & & 0.6$^{+0.4}_{-0.5}$ & & 0.2$^{+0.4}_{-0.1}$ \\
Si & & 1.1$^{+0.6}_{-0.2}$ & & 0.62$^{+0.24}_{-0.10}$ \\
S & 1(fix) & 1.1$^{+0.6}_{-0.2}$ & 1(fix) & 0.59$^{+0.24}_{-0.12}$ \\
Ar & & 0.9$^{+0.5}_{-0.3}$ & & 0.32$^{+0.23}_{-0.18}$ \\
Ca & & 2.2$^{+1.3}_{-0.8}$ & & 0.5$^{+0.6}_{-0.4}$ \\
Fe & & $<$0.08 &  & $<$0.5 \\
others & & 1(fix) & & 1(fix) \\ \hline
$f_{6.4}$$^\ddag$ & \multicolumn{2}{c}{2.1$\pm$0.9} & \multicolumn{2}{c}{$<$0.5} \\ \hline
$\chi^2$ / d.o.f & \multicolumn{2}{c}{332.72/275} & \multicolumn{2}{c}{306.32/266} \\ \hline

\end{tabular}
\end{center}
$^*$ The uncertainties are the 90\% confidence range. \\
$^\dag$ Volume emission measure $\int n_{\mathrm{e}} n_{\mathrm{p}} \mathrm{d}V$ at the distance of 8~kpc, where $n_{\mathrm{e}}$, $n_{\mathrm{p}}$ and $V$ are the electron and proton number densities (cm$^{-3}$) and the emitting volume (cm$^{3}$), respectively.\\
$^\ddag$ The units are 10$^{-8}$~photons~cm$^{-2}$~s$^{-1}$~arcmin$^{-2}$. The uncertainties are the 1 $\sigma$ confidence range.  \\
\label{tbl:par dist}
\end{table}

\section{Discussion}
\label{sec:discussion}

The X-ray spectrum of 3C 391 is represented by two plasma models: a low temperature CIE and a high temperature RP. The CIE plasma is probably emitted by the ISM heated by the blast waves, because it has 1 solar abundances. The abundances of the  RP are given in figure~\ref{fig:mass}, together with some theoretical model of Ia (Iwamoto et al. 1999) and core-collapse supernova (CC SN; Woosely and Weaver 1995). Although the error is large, the abundance pattern except Fe is similar to a CC SN of progenitor mass of $\sim$15~\Mo.
Thus we regard that the RP has an ejecta origin from a CC SN of a $\sim$15~\Mo~progenitor star.
In Section 4.1, we discuss consistency of the observed data with this assumption.

The abundance of Fe in ejecta largely depends on the mass cut of the CC SN.
If a major fraction of Fe would be captured into a collapsed object (neutron star or black hole) in the case of 3C 391, a small abundance of Fe in the ejecta would be reasonable, unless the explosion is highly asymmetric as is  demonstrated by Yasumi et al. 2014.
Another possibility is that only a small fraction of the Fe-rich ejecta has been shocked by the reverse shock (Fe-rich ejecta are expected to be located at the very inner part of the remnant).
Since the Fe abundance estimated using the Fe-L lines only has a large uncertainty due to their incompleteness, we can not conclude why the abundance of Fe is lower than expected.

The recombination parameter ($n_{\mathrm{e}}t \sim 1.4 \times 10^{12}$~cm$^{-3}$~s) is the largest among any RP discovered so far in MM-SNRs
(Yamaguchi \etal\ 2009, 2012, Ozawa \etal\ 2009, Ohnishi \etal\ 2011, Sawada \& Koyama 2012, Uchida \etal\ 2012, Yamauchi \etal\ 2013).
\begin{figure}[htbp]
\begin{center}
\includegraphics[width=9cm]{figure/figure6.eps}
\caption{Best-fit metal abundances of 3C 391 relative to Si abundance as a function of atomic number. The dashed-dotted line shows Type Ia SN model (CDD1; Iwamoto et al. 1999). The solid and dashed lines represent CC SN models with progenitor masses of 15~\Mo and 40~\Mo, respectively (Woosley \& Weaver 1995).}
\label{fig:mass}
\end{center}
\end{figure}
The spectra of the SE and NW also show the RP. Since the extended OH emission reported in the NW region suggests the interaction with molecular clouds, the slightly higher $N_{\mathrm{H}}$ than the SE would be reasonable.
On the other hand, $n_{\mathrm{e}}t$ and $kT$ show no significant difference between the two regions.

We found a hint of line emission at 6.4 keV, Fe\emissiontype{I}~K$\alpha$  line at $2.4\sigma$ level from the SE region, and not from the NW region where the SNR interacts with molecular clouds.
However the SE region is coincident with OH masers. One possibility is that the  Fe\emissiontype{I}~K$\alpha$
line is due to low energy cosmic-ray electrons, which are preferentially made in the SE region.
The gyro radius of the lower energy electrons is extremely small, and hence diffusion
length is far smaller than the SNR size. The absence of the Fe \emissiontype{I}~K$\alpha$ line at the NW, where cool gas is denser than the SE, would be due to this limited diffusion length.
Deeper observations of hard X-ray will probably detect bremsstrahlung by low energy cosmic-rays interacting with molecular clouds.
In any case, the detection of Fe\emissiontype{I}~K$\alpha$ line is marginal, thus we need more detailed observations in the future.

\subsection{The abundances and mass of the Recombining Plasma}

The abundances and emission measure of RP given in table 3 are based on the H dominant plasma. We assume that the RP originates from an ejecta of $\sim$15\Mo~progenitor (figure~\ref{fig:mass}), which indicates super-solar abundances even for the light elements such as He, O and Ne. The estimations of emission measure and abundances of heavy elements largely depend on the abundances of He, O and Ne; large abundances
of these light elements enhance the continuum (mainly bremsstrahlung) flux, although the relative spectral shape is not affected because emission lines of He--Ne are absent in the relevant energy band of 1.2--7.0~keV.
We thus re-estimate the emission measure and abundances of heavy element assuming the light element mass distribution is the same as the progenitor star of 15\Mo.
The abundances of Mg--Ca relative to Si in the RP component do not change from the original H dominant plasma but the averaged abundance of Si--Fe relative to hydrogen becomes $\sim$15 solar, confirming its ejecta origin. The emission measure becomes $n_{\rm e} n_{\rm H} V f \sim 2.1^{+0.2}_{-1.7}\times10^{58}~d_8^2$~cm$^{-3}$, where $f$ and $d_8$ are a filling factor and the SNR distance in the unit of 8~kpc, respectively. The ratio of the electron to the atomic hydrogen densities is  $n_{\rm e}/n_{\rm H} = 1.5$  and the number ratio of all the elements to hydrogen is 2.0.
Adopting the source radii of $7d_8$~pc, the ejecta mass is estimated to be $\sim 40~f^{1/2}~d_8^{5/2}$~\Mo. As is seen in Figure 1 of Chen \etal\ 2004, filling factor would be very small, hence we assume $f$ is in the range of 0.3--0.1.  Then the ejecta mass is $\sim$ 10--25~\Mo. This value is consistent with the initial assumption that 3C 391 is a remnant of CC SN with a progenitor mass of $\sim$ 15\Mo.

The ionization age of the RP is estimated using $n_{\mathrm{e}} t$. The electron density $n_{\mathrm{e}}$ is $0.9f^{-1/2}d_8^{-1/2}$~cm$^{-3}$.
Then the elapsed time $t$ is $6.5\times10^3f^{-1/2}$ ($n_{\mathrm{e}}/0.9~\mathrm{cm}^{-3}$) years, which place this SNR as a rather old SNR.
If we assume a small filing factor, the age of $1.7 \times 10^4$ yr estimated by Chen \& Slane (2001) has a very similar value.

\subsection{Origin of the Recombining Plasma}

Several scenarios are proposed to explain the formation of RPs in SNRs.
One is the rapid electron cooling by the thermal conduction from cold matters around SNRs (Kawasaki \etal\ 2002) or the adiabatic rarefaction (Itoh and Masai 1989, Shimizu \etal\ 2012).  The other is the ionization by the suprathermal or non-thermal particles (Masai \etal\ 2002, Ohnishi \etal\ 2011) or the high energy photons (Kawasaki \etal\ 2002).
Therefore, the presence of RP in 3C 391 means that the plasma experienced the rapid electron cooling or extra-ionization.

We first discuss the electron cooling scenario.
If the electron cooling is due to thermal conduction, a timescale of the thermal conduction is
\begin{equation}
t_{\rm cond} \sim 1.5 \times 10^{5}~\left( \frac{n_e}{0.9~{\rm cm}^{-3}} \right) \left( \frac{l}{7~{\rm pc}} \right)^{2} \left( \frac{k T}{0.50~{\rm keV}} \right)^{-\frac{5}{2}} d_8~{\rm yr},
\end{equation}
where $l$ is the temperature gradient scale length (Kawasaki et al. 2002). This timescale is much longer than the estimated age of 3C 391, therefore the thermal conductivity is unlikely to produce the whole RP in 3C 391 of which the radius is about 7~pc.

Next scenario is rarefaction, which is the possible origin of the RP in W28 (Sawada \& Koyama 2012). If the progenitor of 3C 391 was a massive star with a strong stellar wind activity, there can be a dense circumstellar media (CSM) surrounding the ejecta. The blastwave breaking out of the shell can lead to rarefaction of the PI or near CIE plasma.
Thereafter the electron temperature can drop rapidly due to adiabatic expansion but the ionization states can stay more or less the same.
This scenario is supported by the fact that the recombination timescale is close to the putative age of 3C 391.
While Reynolds and Moffett (1993) estimated that the shell ``break-out" occurred at about 1600~yr after the supernova, the blast wave breaks out of the CSM at only $\sim$100~yr (Itoh and Masai 1989, Shimizu \etal\ 2012).
Since no significant spectral differences except the possible presence of a 6.4~keV line in the NW and a slightly larger $N_{\rm H}$ in the SE, we argue that the rarefaction of ejecta plasma was roughly symmetrical, unlike W49B as suggested by some models (e.g. Miceli et al 2010). Our results show that the RP of 3C 391 was produced by the ``break-out" from the CSM and evolved independently from the interstellar environment.
For 3C 391, we apply a model of an early phase break-out (Shimizu et al. 2012), while Zhou et al. 2011 proposed a later phase break-out for W49B.  This difference is due to their different circumstellar environments; 3C 391 would have a denser and more compact CSM compared to that of W49B.
Although the extra-ionization process could be an alternative interpretation, it is still impossible to identify the origin of RP with the present data alone. We hence encourage deeper observation of 3C 391.

\section{Conclusions}

We observed the middle-aged SNR 3C 391 with Suzaku for 100 ks.
We generated a background model for the GRXE and analyzed the X-ray spectrum of 3C 391.
Our conclusions are summarized below:

\begin{itemize}
\item The X-ray spectrum of 3C 391 is well described by a CIE+RP model. 3C 391 has the highest $n_{\mathrm{e}}t$ value among the RP SNRs ever discovered. This means the RP of 3C 391 approaches ionization equilibrium the most.
\item Estimated progenitor mass of $\sim$15~\Mo~roughly agrees with the X-ray emitting mass of the RP derived from the corrected emission measure. This means only the ejecta plasma is overionized.
\item The parameters of RP have no significant difference between the NW and SE regions. Thermal conduction is unlikely to be the origin of the RP at 3C 391.
The symmetrical evolution of RP is consistent with a rarefaction of the plasma in the early phase.
In order to draw a more conclusive picture we need deeper observations with more sensitive instruments, such as those to be onboard the ASTRO-H mission (Takahashi \etal\ 2010).
\item Our detailed analysis of the spectra of 3C 391 suggests a hint of Fe\emissiontype{I}~K$\alpha$ emission at 6.4 keV ($\sim 2.4\sigma$), which can be explained by the interaction with a molecular cloud.
\end{itemize}

\bigskip

The authors express  sincere thanks  to all the Suzaku team members.
This work is supported by JSPS Scientific Research grant number 24540229 (K.K.). et al.

redpajama_set_name: RedPajamaArXiv


text:
Golf Roundup : Lohr Gets Day Off but Still Leads by One at Las Vegas
From Times Wire Services
Bob Lohr, enjoying a rare Friday off, maintained his one-stroke lead as 71 players finished the delayed second round of the $1.45-million Las Vegas Invitational golf tournament.
Lohr concluded his round Thursday with a two-day total of eight-under-par 136 before wind gusts of more than 50 m.p.h. forced suspension of play.
When the second round resumed Friday, Curt Byrum, who was a stroke off the lead through 15 holes at Desert Inn, bogeyed No. 7 (his 16th) but birdied No. 9 to move back within one stroke of Lohr.
Peter Jacobsen, who shot a 66 at Desert Inn Thursday, was tied with Byrum at 137. Another shot back were Keith Clearwater, who shot a 70 Thursday at Spanish Trail, and Ben Crenshaw, who had a 69 Thursday at Desert Inn.
The third round will be played today; the field will be cut to the low 70 and ties, and the fourth, and now final, round will be contested Sunday. First prize in what originally was a five-round tourney is $250,000.
Greg Norman, who called Thursday's conditions at Spanish Trail the worst he has played in, finished with a 75 and was at 143.
Bobby Wadkins, winless in 14 years on the PGA Tour, began the second round at eight under par, one stroke ahead of Byrum and Mark O'Meara. He had a 79 at Spanish Trail and was at 143.
Kim Shipman shot a career-best seven-under-par 65 to take a three-shot lead in the first round of the LPGA's Crestar tournament at Suffolk, Va.
Shipman, who has yet to win in four years on the tour, needed only 27 putts in her round and was on track to tie the course record of 64, but she bogeyed her final hole on the 6,215-yard Portsmouth Sleepy Hole Golf Course.
Sherri Turner and Missie Berteotti were tied for second place at 68.
At 69 were Betsy King, Colleen Walker, Kathy Postlewait and defending champion Jody Rosenthal.
Bobby Nichols shot a four-under-par 68 for a one-stroke lead in the first round of the $250,000 Vantage at The Dominion seniors tournament in San Antonio, Tex.
Al Geiberger, Jim King and Walter Zembriski were tied for second place after shooting 69s.

redpajama_set_name: RedPajamaCommonCrawl


To use prepostseo Reverse Ip Domains Checker, Paste Domain name or IP Address in the input box given below and click on check reverse ip domains Button.
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text:
Q: Is it possible to manage calls on an iPhone? I just would like to know if it is possible (and if yes how) to manage receiving calls on iPhone ?
For example, send automatically a call to the voice message service by activating an "in-app option" (for example a game), in order to not to be disturb during the game !
Thanks for answer.

A: No, Apple doesn't provide public API to manage call thru the third party app.

redpajama_set_name: RedPajamaStackExchange


Start taking classes at EVO 24 FIT Centre and other studios!
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text:
The Vampire, film sorti en 1910
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Voir aussi

redpajama_set_name: RedPajamaWikipedia


text:
Motley Crue's Vince Neil Discusses Las Vegas Residency Challenge + 'The Dirt' Film
Karen Bliss
Karen Bliss Published: August 16, 2013
Motley.com
Motley Crue's second Las Vegas residency at the Hard Rock Hotel venue the Joint will be a little different than last time out with "a lot of cool stuff," frontman Vince Neil said in an interview with Vegas.com.
"Technology changes so rapidly and new stuff comes out all the time," explained Neil. "All of a sudden someone goes, look at this, and we go, 'Holy s--t, that's cool.' We have to outdo ourselves every time we put something new together. This one -- I don't know how we're going to top this one. There's some crazy stuff going on in this thing and just a lot of fire and smoke and monsters and all kinds of cool stuff."
Dubbed 'An Evening in Hell,' the 12-show residency kicks off Sept. 18 and runs until Oct. 6. Neil, who lives in Vegas, said, "Being able to, especially for me living here, pack a lunch and f---in' walk to work, you know? Basically, we're touring without having to really tour. It's great to play every night here at home for me and not have to be on a bus or an airplane."
For the set list, he added, "We'll dig a little deeper in our bag of songs and do a lot of stuff that we haven't done in many, many years."
Neil, who in earlier interviews had stopped talking about the long-awaited film on the band called 'The Dirt' (based on their book) because he was fed up with it never happening, also told the site that Motley Crue is now recording songs for the soundtrack and that the film will be out "in late winter, early spring of next year."
He maintains there will be a farewell tour, beginning in 2014.
Next: Nikki Sixx Selling Played Basses At Las Vegas Residency
Filed Under: Motley Crue, Vince Neil


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Explore how far you can travel by car, bus, bike and foot from 1120 Litton Avenue.
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The Nettle Creek School Corporation was seeking a new look and feel for their school's brand. They selected IG to give them a new brand position/tagline, corporate identity, brand anthem video and a responsive website. IG researched the school's history, especially pertaining to the consolidation of the 5 school districts. There were interviews conducted with faculty, students and Alumni, as well as a schoolwide parent survey.
behind. "Grow @ The Creek" was developed and embraced by the entire community.


Since we feel pretty confident about our hypothesis as to what happened, we now can move on to the final step of our root cause analysis; preventing the issue from reoccurring.
As we discussed in the beginning of our chapter, all useful root cause analysis reports include a plan of action. Sometimes, this plan of action is something to be performed immediately at the time of the issue. Sometimes, this plan is to be performed later as a long-term resolution.
For our issue, we are going to have both, immediate actions and long-term actions.


text:
package org.jetbrains.jps.incremental.artifacts.impl;

import com.intellij.openapi.diagnostic.Logger;
import com.intellij.openapi.util.Pair;
import com.intellij.openapi.util.Ref;
import com.intellij.openapi.util.io.FileUtil;
import com.intellij.openapi.util.text.StringUtil;
import com.intellij.util.ArrayUtil;
import com.intellij.util.graph.CachingSemiGraph;
import com.intellij.util.graph.DFSTBuilder;
import com.intellij.util.graph.GraphGenerator;
import com.intellij.util.graph.InboundSemiGraph;
import com.intellij.util.io.ZipUtil;
import org.jetbrains.annotations.NonNls;
import org.jetbrains.annotations.NotNull;
import org.jetbrains.annotations.Nullable;
import org.jetbrains.jps.api.GlobalOptions;
import org.jetbrains.jps.builders.BuildOutputConsumer;
import org.jetbrains.jps.builders.JpsBuildBundle;
import org.jetbrains.jps.builders.logging.ProjectBuilderLogger;
import org.jetbrains.jps.incremental.CompileContext;
import org.jetbrains.jps.incremental.FSOperations;
import org.jetbrains.jps.incremental.ProjectBuildException;
import org.jetbrains.jps.incremental.artifacts.ArtifactOutputToSourceMapping;
import org.jetbrains.jps.incremental.artifacts.IncArtifactBuilder;
import org.jetbrains.jps.incremental.artifacts.instructions.*;
import org.jetbrains.jps.incremental.messages.BuildMessage;
import org.jetbrains.jps.incremental.messages.CompilerMessage;
import org.jetbrains.jps.incremental.messages.ProgressMessage;

import java.io.*;
import java.util.*;
import java.util.jar.Attributes;
import java.util.jar.JarFile;
import java.util.jar.JarOutputStream;
import java.util.jar.Manifest;
import java.util.zip.ZipEntry;
import java.util.zip.ZipOutputStream;

public final class JarsBuilder {
  private static final Logger LOG = Logger.getInstance(JarsBuilder.class);
  private final Set<JarInfo> myJarsToBuild;
  private final CompileContext myContext;
  private Map<JarInfo, File> myBuiltJars;
  private final BuildOutputConsumer myOutputConsumer;
  private final ArtifactOutputToSourceMapping myOutSrcMapping;
  private final @Nullable Long buildDateInMillis;

  public JarsBuilder(Set<JarInfo> jarsToBuild, CompileContext context, BuildOutputConsumer outputConsumer,
                     ArtifactOutputToSourceMapping outSrcMapping) {
    myOutputConsumer = outputConsumer;
    myOutSrcMapping = outSrcMapping;
    DependentJarsEvaluator evaluator = new DependentJarsEvaluator();
    for (JarInfo jarInfo : jarsToBuild) {
      evaluator.addJarWithDependencies(jarInfo);
    }
    myJarsToBuild = evaluator.getJars();
    myContext = context;
    String buildDateInSeconds = context.getBuilderParameter(GlobalOptions.BUILD_DATE_IN_SECONDS);
    if (buildDateInSeconds == null) {
      buildDateInSeconds = System.getenv(GlobalOptions.BUILD_DATE_IN_SECONDS);
    }
    buildDateInMillis = buildDateInSeconds != null ? Long.valueOf(buildDateInSeconds) * 1000 : null;
  }

  public boolean buildJars() throws IOException, ProjectBuildException {
    myContext.processMessage(new ProgressMessage(JpsBuildBundle.message("progress.message.building.archives")));

    final JarInfo[] sortedJars = sortJars();
    if (sortedJars == null) {
      return false;
    }

    myBuiltJars = new HashMap<>();
    try {
      for (JarInfo jar : sortedJars) {
        myContext.checkCanceled();
        buildJar(jar);
      }

      myContext.processMessage(new ProgressMessage(JpsBuildBundle.message("progress.message.copying.archives")));
      copyJars();
    }
    finally {
      deleteTemporaryJars();
    }

    return true;
  }

  private void deleteTemporaryJars() {
    for (File file : myBuiltJars.values()) {
      FileUtil.delete(file);
    }
  }

  private void copyJars() throws IOException {
    for (Map.Entry<JarInfo, File> entry : myBuiltJars.entrySet()) {
      File fromFile = entry.getValue();
      final JarInfo jarInfo = entry.getKey();
      DestinationInfo destination = jarInfo.getDestination();
      if (destination instanceof ExplodedDestinationInfo) {
        File toFile = new File(FileUtil.toSystemDependentName(destination.getOutputPath()));
        FileUtil.rename(fromFile, toFile);
      }
    }
  }

  private JarInfo @Nullable [] sortJars() {
    final DFSTBuilder<JarInfo> builder = new DFSTBuilder<>(GraphGenerator.generate(CachingSemiGraph.cache(new JarsGraph())));
    if (!builder.isAcyclic()) {
      Map.Entry<JarInfo, JarInfo> dependency = builder.getCircularDependency();
      String message = JpsBuildBundle.message("build.message.cannot.build.circular.dependency.found.between.0.and.1", dependency.getKey().getPresentableDestination(),
                                              dependency.getValue().getPresentableDestination());
      myContext.processMessage(new CompilerMessage(IncArtifactBuilder.getBuilderName(), BuildMessage.Kind.ERROR, message));
      return null;
    }

    JarInfo[] jars = myJarsToBuild.toArray(new JarInfo[0]);
    Arrays.sort(jars, builder.comparator());
    jars = ArrayUtil.reverseArray(jars);
    return jars;
  }

  private void buildJar(final JarInfo jar) throws IOException {
    final String emptyArchiveMessage =
      JpsBuildBundle.message("build.message.archive.0.doesn.t.contain.files.so.it.won.t.be.created", jar.getPresentableDestination());
    if (jar.getContent().isEmpty()) {
      myContext.processMessage(new CompilerMessage(IncArtifactBuilder.getBuilderName(), BuildMessage.Kind.WARNING, emptyArchiveMessage));
      return;
    }

    myContext.processMessage(new ProgressMessage(JpsBuildBundle.message("progress.message.building.jar.0", jar.getPresentableDestination())));
    File jarFile = FileUtil.createTempFile("artifactCompiler", "tmp");
    myBuiltJars.put(jar, jarFile);

    FileUtil.createParentDirs(jarFile);
    final String targetJarPath = jar.getDestination().getOutputFilePath();
    List<String> packedFilePaths = new ArrayList<>();
    Pair<Manifest, File> manifestData = loadManifest(jar, packedFilePaths);
    Manifest manifest = manifestData != null ? manifestData.first : null;
    if (manifest != null && manifest.getMainAttributes().getValue(Attributes.Name.MANIFEST_VERSION) == null &&
        manifest.getMainAttributes().getValue(Attributes.Name.SIGNATURE_VERSION) == null && !manifest.getMainAttributes().isEmpty()) {
      String messageText = JpsBuildBundle.message("build.message.manifest.file.0.included.into.archive.does.not.contain.required.attribute", manifestData.second,
                                                  jar.getPresentableDestination(), Attributes.Name.MANIFEST_VERSION);
      myContext.processMessage(new CompilerMessage(IncArtifactBuilder.getBuilderName(), BuildMessage.Kind.WARNING, messageText));
    }
    BufferedOutputStream outputStream = new BufferedOutputStream(new FileOutputStream(jarFile));
    JarOutputStream jarOutputStream = new JarOutputStream(outputStream);

    final Set<String> writtenPaths = new HashSet<>();
    try {
      if (manifest != null) {
        addManifestEntry(jarOutputStream, manifest, writtenPaths);
      }

      for (Pair<String, Object> pair : jar.getContent()) {
        final String relativePath = pair.getFirst();
        if (pair.getSecond() instanceof ArtifactRootDescriptor) {
          final ArtifactRootDescriptor descriptor = (ArtifactRootDescriptor)pair.getSecond();
          final int rootIndex = descriptor.getRootIndex();
          if (descriptor instanceof FileBasedArtifactRootDescriptor) {
            addFileToJar(jarOutputStream, jarFile, descriptor.getRootFile(), descriptor.getFilter(), relativePath, targetJarPath, writtenPaths,
                         packedFilePaths, rootIndex);
          }
          else {
            final String filePath = FileUtil.toSystemIndependentName(descriptor.getRootFile().getAbsolutePath());
            packedFilePaths.add(filePath);
            myOutSrcMapping.appendData(targetJarPath, rootIndex, filePath);
            extractFileAndAddToJar(jarOutputStream, (JarBasedArtifactRootDescriptor)descriptor, relativePath, writtenPaths);
          }
        }
        else {
          JarInfo nestedJar = (JarInfo)pair.getSecond();
          File nestedJarFile = myBuiltJars.get(nestedJar);
          if (nestedJarFile != null) {
            addFileToJar(jarOutputStream, jarFile, nestedJarFile, SourceFileFilter.ALL, relativePath, targetJarPath, writtenPaths,
                         packedFilePaths, -1);
          }
          else {
            LOG.debug("nested JAR file " + relativePath + " for " + jar.getPresentableDestination() + " not found");
          }
        }
      }

      if (writtenPaths.isEmpty()) {
        myContext.processMessage(new CompilerMessage(IncArtifactBuilder.getBuilderName(), BuildMessage.Kind.WARNING, emptyArchiveMessage));
        return;
      }

      final ProjectBuilderLogger logger = myContext.getLoggingManager().getProjectBuilderLogger();
      if (logger.isEnabled()) {
        logger.logCompiledPaths(packedFilePaths, IncArtifactBuilder.BUILDER_ID, "Packing files:");
      }
      myOutputConsumer.registerOutputFile(new File(targetJarPath), packedFilePaths);

    }
    finally {
      if (writtenPaths.isEmpty()) {
        try {
          jarOutputStream.close();
        }
        catch (IOException ignored) {
          try {
            outputStream.close();
          }
          catch (IOException ignored1) {
          }
        }
        FileUtil.delete(jarFile);
        myBuiltJars.remove(jar);
      }
      else {
        try {
          jarOutputStream.close();
        }
        catch (IOException e) {
          try {
            outputStream.close();
          }
          catch (IOException ignored) {
          }
          FileUtil.delete(jarFile);
          String messageText = JpsBuildBundle.message("build.message.cannot.create.0.1", jar.getPresentableDestination(), e.getMessage());
          myContext.processMessage(new CompilerMessage(IncArtifactBuilder.getBuilderName(), BuildMessage.Kind.ERROR, messageText));
          LOG.debug(e);
        }
      }
    }
  }

  @Nullable
  private Pair<Manifest, File> loadManifest(JarInfo jar, List<? super String> packedFilePaths) throws IOException {
    for (Pair<String, Object> pair : jar.getContent()) {
      if (pair.getSecond() instanceof ArtifactRootDescriptor) {
        final String rootPath = pair.getFirst();
        if (!JarFile.MANIFEST_NAME.startsWith(rootPath)) {
          continue;
        }
        final String manifestPath = JpsArtifactPathUtil.trimForwardSlashes(JarFile.MANIFEST_NAME.substring(rootPath.length()));
        final ArtifactRootDescriptor descriptor = (ArtifactRootDescriptor)pair.getSecond();
        if (descriptor instanceof FileBasedArtifactRootDescriptor) {
          final File manifestFile = new File(descriptor.getRootFile(), manifestPath);
          if (manifestFile.exists()) {
            final String fullManifestPath = FileUtil.toSystemIndependentName(manifestFile.getAbsolutePath());
            packedFilePaths.add(fullManifestPath);
            try (FileInputStream stream = new FileInputStream(manifestFile)) {
              return new Pair<>(createManifest(stream, manifestFile), manifestFile);
            }
          }
        }
        else {
          final Ref<Manifest> manifestRef = Ref.create(null);
          ((JarBasedArtifactRootDescriptor)descriptor).processEntries(new JarBasedArtifactRootDescriptor.EntryProcessor() {
            @Override
            public void process(@Nullable InputStream inputStream, @NotNull String relativePath, ZipEntry entry) throws IOException {
              if (manifestRef.isNull() && relativePath.equals(manifestPath) && inputStream != null) {
                try (InputStream stream = inputStream) {
                  manifestRef.set(createManifest(stream, descriptor.getRootFile()));
                }
              }
            }
          });
          if (!manifestRef.isNull()) {
            return new Pair<>(manifestRef.get(), descriptor.getRootFile());
          }
        }
      }
    }
    return null;
  }

  @Nullable
  private Manifest createManifest(InputStream manifestStream, File manifestFile) {
    try {
      return new Manifest(manifestStream);
    }
    catch (IOException e) {
      myContext.processMessage(new CompilerMessage(IncArtifactBuilder.getBuilderName(), BuildMessage.Kind.ERROR,
                                                   JpsBuildBundle.message("build.message.cannot.create.manifest.mf.from.0.1",
                                                                          manifestFile.getAbsolutePath(), e.getMessage())));
      LOG.debug(e);
      return null;
    }
  }

  private void extractFileAndAddToJar(final JarOutputStream jarOutputStream, final JarBasedArtifactRootDescriptor root,
                                      final String relativeOutputPath, final Set<? super String> writtenPaths)
    throws IOException {
    final long timestamp = buildDateInMillis != null ? buildDateInMillis : FSOperations.lastModified(root.getRootFile());
    root.processEntries(new JarBasedArtifactRootDescriptor.EntryProcessor() {
      @Override
      public void process(@Nullable InputStream inputStream, @NotNull String relativePath, ZipEntry entry) throws IOException {
        String pathInJar = addParentDirectories(jarOutputStream, writtenPaths, JpsArtifactPathUtil
          .appendToPath(relativeOutputPath, relativePath));

        if (inputStream == null) {
          if (!pathInJar.endsWith("/")) {
            addDirectoryEntry(jarOutputStream, pathInJar + "/", writtenPaths);
          }
        }
        else if (writtenPaths.add(pathInJar)) {
          ZipEntry newEntry = new ZipEntry(pathInJar);
          newEntry.setTime(timestamp);
          if (entry.getMethod() == ZipEntry.STORED) {
            newEntry.setMethod(ZipEntry.STORED);
            newEntry.setSize(entry.getSize());
            newEntry.setCrc(entry.getCrc());
          }
          jarOutputStream.putNextEntry(newEntry);
          FileUtil.copy(inputStream, jarOutputStream);
          try {
            jarOutputStream.closeEntry();
          }
          catch (IOException e) {
            String messageText = JpsBuildBundle.message("build.message.cannot.extract.0.from.1.while.building.2.artifact.3", pathInJar,
                                                        root.getRootFile().getAbsolutePath(),
                                                        root.getTarget().getArtifact().getName(), e.getMessage());
            myContext.processMessage(new CompilerMessage(IncArtifactBuilder.getBuilderName(), BuildMessage.Kind.ERROR, messageText));
            LOG.debug(e);
          }
        }
      }
    });

  }

  private void addFileToJar(final @NotNull JarOutputStream jarOutputStream, final @NotNull File jarFile, @NotNull File file,
                            SourceFileFilter filter, @NotNull String relativePath, String targetJarPath,
                            final @NotNull Set<? super String> writtenPaths, List<? super String> packedFilePaths, final int rootIndex) throws IOException {
    if (!file.exists() || FileUtil.isAncestor(file, jarFile, false)) {
      return;
    }

    relativePath = addParentDirectories(jarOutputStream, writtenPaths, relativePath);
    addFileOrDirRecursively(jarOutputStream, file, filter, relativePath, targetJarPath, writtenPaths, packedFilePaths, rootIndex);
  }

  private void addFileOrDirRecursively(@NotNull ZipOutputStream jarOutputStream,
                                       @NotNull File file,
                                       SourceFileFilter filter,
                                       @NotNull String relativePath,
                                       String targetJarPath,
                                       @NotNull Set<? super String> writtenItemRelativePaths,
                                       List<? super String> packedFilePaths,
                                       int rootIndex) throws IOException {
    final String filePath = FileUtil.toSystemIndependentName(file.getAbsolutePath());
    if (!filter.accept(filePath) || !filter.shouldBeCopied(filePath, myContext.getProjectDescriptor())) {
      return;
    }

    if (file.isDirectory()) {
      final String directoryPath = relativePath.length() == 0 ? "" : relativePath + "/";
      if (!directoryPath.isEmpty()) {
        addDirectoryEntry(jarOutputStream, directoryPath, writtenItemRelativePaths);
      }
      final File[] children = file.listFiles();
      if (children != null) {
        for (File child : children) {
          addFileOrDirRecursively(jarOutputStream, child, filter, directoryPath + child.getName(), targetJarPath, writtenItemRelativePaths,
                                  packedFilePaths, rootIndex);
        }
      }
      return;
    }

    final boolean added = ZipUtil.addFileToZip(jarOutputStream, file, relativePath, writtenItemRelativePaths, null);
    if (rootIndex != -1) {
      myOutSrcMapping.appendData(targetJarPath, rootIndex, filePath);
      if (added) {
        packedFilePaths.add(filePath);
      }
    }
  }

  private String addParentDirectories(JarOutputStream jarOutputStream, Set<? super String> writtenPaths, String relativePath) throws IOException {
    while (StringUtil.startsWithChar(relativePath, '/')) {
      relativePath = relativePath.substring(1);
    }
    int i = relativePath.indexOf('/');
    while (i != -1) {
      String prefix = relativePath.substring(0, i+1);
      if (prefix.length() > 1) {
        addDirectoryEntry(jarOutputStream, prefix, writtenPaths);
      }
      i = relativePath.indexOf('/', i + 1);
    }
    return relativePath;
  }

  private void addDirectoryEntry(final ZipOutputStream output, @NonNls final String relativePath, Set<? super String> writtenPaths) throws IOException {
    if (!writtenPaths.add(relativePath)) return;

    ZipEntry e = new ZipEntry(relativePath);
    if (buildDateInMillis != null) {
      e.setTime(buildDateInMillis);
    }
    e.setMethod(ZipEntry.STORED);
    e.setSize(0);
    e.setCrc(0);
    output.putNextEntry(e);
    output.closeEntry();
  }

  private void addManifestEntry(ZipOutputStream output, Manifest manifest, Set<? super String> writtenPaths) throws IOException {
    ZipEntry manifestEntry = new ZipEntry(JarFile.MANIFEST_NAME);
    if (buildDateInMillis != null) {
      manifestEntry.setTime(buildDateInMillis);
    }
    output.putNextEntry(manifestEntry);
    manifest.write(new BufferedOutputStream(output));
    output.closeEntry();
    writtenPaths.add(JarFile.MANIFEST_NAME);
  }

  private class JarsGraph implements InboundSemiGraph<JarInfo> {
    @Override
    @NotNull
    public Collection<JarInfo> getNodes() {
      return myJarsToBuild;
    }

    @NotNull
    @Override
    public Iterator<JarInfo> getIn(final JarInfo n) {
      Set<JarInfo> ins = new HashSet<>();
      final DestinationInfo destination = n.getDestination();
      if (destination instanceof JarDestinationInfo) {
        ins.add(((JarDestinationInfo)destination).getJarInfo());
      }
      return ins.iterator();
    }
  }
}

redpajama_set_name: RedPajamaGithub


Seriously guys, stop being haters and let's be reasonable here. Sure, a box of cereal is only gonna cost you AED 18-20 at a supermarket... as opposed to the AED 20 you would pay for the regular bowl (with 2 kinds of cereal) at the Cereal Killer Cafe, but how often are you really gonna buy yourself whole boxes of sugary fruit loops, flavoured cheerios and cocoa puffs all at the same time? Not that I am advocating sugar or even this combination, but my point is how often are you gonna have over 100 cereal choices available to you in one sitting, and that too, in the midst of a shopping spree at Dubai Mall?
Regardless, do you really want to have a couple of massive boxes of that sugary cereal around the house at all times? You definitely don't wanna be eating that on a regular basis, and you probably don't want your kids to do that either. Instead, why not make it a treat once in a while?
You don't even have to get the sugary ones, you might simply want to experiment with a cereal that you haven't bought before, or simply have a healthy breakfast or snack on the go.
Give the poor guys a break, they have to pay rent for that prime location behind the Dubai Fountain as well as a franchise fee. Besides, its a fun concept and your kids can get creative. They can top it off with all kinds of fun toppings like marshmallows, m&m's and the works, or perhaps they can have a cereal shake with caramel and whipped cream, all while lounging on a colourful "bed" that overlooks the fountain.


Two days and a whole lot of nothing. I know that is exactly what little Frida is thinking of this. She wanted to go outside and romp on the grass, and smell the flowers, and chase robins and grasshoppers, but it was so hot, and then it was so wet. She sulked for two days until today finally I took her outside.
While we waited for the weather to turn somewhat decent, we played. Oh! how we played. We played dress up with all her pretty clothes, and we talked about the south and the food and the monsoon. We pretended to attend lavish mexican fiestas while dressed in silk and shell buttons with a pretty lace headband reminiscent of the 1930s.
Then we decided to play "a la escuelita" and she changed into more appropriate "off to school" clothes. Silly vents on the sides of the blouse and beautiful vintage shell buttons, a little bit of lace and a little bit of linen for her. To ward off the crazy weather.
Until the time came. To finally go outside. The first thing she did was to lose one shoe...then lie down on the grass and contemplate the clouds go by. I like this girl.
Frida still wanted to chase the birds and see wether we could find some ducks to feed but we didn't have such luck. We returned home ecstatic but knowing that soon enough she won't be here with me to chase the sun.
It started to get a little chilly so she grabbed her wool shawl and sat down to watch me fumble. It took forever to find her shoe, only to discover a silly pulled thread. I promised Frida to fix it before I sent her home. As the light started to go down, Frida and I held hands, admiring the Sun in all its glory.
Thank you for this adventure Frida.
You will always remind me of chasing the golden hour and a silly shoe.


An amazing new amaro from Italy's Varnelli family, a producer from the Marche region that has been distilling since 1868. This is quite bitter, made with gentian root, it's herbal with soft hints of chocolate and a very supple mouthfeel. Definitely not for everyone, but wow is it interesting. For those who truly love the wonderful world of bitter liqueurs--you'll go bananas for this.


text:
Jersey Shoreline: Oct. 30
The Jersey Shoreline is a weekly round-up from New Jersey Sea Grant Consortium that scours the Garden State's press and broadcasters for reports on several key topics related to the consortium's research and outreach.
It was three years ago this week that Hurricane Sandy pummeled the Jersey Shore, the banks of the Hudson River and the Meadowlands, with a massive storm surge on top of a very high tide. Largely, the state media took the chance to take stock of what has happened since.
Hurricane Sandy Anniversary
Should N.J. have left Hurricane Sandy inlet open? (VIDEO) — Today's video focuses on Mantoloking, a town on the northern barrier island in Ocean County where Sandy cut a pair of new inlets (or re-opened an old one). There, officials made a decision to quickly close the gap, driven by a desire to restore traffic and make whole the owners of a half dozen expensive homes in one of the wealthiest towns on the state. Read more at NJ.com.
Union Beach 3 Years After Sandy: Then and Now — It has been three years now since Hurricane Sandy decimated the Jersey Shore. Union Beach was one of the towns that was hit hardest by the 2012 fall storm. Read more at NJ.com.
North Jersey's on guard against the next superstorm — From adding a pump station in Little Ferry to elevating Borough Hall in Moonachie, officials in the low-lying areas of the Meadowlands – which suffered devastating flooding from Superstorm Sandy – say they have spent the last three years fortifying their towns to better survive another major storm. Read more at the Record.
3 years after Sandy, North Jersey towns recall fury of storm — Five feet of water flooded into the Bazzarelli Ristorante during Superstorm Sandy, destroying equipment, toppling over refrigerators, even seeping into the chair cushions. Read more at the Record.
Miles from ocean, Cumberland has its own Sandy pain — In Cumberland County, damage was significant in many of the rural and sparsely populated communities along the Delaware Bay. Read more at the Press of Atlantic City.
Dune replenishment fears hang over Sandy anniversary — As the third anniversary since Superstorm Sandy wrecked the Jersey Shore approaches, the lack of progress on beach and dune replenishment puts fear into many homeowners, who worry each time a storm approaches the area. Read more at the Asbury Park Press.
Three years after Sandy, some Delaware Bay shore residents resist giving way to nature — Kate Nelson lives in a tiny town called Bay Point in a small house she and her husband, Mike, are fixing up. They used to have a larger home along the Delaware Bay, but Superstorm Sandy destroyed it. Read more at Newsworks.
Jersey Shore At Varying Stages Of Recovery Three Years After Superstorm Sandy —Three years after Superstorm Sandy, New Jersey is a work in progress. More than 80,000 housing units were damaged or destroyed in the October 2012 storm. The cost: roughly $30 billion. Read more at CBS.
Three years after Sandy, a fight over coastal protection — After Superstorm Sandy left the New Jersey coastline in ruins three years ago, residents and officials were left with two big questions: first, how would the communities rebuild? And second, how would they protect the coastline along the Atlantic Ocean from the next big storm? Read more at Newsworks.
Birds or bivalves frames Delaware Bay debate — A new study suggests the growing oyster aquaculture industry on the Delaware Bay tide flats is harming an endangered migratory shorebird. Read more at the Press of Atlantic City.
Coastal Processes & Concerns
PROFILE: THE MAN WHO WORKS TO MAKE THE HACKENSACK RIVER CLEAN AND CLEAR — Part 'first responder for the river,' and part environmental activist and teacher, Bill Sheehan says restoring the Hackensack is a 24/7 job. Read more at NJSpotlight.
Thousands volunteer for Beach Sweeps along the Shore — The 30th annual Fall Clean Ocean Action Beach Sweeps drew 3,000 volunteers to Jersey Shore beaches to pick up hundreds of pieces of trash and debris. From Sandy Hook to Cape May, Individuals and teams of volunteers gave up their morning to help Clean Ocean Action analyze the debris for their annual report to identify pollution problems in hopes of getting stricter enforcement of existing laws to protect the marine environment. Read more at NJ101.5.
Measure to protect coral habitat off the Jersey Coast wins key support — The Mid-Atlantic Fishery Management Council recently voted in favor of a measure to preserve 38,000 miles of deep sea coral habitats off the Eastern Seaboard that are instrumental to New Jersey, according to officials at Monmouth University's Urban Coast Institute (UCI). Read more at NJ101.5.
Community Resilience & Climate Adaptation
$57.6 million beach project completed in Cape May County — The Department of Environmental Protection and U.S. Army Corps of Engineers (USACE) announced the completion of the beach and dune portion of a $57.6 million project in Cape May County. The announcement came on the third anniversary of Superstorm Sandy. Read more at NJ Environment News.
VIDEO: Oyster Reefs Built to Protect Shores — Oyster reef breakwater structures are being built along the Gandy's Beach shoreline to protect from storms and stop erosion. Watch at SNJ Today.
Marine Recreation & Jersey Shore Tourism
Striped bass turn on in Raritan Bay — After some up and down bass fishing, the stripers turned on big time in Raritan Bay on Sunday with the bite continuing through Monday. The fish also showed up in the suds and just off the beach in a couple of other spots. Read more at the Asbury Park Press.
Stripers arrive in force in Raritan Bay — It took a while, but the striped bass fishing finally broke open in Raritan Bay this week. Fish of various sizes showed up in different areas and were caught on the troll, with jigs, snagging bunker and even a fly rod. Read more at the Asbury Park Press.
Water Resources & Coastal Access
Fate Of Route 72 Basin Expansion Could Be Decided Soon — Officials are hopeful the long-awaited Neptune Basin expansion project beside Route 72 could receive a green-light from state officials soon. Read more at Micromedia Publications.
Another brown plume in Barnegat Bay angers environmental group — Another brown plume has surfaced in the Barnegat Bay in Seaside Park as crews continue to seal the pipes of a pumping system designed to reduce flooding in the area. Read more at NJ.com.


text:
Themes, Topics, Multi-Faith
Our services are often clustered in themes, like "Many Gardens – One World" (Autumn 2003) or "Dreams in the Night – Stories for the Journey--a look at the vision stories from the Hebrew scriptures. (Lent 2003), "SpiritWorks" (Autumn 2004), and "That We May Know Each Other: Muslim – United Church Dialogue" (Winter 2005).
We examine each theme in a series of topics. "SpiritWorks" explored the presence and relationship of creative Spirit in some of our members' workplaces, school-days, and creative writing.
Often, compelling topics lead Bathurst to respond with a special service or do something out of the ordinary. Since 2002 we have attended a screening at Planet In Focus: the Toronto International Environmental Film and Video Festival. The festival takes place on the first Sunday of October. We have also taken part in a multi-faith celebration organized as part of Planet in Focus.
Other services that called our attention to special themes or events have included "Braiding Remembrance and Hope: A Service to Commemorate the National Day of Remembrance and Action on Violence Against Women," (December 2002), and the United Church of Canada HIV/AIDS campaign, Beads of Hope (January 2002).
We also celebrate traditional events like Advent, Christmas, Lent and Easter in our own way, and non-traditional festivals like Black History Month and Summer Solstice and Pride Sunday.
Someone once said "Anything can happen at a Bathurst service." While this is certainly true, there is also something familiar to be found for regular worshipers and visitors on a Sunday morning.
Bathurst is committed to a multi-faith sensitivity. We seek to be attentive to the important religious festivals our neighbours celebrate. We would try to pray for members of the Jewish community during Rosh Hashanah or Yom Kippur. Our prayers embody the principles established by the United Church of Canada on relations with Jews and Judaism in "Bearing Faithful Witness" and for our Muslim neighbors during Ramadan. As part of our commitment to Right Relation with Peoples of the First Nations, we try to draw on traditional Aboriginal teachings.
Worship teams plan and lead individual services, picking up on suggestions from the congregation. Since our minister is half-time, lay members enjoy many opportunities to preach, plan and lead services.
Services include singing – old favourites and contemporary songs from global and feminist collections - scripture, prayer, silence, tactile activities and body movement. Our hymns and readings use inclusive language that is non-sexist and non-militaristic.
Bathurst is committed to the participation of all generations in our worshipping. We don't have a Sunday School, but we encourage children and youth to be present throughout the service. A round table, a focal point for our services, always has inviting crafts that the young – or young at heart – can work on during a service. Children and youth often share in a ministry of leadership by preaching the sermon, offering prayers and helping with Holy Communion.
The children offer the whole congregation unique contributions based on their ages and abilities. The spiritual formation of the children occurs by "osmosis" and through inter-generational activities during "Table Talk."
Child-care volunteers support parents with infants and young children, taking restless children out if necessary to play in the gym or do a craft in the church office. Most of the time the children are happy staying at the round table.
Bathurst usually celebrates Holy Communion on the first Sunday of the month. We use a communion liturgy developed by members on the congregation.
Baptism (Christening) is celebrated at Bathurst; for infants and for youth or adults, after suitable preparation. A blessing or welcome rite for an infant can also be planned.
Bathurst also marks the passing of it members with memorial or funeral services in consultation with the family and friends of those who have died.
Bathurst's ministers are available for weddings.
We do not hold Sunday services during July and August. Instead, members meet informally on Wednesday evenings for a pot-luck supper and discussion. The mid-week gatherings are at College Street United Church.


Well, we had a fantastic B2B breakfast on the 6th of April. With over 40 people attending to listen to both Jason Dunstone, founder of Square Holes and Ali Uren, founder of Kiik Start , present on Understanding Consumer Expectations.
Jason started off with a presentation on how to build a business and where business owners should be focusing. He went over bad habits and where to improve them. Giving the audience excellent food for thought on how to grow a business and become successful.
Ali revealed her results from her mystery shopping program she had completed on various shops around Gawler. Without naming any retail business names she managed to describe what was desirable to consumers and what areas business owners needed to improve upon.
It was a breakfast encompassing great presenters who shared their knowledge and facts and I encourage everyone to come out to as many B2B breakfasts as possible.