------------------------------------------------------------------------
From: Takeshi Go Tsuru  tsuru@cr.scphys.kyoto-u.ac.jp 
To: gcnews@aoc.nrao.edu
Cc: Takeshi Go Tsuru <tsuru@cr.scphys.kyoto-u.ac.jp>
Subject: submit sgrc_sb_v201.tex PASJ, Jan 2009

%astro-ph/0902.1308

\documentclass[proof]{pasj00}
\begin{document}

\title{A New Supernova Remnant Candidate and an Associated Outflow 
in the Sagittarius~C Region}

\author{
   Takeshi Go \textsc{Tsuru},\altaffilmark{1}
   Hiroshi \textsc{Nakajima},\altaffilmark{2}
   Katsuji \textsc{Koyama},\altaffilmark{1}
}
\altaffiltext{1}{
    Department of Physics, Graduate School of Science, Kyoto
    University,
    Sakyo-ku, Kyoto, 606-8502}
\email{tsuru@cr.scphys.kyoto-u.ac.jp}
\altaffiltext{2}{
   Department of Earth and Space Science, Graduate School of Science,
   Osaka University, Toyonaka, Osaka, 560-0043}
\altaffiltext{3}{
   Faculty of Humanities and Social Sciences, Iwate University,
   3-18-34 Ueda, Morioka, Iwate 020-8550}

\maketitle

\begin{abstract}

We present the Suzaku results on a new candidate of a supernova 
remnant
(SNR) in the Sagittarius~C region.
We detected diffuse X-rays of an elliptical shape (G\,359.41$-$0.12)
and chimney-like structure (the Chimney), both of which
are fitted with a thin thermal model of \KT$\sim 1$~keV temperature.
The absorption columns are same between these two structures,
indicating the both are located at the same distance in the same 
line of sight.
The narrow band image and one-dimensional profile
of S\emissiontype{XV} K$\alpha$ at 2.45~keV
show that the  Chimney is emanating from G\,359.41$-$0.12.
Therefore these two sources are physically connected with each 
other.
The sum of thermal energies of the Chimney and G\,359.41$-$0.12 is
estimated to be $1.4\times 10^{50}$~ergs, typical for a Galactic 
SNR.
G\,359.41$-$0.12 is likely a new SNR candidate
and the Chimney is an associated outflow.
\end{abstract}

\section{Introduction}

The Galactic center diffuse X-rays (GCDX) is characterized by many
K-shell lines from highly ionized atoms covering a large area of the
Galactic center (GC) \citep{Koyama89, Yamauchi90, Koyama96, 
Koyama07c}.
This indicates the presence of a large scale plasma of temperature
\KT = 1--10 keV. If this plasma is truly diffuse and extending in 
the GC,
it contains a huge thermal energy ($\sim 10^{53-54}$~ergs).
Since the high temperature plasma can not be confined by the 
Galactic
gravity, it may escape from the GC in a short time ($\sim 10^5$~yr),
the escape time scale.
Thus, we need a huge energy input of $\sim 
10^{48-49}$~ergs~yr$^{-1}$.

One plausible hypothesis is a multiple ($\sim 1000$) supernovae
in the GC region.
However, only a few supernova remnants (SNRs) had so far been 
detected
in the X-ray band.
This situation has been changing after the launch of the Suzaku 
satellite.
The X-ray Imaging Spectrometer (XIS) combined with the X-Ray 
Telescope
(XRT) onboard Suzaku has superior performance, a large
collecting area, a stable and low non-X-ray background (NXB) and a 
high
energy-resolution.
In order to make the most of these superiority, a significant amount 
of
the Suzaku observation time are allocated to the GC.
As a result, Suzaku has discovered several new SNRs located
in the Sagittarius (Sgr)~A, Sgr~B1, B2 and Sgr~D
regions \citep{Koyama07b, Nobukawa08, Sawada08, Mori08a, Mori08b}.

Sgr~C is one of the brightest radio complexes in the GC.
There are well-defined non-thermal radio filaments (NTFs),
some compact and evolved H\emissiontype{II} regions,
far-IR and submillimeter sources, and giant molecular clouds
\citep{Liszt85, Tsuboi91, Lis94, Liszt95}.
Accordingly, a rich variety of X-ray features may be expected.
However, the X-ray studies have been concentrated on the
diffuse 6.4~keV line emission (Fe\emissiontype{I} K$\alpha$)
\citep{Murakami01, Yusef07, Nakajima08};
few results on thermal diffuse emissions have been reported so far.
Thus, we conducted the studies of thermal emissions from the Sgr~C
region with Suzaku.
\citet{Nakajima08} reported the 6.4~keV clumps in the Sgr C region.
Using the same data set, we searched for thermal features, and
found clumpy emissions of thin thermal nature. We report on the 
results
and discuss the origin of the diffuse thermal X-rays.

Following \citet{Nakajima08}, ``the east'' and ``the north'' are 
referred
as the positive Galactic longitude side,
and the positive Galactic latitude side, respectively.
The distance to Sgr~C is assumed to be 8.5~kpc.
The solar abundance and photoelectric absorption cross-section are
taken from the tables of \citet{Anders89} and \citet{Church92},
respectively.

\section{X-Ray Data Processing}\label{sect:obs}

The Sgr~C region was observed with the XIS from 2006 Feb. 20 to 23,
and the XIS data were obtained with
the 3$\times$3 and 5$\times$5 modes and with the normal clocking 
mode.
The pointing position was R.A.=\timeform{17h44m37s.30},
Decl.= \timeform{-29D28'10''.2} (J2000.0).
The XIS consists one (XIS~1) back-illuminated (BI) CCD and three 
sensors
(XIS~0, 2 and 3) front-illuminated (FI) CCDs.
The detailed descriptions of the Suzaku satellite, XRT, and XIS can
be found in \citet{Mitsuda07}, \citet{Serlemitsos07} and 
\citet{Koyama07a},
respectively.

The data reduction and screenings are essentially the same as
\citet{Nakajima08}, but we applied the calibration database
(CALDB) released on
2008 July 2\footnote{http://www.astro.isas.jaxa.jp/suzaku/caldb/}.
For the data processing, we selected X-ray events by subtracting the
NXB from the raw data.
Since the flux of the NXB depends on the geomagnetic cut-off 
rigidity (COR)
\citep{Tawa08},
we applied the COR-sorted NXB (using the data sets provided by the 
XIS
team\footnote{http://www.astro.isas.jaxa.jp/suzaku/analysis/xis/nte/}),
to become the same COR distribution as that in the Sgr~C 
observation.
We exclude the data of the corners in the field of view (FOV)
illuminated by the onboard calibration sources of $^{55}$Fe.


\section{Analysis and Results}

\subsection{Imaging of Thermal Emissions}\label{sec:imaging ana}

We searched for a thin thermal plasma in the images of
S\emissiontype{XV} K$\alpha$ lines at 2.45 keV
(for a plasma temperature of \KT $\lesssim 1$~keV)
and/or Fe\emissiontype{XXV} K$\alpha$ lines at 6.68 keV
(for a plasma temperature of \KT $\gtrsim 1$~keV).
For the data processing and analysis of the imaging study, we 
co-added
the four CCD (XIS~0, 1, 2, and 3) data and made the exposure and
vignetting corrections.
In the Fe\emissiontype{XXV} K$\alpha$ image (6.6--6.8~keV),
we found no significant structure.
However, in the narrow band image of
the S\emissiontype{XV} K$\alpha$ line at 2.45 keV (2.40--2.50~keV),
we found a bright extended source at
$(l,b)=(\timeform{359D.41}, \timeform{-0D.12})$,
hence designated as G\,359.41$-$0.12 hereafter
(figure~\ref{fig:2.45keV_image}).
Another diffuse emission has a chimney-like structure extending
from G\,359.41$-$0.12 to the north direction,
which we call as ``the Chimney''.
Two known bright point sources, 1E\,1740.7$-$2942
($\sim 5\times 10^{-10}$\UNITEFLUX)
and A1742-294 ($\sim 3$--$6\times 10^{-10}$\UNITEFLUX), are
located outside the FOV in the western and south-east directions,
respectively (e.g., Sidoli et al. 1999).
The contamination due to the stray-light from the two sources
is only $\sim 2-3$\% of the flux of the Chimney in the energy band 
of
2.40--2.50~keV \citep{Serlemitsos07}.
Thus, the Chimney is a real structure.

\begin{figure}
   \begin{center}
     \FigureFile(80mm,80mm){fig1.eps} %
   fig/SGRC_2.4-2.5keV_080801_mod1_Fig1.eps
   \end{center}
   \caption{
     The 2.45~keV-line (S\emissiontype{XV} K$\alpha$) image
     in the energy band of 2.40--2.50~keV after the smoothing
     with the Gaussian kernel of 60~pixels ($\timeform{1'.04}$).
%     Contour levels are set at
%     $(2.9$, $3.4$, $4.0$, $4.6$, $5.4$, $6.3$,
%     $7.3$, $8.5$, $10.0$,
%     $11.6)\times 10^{-4}$ counts~s$^{-1}$~arcmin$^{-2}$.
     Contour levels are set at
     $(4.2$, $4.9$, $5.7$, $6.6$, $7.8$, $9.0$,
     $10.6$, $12.3$, $14.4$, $16.8)
     \times 10^{-7}$ ph~s$^{-1}$~cm$^{-2}$~arcmin$^{-2}$.
     The typical 1$\sigma$ error is
     0.5$\times 10^{-7}$ ph~s$^{-1}$~cm$^{-2}$~arcmin$^{-2}$.
     We collected the source and background spectra of the Chimney
     from the regions shown with solid blue and dashed black lines,
     respectively.
     Extraction of the source spectra of G\,359.41$-$0.12
     were made from the region given with the solid line,
     while its background spectra were obtained from the region
     of dashed blue lines but the source area (solid bule circle)
     was excluded.
     Also the data within the red dashed ellipses (M\,359.43$-$0.07
     and
     M\,359.47$-$0.15) were excluded to minimize the contamination
     from the strong 6.4~keV emission line and its associated
     continuum.
     The green box with the size of $\timeform{18'.5}\times
     \timeform{3'}$
     gives the region for the one-dimensional profile shown in
     figure~\ref{fig:profile}.
     }
  \label{fig:2.45keV_image}
\end{figure}

To see if the Chimney is connected with G\,359.41$-$0.12 
quantitatively,
we constructed an one-dimensional surface brightness profile
at 2.45~keV with the length of $\timeform{18'.5}$
along the green rectangle in figure~\ref{fig:2.45keV_image}.
The origin of the profile is defined at the northern side of the 
box.
The background level was obtained from the background regions of
the spectra of the Chimney and G\,359.41$-$0.12 shown in
figure~\ref{fig:2.45keV_image}.
The 2.45~keV profile shown in figure~\ref{fig:profile} clarifies 
that
the surface brightness from G\,359.41$-$0.12 to the Chimney are well
above the background level.
On the other hand, the profile is not smooth but has two dips at
distances of $\sim \timeform{3'.5}$ and $\sim \timeform{7'}$.

\begin{figure}
   \begin{center}
     \FigureFile(80mm,80mm){fig2.eps} %
   fig/projection_2.3-2.6keV_bin16_vigcor-bgdAB_mod2.eps
   \end{center}
   \caption{
     One-dimensional surface brightness profile at 2.45~keV
     (2.30--2.60~keV)
     along the green box connecting the Chimney with G\,359$-$0.12
     (figure~\ref{fig:2.45keV_image}).
     The origin of the profile is defined at the northern side of
     the rectangle.
     The dotted line shows the background level obtained from the
     the background regions for the Chimney and G\,359.41$-$0.12
     indicated in figure~\ref{fig:2.45keV_image}.
     ``MC\,1'' and ``MC\,2'' show the positions of ridges of the
     molecular clouds crossing the Chimney
     (see figure~\ref{fig:13CO_2.45keV_image}).
     }
  \label{fig:profile}
\end{figure}

As mentioned above, a bright source 1E\,1740.7$-$2942
is located outside the FOV in the western direction.
A possible radio SNR having a size of 22~pc$\times$10~pc,
G\,359.07$-$0.02, is cataloged in \citet{LaRosa00}.
Thus, the western excess would be due to the XRT PSF (point spread 
function)
tail of 1E\,1740.7$-$2942 and/or eastern edge of G\,359.07$-$0.02.
At the time of writing this paper,
Suzaku already made a pointing observation of the western adjacent 
region.
However, the exposure time was only $\sim 20$~ksec,
and hence it is not clear whether the excess near
the western edge of the FOV is a real excess or a spill over of
these X-ray sources. We therefore will not discuss on this excess in
this paper.

\subsection{Spectral Analyses}

In the spectral studies, we treated the co-added FIs (XIS~0,2,3) 
data
and BI (XIS~1) data separately because the response function of FIs 
and
BI are significantly different.
The spectra were extracted from the regions
shown in figure~\ref{fig:2.45keV_image}.
Since the surface brightness of the GCDX, the most significant
background component, depends on the Galactic latitude, the 
background
regions for the Chimney and G\,359.41$-$0.12 were selected to have 
the
same latitude as those of corresponding source areas.
The energy-dependent vignetting were corrected by multiplying the
effective-area ratio of the source region to the corresponding
background area for each energy bin.
Since the 6.4 keV clumps, M\,359.43$-$0.07 and M\,359.47$-$0.15 have
a strong 6.4~keV-line and associated continuum emission 
\citep{Nakajima08},
we excluded the regions of these 6.4~keV clumps from both of the 
source and
background areas, in order to minimize the contamination of the 
clumps.

\begin{figure}
   \begin{tabular}{cc}
     \begin{minipage}{0.5\textwidth}
       \FigureFile(80mm,80mm){fig3a.eps} %
     fig/regionC_new_fit_t1_FI_mod1.eps
     \end{minipage}
     \begin{minipage}{0.5\textwidth}
       \FigureFile(80mm,80mm){fig3b.eps} %
     fig/regA-BGD_regA_0721_ALL_t30_FI_mod1.eps
     \end{minipage}
   \end{tabular}
   \caption{The background subtracted FIs spectra of (a) the Chimney
     and (b) G\,359.41$-$0.12 with the best fit model spectra.
     Although, we simultaneously fitted the FIs and BI spectra,
     only the FI results are given for brevity.}
  \label{fig:spec}
\end{figure}

The background (the GCDX) subtracted FIs spectrum of the Chimney is 
shown
in figure~\ref{fig:spec}~(a).
We see two conspicuous emission
lines from highly ionized atoms, S\emissiontype{XV} K$\alpha$ 
(2.45~keV)
and Ar\emissiontype{XVII} K$\alpha$ (3.12~keV).
We, therefore, fitted the spectrum by a thin thermal plasma model in
collisional ionization equilibrium affected by photoelectric
absorption (\verb/vapec/ and \verb/wabs/ models in XSPEC, 
respectively).
The fit was reasonably good as is shown in 
table~\ref{tab:fitresults2}.

The background (the GCDX) subtracted spectra of G\,359.41$-$0.12 
shows
prominent 6.4~keV emission lines from Fe\emissiontype{I} K$\alpha$ 
as well as
S\emissiontype{XV} K$\alpha$ and Ar\emissiontype{XVII} K$\alpha$.
This 6.4~keV line emission come from a 6.4~keV clump, 
M\,359.43$-$0.12,
which is located inside the source region of G\,359.41$-$0.12 and
hence difficult to specially exclude \citep{Nakajima08}.

The bight 6.4~keV clumps of M\,359.43$-$0.07 and M\,359.47$-$0.15,
locating near G\,359.41$-$0.12 and M\,359.43$-$0.12,
have essentially the same spectrum \citep{Nakajima08}.
Thus, assuming M\,359.43$-$0.12 also has the same spectrum,
we added a model of the fixed absorption column, photon
index and equivalent widths of the best-fit of
M\,359.43$-$0.07 and M\,359.47$-$0.15, and fit with the same model
as the Chimney (a thin thermal model).
The fit was acceptable as is shown in table~\ref{tab:fitresults2}.
We further examined how the results of G\,359.41$-$0.12
depend on the spectral shape of the M\,359.43$-$0.12, by
changing the model parameters within the errors.
Then we found no significant change of the results;
only the errors of the best-fit parameters of G\,359.41$-$0.12 
become larger
by a factor of $\sim 1.5$.

%  The background (the GCDX) subtracted spectra of G\,359.41$-$0.12 
%  shows
%  prominent 6.4~keV emission lines from Fe\emissiontype{I} 
%  K$\alpha$ as well as
%  S\emissiontype{XV} K$\alpha$ and Ar\emissiontype{XVII} K$\alpha$.
%  This 6.4~keV line emission comes from a 6.4~keV clump, 
%  M\,359.43$-$0.12,
%  which is located inside the source region of G\,359.41$-$0.12 and
%  hence difficult to exclude \citep{Nakajima08}.
%  Thus, we added  the best-fit model of fixed photon index and 
%  equivalent
%  widths of the M\,359.43$-$0.12 (\cite{Nakajima08}
%  and fit with the same model as the Chimney (a thin thermal 
%  model).
%  The fit was acceptable as is shown in 
%  table~\ref{tab:fitresults2}.


\begin{table}
   \begin{center}
     \caption{Best-fit parameters of the Chimney and
     G\,359.41$-$0.12}
     \label{tab:fitresults2}
     \begin{tabular}{lcc}
       \hline
       Parameters
          &  the Chimney
          &  G\,359.41$-$0.12 \\
       \hline
       \ \ $N_{\rm H}$ ($10^{22}$~cm$^{-2}$)
          &  10.1 (8.6--12.2)
          &  12.0 (11.5--12.4) \\
      \ \ \KT\ (keV)
          &  1.15 (0.93--1.37)
          &  0.90 (0.84--0.94) \\
      \ \ $Z_{\rm S}$, $Z_{Ar}$ ($Z_\odot$) \footnotemark[$\dagger$]
          &  1.73 (1.11--2.65)
          &  1.72 (1.51--2.07) \\
       \hline
       $f_{\rm X}$\footnotemark[$\sharp$] (thermal) (\UNITEFLUX )
          &  $3.23\times 10^{-13}$
          &  $3.11\times 10^{-13}$ \\
      $f_{\rm X}$\footnotemark[$\sharp$] (power-law) (\UNITEFLUX )
          &  $\cdots$
          &  $2.39\times 10^{-13}$ \\
       \hline
       $\chi ^{2}$/d.o.f.
          &  $74.9/55$
          &  $128.4/91$  \\
       \hline
       \multicolumn{3}{@{}l@{}}{\hbox to
       0pt{\parbox{100mm}{\footnotesize
         Notes. --
           The values in parentheses represent the 90\% confidence
           intervals.
             \par\noindent
         \footnotemark[$\dagger$]The values of $Z_{\rm S}$ and
            $Z_{\rm Ar}$ are fixed to one another.
            $Z$ of the other elements are fixed to the solar values.
          \footnotemark[$\sharp$]Observed (absorption not corrected)
             flux at the 1.5--8.0~keV band.
             \par\noindent
           }\hss}}
     \end{tabular}
  \end{center}
\end{table}

\section{Discussion}

We discovered two diffuse X-ray
sources with the 2.45~keV emission line
(S\emissiontype{XV} K$\alpha$), G\,359.41$-$0.12 and the Chimney.
There is a well-defined non-thermal radio filament, 
G\,359.45$-$0.06,
running north-western direction in the Sgr~C region
\citep{Liszt85, Liszt95}.
However, the position angle of G\,359.45$-$0.06 disagree with
that of the Chimney by $\sim \timeform{40D}$, and hence the Chimney 
is
not related to G\,359.45$-$0.06 
(figure~\ref{fig:13CO_2.45keV_image}).
In the followings, we discuss the structure and origin of the 
plasmas.

\subsection{Plasma Parameters}

We first derived physical parameters of the Chimney and 
G\,359.41$-$0.12,
summarized in table~\ref{tab:physparam}.
We assumed the Chimney and G\,359.41$-$0.12 have the plasmas of an
cylinder with the diameter of $7.4$~pc (\timeform{3.0'})
and length of $20$~pc (\timeform{8.0'}), and
an ellipsoid with the dimensions of
8.6~pc$\times$ 8.6~pc $\times$ 12.4~pc
($\timeform{3.5'}\times\timeform{3.5'}\times \timeform{5.0'}$),
respectively.

The plasma temperatures give sound velocities of
$C_{\rm s}=560$~km~s$^{-1}$ and $480$~km~s$^{-1}$ for
the Chimney and G\,359.41$-$0.12, respectively.
Hence, dividing the length or major axis by the sound
velocities, we can estimate the dynamical time scales of
the Chimney and G\,359.41$-$0.12 to be $4.0\times 10^4$~yr
and $2.5\times 10^4$~yr.

\begin{table}
   \begin{center}
     \caption{Physical parameters of the Chimney and
     G\,359.41$-$0.12.
       \footnotemark[$*$]}
     \label{tab:physparam}
     \begin{tabular}{lcc}
       \hline
       Parameters
          &  the Chimney             % Note No.17 p114
          &  G\,359.41$-$0.12 \\     % Note No.17 p126
       \hline
       $\int n_{e}n_{\rm H} dV$~(cm$^{-3})$
          &  $4.9\times 10^{57}$
          &  $1.3\times 10^{58}$ \\
      $V$ (pc$^{3}$)
          &  $8.5\times 10^2$
          &  $4.8\times 10^2$ \\
      $n_{\rm e}$ (cm$^{-3}$)
          &  $0.49f^{-1/2}$
          &  $1.1f^{-1/2}$ \\
      $M$ (\MO)
          &  $14f^{1/2}$
          &  $14f^{1/2}$ \\
      $E_{\rm th}$ (ergs)
          &  $7.6\times 10^{49}f^{1/2}$
          &  $5.9\times 10^{49}f^{1/2}$ \\
       \hline
       $L_{\rm X}$\footnotemark[$\natural$] (\UNITLUMI )
          &  $2.2\times 10^{34}$
          &  $3.9\times 10^{34}$ \\
       \hline
       \multicolumn{3}{@{}l@{}}{\hbox to
       0pt{\parbox{80mm}{\footnotesize
         Notes. -- The distance is assumed to be 8.5~kpc.
         $M$, $E_{\rm th}$ and $f$ are the mass, thermal energy
         and filling factor of the plasma, respectively.
         The other notations refer to table~\ref{tab:fitresults2}.
         \footnotemark[$\natural$]Unabsorbed luminosity between
         1.5-8.0~keV.
%            \par\noindent
           }\hss}}
     \end{tabular}
  \end{center}
\end{table}

\subsection{Physical Connection of the Chimney and G\,359.41$-$0.12}
\label{sec:phys connect}

We discuss if the plasmas of the Chimney and G\,359.41$-$0.12
are connected with each other.
The one-dimensional profile in figure~\ref{fig:profile} suggests 
that the
X-ray emission continuously distributes between the two objects 
without
break.
The absorption columns of the Chimney and G\,359.41$-$0.12
are almost identical at \NH=(10-12)$\times 10^{22}$~cm$^{-2}$,
suggesting that these two sources are at the same distance in the
same line of sight.
The temperatures and metal abundances of these sources
are essentially the same.
Therefore, we can infer that the Chimney and G\,359.41$-$0.12 are
physically connected with a similar nature.

\subsection{Absorption by Molecular Clouds}

Figure~\ref{fig:13CO_2.45keV_image} shows $\atom{CO}{}{13}$ emission 
over the
range $-84$ to $-24$~km~s$^{-1}$ overlaid on the X-ray image at 
2.45~keV
\citep{Liszt95}.
Anti-correlation among the four molecular clouds (MC\,1, 2, 3, 4) 
and
X-ray emission is clearly seen.
The positions of MC\,1 and MC\,2 agree well with the two dips seen
in the one-dimensional profile (figure~\ref{fig:profile}).
The hydrogen column densities of MC\,1 and MC\,2 estimated from the
$\atom{CO}{}{13}$ emission are \NH$\sim 2\times 10^{22}$~\UNITNH\
($\sim 40$\% absorption at 2.45~keV).
The unabsorbed counting rates plus the background level are obtained
to be $\sim 8\times 10^{-4}$ and $\sim 1.0\times 
10^{-3}$~counts~s$^{-1}$
at the position of MC\,1 and MC\,2, respectively.
Thus, we can assume that MC\,1 and MC\,2 are located in front of
the Chimney and absorb the X-ray emission; the dips would be due to
the absorption by the molecular clouds and
the unabsobed one-dimensional profile in the Chimney would
decrease monotonically from G\,359.41$-$0.12 without a significant 
dip.
This result enforces the idea that G\,359.41$-$0.12 and the Chimney
are physically connected with each other (section~\ref{sec:phys 
connect}).

Figure~\ref{fig:13CO_2.45keV_image} also shows that the surface 
brightness
at the 2.45~keV band is low at the positions of MC\,3 and MC\,4.
The column densities of MC\,3 and MC\,4 obtained from the 
$\atom{CO}{}{13}$
emission are \NH$\sim 7\times 10^{22}$~cm$^{-2}$ and
$\sim 3\times 10^{22}$~cm$^{-2}$, respectively.
Thus, one can explain the anti-correlation
would be due to the absorption by MC\,3 ($\sim 80$\%)
and MC\,4 ($\sim 50$\%), as applied to MC\,1 and MC\,2.
On the other hand,
since the shapes of MC\,3 and MC\,4 trace the rim of 
G\,359.41$-$0.12 well,
the other possibility is that the molecular clouds block the plasma 
to
expand further out.
Since the surface brightness in the region of MC\,3 and MC\,4 is 
very low,
further deep observation is necessary to clarify these two 
possibilities.

\begin{figure}
   \begin{center}
     \FigureFile(80mm,80mm){fig4.eps} %
   fig/SGRC_2.4-2.5keV_080801_mod1_Fig4.eps
   \end{center}
   \caption{
     The contours of $\atom{CO}{}{13}$ at $-84$ to $-24$~km~s$^{-1}$
     (red)
     and the schematic diagram of the radio continuum sources of
     G\,359.45$-$0.06 and G\,359.43$-$0.09 (blue) are
     overlaid on the 2.45~keV-line (S\emissiontype{XV} K$\alpha$)
     image.
     The radio data are adopted from \citet{Liszt95}.
     MC\,1, 2, 3, and 4 indicate the molecular clouds.
     The region for the one-dimensional profile in
     figure~\ref{fig:profile} is shown with the green box
     ($\timeform{18'.5}\times \timeform{3'}$).
     }
  \label{fig:13CO_2.45keV_image}
\end{figure}

\subsection{Origin of the Plasmas}

First, we discuss the origin as star clusters.
The observed X-ray luminosities of G\,359.41$-$0.12 and the Chimney 
are
(2--4)$\times 10^{34}$~\UNITLUMI\ in the 1.5--8~keV band. These 
luminosities
are comparable with or higher than those of the Arches
($\sim 3\times 10^{34}$~\UNITLUMI) and Quituplet
($\sim 4\times 10^{33}$~\UNITLUMI) clusters,
the X-ray brightest star clusters in the Galaxy
\citep{Tsujimoto07, Wang06}.
The canonical metal abundance of the Galactic H\emissiontype{II}
regions obtained with X-ray spectroscopies is 0.3 solar
(e.g., Getman et al. 2005),
while G\,359.41$-$0.12 and the Chimney have metal abundances of
$1\sim 2$ solar.
% This is not the case of G\,359.41$-$0.12 or the Chimney.
There is a radio bright H\emissiontype{II} region, G\,359.43$-$0.09
(Sgr~C) as shown in figure~\ref{fig:13CO_2.45keV_image}
\citep{Liszt95}. However, the peak position of G\,359.41$-$0.12 is
$\timeform{2'.4}$ shifted from that of G\,359.43$-$0.09.
%  No significant X-ray peak is found at the position of the
%  Sgr~C H\emissiontype{II} region.
Thus, it is unlikely that the X-rays of G\,359.41$-$0.12 and the 
Chimney
come from  the H\emissiontype{II} regions.

A pulsar wind nebula and jet from a compact source are also unlikely
as the origin of the Chimney and G\,359.41$-$0.12, because a power 
law
model failed to fit the observed spectra.

The X-ray luminosity, temperature, and the other physical parameters 
of
G\,359.41$-$0.12 and the Chimney  are consistent with those of the 
SNRs
detected in the GC \citep{Nobukawa08, Mori08a, Sawada08, Mori08b}.
The sum of thermal energies of the Chimney and G\,359.41$-$0.12 is
$1.4\times 10^{50}$~ergs, typical for a Galactic SNR.
Including the possible energy of the plasma bulk motion
with the sound velocity into the total energy,
it is still consistent with a single supernova.
Therefore, we propose G\,359.41$-$0.12 is a new SNR candidate
and the Chimney is an outflow plasma from the SNR.
The molecular clouds of MC\,3 and MC\,4 can block the plasma from
expanding except in the northern direction.
Then, the outflow in the direction of the north may be formed.
In any case, the morphology of single SNR plus a chimney-like 
thermal
outflow with the dimension of $\sim$ 8~pc $\times$ 8~pc $\times$ 
34~pc is
very unusual as a SNR.
Thus, further deep observation is highly required.

\bigskip
\bigskip
%\section*{Acknowledgment}

We are grateful to all members of the Suzaku hardware and software
teams and the science working group.
This work was supported by the Grant-in-Aid for the Global COE 
Program
``The Next Generation of Physics, Spun from Universality and
Emergence'' from the Ministry of Education, Culture, Sports, Science
and Technology (MEXT) of Japan.
This work was also supported by Grants-in-Aid of Ministry of
Education, Culture, Sports, Science and Technology No. 18204015 and
20340043.
MN and HN are financially supported by the Japan Society for the
Promotion of Science.

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\end{document}
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