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    {\small\rm\thepage\hfill
    \quad\quad ACTA ASTRONOMICA SINICA \hfill
    \hspace{2mm} Vol.44\vspace{2mm}}}} %%%%%%%
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    {\small\rm  suppl.\hfill M. Zhao et al.: CO Studies of IRAS 00117+6412  %%（作者：题目名称）
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\zihao{5}\songti

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    \zihao{6}\songti
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    Vol.44~ Suppl.
    \hfill\hspace{8mm} %%% if ``October/January'' then \hspace{8/10 mm} July
    \small ACTA ASTRONOMICA SINICA
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      Feb.,~2003 \\[-1.5 true mm] %%January
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\vs\vs\vs \bc {\Large\bf
CO Studies of IRAS 00117+6412    %%（文题）
%\\[1ex]
%$\!\!^*$
}

\vs\vs{\normalsize Ming Zhao\up{1},\hs\hs Yuefang Wu\up{1},\hs\hs
Martin Miller\up{2}\hs\&\hs
  Ruiqing Mao\up{3}}  %%（本文作者）

\vs ({\footnotesize 1~{\it Astronomy Department,CAS-PKU Joint
Beijing
Astrophysics Center,Peking University,Beijing }~ 100871}) \\%%（本文作者单位）
 ({\footnotesize 2~ {\it Physics Institute, Koln University, Germany}~ D-50937})\\
 (\footnotesize 3~ \pmo)\\
\vs\vs \ec

\normalsize
\begin{quotation}

 \no{\bf A{\scriptsize\bf BSTRACT }}~~~\small
CO $J=3-2$ maps and  $^{13}$CO $J=1-0$ maps were made for IRAS
00117+6412. A bipolar molecular outflow is certified, which is
driven by the center IRAS source. There is approximately
45.5\,M$_{\odot}$ of molecular materials in the outflow. The mass
loss rate is 0.04$\times$10$^{-3}$\,M$_{\odot}$/yr, and the
bolometric luminosity and dust temperature are 4.6$\times$10$^{3}$
L$_{\odot}$ and 30.2\,K, respectively. The spectrum also exhibits
a well-behaved power-law fit. The molecular core has
4$\times10^{3}$ M$_{\odot}$ materials.  All of the results
indicate that it is a high mass star formation region and has a
short time scale. The FIR source is deeply embedded in dense
molecular core and associated with two water masers and it may be
the driving source of the outflow.

 \vn
 \no{\bf Key words}~~  star: formation --
                ISM: clouds, outflow --ISM: kinematics and dynamics
\end{quotation}

%%%% 正文
 \para{\large\bf{1}~~ Introduction}

\vs\vs
       Bipolar outflows play a very important
   role in the course of star formation (Lada 1985).
   They provide abundant information for dynamic process of star
   formation. Search of outflows and their driving sources is also a crucial
    work.

 IRAS 00117+6412 (R.A.$= 00^h11^m44.6^s$, Dec.$= 64\dg12'04.01''$) is an
infrared source and associated with water masers. Wu et al. (2001)
have already shown its bolometric features as a candidate of
outflow with CO $J=1-0$ observations. Their results indicated that
the source had evidence of red-wing, which implies it is a good
candidate for our research on molecular cores and outflows.

 \para{\large\bf{2}~~Observation}

\vs\vs
  Observation of the CO $J=3-2$ transition was made with KOSMA 3\,m telescope
  in April, 1999.
   The half-power beam width of the telescope was $80''$ at 345\,GHz.
    The pointing accuracy was better than $10''$.
    The main beam efficiency was 100\% at 345\,GHz and the forward efficiency was
    93\%.

  Another observation was conducted with PMO 13.7\,m telescope on $^{13}$CO $J=1-0$
   transition in March, 2002.
   The central frequency is 110.2\,GHz with the efficiency of 50\%.
    The beam size is $55''$, and the pointing and tracking accuracy is better than
    $10''$.

 The CO data were reduced by CLASS and Greg, and the $^{13}$CO data by Drawspec.

\newpage
\vspace*{1mm}
\para{\large\bf{3}~~Results and  Conclusion}

\vs\vn{\bf{3.1~~ Dense Molecular Core}}

    From the maps of the region, we can see IRAS 00117+6412 has an
isolated core, with relatively stable ambient. It has two water
masers associated with the center FIR source, which indicates it
is still undergoing a young evolution stage (Zhang et al. 2001).
With the data of Wu et al. (2001), we have derived the mass of the
molecular core, to be 4$\times10^{3}$\,M$_{\odot}$. We also get
the bolometric luminosity of 4.6$\times10^{3}$ L$_{\odot}$ with
IRAS fluxes. The source satisfies the criteria of Wood $\&$
Churchwell (1989), but it is not really an ultra compact HII
region. It is probably a high mass star formation region
(HMSF).

  Another FIR source, IRAS 00115+6413 is located to the northwest
   of the center. Because it is far away from the center of the
    core, it cannot be the driving source.

\vn{\bf{3.2~~ The outflow}}

  The morphology and contours of the FIR source IRAS 00117+6412 show that
there is a bipolar outflow in the region, with a scale of 0.81pc.
We derived the distance of 3.3\,kpc using the rotational curve
(Wouterlovt \& Brand, 1989).
   Under the assumption that the $T_{\rm ex}=15$\,K and [H$_2$]/[CO]=10$^{-4}$  ,
    we also obtained the parameters of the outflow,
     which is listed in Table 1.

\bc{\small\bf

 Table 1~~ The parameters of the molecular outflow
}\\[2mm]

\fns \tabcolsep 0.8mm
\begin{tabular}{ccccccccccc}
\hline\\[-3.6mm]\hline
 D& $R_{\max}$&Mass  &$M_{\rm lost}$&P&E&t&$L_{\rm
 bol}$&$L_{\,mech}$&F&$T_D$\\
 kpc&pc &M$_{\odot}$&M$_{\odot}{\cdot}$yr$^{-1}$&M$_{\odot}{\cdot}$\,km${\cdot}$s$^{-1}$&
 erg&yr&L$_{\odot}$&L$_{\odot}$&M$_{\odot}{\cdot}$km${\cdot}$s$^{-1}{\cdot}$yr$^{-1}$&K\\
\hline
3.3 & 0.81 & 45.5 & 4$\times10^{-5}$ & 321.8&
8$\times10^{47}$ & 0.8$\times10^{5}$
& 4.6$\times10^{5}$ & 8.2 &  4$\times10^{-3}$ & 30.2  \\
 \hline\\[-3.6mm]\hline%\\[-4.5mm]\hline
 \end{tabular}
 \ec

There is 45.5\,M$_{\odot}$ materials in the high velocity
components and the mass loss rate is
4$\times$10$^{-5}$\,M$_{\odot}$/yr. Its momentum is
321.8\,M$_{\odot}$\,km/s, and the kinetic energy is
0.8$\times$10$^{47}$\,erg, all of which are obviously larger
than those of low mass stars.

 IRAS 00117+6412 may be the driving source, because it is close
to the center and associated with water masers. The ratios
$\log(\frac{L_{\rm bol}}{L_{\rm co}})\ll 1$,$\&$ $\frac{L{\rm
bol}}{cF}\ll 1 $, suggest that despite of the strong radiation
from the center source, the radiation pressure still cannot supply
enough force to drive such a massive outflow (Wu et al. 1998).

To see its difference from low mass stars, we assume $T_A$ as a
function of $|V_0-V_{\rm LSR}|$ and get a power-law fit. The
result shows there is a break between the high velocity and low
velocity components in the red lobe. The slope of both blue and
red lobes is relatively high than those of low mass stars
(Shepherd et al. 1998), which shows the difference between high
mass stars and low mass ones, although they maybe have a similar
evolution process (e.g. Henning et al.
 2000, Zhang et al. 2001).

\para{\large\bf{4}~~Summary}

\vs\vs In summary, we have presented the results of IRAS
00117+6412 by mapping the CO $J=3-2$\& $^{13}$CO $J=1-0$
transition. The molecular core is isolated and relatively young.
Its mass is $4\times 10 ^{3}$\,M$_{\odot}$. An asymmetric bipolar
outflow with 45.5\,M$_{\odot}$ materials is identified, its
kinetic energy, luminosity, and other parameters are derived too.
The center FIR source seems to be the driving source. And its
difference with low
mass outflows is highlighted by the power-fit.

\vs\vn{\bf ACKNOWLEDGEMENTS}~~ We thank all the staff in Qinghai
station of PMO for their assistant of observations. The project is
supported by 10128306 NSFC, 10133020 NSFC and G1999075405 NKBRSF.

\bc {\bf References} \ec

\vspace{-4mm} \no \fns

 \no Henning Th., Schreyer K., et al. APJ, 2000, 353, 211 \\
\no Lada C.J., et al. Ann. REV. A\&A 1985, 23:267 \\
\no Shepherd D.S, Watson A.M., et al. APJ, 1998, 507, 861\\
\no Wood D., Churchwell E., APJ, 1989, 340, 265\\
\no Wouterlovt T.G.A, Brand T.,  A\&A, 1989,80:189\\
\no Wu Y., et al., AAS, 1998, 18(3), 243\\
\no Wu Y., Wu J., Wang J., A\&A, 2001, 380, 665 \\
\no Zhang Qi., Hunter T.R., et al., APJ, 2001, 552, L167 \\

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