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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 W. Yu et al.: Mapping Studies of High Velocity Gas near \\
      IRAS02310+6133   %%（作者：题目名称）
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    Vol.44~ Suppl.
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    \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
Mapping Studies of High Velocity Gas near \\[2mm]
      IRAS02310+6133    %%（文题）
%\\[1ex]
%$\!\!^*$
}

\vs\vs{\normalsize W. Yu\up{1},\hs\hs Y. Wu\up{1}\hs\&\hs L. Wang\up{2}}  %%（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 Qinghai Observation Station, Purple Mountain
 Observatory, NAOC, De Ling Ha}~871000})\\
\vs\vs \ec

\normalsize
\begin{quotation}

 \no{\bf A{\scriptsize\bf BSTRACT }}~~~\small
 Mapping observations in CO J=1-0 lines were made towards IRAS
02310+6133 with the 13.7m telescope at Qinghai Station of Purple
Mountain Observatory. There exists the line-centre velocity shift,
probably caused by rotation. Taking the shift into account, we
made the wing emission intensity contours and the core contours.
In the wing emission intensity contours, there is a bipolar
structure, and we calculate the outflow parameters. From the core
contours, IRAS 02310+6133 is deviated from the core emission peak.
Maybe it is a new star formation region.

 %\vn
 %\no{\bf Key words}~~  pulsar-mode  change-spectrum
\end{quotation}

%%%% 正文
 \vs\vs

 There are three major reasons why we observed IRAS
02310+6133. First, this region is a massive star formation region
(Wu et al. 1998). Second, it is associated with two H$_2$O masers
(Comoretto et al. 1990); In addition, there is no coincidence with
HII region. All these three characteristics show that the
evolution stage of this region is earlier than the ultra
compact(UC) HII, which is a good target to probe the early status
of massive stellar objects. High-velocity gas detected in this
region has not been identified to be an outflow (Wu et al. 1998).
Mapping CO J=1-0 is necessary and useful to further study this
region.

 Our observation for IRAS 02310+6133 was made with 13.7\,m
telescope at Qinghai Station of Purple Mountain Observatory, NAOC,
in April 2002. At the observing frequency of 115.271\,GHz, the
width
 of the half-power beam is $54''$. The pointing and tracking accuracy
 is better than $10''$. An AOS spectrometer was used, which has 1024
  channels and with a total bandwidth of 170\,MHz. The equivalent
  velocity resolution is 0.43\,km/s. The spectral line intensity
  $T^*_A$ was calibrated with ambient temperature. The antenna
  efficiency $\eta_{\rm fss}$ is 0.50. All spectra were taken in the absolute
   position-switching mode. The 7$\times$7 points maps were made almost
   centered on IRAS 02310+6133, whose equatorial coordinates is
   $\alpha(1950)=02^h30^m56.4^s$, $\delta(1950)=61^o33'15''$. The grid spacing
    was 1'. Data were reduced with Drawspec software package. Winsurf
    was used for the analysis of the contours and spectra.

From the spectra detected, we can see line wings, and also find
line-centre velocity shift. There are two possible reasons for
this shift (Jiang et al. 2001): one is the rock effect and the
other is the rotation. Compared the distribution of line-centre
velocity grids with the contours of the outflow, the shift is
possibly caused by rotation. If we ignore this, the outflow
analysis and the core emission intensity will be affected.

 Taking the shift into account, we get the wing emission
intensity contours. The result shows that, the red lobe is
compact. The blue lobe is not as compact as the red one.
Nevertheless, a bipolar structure is apparent. Though there are
two IRAS sources in this region, the real source that dominates
this region is IRAS02310+6133. The outflow parameters are listed
in Table1. Column 1 is the distance from us. Column 2 is mean size
of the outflows. Column 3 is its mass. Column 4 is the mass lost
rate. Momentum, energy and time scale are listed in column 5, 6
and 7, respectively. Column 8 represents the mean velocity of the
outflow. Column 9 is the mechanical luminosity and the force is
listed in the last column. Their unit are listed in the second
row.

 In the core emission contours, two H$_2$O masers are close
to the dominant IRAS source (Zinchenko et al. 1998; Palagi et al.
1993). We can also find that IRAS 02310+6133 is deviated from the
core emission peak. Maybe the core is a new star formation region.

 The observations show that there are wings in CO
$J=1-0$ spectra.
 Also, there are line-centre velocity shift, which may be caused
  by rotation. Taken the shift into account, emissions of wings and
   the core were analyzed. From the wing emission intensity
   contours, a bipolar structure is apparent and its parameters are
   calculated. IRAS 02310+6133 is deviated from the core emission peak.
   Maybe the core is a new star formation region.

\bc{\small\bf

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

\fns \tabcolsep 1mm
\begin{tabular}{cccccccccc}
\hline\\[-3.6mm]\hline
 D   & $R_{\rm mean}$& Mass      &  $M_{\rm lost}$  &P &E&t&v&$L_{\rm
 mech}$&F\\
 kpc & pc & M$_{\odot}$ &  M$_{\odot}{\cdot}$yr$^{-1}$&
 M$_{\odot}{\cdot}$km${\cdot}$s$^{-1}$&erg&yr&km/s&L$_{\odot}$&M$_{\odot}{\cdot}
 $km${\cdot}
 $s$^{-1}{\cdot}$yr$^{-1}$\\
 \hline
3.8&2.06&508.1& 2.45$\times10^{-5}$ & 2.52$\times10^3$ &1.0$\times10^{47}$
& 5.15$\times10^{5}$
& 4.98&1.59& 3.1$\times10^{-3}$ \\
 \hline\\[-3.6mm]\hline%\\[-4.5mm]\hline
 \end{tabular}
 \ec

 \vs\vn{\bf ACKNOWLEDGEMENTS}~~ We are grateful to
the faculty of Qinghai Station, Purple Mountain Observatory for
the CO J=1-0 observations. This research was supported, in part by
NSFC grant 10128306, NSFC grant 10133020 and NKBRSF G1999075405.

\bc {\bf References} \ec

\vspace{-4mm} \no \fns

 \no Comoretto G., Palagi F., Cesaroni R., et al., A\&A, 1990, 84,179C\\
\no Jiang L., Wu Y., Miller M., CSB, 2001, 46, 1514\\
\no Palagi F., Cesaroni R., Comoretto G., et al., A\&AS, 1993, 101, 153P\\
\no Wu Y., Li Y., L$\ddot{u}$ J., et al., ACTA Astrophysica Sinica, 1998, 18, 415\\
\no Zinchenko I., Pirogov L., Torisevo M., A\&AS, 1998, 133, 137\\

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