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    {\small\rm\zihao{6}\songti\thepage\hfill
    \quad\quad ACTA ASTRONOMICA SINICA \hfill
    \hspace{2mm} Vol.44\vspace{2mm}}}} %%%%%%%
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    {\small\rm \zihao{6}\songti suppl.\hfill Y. Wang \& Y. F. Wu: A Mapping Study of High-velocity Gas near Young Stellar Object  %%（作者：题目名称）
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    \zihao{6}\songti
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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 A Mapping Study of High-velocity Gas near \\[2mm]Young Stellar Object    %%（文题）
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\vs\vs{\normalsize\zihao{4}\fangsong Y. Wang \hs\&\hs Y. F. Wu  }  %%（本文作者）

\vs (\footnotesize{\it School of Physics, Peking University,
Beijing}~100871 ) \vs\vs \ec

\normalsize
\begin{quotation}

 \no{\bf A{\scriptsize\bf BSTRACT }}~~~\small It is generally believed that during the earliest stages of
evolution, stars undergo a phase of very energetic mass ejection,
frequently characterized by the occurrence of massive bipolar
outflows of molecular gas. The broad molecular emission line is an
evidence of high-velocity molecular gas, but it also the evidence
of turbulence and rotation. So mapping the region of high-velocity
is an effective method to identify the outflows. The Outflows
Catalog (Wu et al. 1996) still have some objects that did not
mapped. We identified the high high-velocity gas of three outflow
candidates with the observation by 13.7m telescope at Qinhai
Station. In this paper we present the result and discussion.

\end{quotation}

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

\vs\vs
 Star formation have many kinetic phases. Molecule outflows are an important
phenomenon in the formation process. Observations of the ambient
molecular gas accelerated by stellar winds are a powerful means to
study the energetic phenomenon in the star formation process
(Snell et al. 1990). Particularly, mapping is useful to
investigate the property of high velocity gas. In 1985 the first
Outflows Catalog is made by Lada, that includes 67 sources, some
unmapped. The second catalog is made by Fukui in 1989, that
includes 144 sources, all mapped. The third catalog is made by Wu
et al.in 1996, that includes 264 sources, 28 unmapped. In 2002,
our group try to renew the old Outflow Catalog
 and the select criterion is all sources must be mapped. We selected
 three sources from the Outflows Catalog (Wu et al. 1996) which are not mapped
 and listed in Table 1.

 \bc{\small\bf

 Table 1~~   Selected sources
}\\[2mm]

\fns \tabcolsep 4mm
\begin{tabular}{ccc}
\hline\\[-3.6mm]\hline
 NAME & $\alpha$ (1950)  & $\delta$ (1950) \\
\hline
05379-0757 & 05:37:56.0 & -07:57:390) \\
LKH $\alpha$ 325 & 03:25:48.0 & 30:34:00 \\
RNO131 & 21:02:24.0 &   67:55:00 \\
 \hline\\[-3.6mm]\hline%\\[-4.5mm]\hline
 \end{tabular}
 \ec


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

\vs\vs
  The observation of the J=1-0 transition of  CO were obtained with
  the 13.7\,m telescope of Qinghai station of Purple Mountain Observatory
  from March to May in
2002. The center frequency is 115.271\,GHz, and the beam size is
54$''$ in corresponding  frequency. Point and track precision is
better than 10$''$. An AOS spectrum meter was used, which has 1024
channels and a total bandwidth of 170\,MHz. The data calibration
was made with software of Drawspec and protract by Surfer7.0.

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

\vs\vs  The three sources were detected in CO J=1-0 emission as
point sources(Morgan \& Bally 1991; Ball \& Lada 1983; Cohen
1980). We got the 7X7 point maps, spaced by 54", centered on each
of the reference position listed in Table 1. The strategy reduced
the chance of missing outflows, since outflow emission is often
extended and separated from the driving stellar source (Snell et
al. 1990).


 Based on our mapping data, we analysed two respects for identifying
 outflow activity: 1. emission over a large velocity extent must be present.
 A typical outflow appears as spatially confined wings beyond the emission from
the cloud core;
 2. the high-velocity emission must be spatially confined to the region near the
 far-infrared source. The blueshifted and redshifted gas emission intensities
 are calculated.

1) LKH$\alpha$ 325

This source lies adjacent to IRAS 03257+3034. And it is at a
distance of 0.5\,kpc.  CO spectra have a velocity extent of
13\,km/s. We didn't get an obvious outflow structure either.

2) 05379-0757

This is an IR source that lies adjacent to another IRAS 05379-0758.
And it is
 at a distance of 0.5\,kpc. From the  CO spectra we can see a velocity extent about
 9.1\,km/s. We made contours of integrate CO emission to both core and
 in blue and red line wings. Although we can see the obvious line wings in
spectra, we did not get a visible outflow component in these maps.

3) RNO131

 This source lies adjacent to IRAS 21023+6754. The  CO spectra velocity extent
 are about 14\,km/s. We may get an outflow component in the northeast. Because the
 center of the component seem to out of our grid map, we can not confirm that
 it is really an outflow.


  We check the environment of the three sources by Simbad and find that there
  are a few IR sources around the 05379-0757. We think that there would be a
  star cluster and the environment is complicated that we can not detect a
  visible outflow
 structure. And the environment of LKH$\alpha$325 is clean, maybe this region is
 in an early phase that do not have outflows. Toward RNO131 we need to map a
 larger region
to identify the outflow component in the northeast in the future.

 \vs\vn{\bf ACKNOWLEDGEMENTS}~~ This project
is supported by the G1999075405 NKBRSF, the NSFC Grant 10128306
and 10133020.


\bc {\bf References} \ec

\vspace{-4mm} \no \fns

 \nref Wu Y, Huang M, He J. A\&A, 1996, 283: 115
 \nref Snell R L, Dickman R L, Huang Y L. ApJ, 1990,352: 139
 \nref Morgan J A, John B. ApJ, 1991, 372: 507
 \nref Bally, J., Lada C J. ApJ, 1983, 265: 827
 \nref Fukui, Y., 1989, in Reipurth, B.(ed.) ESO workshop on Low Mass Star Formation and Pre-Main Sequence Objects. P. 95
 \nref Lada, C. J., 1985, ARA\&A, 23, 267
 \nref Martin C. AJ, 1980, 85: 31c

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