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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 S. L. Qin \& Y. F. Wu: Two new outflows %%（作者：题目名称）
    \vspace{1.5mm}
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    \normalsize\rm
\zihao{5}\songti

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    \small\rm
    \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 Two New Outflows    %%（文题）
%\\[1ex]
%$\!\!^*$
}

\vs\vs{\normalsize\zihao{4}\fangsong  S.L. Qin\hs\&\hs Y.F. Wu}  %%（本文作者）

\vs
(\pka) \\%%（本文作者单位）
 (\bac)\\
 \vs\vs \ec

\normalsize

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

\vs\vs
High velocity outflows are useful to understanding the
 essential problems of star formation, e.g. the angle momentum problem
 and high star formation rate (Lada 1985, Bachiller 1996). Recently we searched
 a number of H$_{2}$O masers
and IRAS sources with $^{13}$CO J=1-0, C$^{18}$O J=1-0 and
$^{12}$CO J=1-0 lines, part of which are characteristic of high
velocity (Wu et al. 2000). The results of mapping for IRAS
05339-0646 and IRAS 07028-1100 with the $^{12}$CO J=1-0 line are presented.

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

\vs\vs
Observations for IRAS 05339-0646 and IRAS 07028-1100 were made
with 13.7\,m millimeter wave telescope at QingHai Station of Purple
Mountain Observatory in 2001. The $7\times7$ points maps of IRAS 05339-0646 and
IRAS 07028-1100 were centered at $\alpha(1950)=05^{\rm h}33^{\rm m}57.9^{\rm s},
\delta(1950)=-06^{\circ}46^{\prime}33.0^{\prime\prime}$ and
$\alpha(1950)=07^{\rm h}02^{\rm m}51.9^{\rm s},
\delta(1950)=-11^{\circ}00^{\prime}05.0^{\prime\prime}$,
respectively. The grid spacing was $1^{\prime}$, and the
integration time was 2 minutes for each position. Data were
reduced with Drawspec software package. Winsurf and Origin were
used for analyses of the contours and spectra.

   We analyzed every CO spectrum, then calculated emission intensities
   and  made contours for the two sources.
Both of them have the
high velocity, large measurable extents and the bipolar structure.
All these suggest that the wings result in outflow motions rather
than rotation, turbulence or collapse (Lada 1985, Myers 1988).



Figure1 is contours of these two sources, respectively. Symbol
triangle, plus, square and diamond represent IRAS sources, maser, HII region
and HH object, respectively.
 IRAS 05339-0646 locates in Ori A cluster. A compact core centered on
($\alpha(1950)=05^{\rm h}33^{\rm m}57.9^{\rm s},
\delta(1950)=-06^{\circ}46^{\prime}33.0^{\prime\prime}$) was measured
with $NH_{3}(1,1)$ line (Jijina et
al. 1999). Simbad data show that there
are one IRAS source, nine radio continuum, eight H$_{2}$O masers, one HII region and
twenty-two HH objects. HH objects are lined up in south-north direction, which are
the evidence of jet driven.

There is another IRAS source, i.e., IRAS 07027-1101 near IRAS 07028-1100.
From IRAS Point Source Catalogue, the fluxes of this two IRAS sources at
12, 25, 60, 100\,$\mu$m are 0.2893, 1.491, 35.09,  218.0\,Jy and
1.858,6.319, 35.09,121.7\,Jy, respectively. The fluxes at 12, 25\,$\mu$m of
IRAS 07027-1101 are smaller than
those of IRAS 07028-1100, but the flux at 100\,$\mu$m is larger than latter,
which suggest that IRAS 07028-1100 is older
than IRAS 07027-1101, that is, the former evolves earlier than the latter.

Using the method by Goldsmith et al.(1984), we calculated the outflow parameters.
Under the assumption of local thermodynamic equilibrium (LTE) and the
    wing being optical thin, the total column density of CO molecules can be
    obtained as below:

    \begin{eqnarray*}
 N_{\rm CO}={{4.2\times 10^{13}}\over{eXp(-5.5/T_{\rm ex})}}
T_{\rm ex}\int{T_{R}(v)dv}({\rm cm}^{-2})\,,
\end{eqnarray*}

\begin{figure}[h]
%\vspace*{-10mm}
\center {\includegraphics [bb=0 37 408 494,scale=0.6]{qsl.eps}}

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   %{\hspace{3.5cm}
  { %\center
   \footnotesize
    Fig.\,1~~ (a) Contour map of $^{12}$CO J=1-0 line wing integrated
intensities for IRAS 05339-0646. The blue wing contours (real line)
and the red wing contours(dashed line)
start at 12 and 8\,Kkms$^{-1}$ and increase at step of 2\,Kkms$^{-1}$,respectively
(b) Contour map of $^{12}$CO J=1-0 core integrated intensities for
IRAS 05339-0646. The contours start at 120\,Kkms$^{-1}$ with 10\,Kkms$^{-1}$ spacing.
(c)Contour map of $^{12}$CO J=1-0 line wing integrated
intensities for IRAS 07028-1100. The blue wing contours (real line) and the red
wing contours (dashed line) start at 22 and 10\,Kkms$^{-1}$ and increase
at step of 4 and 1.5\,Kkms$^{-1}$, respectively. Contour map of $^{12}$CO J=1-0 core
integrated intensities for IRAS 07028-1100. The contours extend
from 70\,Kkms$^{-1}$ with 10\,Kkms$^{-1}$ spacing.}

    \end{figure}

\no Here, $T_{\rm ex}$ is excited temperature. We take $T_{\rm ex}$ as 27 and 15\,K
for IRAS 05339-0646 and IRAS 07028-1100.
   If we further assume a CO abundance $X_{\rm CO}=[\rm CO]/[{\rm H}_2]=10^{-4}$,
   the column density of the HV gas is $N=N_{\rm CO}/{X_{\rm CO}}$.
   Outflow mass $M$ is obtained by summing the products of the column density and
   the area of all detected points in the map.
   The momentum P and energy E of the outflow are respectively proportional to the
   quantities $\sum\int T(v)vdv$   and   $\sum\int T(v)v^{2}dv$
     and can be evaluated similarly to the mass. The characteristic velocity of the
     wing is given by V=P/M.
     A dynamic time scale can be determined by $t_{d}=R/V$, where R is mean size of
     the outflow. We can estimate the force required to drive
      the outflow by $F=P/t_{d}$. The mechanical luminosity and the mass loss rate of
      the central star of the outflow are $L_{\rm mech}=E/t_{d}$ and
       $M_{\rm loss}=P/(t_{d}v_{w})$, where the final wind velocity is taken
      to be $v_{w}=100$\,km/s. The results of calculation are listed in Table
1.

The parameters of the central infrared sources are given in Table
2, where the fluxs are taken from the IRAS PSC and the bolometric luminosities are
calculated by using the formula
of Casoli et al (1986).

\bc{\small\bf

 Table 1~~   Outflow parameters
}\\[2mm]

\fns \tabcolsep 3mm
\begin{tabular}{ccccc}
\hline\\[-3.6mm]\hline
 Source    & size&           M  &         P                    &        E\\
 Name      & (pc)& ($M_{\odot}$)& ($M_{\odot}\,{\rm kms}^{-1}$)&(\rm erg)\\
 \hline
05339-0646 &  0.3&    3.5       &  32                          &   $2.4\times10^{45}$\\
07028-1100 &  1.2&     44       & 267                          & $13.5\times10^{45}$\\
\\

V          & t   & F            & L$_{\rm mech}$               & M$_{\rm loss}$\\
(M$_{\odot}$kms$^{-1}$)&(yr)& (kms$^{-1}$yr$^{-1}$)&($L_{\odot}$)&(M$_{\odot}$yr$^{-1}$)\\
\hline
 9.2& $4\times10^{4}$ & $0.9\times10^{-3}$ & 0.6 & $0.9\times10^{-5}$\\
  6.1& $24\times10^{4}$& $1.1\times10^{-3}$& 0.5&$1.1\times10^{-5}$\\
 \hline\\[-3.6mm]\hline
\end{tabular}
\ec

\vs\bc{\small\bf

 Table 2~~   Parameters of the infrared sources
}\\[2mm]

\fns \tabcolsep 4mm
\begin{tabular}{ccccccc}
\hline\\[-3.6mm]\hline
 Source&D    & $F_{12}$& $F_{25}$& $F_{60}$ & $F_{100}$& $L_{\rm bol}$\\
 Name  &(kpc)& (Jy)    & (Jy)    & (Jy)    & (Jy)     & ($L_{\odot}$)\\
\hline
05339-0646 &  0.5&    1.235&  5.404&   75.9& 192.9& 54\\
07028-1100 &  1.4&     1.858& 6.319& 35.09& 121.7& 279\\
\hline\\[-3.6mm]\hline
\end{tabular}
\ec

From Table 2, we can see that the bolometric luminosities of IRAS 05339-0646
and IRAS 07028-110
are 54 and 279$L_{\odot}$, respectively. The former is a low mass star, and the
latter belongs to medium
mass star. We also find that parameters of the outflow associated with
IRAS 07028-1100 are larger
than those of IRAS 05339-0646. Both of them are lower than that of high mass
outflows (Wu et al. 1996).

\vs\vn{\bf ACKNOWLEDGEMENT}~~ This project was supported by G1999075405 of
NKBRSF, 10128306 and 10133020.

\bc
{\bf References}
\ec

\vspace{-4mm}
\no \fns

 \no Bachiller R,  ARA\&A, 1996, 34: 111\\
\no Casoli F, Combes F, Dupraz C, et al.  A\&A, 1986, 169: 281\\
\no Goldsmith P F, Snell R L, Hemeno-Heyer M.  ApJ, 1984, 286: 599\\
\no Jijina J, Myers P C, Adams F C. ApJS, 1999, 125: 161\\
\no Lada C J.  ARA\&A, 1985, 23: 267\\
\no Myers P C, Snell R L, Goldsmith P F, et al.  ApJ, 1988, 324: 907\\
\no Wu Y, WU J, Wang J, et al.  ACTA, 2000, 20: 383\\
\no Wu Y, Huang M, He J.  A\&AS, 1996, 115: 283\\

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