Table 4: Abundances for the two components of the IRAS 2A outflow compared to other outflows and protostellar environments.
Molecule IRAS 2A corea IRAS 2A winga L1157b HH2c BHR71d IRAS 2A env.e IR16293f L134Ng
CO =1 $~\times~ 10^{-4}$ =1 $~\times~ 10^{-4}$ =1 $~\times~ 10^{-4}$ =1 $~\times~ 10^{-4}$ =1 $~\times~ 10^{-4}$ 2 $~\times~ 10^{-5}$ 4 $~\times~ 10^{-5}$ =1 $~\times~ 10^{-4}$
CH3OH 6.7 $~\times~ 10^{-7}$ 4.8 $~\times~ 10^{-6}$ 2 $~\times~ 10^{-5}$ 2 $~\times~ 10^{-8}$ 2 $~\times~ 10^{-7}$ 2 $~\times~ 10^{-9}$ 3 $~\times~ 10^{-7}$$\dagger$ 8 $~\times~ 10^{-9}$
CS 1.1 $~\times~ 10^{-8}$ 2.7 $~\times~ 10^{-8}$ 2 $~\times~ 10^{-7}$ 7 $~\times~ 10^{-10}$ 6 $~\times~ 10^{-9}$ 3 $~\times~ 10^{-9}$ 3 $~\times~ 10^{-9}$ 1 $~\times~ 10^{-9}$
HCN 2.2 $~\times~ 10^{-9}$ 4.8 $~\times~ 10^{-9}$ 5 $~\times~ 10^{-7}$ 1 $~\times~ 10^{-9}$ - 2 $~\times~ 10^{-9}$ 1 $~\times~ 10^{-9}$ 7 $~\times~ 10^{-9}$
HCO+ 1.3 $~\times~ 10^{-9}$ 2.9 $~\times~ 10^{-9}$ 3 $~\times~ 10^{-8}$ 3 $~\times~ 10^{-8}$ 9 $~\times~ 10^{-10}$ 3 $~\times~ 10^{-9}$ 1 $~\times~ 10^{-9}$ 8 $~\times~ 10^{-9}$
H2CO 1.7 $~\times~ 10^{-8}$ 1.5 $~\times~ 10^{-8}$ 3 $~\times~ 10^{-7}$ 2 $~\times~ 10^{-8}$ - 8 $~\times~ 10^{-10}$ 6 $~\times~ 10^{-8}$$\dagger$ 2 $~\times~ 10^{-8}$
N2H+ 1.8 $~\times~ 10^{-9}$ $\ldots$ $\ldots$ - - 5 $~\times~ 10^{-9}$ 1 $~\times~ 10^{-10}$ 6 $~\times~ 10^{-10}$
SiO $\ldots$ 1.1 $~\times~ 10^{-7}$ 7 $~\times~ 10^{-8}$ $\ldots$ 7 $~\times~ 10^{-10}$ <5 $~\times~ 10^{-11}$ 5 $~\times~ 10^{-9}$$\dagger$ <1 $~\times~ 10^{-11}$h
SO 1.2 $~\times~ 10^{-8}$ 1.2 $~\times~ 10^{-7}$ 3 $~\times~ 10^{-7}$ 8 $~\times~ 10^{-9}$ - 3 $~\times~ 10^{-9}$ 3 $~\times~ 10^{-7}$$\dagger$ 6 $~\times~ 10^{-9}$
Notes: "-'' Molecule not observed. "$\ldots$'' Molecule observed but not detected.
aCore and wing part of IRAS 2A outflow (this paper).
bThe L1157 outflow (Bachiller & Pérez Gutiérrez 1997).
cThe HH2 molecular condensation (Girart et al. 2002).
dThe BHR71 outflow (Garay et al. 1998).
eThe IRAS 2A protostellar envelope (Jørgensen et al. 2002,2004b).
fThe IRAS 16293-2422 envelope (Schöier et al. 2002). "$\dagger$'' indicate abundances for the warm inner part of the envelope; other abundances are averages over the entire envelope.
gThe "C'' position of the L134N dark cloud (Dickens et al. 2000).
hDerived using upper limits on [SiO]/[HCN] abundance ratio for L134N of 0.0015 from Ziurys et al. (1989).

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