We present a high-angular-resolution molecular line and millimeter continuum study of the massive star formation site IRAS 05358+3543 .
Observations with the Plateau de Bure Interferometer in CO 1–0 , SiO 2–1 and H ^ { 13 } CO ^ { + } 1–0 reveal at least three outflows which can not be separated in single-dish data .
Observations at millimeter and sub-millimeter wavelengths from the IRAM 30 m telescope and the CSO provide additional information on the region .
The most remarkable feature is a highly collimated ( collimation factor \sim 10 ) and massive ( > 10 M _ { \odot } ) bipolar outflow of \sim 1 pc length , which is part of a quadrupolar outflow system .
The three observed molecular outflows forming the IRAS 05358+3543 outflow system resemble , in structure and collimation , those typical of low-mass star-forming regions .
They might therefore , just like low-mass outflows , be explained by shock entrainment models of jets .
We estimate a mass accretion rate of \sim 10 ^ { -4 } M _ { \odot } /yr , sufficient to overcome the radiative pressure of the central object and to build up a massive star , lending further support to the hypothesis that massive star formation occurs similarly to low-mass star formation , only with higher accretion rates and energetics .
In the millimeter continuum , we find three sources near the center of the quadrupolar outflow , each with a mass of 75–100 M _ { \odot } .
These cores are associated with a complex region of infrared reflection nebulosities and their embedded illuminating sources .
The molecular line data show that SiO is found mostly in the outflows , whereas H ^ { 13 } CO ^ { + } traces core-like structures , though likely with varying relative abundances .
Thermal CH _ { 3 } OH comprises both features and can be disentangled into a core-tracing component at the line center , and wing emission following the outflows .
A CO line-ratio study ( using data of the J = 1 - 0 , 2 - 1 \leavevmode \nobreak \& \leavevmode \nobreak 6 - 5 transitions ) reveals local temperature gradients .