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Aims: Previous observations of the young massive star formation region IRAS19410+2336 have revealed strong outflow activity with several interactingoutflows. We aim to get a better understanding of the outflow activity in thisregion by observing the SiO and H$^{13}$CO$^+$ emission with high angularresolution. SiO is known to trace shocked gas, which is often associated withyoung energetic outflows. With the H$^{13}$CO$^+$ data, we intend to betterunderstand the distribution of the quiescent gaseous component of the region.Methods: The SiO observations in the J=2-1 v=0 transition and H$^{13}$CO$^+$J=1-0 observations were performed by the Plateau de Bure Interferometer,combined with IRAM 30 m single-dish observations, in order to get the missingshort-spacing information. We complement this new high-resolution observationwith earlier CO and H$_2$ data. Results: The SiO observations do not trace thepreviously in CO and H$_2$ identified outflows well. Although we identifyregions of highly increased SiO abundance indicative of shock interaction,there are hardly any bipolar structures in the data. The southern part of theregion, which exhibits strong H$_2$ emission, shows almost no SiO. The CO andSiO data show only weak similarities, and the main SiO emission lies betweenthe two dominating dust clumps of the region. Conclusions: Most SiO emission islikely to be a result of high-velocity shocks due to protostellar jets.However, this does not explain all the emission features and additionaleffects; for example, colliding gas flows at the interface of the two mainregions may play an important role in the origin of the emission. The presentSiO data show that several different effects can influence SiO emission, whichmakes the interpretation of SiO data more difficult than often assumed.

SiO: Not the perfect outflow tracer: Outflow studies of the massive star formation region IRAS 19410+2336