Herschel observations of extra-ordinary sources: Sulfur carbon chains and silicon bearing species in Orion KL

Details Herschel observations of extra-ordinary sources: Sulfur carbon chains and silicon bearing species in Orion KL Herschel observations of extra-ordinary sources: Sulfur carbon chains and silicon bearing species in Orion KL

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..280p.351t&link_type=abstract

The Molecular Universe, Posters from the proceedings of the 280th Symposium of the International Astronomical Union held in Tole

Astronomy and Astrophysics

Astronomy

Scientific paper

We present a study of sulphur carbon chains (CS and OCS) and silicon bearing molecules (SiO and SiS) in the Orion KL region at the HIFI frequencies (479.5-801.2, 858.1-1239.0, 1425.9-1906.7 GHz). The study of these species at the HIFI domain together with a previous and parallel work done with the IRAM 30m telescope allow us to constraint the physical parameters of the Orion KL components. Due to the large number of transitions in different vibrationally excited states covered by our data, we can provide reliable source average column densities (and therefore, isotopologue abundances and vibrational temperatures) for the detected molecules. In addition, we provide a wide study of the physical properties of the source based on the different spectral components found in the emission lines. We have modeled the lines of the detected molecules using a radiative transfer code, which permit us to choose between Large Velocity Gradient (LVG) and Local Thermodynamic Equilibrium (LTE) approximations depending on the physical conditions of the gas. We have detected C32S, C34S, 13CS, C33S, OCS, OC34S, SiO, 29SiO, 30SiO, SiS in the ground vibrationally state. For 13C34S, CS v}=1, O13CS, OCS ν_2=1, Si18O, SiO v}=1, 29SiS, Si34S, and SiS v}=1 we present only tentative detections. As for the 30m results, SiS shows its peak emission at 16 km s-1; this feature could be an extended component that probably arises from the interaction of the outflow with the ambient cloud. In the modelize of the source, we have to introduce different stratifications of the three well known components of Orion KL plateau, hot core, and compact ridge to better reproduce the line profiles of the emission lines, providing a deeper view on the physical parameters in this source.

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