CH3CN J = 8 - 7 and CS J = 3 - 2 emission in orion KL

Details CH3CN J = 8 - 7 and CS J = 3 - 2 emission in orion KL CH3CN J = 8 - 7 and CS J = 3 - 2 emission in orion KL

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995ap%26ss.229..301z&link_type=abstract

Astrophysics and Space Science, Volume 229, Issue 2, pp.301-310

Astronomy and Astrophysics

Astrophysics

3

Star Formation, Molecular Lines, Radiation Transfer, Orion Kl

Scientific paper

The data of the line series CH3CN 8(K) - 7(K) K = 0 - 7 and line CS J = 3 - 2 were taken simultaneously. At beam size of 16″ the emissions of CH3CN and CS have a common center position located near IRc2 with deviations Δα ˜ -8″ and Δδ ˜ 5″. The observed data show that in Orion KL core the integrated intensities of the two species have double peaks separated by a space of 14″. The 2-dimension Gaussian fitting plots (FWHM) are ellipses ofD maj = 26″ andD min = 22″ for CH3CN 8(K) - 7(K) K = 3 - 6 andD'maj = 39″ D'min = 31″ for CS J = 3 - 2 at a distance about 450 pc. Towards the multiple line emission region of CH3CN 8(K) - 7(K) K = 3 - 6, using a simplified very large velocity gradient model to solve the statistical equilibrium and radiative transfer equations, we find to fit the observed results, the optimum physical parameters and kinetic temperatureT k˜ 120 K, densityn(H a) ˜ 1.2 × 105 cm-3, velocity gradientV gr˜ 92 km s-1 pc-1 and the local abundance of CH3CNF ab˜ 3 × 10-8. However towards the region of single line emission of CS J = 3 - 2 we have to use LTE and the optical thin approximation on the assumption ofT k= 120 K to obtain the lower limits of column density and then, an averaged abundance of CS of 6 × 10-8.

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