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Modelling the emission of HNCO towards IRAS16293-2422 using a new set of collisional coefficients

Published online by Cambridge University Press:  04 September 2018

A. Hernández-Gómez
Affiliation:
Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Morelia 58089, Mexico IRAP, Université de Toulouse, CNRS, UPS, CNES, Toulouse, France
E. Sahnoun
Affiliation:
Université de Tunis El Manar, Tunisia
E. Caux
Affiliation:
IRAP, Université de Toulouse, CNRS, UPS, CNES, Toulouse, France
L. Wiesenfeld
Affiliation:
Université Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France
L. Loinard
Affiliation:
Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Morelia 58089, Mexico
S. Bottinelli
Affiliation:
IRAP, Université de Toulouse, CNRS, UPS, CNES, Toulouse, France
K. Hammami
Affiliation:
Université de Tunis El Manar, Tunisia
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Abstract

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Isocyanic acid (HNCO) is a simple molecule containing the four main atoms essential for life and can be considered as a prebiotic molecule. To model the HNCO emission in the IRAS16293-2422 class 0 low-mass protostar, we used a new set of HNCO collisional coefficients with ortho-H2 and para-H2, computed from a set of rotational excitation quenching rates between HNCO and H2 based on a novel potential energy surface for the rigid molecules interactions. We present here the HNCO Potential Energy Surface used to compute this new set of collisional coefficients and the result of the IRAS16293-2422 HNCO spectrum modelling using them.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2018 

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