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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

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

Keywords

Protostarsmolecular emissionnon-LTE modelling
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S332: Astrochemistry VII: Through the Cosmos from Galaxies to Planets , March 2017 , pp. 435 - 439
Copyright
Copyright © International Astronomical Union 2018 

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