Hot Molecular Gas in NGC 2024

M. Emprechtinger; M.C. Wiedner; R. Simon; G. Wieching; N.H. Volgenau; U.U. Graf; R. Güsten; C.E. Honingh; K. Jacobs; J. Stutzki; F. Wyrowski

doi:10.1051/eas:0831034

All issues

Volume 31 (2008)

EAS Publications Series, 31 (2008) 173-175

Abstract

Issue		EAS Publications Series Volume 31, 2008 Far-Infrared Workshop 2007


Page(s)		173 - 175
DOI		https://doi.org/10.1051/eas:0831034
Published online		04 October 2008

Far-Infrared Workshop 2007
C. Kramer, S. Aalto and R. Simon (eds)
EAS Publications Series, 31 (2008) 173-175

Hot Molecular Gas in NGC 2024

M. Emprechtinger¹, M.C. Wiedner¹, R. Simon¹, G. Wieching¹^,2, N.H. Volgenau¹, U.U. Graf¹, R. Güsten², C.E. Honingh¹, K. Jacobs¹, J. Stutzki¹ and F. Wyrowski²

¹ I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany
² Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany

Abstract

We present observations of five ¹²CO and ¹³CO lines in NGC 2024, including the first velocity resolved observations of lines above 1 THz in this object (J = 13–12). We analysed the observations using radiative transfer codes and derived a more consistent model of this complex source. We found that the high-J CO emission stems from a dense (n ~ 10⁶ cm^-3) and hot (~300 K) component, located at the interface of the H II region and the molecular cloud.