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Extragalactic Ammonia

Published online by Cambridge University Press:  30 March 2016

C. Henkel ,
K.M. Menten ,
J. Braatz ,
R. Mauersberger ,
A. Weiß ,
M. Lebrón ,
A. Tarchi ,
A. B. Peck ,
C. L. Carilli  and
D. A. Lubowich
C. Henkel
Affiliation:
MPIfR, Auf dem Hügel 69, D-53121 Bonn, Germany
K.M. Menten
Affiliation:
MPIfR, Auf dem Hügel 69, D-53121 Bonn, Germany
J. Braatz
Affiliation:
NRAO, PO Box 2, Green Bank, WV 24944, USA
R. Mauersberger
Affiliation:
IRAM, Avda. Divina Pastora 7, E-18012 Granada, Spain
A. Weiß
Affiliation:
IRAM, Avda. Divina Pastora 7, E-18012 Granada, Spain
M. Lebrón
Affiliation:
Arecibo Observatory, PO Box 53995, Arecibo, PR 00612, USA
A. Tarchi
Affiliation:
Istituto de Radioastronomia, CNR, 1-40129 Bologna, Italy
A. B. Peck
Affiliation:
CfA, SAO/SMA Project, PO Box 824, Hilo, HI 96721, USA
C. L. Carilli
Affiliation:
NRAO, PO Box 0, Socorro, NM 87801, USA
D. A. Lubowich
Affiliation:
Hofstra University and AIP, Hempstead, NY 11550, USA

Abstract

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Multi-line data of ammonia (NH3) are presented for Maffei 2, IC 342, and the starburst galaxies NGC 253 and M 82. While in M 82 the NH3 emitting gas is cool, presumably arising from well shielded dense cores deeply embedded in an environment dominated by Photon Dominated Regions, the other galaxies show ‘warm’ and ‘hot’ components that may be heated by shocks, ion-slip or cosmic rays. Interferometric observations show the detailed large scale distribution of NH3 in galaxies for the first time. The first multi-line studies of ammonia at significant redshifts (z = 0.65 and 0.89) are also reported and rotational temperatures, measures of the kinetic temperature of the emitting gas, are derived for all sources.

Type
I. Joint Discussions
Information
Highlights of Astronomy , Volume 13 , 2005 , pp. 879 - 881
Copyright
Copyright © Astronomical Society of Pacific 2005

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