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Molecular Gas in Tidal Dwarf Galaxies: On-going Galaxy Formation

Published online by Cambridge University Press:  26 May 2016

J. Braine ,
P.-A. Duc ,
U. Lisenfeld ,
E. Brinks ,
V. Charmandaris  and
S. Leon
J. Braine
Affiliation:
Observatoire de Bordeaux, UMR 5804, B.P. 89, F-33270 Floirac, France
P.-A. Duc
Affiliation:
CEA/DSM/DAPNIA, Service d'Astrophysique, Saclay, France
U. Lisenfeld
Affiliation:
IAA, CSIC, Granada, Spain
E. Brinks
Affiliation:
INAOE, Puebla, Mexico
V. Charmandaris
Affiliation:
Cornell University, Astronomy Department, Ithaca, NY, USA
S. Leon
Affiliation:
IAA, CSIC, Granada, Spain

Abstract

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We investigate the process of galaxy formation as can be observed in the only currently forming galaxies - the so-called Tidal Dwarf Galaxies, hereafter TDGs - through observations of the molecular gas detected via its CO (Carbon Monoxide) emission. Molecular gas is a key element in the galaxy formation process, providing the link between a cloud of gas and a bona fide galaxy. We have now detected CO in 9 TDGs with an overall detection rate of 80%, showing that molecular gas is abundant in TDGs, up to a few 108M⊙. The CO emission coincides both spatially and kinematically with the HI emission, indicating that the molecular gas forms from the atomic hydrogen where the HI column density is high. A possible trend of more evolved TDGs having greater molecular gas masses is observed, in accord with the transformation of HI into H2. Although uncertainties are still large for individual objects as the geometry is unknown, we find that the “dynamical” masses of TDGs, estimated from the CO line widths, do not seem to be greater than the “visible” masses (HI + H2 + a stellar component), i.e., TDGs require no dark matter. We provide evidence that TDGs are self-gravitating entities, implying that we are witnessing the ensemble of processes in galaxy formation: concentration of large amounts of gas in a bound object, condensation of the gas, which is atomic at this point, to form molecular gas and the subsequent star formation from the dense molecular component.

Type
Part 4. Recycling
Information
Symposium - International Astronomical Union , Volume 217: Recycling Intergalactic and Interslettar Matter , 2004 , pp. 518 - 525
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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