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Tidal Dwarf Galaxies: Disc Formation at \(z\simeq0\)

Department of Astronomy, Case Western Reserve University, 10900 Euclid Ave, Cleveland, OH 44106,
Laboratoire AIM, CNRS, CEA/DSM, Université Paris Diderot, F-91191 Gif-sur-Yvette, France
Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, AL10 9AB, UK
Author to whom correspondence should be addressed.
Academic Editors: Alexei Moiseev, José Alfonso López Aguerri and Enrichetta Iodice
Galaxies 2015, 3(4), 184-191;
Received: 15 October 2015 / Revised: 28 October 2015 / Accepted: 2 November 2015 / Published: 5 November 2015
Collisional debris around interacting and post-interacting galaxies often display condensations of gas and young stars that can potentially form gravitationally bound objects: Tidal Dwarf Galaxies (TDGs). We summarise recent results on TDGs, which are originally published in Lelli et al. (2015, A&A).We study a sample of six TDGs around three different interacting systems, using high-resolution HI observations from the Very Large Array. We find that the HI emission associated to TDGs can be described by rotating disc models. These discs, however, would have undergone less than one orbit since the time of the TDG formation, raising the question of whether they are in dynamical equilibrium. Assuming that TDGs are in dynamical equilibrium, we find that the ratio of dynamical mass to baryonic mass is consistent with one, implying that TDGs are devoid of dark matter. This is in line with the results of numerical simulations where tidal forces effectively segregate dark matter in the halo from baryonic matter in the disc, which ends up forming tidal tails and TDGs. View Full-Text
Keywords: interacting galaxies; peculiar galaxies interacting galaxies; peculiar galaxies
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Lelli, F.; Duc, P.-A.; Brinks, E.; McGaugh, S.S. Tidal Dwarf Galaxies: Disc Formation at \(z\simeq0\). Galaxies 2015, 3, 184-191.

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