Are Disks of Satellites Comprised of Tidal Dwarf Galaxies?
Abstract
1. Introduction
2. Proposals to Explain the Existence of Disks of Satellites
3. The Simulation of B18
Predicted Proper Motions of the Members of the Disks of Satellites of Andromeda
4. Open Questions, Future Prospects
- Shortly after the simulation of B18 was published, it was found that there is a population of chemically and kinematically distinct stars in the Milky Way. They were interpreted as a remnant of an accreted dwarf galaxy that received the name Gaia-Enceladus [114] or Gaia-Sausage [115] and had a mass greater than the Large Magellanic Cloud. Later, evidence for another merger with a galaxy called Sequoia appeared [116]. Could these peculiar stellar populations have been actually formed by the Milky Way–Andromeda encounter? In our simulation, the encounter formed only a hint of a disk of satellites around the Milky Way. Could the disk of satellites have been formed after the merger with the Gaia-Enceladus/Sausage?
- The simulation of B18 contained several modeling simplifications that can be remedied in the future. It neglected the external field effect and cosmic expansion. As demonstrated by [42], these have an impact on the time since the encounter and the pericentric distance and velocity. The simulations could be improved by adding gas and star formation, which would help to address the formation and survival of tidal dwarf galaxies during the creation of the disks of satellites. The encounter might have caused a burst of star formation whose signature could be looked for observationally. The new simulations should be performed, taking into account the newest constraint on the proper motion of Andromeda. Another important goal would be to explore a larger space of free parameters. The parameters can include not only the proper motion of Andromeda but also the initial sizes and gas fractions of the galaxies. Exploration of the parameter space could, for example, clarify whether the flyby can produce a disk of satellites of the simulated Milky Way that has the correct mass and orientation. It would also clarify whether the planes of non-satellite dwarfs in the Local Group could be produced during the flyby.
- Is the origin of the planes of non-satellite dwarfs in the Local Group different from the disks of satellites?
- If all satellites of the Milky Way are tidal dwarf galaxies, which is suggested by the positions and velocities of the satellites, is it even possible that the Milky Way would have no primordial satellites? Pairs of close galaxies in an expanding universe first recede, following the Hubble flow, until their mutual gravity prevails and the galaxies become bound. They will be called a host and a satellite according to their mass. The satellites that have closer apocenters with respect to their hosts became bound at earlier cosmic epochs. Is it possible that the process of acquisition of satellites, that seems to be universal for any gravity model, had not worked for the Milky Way?
- As pointed out in B18, if the satellites in the disks are tidal dwarf galaxies, then their globular clusters should not be older than the time since the encounter. For the Local Group that means 7–11 Gyr. While, for example, some of the GCs of the Fornax dwarf appear older [117,118,119], it is generally difficult to exactly determine the ages of stellar populations of this age. It would be desirable to investigate this issue in detail in the future.
- Disks of satellites have been detected around all nearby massive galaxies. This suggests that disks of satellites are a common phenomenon. This brings up the question of whether galaxy flybys are frequent enough to explain all of these disks of satellites by the tidal dwarf scenario. It might be, because a few tens of percent of galaxies at high redshifts are seen to be just undergoing an interaction (e.g., [120,121,122]). A detailed comparison will be desirable once we have a better idea about how frequent disks of satellites are. It will be necessary also to address if all non-merging galaxy flybys that lead to mass transfer lead to the formation of disks of satellites.
Author Contributions
Funding
Acknowledgments
Conflicts of Interest
1 | There is currently another suitable public code, RayMOND [86], that can work not only in QUMOND but also in the AQUAL formulation of MOND [56]. It is available at (accessed on 25 October 2021) https://www.ifa.uv.cl/sites/graeme/codes.html. |
2 | Since the CDM model is argued to account for many cosmological phenomena, the cosmology in the final MOND theory, that is yet to be discovered, may resemble that in the CDM model. |
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Bílek, M.; Thies, I.; Kroupa, P.; Famaey, B. Are Disks of Satellites Comprised of Tidal Dwarf Galaxies? Galaxies 2021, 9, 100. https://doi.org/10.3390/galaxies9040100
Bílek M, Thies I, Kroupa P, Famaey B. Are Disks of Satellites Comprised of Tidal Dwarf Galaxies? Galaxies. 2021; 9(4):100. https://doi.org/10.3390/galaxies9040100
Chicago/Turabian StyleBílek, Michal, Ingo Thies, Pavel Kroupa, and Benoit Famaey. 2021. "Are Disks of Satellites Comprised of Tidal Dwarf Galaxies?" Galaxies 9, no. 4: 100. https://doi.org/10.3390/galaxies9040100
APA StyleBílek, M., Thies, I., Kroupa, P., & Famaey, B. (2021). Are Disks of Satellites Comprised of Tidal Dwarf Galaxies? Galaxies, 9(4), 100. https://doi.org/10.3390/galaxies9040100