The various origin of dwarf galaxies revealed by numerical simulations

Massive galaxies like our Milky-Way are surrounded by many dwarf satellite galaxies. Standard cosmological models assume that the later ones were formed very early in the Universe and result from the collapse of primordial fluctuations ; they would then have steered clean of the merging process that destroyed many of their congeneric while hierarchically forming the most massive galaxies. Hence, the observed abundance of these dwarf satellites, as well as their spatial distribution, are fundamental tests for cosmological scenarios, that shed light both on the structure of the Universe and the nature of dark matter haloes in which they are orbiting. The number of dwarf galaxies in our Local Group - much lower than expected - is a serious problem for the standard cosmological scenario. Similarly, the observation of an anisotropic distribution of dwarf galaxies around their massive hosts in large surveys, in particular the Sloan Digital Sky Survey (SDSS), has recently nourished many debates. However, before using dwarf galaxies as a tracer of the evolution of the Universe, one should make sure that they all actually have a primordial cosmological origin. Indeed, another process possibly forming dwarf satellite galaxies has been pointed out for more than a decade : when massive spiral galaxies collide, they build up long Antennae-like tidal tails. In these tails, new dwarf galaxies can form : the so-called « Tidal Dwarf Galaxies ». Whether these tidal dwarfs can survive after the collision of their massive parent galaxies, and subsequently have a noticeable contribution to the total number of dwarf galaxies in the Universe are fundamental questions. Up to now, observational attempts failed to provide satisfying answers. Indeed, it is hard to distinguish dwarf galaxies of tidal origin from primordial dwarfs as soon as they are a few hundred million years old.

tdg-f1.jpg Figure 1 : Example of a numerical simulation of the collision of two spiral galaxies. Each snapshot corresponds to a particular stage of the process : at T=0, beginning of the collision ; at T=300 million years, formation of dense substructures (future dwarf galaxies) in two long tidal tails ; at T=1 billion years, the long-lived tidal dwarfs appear as satellite galaxies orbiting around their progenitors that have now merged into one single massive galaxy (see also the movie below). To the bottom-left, is an enlargement of one of these tidal dwarfs unveiling its internal spiral structure, in a very-high resolution simulation (10 parsecs). The color code is as follows : red for regions dominated by old stars, blue for regions dominated by young stars and interstellar gas. Click on the picture to enlarge it  

Figure 1 : Example of a numerical simulation of the collision of two spiral galaxies. Each snapshot corresponds to a particular stage of the process : at T=0, beginning of the collision ; at T=300 million years, formation of dense substructures (future dwarf galaxies) in two long tidal tails ; at T=1 billion years, the long-lived tidal dwarfs appear as satellite galaxies orbiting around their progenitors that have now merged into one single massive galaxy (see also the movie below). To the bottom-left, is an enlargement of one of these tidal dwarfs unveiling its internal spiral structure, in a very-high resolution simulation (10 parsecs). The color code is as follows : red for regions dominated by old stars, blue for regions dominated by young stars and interstellar gas. Click on the picture to enlarge it  Researchers from Paris Observatory and CEA/Saclay have used numerical simulations to resolve this issue (see Figure 1). They have simulated in a realistic way nearly one hundred of collisions between spiral galaxies, and identified about 600 dwarf galaxies formed in their tidal tails, which enabled them to study their evolution statistically. They have shown that even if a large fraction of tidal dwarfs are short-lived, about one fourth survive several billion years. These long-lived objects look like new satellite galaxies, orbiting around their progenitor - whose collision is over - exactly like primordial dwarf galaxies.

tdg-film.avi Movie of a numerical simulation showing the collision and merging of two massive spiral galaxies. Two long tidal tails develop, inside which several dwarf galaxies form (as well as lower-mass objects, probably globular clusters). Note in particular the object formed at the tip of the tail on top of the movie : this tidal dwarf galaxy contains nearly 2 percent of the mass of its progenitor, and survives for several billion years, orbiting around the central galaxy (the two progenitor spirals finally merge into one single galaxy). Some other objects more rapidly fall back onto their massive parents. Colors correspond respectively to regions dominated by old stars (red) and by young stars and interstellar gas (blue). Click to download the complete high-resolution movie (27 Mo, AVI format)  

Movie of a numerical simulation showing the collision and merging of two massive spiral galaxies. Two long tidal tails develop, inside which several dwarf galaxies form (as well as lower-mass objects, probably globular clusters). Note in particular the object formed at the tip of the tail on top of the movie : this tidal dwarf galaxy contains nearly 2 percent of the mass of its progenitor, and survives for several billion years, orbiting around the central galaxy (the two progenitor spirals finally merge into one single galaxy). Some other objects more rapidly fall back onto their massive parents. Colors correspond respectively to regions dominated by old stars (red) and by young stars and interstellar gas (blue). Click to download the complete high-resolution movie (27 Mo, AVI format)  The statistical analysis of the large set of simulations demonstrates that only a few percents of the dwarf galaxies present in the Universe can have such a tidal origin. Yet, this fraction is likely to be much higher in some regions, like the neighborhood of early-type and elliptical galaxies, as well as compact galaxy groups in which the contribution of tidal dwarfs could even be of the same order as that of primordial ones. Numerical simulations also indicate how tidal dwarfs are spatially distributed around their massive host galaxies : their distribution is anisotropic and limited in radius. Then, the presence of these tidal dwarfs is likely to modify the statistical properties of the overall population of dwarf satellites. This must be accounted for before using statistics on dwarf satellites to constrain cosmological scenarios and the nature of dark matter. Besides, the anisotropic distribution of tidal dwarfs around their host recalls that of observed dwarf satellite in the SDSS survey (see Figure 2).

tdg-f2_en.jpg Figure 2 : Spatial distribution of tidal dwarf galaxies in numerical simulations, compared to the observed distribution of dwarf satellites around their massive hosts (results from the SDSS, Yang et al. 2006). Both distributions are anisotropic : simulated tidal dwarf galaxies, like observed dwarfs, tend to concentrate at low inclinations towards the equatorial plane of their host galaxy. Lastly, this work proves that dwarf galaxies of tidal origin, formed a few billion years ago in collisions of massive galaxies, certainly exist. Their observational quest is now an important goal, for their internal dark matter content is also a fundamental test - only young, still forming, tidal dwarfs have been observed sofar. Whether old tidal dwarfs contain dark matter or not will help refining cosmological scenarios. See also : CEA Press release, and CNRS Press release.

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Reference From Tidal Dwarf Galaxies to Satellite Galaxies Bournaud F. & Duc P.-A. Astronomy and Astrophysics, in press ; astro-ph/0605350

Contact Frederic Bournaud (Observatoire de Paris, LERMA/CNRS)

Figure 2 : Spatial distribution of tidal dwarf galaxies in numerical simulations, compared to the observed distribution of dwarf satellites around their massive hosts (results from the SDSS, Yang et al. 2006). Both distributions are anisotropic : simulated tidal dwarf galaxies, like observed dwarfs, tend to concentrate at low inclinations towards the equatorial plane of their host galaxy. Lastly, this work proves that dwarf galaxies of tidal origin, formed a few billion years ago in collisions of massive galaxies, certainly exist. Their observational quest is now an important goal, for their internal dark matter content is also a fundamental test - only young, still forming, tidal dwarfs have been observed sofar. Whether old tidal dwarfs contain dark matter or not will help refining cosmological scenarios. See also : CEA Press release, and CNRS Press release.

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Reference From Tidal Dwarf Galaxies to Satellite Galaxies Bournaud F. & Duc P.-A. Astronomy and Astrophysics, in press ; astro-ph/0605350

Contact Frederic Bournaud (Observatoire de Paris, LERMA/CNRS)

Lastly, this work proves that dwarf galaxies of tidal origin, formed a few billion years ago in collisions of massive galaxies, certainly exist. Their observational quest is now an important goal, for their internal dark matter content is also a fundamental test - only young, still forming, tidal dwarfs have been observed sofar. Whether old tidal dwarfs contain dark matter or not will help refining cosmological scenarios. See also : CEA Press release, and CNRS Press release.

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Reference From Tidal Dwarf Galaxies to Satellite Galaxies Bournaud F. & Duc P.-A. Astronomy and Astrophysics, in press ; astro-ph/0605350

Contact Frederic Bournaud (Observatoire de Paris, LERMA/CNRS)

Dernière modification le 4 mars 2013