The population of cosmic voids

Details The population of cosmic voids The population of cosmic voids

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007arep...51..787a&link_type=abstract

Astronomy Reports, Volume 51, Issue 10, pp.787-796

Astronomy and Astrophysics

Astronomy

4

98.65.Dx, 95.35.+D, 98.80.-K, Superclusters, Large-Scale Structure Of The Universe, Dark Matter, Cosmology

Scientific paper

We consider the main population of cosmic voids in a heirarchical clustering model. Based on the Press-Schechter formalism modified for regions in the Universe with reduced or enhanced matter densities, we construct the mass functions for gravitationally bound objects of dark matter occupying voids or superclusters. We show that the halo mass functions in voids and superclusters differ substantially. In particular, the spatial density of massive ( M ˜ 1012 M &sun;) halos is appreciably lower in voids than in superclusters, with the difference in the mass functions being greater for larger masses. According to our computations, an appreciable fraction of the mass of matter in voids should be preserved to the present epoch in the form of primordial gravitationally bound objects (POs) with modest masses (to 10% for M PO < 109 M &sun;) keeping baryons. These primordial objects represent “primary blocks” in the heirarchical clustering model. We argue that the oldest globular clusters in the central regions of massive galaxies are the stellar remnants of these primordial objects: they can form in molecular clouds in these objects, only later being captured in the central regions of massive galaxies in the process of gravitational clustering. Primordial objects in voids can be observed as weak dwarf galaxies or Lyα absorption systems.

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