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2006MNRAS.371..885R - Mon. Not. R. Astron. Soc., 371, 885-897 (2006/September-2)
On the formation of dwarf galaxies and stellar haloes.
READ J.I., PONTZEN A.P. and VIEL M.
Abstract (from CDS):
We show that the BBBs have stellar distributions which are spheroidal, of low rotational velocity, old and metal poor: they resemble the dwarf spheroidal galaxies (dSphs) of the Local Group (LG). Unlike the LG dSphs, however, they contain significant gas fractions. We connect these high-redshift BBBs to the smallest dwarf galaxies observed at z = 0 using linear theory. A small fraction (∼100) of these gas-rich BBBs at high redshift fall in to a galaxy the size of the Milky Way (MW). We suggest that 10 per cent of these survive to become the observed LG dwarf galaxies at the present epoch. This is consistent with recent numerical estimates. Those infalling haloes on benign orbits which keep them far away from the MW or Andromeda manage to retain their gas and slowly form stars - these become the smallest dwarf irregular galaxies; those on more severe orbits lose their gas faster than they can form stars and become the dwarf spheroidals. The remaining 90 per cent of the BBBs will be accreted. We show that this gives a metallicity and total stellar mass consistent with the MW old stellar halo.
Abstract Copyright: 2006 The Authors. Journal compilation © 2006 RAS
Journal keyword(s): galaxies: haloes - galaxies: kinematics and dynamics - cosmology: theory
Simbad objects: 4
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