Bibcode
Bahé, Y. M.; Schaye, Joop; Barnes, David J.; Dalla Vecchia, C.; Kay, Scott T.; Bower, Richard G.; Hoekstra, Henk; McGee, Sean L.; Theuns, Tom
Referencia bibliográfica
Monthly Notices of the Royal Astronomical Society, Volume 485, Issue 2, p.2287-2311
Fecha de publicación:
5
2019
Número de citas
62
Número de citas referidas
53
Descripción
We investigate the disruption of group and cluster satellite galaxies
with total mass (dark matter plus baryons) above 10^{10} M_⊙ in the
Hydrangea simulations, a suite of 24 high-resolution cosmological
hydrodynamical zoom-in simulations based on the EAGLE model. The
simulations predict that ˜50 per cent of satellites survive to
redshift z = 0, with higher survival fractions in massive clusters than
in groups and only small differences between baryonic and pure N-body
simulations. For clusters, up to 90 per cent of galaxy disruption occurs
in lower-mass subgroups (i.e. during pre-processing); 96 per cent of
satellites in massive clusters that were accreted at z < 2 and have
not been pre-processed survive. Of those satellites that are disrupted,
only a few per cent merge with other satellites, even in low-mass
groups. The survival fraction changes rapidly from less than 10 per cent
of those accreted at high z to more than 90 per cent at low z. This
shift, which reflects faster disruption of satellites accreted at higher
z, happens at lower z for more massive galaxies and those accreted on to
less massive haloes. The disruption of satellite galaxies is found to
correlate only weakly with their pre-accretion baryon content, star
formation rate, and size, so that surviving galaxies are nearly unbiased
in these properties. These results suggest that satellite disruption in
massive haloes is uncommon, and that it is predominantly the result of
gravitational rather than baryonic processes.
Proyectos relacionados
Astrofísica Numérica: Formación y Evolución de Galaxias
Entre las cuestiones fundamentales en Astronomía y Astrofísica están la formación y evolución de galaxias. Las escalas de tiempo y tamaño son tan astronómicas que su observación en galaxias individuales es imposible. Solo con el uso de simulaciones numéricas es posible entender la formación de estructuras cósmicas dentro del actual marco
Claudio
Dalla Vecchia