4 research outputs found
Are compact groups hostile towards faint galaxies?
The goal of this work is to understand whether the extreme environment of
compact groups can affect the distribution and abundance of faint galaxies
around them. We performed an analysis of the faint galaxy population in the
vicinity of compact groups and normal groups. We built a light-cone mock galaxy
catalogue constructed from the Millennium Run Simulation II plus a
semi-analytical model of galaxy formation. We identified a sample of compact
groups in the mock catalogue as well as a control sample of normal galaxy
groups and computed the projected number density profiles of faint galaxies
around the first- and the second-ranked galaxies. We also compared the profiles
obtained from the semi-analytical galaxies in compact groups with those
obtained from observational data. In addition, we investigated whether the
ranking or the luminosity of a galaxy is the most important parameter in the
determination of the centre around which the clustering of faint galaxies
occurs. There is no particular influence of the extreme compact group
environment on the number of faint galaxies in such groups compared to control
groups. When selecting normal groups with separations between the 1st and 2nd
ranked galaxies similar to what is observed in compact groups, the faint galaxy
projected number density profiles in compact groups and normal groups are
similar in shape and height. We observed a similar behaviour of the population
of faint galaxies in observations and simulations in the regions closer to the
1st and 2nd ranked galaxies. Finally, we find that the projected density of
faint galaxies is higher around luminous galaxies,regardless of the ranking in
the compact group. The semi-analytical approach shows that compact groups and
their surroundings do not represent a hostile enough environment to make faint
galaxies to behave differently than in normal groups.Comment: 12 pages, 10 figures. Accepted for publication in Astronomy &
Astrophysic
Are compact groups hostile towards faint galaxies?
Aims: The goal of this work is to understand whether the extreme environment of compact groups (CGs) can affect the distribution and abundance of faint galaxies around them. Methods: We performed an analysis of the faint galaxy population in the vicinity of compact and normal groups. We built a light-cone mock galaxy catalogue constructed from the Millennium Run Simulation II plus a semi-analytical model of galaxy formation. We identified a sample of CGs in the mock catalogue as well as a control sample of normal galaxy groups and computed the projected number density profiles of faint galaxies around the first and the second ranked galaxies. We also compared the profiles obtained from the semi-analytical galaxies in CGs with those obtained from observational data. In addition, we investigated whether the ranking or the luminosity of a galaxy is the most important parameter in the determination of the centre around which the clustering of faint galaxies occurs. Results: There is no particular influence of the extreme compact group (CG) environment on the number of faint galaxies in such groups compared to control groups. When selecting normal groups with separations between the first and second ranked galaxies similar to what is observed in CGs, the faint galaxy projected number density profiles in CGs and normal groups are similar in shape and height. We observed a similar behaviour of the population of faint galaxies in observations and simulations in the regions closer to the first and second ranked galaxies. Finally, we find that the projected density of faint galaxies is higher around luminous galaxies, regardless of the ranking in the CG. Conclusions: The semi-analytical approach shows that CGs and their surroundings do not represent a hostile enough environment to make faint galaxies behave differently than in normal groups.Fil: Zandivarez, Arnaldo Ariel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomia Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomia Teórica y Experimental; ArgentinaFil: Diaz, Maria Eugenia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomia Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomia Teórica y Experimental; ArgentinaFil: Oliveira, Claudia Mendes de. Universidade do Sao Paulo. Instituto Astronomia, Geofisica e Ciencias Atmosfericas; BrasilFil: Gubolin, Henrique. Universidade do Sao Paulo. Instituto Astronomia, Geofisica e Ciencias Atmosfericas; Brasi
Bondi accretion, numerical hydrodynamic simulations
Spherically symmetric hydrodynamical simulations of Bondi accretion, performed in two and three dimensions, using the PLUTO code. <div><br></div><div>These simulations reproduce the B1 and G3 cases of Ruffert et al. 1994 ApJ.</div><div><br></div><div>Part of MsC dissertation work of Henrique Gubolin, under the supervision of Prof. Rodrigo Nemmen.</div><div><br></div><div>Included are:</div><div>• DBL datasets with grids, density, velocities and pressure fields</div><div>• initial and boundary condition information necessary to reproduce the simulations with Pluto</div><div>• movies showing the evolution of some fields</div
Simple 2D torus simulation with alpha viscosity
2D hydrodynamical simulations of a torus with alpha viscosity and Newtonian potential. Very similar to the setup of Stone et al. 1999 (MNRAS).<div><br></div><div>Each file in the dataset contains 100 DBL with snapshots of the density field in successive times. <div><br></div><div>Generated with the Pluto MHD code. Problem setup, including initial and boundary conditions in file `pluto_init.zip`. </div><div><br></div><div>Movies of time evolution of density and mass accretion rate in `movies.zip`.</div></div