scholarly journals Interactions of Satellite Galaxies in Cosmological Dark Matter Halos

2004 ◽  
Vol 21 (2) ◽  
pp. 216-221 ◽  
Author(s):  
Alexander Knebe ◽  
Stuart P. D. Gill ◽  
Brad K. Gibson
Keyword(s):  
Dark Matter ◽  
Statistical Analysis ◽  
Dark Matter Halos ◽  
Simulation Data ◽  
Clear Trend ◽  
Satellite Galaxy ◽  
Self Consistent ◽  
Cluster Satellite ◽  
Satellite Galaxies ◽  
A New Technique

AbstractWe present a statistical analysis of the interactions between satellite galaxies in cosmological dark matter halos taken from fully self-consistent high-resolution simulations of galaxy clusters. We show that the number distribution of satellite encounters has a tail that extends to as many as three to four encounters per orbit. On average 30% of the substructure population had at least one encounter (per orbit) with another satellite galaxy. However, this result depends on the age of the dark matter host halo with a clear trend for more interactions in younger systems. We also report a correlation between the number of encounters and the distance of the satellites to the centre of the cluster — satellite galaxies closer to the centre experience more interactions. However, this can be simply explained by the radial distribution of the substructure population and merely reflects the fact that the density of satellites is higher in those regions.In order to find substructure galaxies we applied (and present) a new technique based upon theN-body code MLAPM. This new halo finder MHF (MLAPM’s halo finder) acts with exactly the same accuracy as theN-body code itself and is therefore free of any bias and spurious mismatch between simulation data and halo finding precision related to numerical effects.

scholarly journals Warm dark matter model with a few keV mass is bad for the too-big-to-fail problem

2019 ◽  
Vol 491 (2) ◽  
pp. 2520-2535 ◽  
Author(s):  
Xi Kang
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Analytical Description ◽  
Realistic Model ◽  
Analytical Models ◽  
Satellite Galaxy ◽  
The Galaxy ◽  
Dynamical Simulations ◽  
Satellite Galaxies ◽  
Tidal Heating

ABSTRACT Theoretical studying of the very inner structure of faint satellite galaxy requires very high-resolution hydro-dynamical simulations with realistic model for star formation, which are beginning to emerge recently. In this work, we present an analytical description to model the inner kinematic of satellites in the Milky Way (MW). We use a Monte Carlo method to produce merger trees for MW mass halo and analytical models to produce stellar mass in the satellite galaxies. We consider two important processes which can significantly modify the inner mass distribution in satellite galaxy. The first is baryonic feedback which can induce a flat inner profile depending on the star formation efficiency in the galaxy. The second is the tidal stripping to reduce and re-distribute the mass inside satellite. We apply this model to MW satellite galaxies in both CDM and thermal relic WDM models. It is found that tidal heating must be effective to produce a relatively flat distribution of the satellite circular velocities, to agree with the data. The constraint on WDM mass depends on the host halo mass. For a MW halo with dark matter mass lower than $2\times 10^{12}\, \text{ M}_\odot$, a 2 keV WDM model can be safely excluded as the predicted satellite circular velocities are systematically lower than the data. For WDM with mass of 3.5 keV, it requires the MW halo mass to be larger than $1.5\times 10^{12}\, {\text{ M}}_{\odot }$.

scholarly journals Self-consistent construction of virialized wave dark matter halos

2018 ◽  
Vol 97 (10) ◽  
Author(s):  
Shan-Chang Lin ◽  
Hsi-Yu Schive ◽  
Shing-Kwong Wong ◽  
Tzihong Chiueh
Keyword(s):  
Dark Matter ◽  
Dark Matter Halos ◽  
Self Consistent ◽  
Wave Dark Matter

Learning from interactions between the Milky Way and satellite galaxies

2017 ◽  
Vol 13 (S334) ◽  
pp. 349-350
Author(s):  
Go Ogiya
Keyword(s):  
Dark Matter ◽  
High Resolution ◽  
Gravitational Force ◽  
Milky Way ◽  
Tidal Force ◽  
Dark Matter Halos ◽  
Density Structure ◽  
Internal Structures ◽  
Satellite Galaxies

AbstractThe Milky Way (MW) is interacting with its satellite galaxies and the tidal remnants of satellite galaxies have been observed especially in the MW halo. Understanding the spatial and velocity distributions of stars stripped from satellite galaxies will be of particular importance when interpreting the data from upcoming observations, such as Gaia, Subaru-HSC and PFS. We study tidal stripping events of satellite galaxies with various internal structures using high resolution N-body simulations. The dynamics of satellite galaxies is dominated by dark matter halos, but their density structure is still uncertain. The simulations reveal satellite galaxies with more tightly bound dark matter halos are more robust against the tidal force of the MW and have longer lifetimes than loosely bound ones (Ogiya et al., in prep.). Density scratches on the MW caused by the gravitational force of satellite galaxies and the observability are also discussed (Ogiya & Burkert 2016).

scholarly journals Red Galaxies Growing in Dark Matter Halos

2009 ◽  
Vol 5 (H15) ◽  
pp. 87-87
Author(s):  
Michael J. I. Brown ◽  
Keyword(s):  
Dark Matter ◽  
Luminosity Function ◽  
Slow Growth ◽  
Stellar Mass ◽  
Dark Matter Halos ◽  
Massive Galaxies ◽  
Central Galaxy ◽  
Satellite Galaxies ◽  
Massive Halos ◽  
Red Galaxies

AbstractTo understand the slow growth of massive galaxies at z < 1, we have modeled how these galaxies populate dark matter halos. The models are constrained with the observed luminosity function and clustering of z < 1 red galaxies. In the most massive halos, much of the stellar mass resides within multiple satellite galaxies rather than a single central galaxy. Consequently, massive galaxies grow slowly within rapidly growing dark matter halos.

scholarly journals Self‐consistent Models of Cuspy Triaxial Galaxies with Dark Matter Halos

2007 ◽  
Vol 666 (1) ◽  
pp. 165-180 ◽  
Author(s):  
R. Capuzzo‐Dolcetta ◽  
L. Leccese ◽  
D. Merritt ◽  
A. Vicari
Keyword(s):  
Dark Matter ◽  
Dark Matter Halos ◽  
Self Consistent

scholarly journals Self‐Consistent Massive Disks in Triaxial Dark Matter Halos

2007 ◽  
Vol 667 (1) ◽  
pp. 191-201 ◽  
Author(s):  
Jeremy Bailin ◽  
Joshua D. Simon ◽  
Alberto D. Bolatto ◽  
Brad K. Gibson ◽  
Chris Power
Keyword(s):  
Dark Matter ◽  
Dark Matter Halos ◽  
Self Consistent

scholarly journals Modeling a high velocity LMC: The formation of the Magellanic Stream

2008 ◽  
Vol 4 (S256) ◽  
pp. 117-121
Author(s):  
Chiara Mastropietro
Keyword(s):  
Dark Matter ◽  
Vertical Structure ◽  
Milky Way ◽  
Large Magellanic Cloud ◽  
Low Density ◽  
Dark Matter Halos ◽  
Tidal Forces ◽  
Ram Pressure ◽  
Self Consistent ◽  
Magellanic Stream

AbstractI use high resolution N-body/SPH simulations to model the new proper motion of the Large Magellanic Cloud (LMC) within the Milky Way (MW) halo and investigate the effects of gravitational and hydrodynamical forces on the formation of the Magellanic Stream (MS). Both the LMC and the MW are fully self consistent galaxy models embedded in extended cuspy ΛCDM dark matter halos. I find that ram-pressure from a low density ionized halo is sufficient to remove a large amount of gas from the LMC's disk forming a trailing Stream that extends more than 120 degrees from the Cloud. Tidal forces elongate the satellite's disk but do not affect its vertical structure. No stars become unbound showing that tidal stripping is almost effectless.

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