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 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 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

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.

Constraints on the Clumpiness of Dark Matter Halos Through Heating of Disk Galaxies

2003 ◽  
Vol 10 ◽  
pp. 95-95
Author(s):  
E. Ardi ◽  
T. Tsuchiya ◽  
A. Burkert
Keyword(s):  
Dark Matter ◽  
Disk Galaxies ◽  
Dark Matter Halos

Constrained Simulations of Dark Matter Halos

2006 ◽  
Vol 20 ◽  
pp. 15-18
Author(s):  
Y. Hoffman ◽  
E. Romano-Díaz ◽  
A. Faltenbacher ◽  
D. Jones ◽  
C. Heller ◽  
...  
Keyword(s):  
Dark Matter ◽  
Dark Matter Halos

scholarly journals Modeling dark matter halos with nonlinear field theories

2021 ◽  
Vol 103 (10) ◽  
Author(s):  
R. A. C. Correa ◽  
P. H. R. S. Moraes ◽  
A. de Souza Dutra ◽  
O. L. Dors ◽  
W. de Paula ◽  
...  
Keyword(s):  
Dark Matter ◽  
Field Theories ◽  
Dark Matter Halos ◽  
Nonlinear Field

scholarly journals On the formation and stability of fermionic dark matter halos in a cosmological framework

2020 ◽  
Author(s):  
Carlos R Argüelles ◽  
Manuel I Díaz ◽  
Andreas Krut ◽  
Rafael Yunis
Keyword(s):  
Black Hole ◽  
Dark Matter ◽  
Space Distribution ◽  
Coarse Grained ◽  
Dark Matter Halos ◽  
The Core ◽  
The Galaxy ◽  
Gravitating Systems ◽  
The Given ◽  
First Time

Abstract The formation and stability of collisionless self-gravitating systems is a long standing problem, which dates back to the work of D. Lynden-Bell on violent relaxation, and extends to the issue of virialization of dark matter (DM) halos. An important prediction of such a relaxation process is that spherical equilibrium states can be described by a Fermi-Dirac phase-space distribution, when the extremization of a coarse-grained entropy is reached. In the case of DM fermions, the most general solution develops a degenerate compact core surrounded by a diluted halo. As shown recently, the latter is able to explain the galaxy rotation curves while the DM core can mimic the central black hole. A yet open problem is whether this kind of astrophysical core-halo configurations can form at all, and if they remain stable within cosmological timescales. We assess these issues by performing a thermodynamic stability analysis in the microcanonical ensemble for solutions with given particle number at halo virialization in a cosmological framework. For the first time we demonstrate that the above core-halo DM profiles are stable (i.e. maxima of entropy) and extremely long lived. We find the existence of a critical point at the onset of instability of the core-halo solutions, where the fermion-core collapses towards a supermassive black hole. For particle masses in the keV range, the core-collapse can only occur for Mvir ≳ E9M⊙ starting at zvir ≈ 10 in the given cosmological framework. Our results prove that DM halos with a core-halo morphology are a very plausible outcome within nonlinear stages of structure formation.

Clustering dependence of Chandra COSMOS Legacy AGN on host galaxy properties

2019 ◽  
Vol 15 (S356) ◽  
pp. 226-226
Author(s):  
Viola Allevato
Keyword(s):  
Dark Matter ◽  
Formation Rate ◽  
Stellar Mass ◽  
Active Galaxies ◽  
Host Galaxy ◽  
Mass Star ◽  
Mass Relation ◽  
Dark Matter Halos ◽  
X Ray

AbstractThe presence of a super massive BH in almost all galaxies in the Universe is an accepted paradigm in astronomy. How these BHs form and how they co-evolve with the host galaxy is one of the most intriguing unanswered problems in modern Cosmology and of extreme relevance to understand the issue of galaxy formation. Clustering measurements can powerfully test theoretical model predictions of BH triggering scenarios and put constraints on the typical environment where AGN live in, through the connection with their host dark matter halos. In this talk, I will present some recent results on the AGN clustering dependence on host galaxy properties, such as galaxy stellar mass, star formation rate and specific BH accretion rate, based on X-ray selected Chandra COSMOS Legacy Type 2 AGN. We found no significant AGN clustering dependence on galaxy stellar mass and specif BHAR for Type 2 COSMOS AGN at mean z ∼ 1.1, with a stellar - halo mass relation flatter than predicted for non active galaxies in the Mstar range probed by our sample. We also observed a negative clustering dependence on SFR, with AGN hosting halo mass increasing with decreasing SFR. Mock catalogs of active galaxies in hosting dark matter halos with logMh[Msun] > 12.5, matched to have the same X-ray luminosity, stellar mass and BHAR of COSMOS AGN predict the observed Mstar - Mh, BHAR - Mh and SFR-Mh relations, at z ∼ 1.

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