scholarly journals Precision Determination of the Mass Function of Dark Matter Halos

2006 ◽  
Vol 646 (2) ◽  
pp. 881-885 ◽  
Author(s):  
Michael S. Warren ◽  
Kevork Abazajian ◽  
Daniel E. Holz ◽  
Luis Teodoro
Keyword(s):  
Dark Matter ◽  
Mass Function ◽  
Dark Matter Halos ◽  
Precision Determination

scholarly journals The emergence of the red sequence at z~2 seen through galaxy clustering in the UKIDSS UDS

2012 ◽  
Vol 8 (S295) ◽  
pp. 105-108
Author(s):  
William G. Hartley ◽  
Omar Almaini ◽  
Alice Mortlock ◽  
Chris Conselice ◽  
Keyword(s):  
Dark Matter ◽  
Cross Correlation ◽  
Near Infrared ◽  
Correlation Technique ◽  
Dark Matter Halos ◽  
Star Forming ◽  
Deep Survey ◽  
Cross Correlation Technique ◽  
Infrared Survey

AbstractWe use the UKIDSS Ultra-Deep Survey, the deepest degree-scale near-infrared survey to date, to investigate the clustering of star-forming and passive galaxies to z ~ 3.5. Our new measurements include the first determination of the clustering for passive galaxies at z > 2, which we achieve using a cross-correlation technique. We find that passive galaxies are the most strongly clustered, typically hosted by massive dark matter halos with Mhalo > 1013 M⊙ irrespective of redshift or stellar mass. Our findings are consistent with models in which a critical halo mass determines the transition from star-forming to passive galaxies.

scholarly journals Zeldovich and the Missing Baryons, Results from Gravitational Lensing

2014 ◽  
Vol 11 (S308) ◽  
pp. 380-381
Author(s):  
Rudolph E. Schild
Keyword(s):  
Dark Matter ◽  
Distribution Function ◽  
Gravitational Lensing ◽  
Mass Function ◽  
Gravitational Theory ◽  
Magellanic Clouds ◽  
Planetary Mass ◽  
Mass Distribution Function ◽  
Baryonic Dark Matter

AbstractCentral to Zeldovich's attempts to understand the origin of cosmological structure was his exploration of the fluid dynamical effects in the primordial gas, and how the baryonic dark matter formed. Unfortunately microlensing searches for condensed objects in the foreground of the Magellanic Clouds were flawed by the assumption that the objects would be uniformly (Gaussian) distributed, and because the cadence of daily observations strongly disfavored detection of planet mass microlenses. But quasar microlensing showed them to exist at planetary mass at the same time that a hydro-gravitational theory predicted the planet-mass population as fossils of turbulence at the time of recombination (z = 1100; Gibson 1996, 2001). Where the population has now been detected from MACHO searches to the LMC (Sumi et al. 2011) we compare the quasar microlensing results to the recent determination of the mass distribution function measured for the planetary mass function, and show that the population can account for the baryonic dark matter.

scholarly journals Testing dark matter halos using rotation curves and lensing: A warning on the determination of the halo mass

2010 ◽  
Vol 82 (2) ◽  
Author(s):  
Darío Núñez ◽  
Alma X. González-Morales ◽  
Jorge L. Cervantes-Cota ◽  
Tonatiuh Matos
Keyword(s):  
Dark Matter ◽  
Dark Matter Halos ◽  
Rotation Curves

scholarly journals Hierarchical Formation of Dark Matter Halos near the Cutoff Scale and Their Impact on Indirect Detections

2015 ◽  
Vol 11 (A29B) ◽  
pp. 742-742
Author(s):  
Tomoaki Ishiyama
Keyword(s):  
Dark Matter ◽  
Dwarf Galaxy ◽  
Theoretical Models ◽  
Mass Range ◽  
Mass Function ◽  
Dark Matter Halos ◽  
Density Profiles ◽  
Present Universe ◽  
Major Merger ◽  
Formation And Evolution

AbstractThe smallest dark matter halos are formed first in the early universe (e.g., Hofmann et al. 2001; Berezinsky et al. 2003; Ishiyama et al. 2010). We present results of very large cosmological N-body simulations of the hierarchical formation and evolution of halos over a wide mass range, beginning from the formation of the smallest halos. In the largest simulation, the motions of 40963 particles in comoving boxes of side lengths 400 pc and 200 pc were followed. The particle masses were 3.4 × 10−11M⊙ and 4.3 × 10−12M⊙, ensuring that halos at the cutoff scale were represented by 30,000 and 230,000 particles, respectively. We found that the central density cusp is much steeper in these halos than in larger halos (dwarf-galaxy-sized to cluster-sized halos), and scales as ρ ∝ r-(1.5–1.3). The cusp slope gradually becomes shallower as the halo mass increases.The slope of halos 50 times more massive than the smallest halo is approximately −1.3. No strong correlation exists between inner slope and the collapse epoch. The cusp slope of halos above the cutoff scale seems to be reduced primarily due to major merger processes. The concentration, estimated at the present universe, is predicted to be 60–70, consistent with theoretical models and earlier simulations, and ruling out simple power law mass-concentration relations. Such halos could still exist in the present universe with the same steep density profiles. Strongly depending on the subhalo mass function and the adopted concentration model, the steeper inner cusps of halos near the cutoff scale enhance the annihilation luminosity of a Milky Way sized halo between 12 to 67 (Ishiyama 2014).

Measuring Dark Matter Halos by Modeling Interacting Galaxies

2004 ◽  
Vol 220 ◽  
pp. 461-462 ◽  
Author(s):  
Christian Theis
Keyword(s):  
Genetic Algorithm ◽  
Dark Matter ◽  
Parameter Space ◽  
Matter Content ◽  
Interacting Galaxies ◽  
Dark Matter Halo ◽  
Dark Matter Halos ◽  
Characteristic Parameters ◽  
Galactic Dark Matter

The richness of tidal features seen in interacting galaxies allows for the determination of their characteristic parameters, provided one can deal with the extended parameter space. Genetic algorithm based methods – like our code minga – have proven to be such a tool. Here I discuss the implementation of dark matter halo descriptions in the restricted N-body simulations of minga. I show that the final morphology of a galaxy encounter strongly depends on the halo properties. Thus, modeling tidal features of interacting galaxies might allow also for conclusions on the galactic dark matter content.

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
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