Results 141 to 150 of about 33,866 (165)

EVOLUTION OF THE GALAXY–DARK MATTER CONNECTION AND THE ASSEMBLY OF GALAXIES IN DARK MATTER HALOS [PDF]

open access: yesAstrophysical Journal, 2012
37pages, 20 figures, major revision, data updated to SDSS DR7, main conclusions remain ...
Xiaohu Yang   +2 more
exaly   +3 more sources

The Connection Between Galaxies and Their Dark Matter Halos [PDF]

open access: yesAnnual Review of Astronomy and Astrophysics, 2018
In our modern understanding of galaxy formation, every galaxy forms within a dark matter halo. The formation and growth of galaxies over time is connected to the growth of the halos in which they form. The advent of large galaxy surveys as well as high-resolution cosmological simulations has provided a new window into the statistical relationship ...
Risa H Wechsler, Jeremy L Tinker
exaly   +3 more sources

THE SPHERICALIZATION OF DARK MATTER HALOS BY GALAXY DISKS [PDF]

open access: yesAstrophysical Journal Letters, 2010
Cosmological simulations indicate that cold dark matter (CDM) halos should be triaxial. Verifying observationally this theoretical prediction is, however, less than straightforward because the assembly of galaxies is expected to modify the halo shapes and to render them more axisymmetric.
Stelios Kazantzidis, Julio F Navarro
exaly   +4 more sources

Dark Matter in the Halo of the Galaxy

2002
We consider a self-gravitating noninteracting fermion gas at nonzero temperature as a model for the dark matter halo of the Galaxy. This fermion gas model is then shown to imply the existence of a supermassive compact dark object at the Galactic center.
Bilić, Neven   +2 more
openaire   +3 more sources

Formation and Evolution of Galaxy Dark Matter Halos and Their Substructure [PDF]

open access: yesAstrophysical Journal, 2007
We use the ``Via Lactea'' simulation to study the co-evolution of a Milky Way-size LambdaCDM halo and its subhalo population. While most of the host halo mass is accreted over the first 6 Gyr in a series of major mergers, the physical mass distribution [not M_vir(z)] remains practically constant since z=1.
Piero Madau
exaly   +4 more sources

Structure and history of Dark Matter halos in galaxies and galaxy systems

International School of Physics “Enrico Fermi”, 2011
We investigate the structure and history of Dark Matter (DM) halos in galaxies and galaxy systems. Our theoretical framework is provided by the two-stage cosmogonical development of DM halos, and by the related “α-profiles”. The latter solve the Jeans equation for the self-gravitating DM equilibria, and yield the radial runs of the ...
Lapi, Andrea, CAVALIERE A.
openaire   +2 more sources

Galaxy halos and the nature of dark matter

AIP Conference Proceedings, 1995
One of the few observational facts that we know about dark matter is that within about one tenth of the virial radius, the dark halos of some galaxies have density profiles which fall with the radius as ρ(r)∝rn, where n≊0. Any successful dark matter candidate must be able to reproduce these observations.
exaly   +2 more sources

The Scaling Relations of Galaxy Clusters and Their Dark Matter Halos [PDF]

open access: yesAstrophysical Journal, 2004
18 pages, 3 figures, ApJ, accepted version.
Alberto Cappi, Giovanni Zamorani
exaly   +3 more sources

Modeling galaxy halos using dark matter with pressure

open access: yesPhysical Review D, 2003
We investigate whether a dark matter with substantial amounts of pressure, comparable in magnitude to the energy density, could be a viable candidate for the constituent of dark matter halos. We find that galaxy halos models, consistent with observations of flat rotation curves, are possible for a variety of equations of state with anisotropic ...
Bharadwaj, Somnath, Kar, Sayan
exaly   +3 more sources

Giant dark matter halos of galaxies

Physics Letters A, 1995
Abstract An analysis of rotation curves of several spiral galaxies is presented. The giant halo dimensions and the effective moments of birth of these galaxies are determined.
A.V. Gurevich, V.A. Sirota, K.P. Zybin
openaire   +1 more source

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