Properties of spherical galaxies and clusters with an NFW density profile
By E. Lokas, G. Mamon. 2000
248 citations recorded by the source corpus.
Using the standard dynamical theory of spherical systems, we calculate the properties of spherical galaxies and clusters whose density profiles obey the universal form first obtained in high-resolution cosmological N-body simulations by Navarro, Frenk & White (NFW). We adopt three models for the internal kinematics: isotropic velocities, constant anisotropy and increasingly radial Osipkov–Merritt anisotropy. Analytical solutions are found for the radial dependence of the mass, gravitational potential, velocity dispersion, energy and virial ratio and we test their variability with the concentration parameter describing the density profile and amount of velocity anisotropy. We also compute structural parameters, such as half-mass radius, effective radius and various measures of concentration. Finally, we derive projected quantities, the surface mass density and line-of-sight as well as aperture-velocity dispersion, all of which can be directly applied in observational tests of current scenarios of structure formation. On the mass scales of galaxies, if constant mass-to-light is assumed, the NFW surface density profile is found to fit Hubble–Reynolds laws well. It is also well fitted by Sersic R1/m laws, for but in a much narrower range of m and with much larger effective radii than are observed. Assuming in turn reasonable values of the effective radius, the mass density profiles imply a mass-to-light ratio that increases outwards at all radii.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/1622d5db1caaae5dc254d94aacbdadc1bb2fe976
How researchers see this paper
The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.
In Astronomy and Astrophysics
Citations in the corpus
- Dark matter in elliptical galaxies — II. Estimating the mass within the virial radius (2004, background): “…interstellar medium contribute to their X-ray emission, and the latter component should contribute non-negligiblyto the 3 Note that the definition ofgd is the inverse of the definition ofg given by Łokas & Mamon (2001) for the NFW model. c© 2005 RAS, MNRAS000, 000–000 mass budget of ellipticals.”
- The ATLAS3D project XV: benchmark for early-type galaxies scaling relations from 260 dynamical models: mass-to-light ratio, dark matter, fundamental plane and mass plane (2012, background): “Our trend in the ratio is more significant than the generally assumed near constancy around 0.40 ± 0.02, first reported by Spitzer (1969) for different polytropes, which agrees with the theoretical value r1/2/rg = (1 + √ 2)/6 ≈ 0.402 for a Hernquist (1990) profile (Mamon 2000; Łokas & Mamon 2001).”
- The distribution and kinematics of early high-σ peaks in present-day haloes: implications for rare objects and old stellar populations (2005, background): “The projected luminosity profiles of elliptical galaxies follow the R1/4 law and resemble rescaled versions of projected CDM halo density profiles (L okas & Mamon 2001; Merrit et al. 2005), similar to the z = 0 profiles of our high-σ subsets.”
- Constraints on star formation driven galaxy winds from the mass–metallicity relation at z= 0 (2010, background): “Roughly speaking, v2vir ∼ Φ ∼ GMhalo Rhalo , (18) where the dependence of the halo radiusRhalo on the halo mass is a function of both cosmology and the structure of the halo (Łokas & Mamon 2001; Ferrarese 2002; Loeb & Peebles 2003; Baes et al. 2003).”
- MAMPOSSt: Modelling Anisotropy and Mass Profiles of Observed Spherical Systems – I. Gaussian 3D velocities (2012, methodology): “We use the NFW model, in projection (Bartelmann 1996; Łokas & Mamon 2001), to fit the projected number density profile of the tracer.”
- Flux- and volume-limited groups/clusters for the SDSS galaxies: catalogues and mass estimation (2014, methodology): “The σsky for the NFW profile is calculated by integrating the projected NFW density (Bartelmann, 1996; Łokas & Mamon, 2001).”