Equilibrium Disk-Bulge-Halo Models for the Milky Way and Andromeda Galaxies

By L. Widrow, John Dubinski. 2005

202 citations recorded by the source corpus.

We describe a new set of self-consistent, equilibrium disk galaxy models that incorporate an exponential disk, a Hernquist model bulge, an NFW halo, and a central supermassive black hole. The models are derived from explicit distribution functions for each component, and the large number of parameters permit detailed modeling of actual galaxies. We present techniques that use structural and kinematic data such as radial surface brightness profiles, rotation curves, and bulge velocity dispersion profiles to find the best-fit models for the Milky Way and M31. Through N-body realizations of these models we explore their stability against the formation of bars. The models permit the study of a wide range of dynamical phenomenon with a high degree of realism.

Subfields: Astronomy and Astrophysics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/48d7dfc4113f203d40f540c74d23e1076f29ac7f

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In Statistical and Nonlinear Physics

Citations in the corpus

Interaction of Massive Black Hole Binaries with Their Stellar Environment. I. Ejection of Hypervelocity Stars (2006, background): “5We modeled the luminous component of the MW as in Miyamoto & Nagai (1975), and the dark matter halo as in Widrow & Dubinski (2005).”
The local dark matter density (2014, methodology): “Garbari et al. (2011) set up a mock Milky Way using a Widrow & Dubinski (2005) model, with 30 × 106 star ‘super-particles’ (see §2 for a definition of ‘super-particles’), and 15× 106 and 0.5× 106 super-particles for the dark matter halo and stellar bulge, respectively.”
Phantom: A Smoothed Particle Hydrodynamics and Magnetohydrodynamics Code for Astrophysics (2017, methodology): “To create a Milky Way-like galaxy, we used GalactICs (Kuijken & Dubinski, 1995b; Widrow & Dubinski, 2005; Widrow et al., 2008) to first create a galaxy con- sisting of a stellar bulge, stellar disc and a dark matter halo.”
Galaxy Masses: A Review (2013, methodology): “Dehnen & Binney (1998) and Widrow & Dubinski (2005) present a statistical method for accomplishing this and incorporate the Brand & Blitz (1993) data into their Galactic model constraints.”
GALAXIES IN ΛCDM WITH HALO ABUNDANCE MATCHING: LUMINOSITY–VELOCITY RELATION, BARYONIC MASS–VELOCITY RELATION, VELOCITY FUNCTION, AND CLUSTERING (2010, result): “We also include the results of mass modeling of the MW and M31 (Klypin et al. 2002; Widrow & Dubinski 2005).”
Gamma Ray Signals from Dark Matter: Concepts, Status and Prospects (2012, methodology): “sothermal proﬁle follow s when setting (α,β,γ) = (2,2,0) and rs ≃ 3.5 kpc (note, however, that matching observational constraints in principle results in a rather large range of allowed values for rs [75, 76]). Typically, kinematic observations of line-of-sight velocities do notsuﬃciently constrain ”
Merger Histories of Galaxy Halos and Implications for Disk Survival (2007, methodology): “Milky Way Comparison The Milky Way has a dark matter halo of mass M0 ≃ 1012h−1M⊙ (Klypin et al. 2002), and its stellar mass is dominated by a thin disk of mass ≃ 3.5 × 1010M⊙ (Klypin et al. 2002; Widrow & Dubinski 2005).”
Dynamical Blueprints for Galaxies (2008, methodology): “Since ourmodels assume a single disk component, we use amassweighted average (Widrow & Dubinski 2005).”