Empirical models for Dark Matter Halos

By Alister W. Graham, D. Merritt, B. Moore, J. Diemand, Balsa Terzic. 2005

202 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/23ad60bc32963bf427226357755267a9f1aa0e7d

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Citations in the corpus

Modified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic Extensions (2011, background): “int towards Einasto [134] proﬁles with dlnρ/dlnr ∝ −r(1/n) (with n slightly varying with halo mass, and n ∼ 6 for a Milky Way-sized halo, meaning that the slope is zero only very close to the nucleus [178], and is still ∼ −1 at 200 pc from the center), ﬁtting such proﬁles to observed galactic kinema”
Formation of Galaxy Clusters (2012, methodology): “Subsequent simulations (Graham et al. 2006, Merritt et al. 2006, Navarro et al. 2004) showed that the Einasto (1965) profile and other similar models signed to describe deprojection of the Sérsic profile (Merritt et al. 2006) provide a more accurate description of the DM density profiles arising…”
Extended gamma-ray emission from Coy Dark Matter (2014, methodology): “The Einasto [56] and Navarro, Frenk and White (NFW) [57] profiles are traditionally used as benchmark profiles as they provide good fits to dark matter numerical simulations [58].”
THE SPLASHBACK RADIUS AS A PHYSICAL HALO BOUNDARY AND THE GROWTH OF HALO MASS (2015, background): “…Rsp can be measured from the halo density profile as the radius where the density profile steepens sharply beyond what is expected from the Navarro–Frenk–White density profile (Navarro et al. 1997, hereafter NFW) or the Einasto profile (Einasto 1965; Navarro et al. 2004; Graham et al. 2006).”
A novel determination of the local dark matter density (2009, unknown): “The latest simulations favor the Einasto profile [45, 46]:”
Inclination- and dust-corrected galaxy parameters: bulge-to-disc ratios and size–luminosity relations (2008, background): “…equations to convert projected densities such as 〈µ〉e into threedimensional densities, are given in Terzić & Graham (2005), Merritt et al. (2006) and Graham et al. (2006a). equation (5) after applying the appropriate stellar mass-toluminosity ratio M/L. Equation (10) has the same functional…”
CLASH: JOINT ANALYSIS OF STRONG-LENSING, WEAK-LENSING SHEAR, AND MAGNIFICATION DATA FOR 20 GALAXY CLUSTERS (2015, background): “…NFW) over a wide range of halo masses and radii, with some intrinsic variance associated with the mass accretion histories of individual halos (Jing & Suto 2000; Tasitsiomi et al. 2004; Graham et al. 2006; Navarro et al. 2010; Ludlow et al. 2013; Diemer & Kravtsov 2014; Adhikari et al. 2014).”
Dark matter annihilations and decays after the AMS-02 positron measurements (2013, methodology): “Besides, ρDM(~r) denotes the density of dark matter particles in the Milky Way halo, which we assume to be spherically symmetric and with a radial distribution described by the Einasto profile [21–23],”
CLASH: WEAK-LENSING SHEAR-AND-MAGNIFICATION ANALYSIS OF 20 GALAXY CLUSTERS (2014, background): “…equilibrium halos (Navarro et al. 1996, hereafter, NFW) over a wide range of halo masses, with some intrinsic variance associated with mass accretion histories of individual halos (Jing & Suto 2000; Merritt et al. 2006; Graham et al. 2006; Navarro et al. 2010; Gao et al. 2012; Ludlow et al. 2013).”