Fitting functions for dark matter density profiles

An, J.; Zhao, Hongsheng

doi:10.1093/mnras/sts175

Cited by 34 publications

(27 citation statements)

References 39 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Notice that the density has a harmonic core at the centre but falls like ρ ∼ r −4 at large radii. When α = 1, we obtain the super-NFW model (e.g., An & Zhao 2013;Lilley et al 2017). This has a central density cusp with ρ ∝ r −1 similar to the Hernquist (1990) or NFW models.…”

Section: Zeroth-order Modelsmentioning

confidence: 99%

“…There are of course other finite mass models which have such desirable properties. A number of models with ρ ∝ r −1 at the centre and with an asymptotic fall off with logarithmic gradient between -3 and -4 are already available in the literature (e.g., An & Zhao 2013). In general, these models are not the zeroth-order terms of any biorthorgonal expansion, so their axisymmetric and triaxial siblings are much more cumbersome to construct.…”

Section: Zeroth-order Modelsmentioning

confidence: 99%

See 1 more Smart Citation

Galaxy halo expansions: a new biorthogonal family of potential-density pairs

Lilley

Sanders

Evans

et al. 2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Efficient expansions of the gravitational field of (dark) haloes have two main uses in the modelling of galaxies: first, they provide a compact representation of numerically-constructed (or real) cosmological haloes, incorporating the effects of triaxiality, lopsidedness or other distortion. Secondly, they provide the basis functions for self-consistent field expansion algorithms used in the evolution of N-body systems. We present a new family of biorthogonal potential-density pairs constructed using the Hankel transform of the Laguerre polynomials. The lowest-order density basis functions are double-power-law profiles cusped like ρ ∼ r −2+1/α at small radii with asymptotic density fall-off like ρ ∼ r −3−1/(2α) . Here, α is a parameter satisfying α ≥ 1/2. The family therefore spans the range of inner density cusps found in numerical simulations, but has much shallower -and hence more realistic -outer slopes than the corresponding members of the only previously-known family deduced by Zhao (1996) and exemplified by Hernquist & Ostriker (1992). When α = 1, the lowest-order density profile has an inner density cusp of ρ ∼ r −1 and an outer density slope of ρ ∼ r −3.5 , similar to the famous Navarro, Frenk & White (1997) model. For this reason, we demonstrate that our new expansion provides a more accurate representation of flattened NFW haloes than the competing Hernquist-Ostriker expansion. We utilize our new expansion by analysing a suite of numerically-constructed haloes and providing the distributions of the expansion coefficients.

show abstract

Section: Zeroth-order Modelsmentioning

confidence: 99%

Section: Zeroth-order Modelsmentioning

confidence: 99%

Galaxy halo expansions: a new biorthogonal family of potential-density pairs

Lilley

Sanders

Evans

et al. 2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…All of these profiles can be generalized to the (α, β, γ)-models [40][41][42] . Here we focus on the NFW profile and the core-modified profile.…”

Section: B Models Of Rotation Velocitymentioning

confidence: 99%

Comparing dark matter models, modified Newtonian dynamics and modified gravity in accounting for galaxy rotation curves

Tang

Lin

2017

Chinese Phys. C

View full text Add to dashboard Cite

We compare six models (including the baryonic model, two dark matter models, two modified Newtonian dynamics models and one modified gravity model) in accounting for the galaxy rotation curves. For the dark matter models, we assume NFW profile and core-modified profile for the dark halo, respectively. For the modified Newtonian dynamics models, we discuss Milgrom's MOND theory with two different interpolation functions, i.e. the standard and the simple interpolation functions. As for the modified gravity, we focus on Moffat's MSTG theory. We fit these models to the observed rotation curves of 9 high-surface brightness and 9 lowsurface brightness galaxies. We apply the Bayesian Information Criterion and the Akaike Information Criterion to test the goodness-of-fit of each model. It is found that non of the six models can well fit all the galaxy rotation curves. Two galaxies can be best fitted by the baryonic model without involving the nonluminous dark matter. MOND can fit the largest number of galaxies, and only one galaxy can be best fitted by MSTG model. Core-modified model can well fit about one half LSB galaxies but no HSB galaxy, while NFW model can fit only a small fraction of HSB galaxies but no LSB galaxy. This may imply that the oversimplified NFW and Core-modified profiles couldn't well mimic the postulated dark matter halo.

show abstract

“…Various profiles of the radial distribution of dark matter in the galaxy have been put forth, see e.g., [37], [38] and [39]. We have used micrOMEGAs package and adopted the profile given and discussed Refs.…”

Section: Gamma-rays From η Annihilationmentioning

confidence: 99%

“…We have used micrOMEGAs package and adopted the profile given and discussed Refs. in [38] and [39] to perform our calculations. We thus take a DM halo density profile ρ(r) normalized to a value of ρ ⊙ at the solar galactic radius of 0.3 GeV/cm 3 .…”

Section: Gamma-rays From η Annihilationmentioning

confidence: 99%

Secluded WIMPs, dark QED with massive photons, and the galactic center gamma-ray excess

Fortes

Pleitez

Stecker

2016

Astroparticle Physics

View full text Add to dashboard Cite

We discuss a particular secluded WIMP dark matter model consisting of neutral fermions as the dark matter candidate and a Proca-Wentzel (PW) field as a mediator. In the model that we consider here, dark matter WIMPs interact with standard model (SM) particles only through the PW field of ∼ MeV -multi-GeV mass particles. The interactions occur via a U(1) ′ mediator, V ′ µ , which couples to the SM by kinetic mixing with U(1) hypercharge bosons, B ′ µ . One important difference between our model and other such models in the literature is the absence of an extra singlet scalar, so that the parameter with dimension of mass M 2 V is not related to a spontaneous symmetry breaking. This QED based model is also renormalizable. The mass scale of the mediator and the absence of the singlet scalar can lead to interesting astrophysical signatures. The dominant annihilation channels are different from those usually considered in previous work. We show that the GeV-energy γ-ray excess in the galactic center region, as derived from Fermi-LAT Gamma-ray Space Telescope data, can be attributed to such secluded dark matter WIMPs, given parameters of the model that are consistent with both the cosmological dark matter density and the upper limits on WIMP spin-independent elastic scattering. Secluded WIMP models are also consistent with suggested upper limits on a DM contribution to the cosmic-ray antiproton flux.

show abstract

Fitting functions for dark matter density profiles

Cited by 34 publications

References 39 publications

Galaxy halo expansions: a new biorthogonal family of potential-density pairs

Galaxy halo expansions: a new biorthogonal family of potential-density pairs

Comparing dark matter models, modified Newtonian dynamics and modified gravity in accounting for galaxy rotation curves

Secluded WIMPs, dark QED with massive photons, and the galactic center gamma-ray excess

Contact Info

Product

Resources

About