The dark matter density at the Sun’s location

By P. Salucci, Fabrizio Nesti, G. Gentile, C. Martins. 2010

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Aims. We derive the value of the dark matter density at the Sun’s location ( ) without globally mass-modeling the Galaxy. Methods. The proposed method relies on the local equation of centrifugal equilibrium and is independent of i) the shape of the dark matter density profile, ii) knowledge of the rotation curve from the galaxy center out to the virial radius, and iii) the uncertainties and the non-uniqueness of the bulge/disk/dark halo mass decomposition. Results. The result can be obtained in analytic form and it explicitly includes the dependence on the relevant observational quantities and takes their uncertainties into account. By adopting the reference, state-of-the-art values for these, we find = 0:43(11)(10) GeV/cm 3 , where the quoted uncertainties are respectively due to the uncertainty in the slope of the circular-velocity at the Sun location and the ratio between this radius and the length scale of the stellar exponential thin disk. Conclusions. We obtained a reliable estimate of , that, in addition has the merit of being ready to take into account any future change/improvement in the measures of the observational quantities it depends on.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/ef33eae9a246799b480b677080c46a6286fc3914

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Citations in the corpus

Low-mass dark matter search with CDMSlite (2017, background): “Although the local dark matter density is also uncertain [56], all experiments are equally affected by its value, so the effect of its uncertainty on the Run 2 limit is not considered further.”
The local dark matter density (2014, background): “The global measures often result in very small error bars (Catena & Ullio 2010; though see Salucci et al. 2010 and Iocco et al. 2011).”
The Local Dark Matter Density (2012, methodology): “A different approach was devised by Salucci et al. (2010); the idea is to resort to the equation of centrifugal equilibrium (see Fall Efstathiou 1980 for details) and to use recent results found in external galaxies (Salucci et al. 2007).”
Dark Matter through the Higgs portal (2019, neutral): “[279–288] for more details.”
Extended gamma-ray emission from Coy Dark Matter (2014, background): “is the local dark matter density [61, 62], 〈σv〉f is the annihilation cross-section to f̄f and”
A tale of tails: Dark matter interpretations of the Fermi GeV excess in light of background model systematics (2014, neutral): “4 GeV cm − 3 [95,96].”
Direct detection of sub-GeV dark matter with semiconductor targets (2015, background): “4 GeV/cm 3 [102, 103], and a Maxwell-Boltzmann velocity distribution with a mean velocity v0 = 230 km/s and escape velocity vesc = 600 km/s, and we take the average Earth velocity to be vE = 240 km/s (see Appendix B for explicit formulae).”
Constraining the Galaxy's dark halo with RAVE stars (2014, result): “Also most other recent studies that do not rely on the separability assumption find value for ρdm, that are in good agreement with our measurement (Salucci et al. 2010; Iocco et al. 2011; McMillan 2011; Nesti & Salucci 2013).”
STARS, GAS, AND DARK MATTER IN THE SOLAR NEIGHBORHOOD (2015, result): “The two references that adopted the weakest priors are fully consistent with our result: Salucci et al. (2010) found M0.”
Colloquium: Annual modulation of dark matter (2013, background): “…as 3Estimates for the local density of the smooth dark matter component are model dependent and vary in the literature by as much as a factor of 2 (Caldwell and Ostriker, 1981; Catena and Ullio, 2010; Pato et al., 2010; Salucci et al., 2010; Weber and de Boer, 2010; Bovy and Tremaine, 2012).”
Numerical simulations of the dark universe: State of the art and the next decade (2012, neutral): “85 GeV cm−3 [151–154].”
The Milky Way's rotation curve out to 100 kpc and its constraint on the Galactic mass distribution (2016, background): “The RC provides important constraints on the mass distribution of our Galaxy, including its dark matter (DM) content, as well as the local DM density (e.g. Salucci et al. 2010; Weber &de Boer 2010).”