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(Referência obtida automaticamente do Web of Science, por meio da informação sobre o financiamento pela FAPESP e o número do processo correspondente, incluída na publicação pelos autores.)

Dynamical constraints on the dark matter distribution in the Milky Way

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Autor(es):
Pato, Miguel [1, 2] ; Iocco, Fabio [3, 4, 5] ; Bertone, Gianfranco [6]
Número total de Autores: 3
Afiliação do(s) autor(es):
[1] Stockholm Univ, Dept Phys, Oskar Klein Ctr Cosmoparticle Phys, Alballova, SE-10691 Stockholm - Sweden
[2] Tech Univ Munich, Phys Dept, D-85748 Garching - Germany
[3] Univ Estadual Paulista, Inst Fis Teor, BR-01140070 Sao Paulo, SP - Brazil
[4] Univ Estadual Paulista, ICTP South Amer Inst Fundamental Res, BR-01140070 Sao Paulo, SP - Brazil
[5] UAM, CSIC, Inst Fis Teor, Madrid 28049 - Spain
[6] Univ Amsterdam, GRAPPA Inst, NL-1090 GL Amsterdam - Netherlands
Número total de Afiliações: 6
Tipo de documento: Artigo Científico
Fonte: Journal of Cosmology and Astroparticle Physics; n. 12 DEC 2015.
Citações Web of Science: 62
Resumo

An accurate knowledge of the dark matter distribution in the Milky Way is of crucial importance for galaxy formation studies and current searches for particle dark matter. In this paper we set new dynamical constraints on the Galactic dark matter profile by comparing the observed rotation curve, updated with a comprehensive compilation of kinematic tracers, with that inferred from a wide range of observation-based morphologies of the bulge, disc and gas. The generalised Navarro-Frenk-White (NFW) and Einasto dark matter profiles are fitted to the data in order to determine the favoured ranges of local density, slope and scale radius. For a representative baryonic model, a typical local circular velocity v(0) = 230 km/s and a distance of the Sun to the Galactic centre R-0 = 8 kpc, we find a local dark matter density rho(0) = 0.420(-0.018)(+0.021) (2 sigma) +/- 0.025 GeV/cm(3) (rho(0) = 0.420(-0.021)(+0.019) (2 sigma) +/- 0.026 GeV/cm(3)) for NFW (Einasto), where the second error is an estimate of the systematic due to baryonic modelling. Apart from the Galactic parameters, the main sources of uncertainty inside and outside the solar circle are baryonic modelling and rotation curve measurements, respectively. Upcoming astronomical observations are expected to reduce all these uncertainties substantially over the coming years. (AU)

Processo FAPESP: 14/11070-2 - Matéria escura na Via Láctea: uma era de precisão
Beneficiário:Fabio Iocco
Linha de fomento: Auxílio à Pesquisa - Apoio a Jovens Pesquisadores