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Penarrubia J.,University of Edinburgh | Penarrubia J.,Institute Astrofisica Of Andalucia Csic | Penarrubia J.,University of Cambridge | Ma Y.-Z.,University of British Columbia | And 4 more authors.
Monthly Notices of the Royal Astronomical Society | Year: 2014

We combine the equations of motion that govern the dynamics of galaxies in the local volume with Bayesian techniques in order to fit orbits to published distances and velocities of galaxies within 3 Mpc. We find a Local Group (LG) mass 2.3 ± 0.7 × 1012M⊙ that is consistent with the combined dynamical masses of M31 and the Milky Way, and a mass ratio 0.54+0.23 -0.17 that rules out models where our Galaxy is more massive than M31 with ~95 per cent confidence. The MilkyWay's circular velocity at the solar radius is relatively high, 245±23 km s-1, which helps to reconcile the mass derived from the local Hubble flow with the larger value suggested by the 'timing argument'. Adopting Planck's bounds on ΩΛ yields a (local) Hubble constant H0 = 67 ± 5 kms-1 Mpc-1 which is consistent with the value found on cosmological scales. Restricted N-body experiments show that substructures tend to fall on to the LG along the Milky Way-M31 axis, where the quadrupole attraction is maximum. Tests against mock data indicate that neglecting this effect slightly overestimates the LG mass without biasing the rest of model parameters.We also show that both the time dependence of the LG potential and the cosmological constant have little impact on the observed local Hubble flow. © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Source

Bonnivard V.,French National Center for Scientific Research | Combet C.,French National Center for Scientific Research | Daniel M.,University of Liverpool | Funk S.,Friedrich - Alexander - University, Erlangen - Nuremberg | And 10 more authors.
Monthly Notices of the Royal Astronomical Society | Year: 2015

Dwarf spheroidal (dSph) galaxies are prime targets for present and future Γ-ray telescopes hunting for indirect signals of particle darkmatter. The interpretation of the data requires careful assessment of their dark matter content in order to derive robust constraints on candidate relic particles. Here, we use an optimized spherical Jeans analysis to reconstruct the 'astrophysical factor' for both annihilating and decaying dark matter in 21 known dSphs. Improvements with respect to previous works are: (i) the use of more flexible luminosity and anisotropy profiles to minimize biases, (ii) the use of weak priors tailored on extensive sets of contamination-free mock data to improve the confidence intervals, (iii) systematic cross-checks of binned and unbinned analyses on mock and real data, and (iv) the use of mock data including stellar contamination to test the impact on reconstructed signals. Our analysis provides updated values for the dark matter content of 8 'classical' and 13 'ultrafaint' dSphs, with the quoted uncertainties directly linked to the sample size; themore flexible parametrizationwe use results in changes compared to previous calculations. This translates into our ranking of potentiallybrightest and most robust targets-namely Ursa Minor, Draco, Sculptor-and of the more promising, but uncertain targets-namely Ursa Major 2, Coma-for annihilating dark matter. Our analysis of Segue 1 is extremely sensitive to whether we include or exclude a few marginal member stars, making this target one of the most uncertain. Our analysis illustrates challenges that will need to be addressed when inferring the dark matter content of new 'ultrafaint' satellites that are beginning to be discovered in southern sky surveys. © 2015 The Authors. Source

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