Where will supersymmetric dark matter first be seen?
Gao, L.; Frenk, C.S.; Jenkins, A.; Springel, V.; White, S.D.M.
Professor Carlos Frenk email@example.com
Professor Adrian Jenkins firstname.lastname@example.org
If the dark matter consists of supersymmetric particles, γ-ray observatories such as the Large Area Telescope aboard the Fermi satellite may detect annihilation radiation from the haloes of galaxies and galaxy clusters. Much recent effort has been devoted to searching for this signal around the Milky Way’s dwarf satellites. Using a new suite of high-resolution simulations of galaxy cluster haloes (the Phoenix Project), together with the Aquarius simulations of Milky Way-like galaxy haloes, we show that higher signal-to-noise ratio and equally clean signals are, in fact, predicted to come from nearby rich galaxy clusters. Most of the cluster emission is produced by small subhaloes with masses less than that of the Sun. The large range of mass scales covered by our two sets of simulations allows us to deduce a physically motivated extrapolation to these small (and unresolved) masses. Since tidal effects destroy subhaloes in the dense inner regions of haloes, most cluster emission is then predicted to come from large radii, implying that the nearest and brightest systems should be much more extended than Fermi’s angular resolution limit. The most promising targets for detection are clusters such as Coma and Fornax, but detection algorithms must be tuned to the predicted profile of the emission if they are to maximize the chance of finding this weak signal.
Gao, L., Frenk, C., Jenkins, A., Springel, V., & White, S. (2012). Where will supersymmetric dark matter first be seen?. Monthly Notices of the Royal Astronomical Society, 419(2), 1721-1726. https://doi.org/10.1111/j.1365-2966.2011.19836.x
|Journal Article Type||Article|
|Publication Date||Jan 11, 2012|
|Deposit Date||Jan 27, 2012|
|Publicly Available Date||Aug 22, 2014|
|Journal||Monthly Notices of the Royal Astronomical Society|
|Publisher||Royal Astronomical Society|
|Peer Reviewed||Peer Reviewed|
|Keywords||Methods: numerical, Galaxies: haloes, Dark matter.|
Published Journal Article
This article has been accepted for publication in Monthly notices of the Royal Astronomical Society © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS Published by Oxford University Press on behalf of Royal Astronomical Society. All rights reserved.
You might also like
Formation of massive disc galaxies in the IllustrisTNG simulation
Constraining the inner density slope of massive galaxy clusters
Ultra-diffuse galaxies in the Auriga simulations
Dark-matter-deficient galaxies in hydrodynamical simulations
The optimal gravitational softening length for cosmological N-body simulations