Dark matter annihilation in the halo of the Milky Way

By Felix Stoehr, Simon D. M. White, Volker Springel, G. Tormen, Naoki Yoshida. 2003

153 citations recorded by the source corpus.

If the dark matter in the Universe is made of weakly self-interacting particles, they may self-annihilate and emit γ-rays. We use high-resolution numerical simulations to estimate directly the annihilation flux from the central regions of the Milky Way and from dark matter substructures in its halo. Although such estimates remain uncertain because of their strong dependence on the structure of the densest regions, our numerical experiments suggest that less direct calculations have overestimated the emission both from the centre and from the halo substructure. We estimate a maximal enhancement of at most a factor of a few with respect to a smooth spherical halo of standard Navarro-Frenk-White (NFW) structure. We discuss detection strategies for the next generation of γ-ray detectors and find that the annihilation flux may be detectable, regardless of uncertainties about the densest regions, for the annihilation cross-sections predicted by currently popular elementary particle models for the dark matter.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c776950d382626aaeac6d527c89ad32beb173249

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Citations in the corpus

The Most Dark-Matter-dominated Galaxies: Predicted Gamma-Ray Signals from the Faintest Milky Way Dwarfs (2007, background): “…well-defined, unlike the search of completely dark substructure, which would rely on serendipitous discovery (Calcaneo-Roldan & Moore 2000; Tasitsiomi & Olinto 2002; Stoehr et al. 2003;Koushiappas et al. 2004; Pieri et al. 2005; Koushiappas 2006; Diemand et al. 2007; Baltz et al. 2007).”
The Galaxy and its stellar halo: insights on their formation from a hybrid cosmological approach (2008, methodology): “In this paper, we use the re-simulations of a ‘Milky Way’ halo (the GA series) described in Stoehr et al. (2002) and Stoehr et al. (2003).”
The population of dark matter subhaloes: mass functions and average mass-loss rates (2007, background): “…principle, though, these truly ‘dark’ subhaloes may potentially be detected viaγ -ray emission due to dark matter annihilation in their central cores (Stoehr et al. 2003; Bertone 2006; Koushiappas 2006; Diemand, Kuhlen & Madau 2007; Pieri et al. 2008), or via their impact on the flux-ratio…”
Dark Matter Subhalos and the Dwarf Satellites of the Milky Way (2008, background): “…its effects on stellar streams (e.g. Ibata et al. 2002; Mayer et al. 2002), or possibly via γ-rays from dark matter annihilation in their cores (Bergstrom et al. 1999; Stoehr et al. 2003); 5. the observed Milky Way satellites approximately follow the overall dark matter distribution of Via Lactea.”
The Dark Matter Annihilation Signal from Galactic Substructure: Predictions for GLAST (2008, methodology): “Following previous work (Stoehr et al. 2003), we define for each subhalo in our allsky map a “detection significance” S = ∑ i Ns,i √ ∑ iNb,i , (11) where Ns,i and Nb,i are the number of source and background gamma-rays received on a given pixel, and the sums are over all pixels with signal-to-noise…”
The subhalo populations of ΛCDM dark haloes (2004, methodology): “Numerical convergence was claimed by Ghigna et al. (2000; hereafter G00), by SWTK and by Stoehr et al (2002, 2003) on the basis of multi-resolution simulations of individual objects.”
HIGH-RESOLUTION MASS MODELS OF DWARF GALAXIES FROM LITTLE THINGS (2015, background): “…R is the galaxy radius and α∼−1.0 (Moore 1994; Navarro et al. 1996b; Navarro et al. 1997; Moore et al. 1999; Ghigna et al. 2000; Klypin et al. 2001; Power et al. 2003; Stoehr et al. 2003; Navarro et al. 2004a; Diemand et al. 2008; Stadel et al. 2009; Navarro et al. 2010; Ishiyama et al. 2013 etc.).”
Bayesian strong gravitational-lens modelling on adaptive grids: objective detection of mass substructure in Galaxies (2008, background): “…its eff cts on stellar streams (e.g., Ibata et al. 2002; Mayer et al. 2002), viaγ-rays from dark matter annihilation (Bergström et al. 1999; Calcáneo-Rold´an & Moore 2000; Stoehr et al. 2003; Colafrancesco et al. 2006) or through gravitational lensing (e.g., Dalal & Kochanek 2002; Koopmans 2005).”
Substructures in hydrodynamical cluster simulations (2008, background): “…matter (DM) only simulations, a consistent picture of the population of subhalos within galaxy clusters has now emerged (e.g., Moore et al. 1999; Ghigna et al. 2000; Springel et al. 2001; Stoehr et al. 2002, 2003; Diemand et al. 2004; Gao et al. 2004; De Lucia et al. 2004; Kravtsov et al. 2004).”
Dark Matter Substructure and Gamma-Ray Annihilation in the Milky Way Halo (2006, background): “Because the diffuse background noise is strongest near the center due to Galactic continuum emission (Stoehr et al. 2003), it is likely that substructure will be more readily detectable at anticenter, and/or at higher latitudes.”
The Aquarius Project: the subhaloes of galactic haloes (2008, background): “This is similar to the substructure mass fractions found by earlier work on galaxy cluster halos (e.g. Ghigna et al., 1998; Springel et al., 2001a; De Lucia et al., 2004) and Galaxy-sized halos (Stoehr et al., 2003) once the different limiting radius (r200 instead of r50) is corrected for.”
The diversity and similarity of simulated cold dark matter haloes (2008, background): “…spatial distribution, and structure of substructure, and their consequences for the discovery and interpretation of possible signals of dark matter annihilation in the gamma-ray sky (Stoehr et al., 2003; Diemand et al., 2007; Kuhlen et al., 2008; Springel et al., 2008a, and references therein).”
Characterization of subhalo structural properties and implications for dark matter annihilation signals (2016, background): “…distribution is expected to significantly boost the DM annihilation signal (Bergstrom et al. 1999; Calcáneo-Roldán & Moore 2000; Aloisio et al. 2004; Stoehr et al. 2003; Koushiappas et al. 2004; Lavalle et al. 2008; Kuhlen et al. 2008; Charbonnier et al. 2011; Sánchez-Conde et al. 2011; Pinzke…”