The Dark Matter Annihilation Signal from Galactic Substructure: Predictions for GLAST

By Michael Kuhlen, J. Diemand, P. Madau. 2008

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We present quantitative predictions for the detectability of individual Galactic dark matter subhalos in gamma rays from dark matter pair annihilations in their centers. Our method is based on a hybrid approach, employing the highest resolution numerical simulations available (including the recently completed 1 billion particle Via Lactea II simulation), as well as analytical models, for extrapolating beyond the simulations’ resolution limit. We include a self-consistent treatment of subhalo boost factors, motivated by our numerical results, and a realistic treatment of the expected backgrounds that individual subhalos must outshine. We show that for reasonable values of the dark matter particle physics parameters (Mχ ∼ 50-500 GeV and ⟨ σ v⟩ ∼ 10−26-10−25 cm3 s−1) GLAST may very well discover a few, even up to several dozen, such subhalos at 5 σ significance, and some at more than 20 σ. We predict that the majority of luminous sources would be resolved with GLAST’s expected angular resolution. For most observer locations, the angular distribution of detectable subhalos is consistent with a uniform distribution across the sky. The brightest subhalos tend to be massive (median Vmax of 24 km s−1) and therefore likely hosts of dwarf galaxies, but many subhalos with Vmax as low as 5 km s−1 are also visible. Typically detectable subhalos are 20-40 kpc from the observer, and only a small fraction are closer than 10 kpc. The total number of observable subhalos has not yet converged in our simulations, and we estimate that we may be missing up to 3/4 of all detectable subhalos.

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c1321544affddd07d180e4b76ff8a1b9718d0c65

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Citations in the corpus

DARK MATTER HALOS IN THE STANDARD COSMOLOGICAL MODEL: RESULTS FROM THE BOLSHOI SIMULATION (2010, background): “…of dark matter subhalos (e.g., Moore et al. 1996; Klypin et al. 1999; Coĺın et al. 1999), the potential annihilation signal of dark matter (e.g., Kuhlen et al. 2008; Springel et al. 2008; Ando 2009), and motion of satellites as a probe for masses of isolated galaxies and groups (e.g., Prada…”
The impact of dark matter cusps and cores on the satellite galaxy population around spiral galaxies (2010, background): “…consequences for the discovery and interpretation of possible signals of dark matter annihilation in gamma-ray surveys (Stoehr et al. 2003; Diemand et al. 2007; Kuhlen et al. 2008; Springel et al. 2008b), since the strength of the signal goes with the square of the dark matter density.”
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).”
The flattening of the concentration–mass relation towards low halo masses and its implications for the annihilation signal boost (2013, background): “The normalization factor A is chosen to match the amount of substructure resolved in current simulations (typically ∼10%, e.g., Kuhlen et al. (2008); Springel et al. (2008)).”
Not so lumpy after all: modelling the depletion of dark matter subhaloes by Milky Way-like galaxies (2017, background): “Predictions for the substructure boost for dark matter annihilation signals in the Galactic center (Kuhlen et al. 2008; Bovy 2009) will decrease.”
SEARCH FOR DARK MATTER SATELLITES USING FERMI-LAT (2012, unknown): “7-the relations (Kuhlen et al. 2008) (6) where rs is in kpc and Ps is in /\118 kpc-3.”
The Aquarius Project: the subhaloes of galactic haloes (2008, background): “We note that our results disagree with those of the re- cent Via Lactea I and II simulations (Diemand et al., 2007a; Madau et al., 2008; Diemand et al., 2008; Kuhlen et al., 2008) on several important points.”
Numerical simulations of the dark universe: State of the art and the next decade (2012, methodology): “Nevertheless, H.E.S.S. [97] and Fermi [95] data have been able to constrain DM parameters, and there is tentative evidence for a ∼ 130 GeV line signal from a subset of the most promising cluster targets [98]. iv) The Galactic Center The most prominent DM annihilation signal is thought to arise from ”
The Search for Spatial Extension in High-latitude Sources Detected by the Fermi Large Area Telescope (2018, background): “…instance, extended emission should be produced in the case of the annihilation or decay of weakly interacting massive particles gravitationally bound in virialized sub-structures of the halo of the Milky Way (e.g., Kuhlen et al. 2008; Pieri et al. 2008; Mirabal et al. 2012; Zechlin & Horns 2012).”
ELVIS: Exploring the Local Volume in Simulations (2013, methodology): “Very high resolution zoom-in simulations of Milky Way (MW) mass haloes have been useful for making and testing predictions of the ΛCDM theory (e.g. Diemand et al. 2008; Kuhlen et al. 2008; Springel et al. 2008), often through com- c© 2013 RAS ar X iv :1 31 0.”
The Phoenix Project: the dark side of rich galaxy clusters (2012, background): “Forexample, recent analyses indicate that total flux of dark matter annihilation radiation is expected to be dominated by low-mass subhaloes (Kuhlen et al. 2008; Springel et al. 2008b; Gao et al. 2011b).”
Subhaloes going Notts: the subhalo‐finder comparison project (2012, background): “…and so survives as separat structures within larger haloes is an important quantity for bothstudies of dark-matter detection (Springel et al. 2008; Kuhlen et al. 2008; Vogelsberger et al. 2009; Zavala et al. 2010) and the apparent ov rabundance of substructure within numerical models when…”
Galactic Searches for Dark Matter (2012, background): “…provide a theoretical treatment of the substructure boost factor (Strigari et al., 2007d; Pieri et al., 2008; Martinez et al., 2009; Charbonnier et al., 2011), which complement the results derived from N-body simulations above their resolution limit (Springel et al., 2008b; Kuhlen et al., 2008).”
The mass–concentration–redshift relation of cold dark matter haloes (2013, background): “…at low masses might lead to important changes in the selfannihilation flux expected from low-mass halos, and to modifications in the importance of the “boost factor” from substructure, which is expected to dominate the annihilation luminosity (e.g. Kuhlen et al. 2008; Springel et al. 2008).”
Characterization of subhalo structural properties and implications for dark matter annihilation signals (2016, methodology): “…(Taylor & Babul 2001; Benson et al. 2002; Ullio et al. 2002; Taffoni et al. 2003; Zentner & Bullock 2003; Peñarrubia & Benson 2005; Oguri & Lee 2004; Taylor & Babul 2005b,a,b; van den Bosch et al. 2005; Zentner 2005; Kuhlen et al. 2008; Gan et al. 2010; Pieri et al. 2011; Purcell & Zentner 2012).”
Disruption of Dark Matter Substructure: Fact or Fiction? (2017, background): “Finally, dark matter substructure boosts the expected dark matter annihilation signal (Bergström et al. 1999), an effect that is typically quantified in terms of a ‘boost-factor’ (e.g., Strigari et al. 2007; Giocoli et al. 2008b; Kuhlen et al. 2008; Pieri et al. 2008; Moliné et al. 2016).”
Gamma Ray Signals from Dark Matter: Concepts, Status and Prospects (2012, background): “This implies that the expected boost factor for GC observations is of order unity [77, 108–110], while it may be as large as O(1000) for galaxy clusters due to the enormous contained hierarchy of masses [111–114].”