Resolving Small-Scale Dark Matter Structures Using Multi-Source Indirect Detection

Ng, Kenny C. Y.; Laha, Ranjan; Campbell, Sheldon; Horiuchi, Shunsaku; Dasgupta, Basudeb; Murase, Kohta; Beacom, John F.

doi:10.48550/arxiv.1310.1915

Cited by 20 publications

(25 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This means that it is subject to constraints from CMB observations, direct/indirect DM searches, and collider experiments. However, for 30 GeV m V 80 GeV, constraints from CMB [29] and indirect searches [6,[30][31][32] can be easily satisfied in our scenario as far as there is no enhancement of annihilation rate relative to the one at freeze-out. So, in this section we consider only low energy phenomenology, direct detection and relic density.…”

Section: Constraintsmentioning

confidence: 81%

Higgs portal vector dark matter forGeVscale γ-ray excess from galactic center

Ko¹,

Park²,

Tang³

2014

J. Cosmol. Astropart. Phys.

114

View full text Add to dashboard Cite

We show that the GeV scale γ-ray excess from the direction of the Galactic Center can be naturally explained by the pair annihilation of Abelian vector dark matter (VDM) into a pair of dark Higgs bosons V V → φφ, followed by the subsequent decay of φ into φ → bb, ττ . All the processes are described by a renormalizable VDM model with the Higgs portal, which is naturally flavor-dependent. Some parameter space of this scenario can be tested at the near future direct dark matter search experiments such as LUX and XENON1T.

show abstract

Section: Constraintsmentioning

confidence: 81%

Higgs portal vector dark matter forGeVscale γ-ray excess from galactic center

Ko¹,

Park²,

Tang³

2014

J. Cosmol. Astropart. Phys.

114

View full text Add to dashboard Cite

show abstract

“…Therefore, one may ask whether the extrapolation of the model down to the minimum halo mass in the top panel of Fig. 1 (and also recently shown in Ng et al (2013)) is entirely justified, and thus if the agreement between P12 and low-mass concentration data is accidental or not. The fact is that, indeed, there is not extrapolation.…”

Section: Halo Concentration At the Present Epochmentioning

confidence: 91%

The flattening of the concentration–mass relation towards low halo masses and its implications for the annihilation signal boost

Sánchez‐Conde

Prada

2014

Monthly Notices of the Royal Astronomical Society

211

392

View full text Add to dashboard Cite

In the standard cold dark matter (CDM) theory for understanding the formation of structure in the Universe, there exists a tight connection between the properties of dark matter (DM) haloes, and their formation epochs. Such relation can be expressed in terms of a single key parameter, namely the halo concentration. In this work, we examine the median concentration-mass relation, c(M), at present time, over more than 20 orders of magnitude in halo mass, i.e. from tiny Earth-mass microhalos up to galaxy clusters. The c(M) model proposed by Prada et al. (2012), which links the halo concentration with the r.m.s. amplitude of matter linear fluctuations, describes remarkably well all the available N-body simulation data down to ∼10 −6 h −1 M ⊙ microhalos. A clear fattening of the halo concentration-mass relation towards smaller masses is observed, that excludes the commonly adopted power-law c(M) models, and stands as a natural prediction for the CDM paradigm. We provide a parametrization for the c(M) relation that works accurately for all halo masses. This feature in the c(M) relation at low masses has decisive consequences e.g. for γ-ray DM searches, as it implies more modest boosts of the DM annihilation flux due to substructure, i.e., ∼ 35 for galaxy clusters and ∼ 15 for galaxies like our own, as compared to those huge values adopted in the literature that rely on such power-law c(M) extrapolations. We provide a parametrization of the boosts that can be safely used for dwarfs to galaxy cluster-size halos.

show abstract

“…In order to derive the boost factor b we follow the prescription presented in [30], as this conforms to recent analysis performed on Fermi-LAT data. This sub-structure boost factor is defined as a luminosity increase caused by integrating over sub-halo luminosities determined by the virial mass and by halo concentration parameters found numerically according to the method discussed in [31]; we note that a similar method is provided in [32]. These methods place the boosting factor of cluster sized halos around b ∼ 30, with the large dwarf-like galaxy Draco having b ∼ 3.…”

Section: Models Of Dark Matter Halos and Multi-frequency Emissionmentioning

confidence: 99%

A Multi-frequency analysis of dark matter annihilation interpretations of recent anti-particle and γ-ray excesses in cosmic structures

Beck

Colafrancesco

2016

J. Cosmol. Astropart. Phys.

View full text Add to dashboard Cite

The Fermi-LAT observation of a γ-ray excess from the galactic-centre, as well as the PAMELA, AMS, and AMS-2 anti-particle excesses, and the recent indications of a Fermi-LAT γ-ray excess in the Reticulum II dwarf galaxy have all been variously put forward as possible indirect signatures of supersymmetric neutralino dark matter. These are of particular interest as the neutralino annihilation models which fit these observations must have observable consequences across the frequency spectrum, from radio to γ-ray emission. Moreover, since dark matter is expected to be a major constituent of cosmic structure, these multi-frequency consequences should be common to such structures across the mass spectrum, from dwarf galaxies to galaxy clusters. Thus, in this work we make predictions for the multi-frequency spectra of three well-known sources dominated by dark matter on cluster, galaxy and dwarf galaxy scales, e.g. the Coma cluster, the galaxy M81, and the Draco dwarf galaxy, using models favoured by dark matter interpretations of the aforementioned observations. We pay special attention to the consequences for these models when their cross-sections are renormalised to reproduce the recent γ-ray excess observed in the Reticulum II dwarf galaxy, as well as using cross-sections from the Fermi-LAT dwarf galaxy limits, which throw a dark matter interpretation of this excess into doubt. We find that the multi-frequency data of Coma and Draco are in conflict with the dark matter interpretation of the AMS, PAMELA and Fermi positron excess. Additionally, models derived from Fermi-LAT galactic centre observations, and AMS-2 re-analysis, present similar but less extensive conflicts. Using the sensitivity projections for the Square Kilometre Array, the Cherenkov Telescope Array, as well as the ASTROGAM and ASTRO-H satellites, we determine the detection prospects for a subset of neutralino models that remain consistent with Planck cosmological constraints. Although the SKA has the greatest sensitivity to dark matter models, we demonstrate that ASTRO-H is well positioned to probe the inverse-Compton scattering emissions from neutralino annihilation and identify characteristics of the spectra which contain information about the neutralino mass and annihilation channel. This means that, given environments with favourable X-ray backgrounds, multi-frequency observation with the next generation of experiments will allow for unprecedented sensitivity to the neutralino parameter space as well as offsetting the individual weaknesses of each observation mode. Finally we show that all of the studied models can be better tested with the SKA phase 1.

show abstract

Resolving Small-Scale Dark Matter Structures Using Multi-Source Indirect Detection

Cited by 20 publications

References 0 publications

Higgs portal vector dark matter forGeVscale γ-ray excess from galactic center

Higgs portal vector dark matter forGeVscale γ-ray excess from galactic center

The flattening of the concentration–mass relation towards low halo masses and its implications for the annihilation signal boost

A Multi-frequency analysis of dark matter annihilation interpretations of recent anti-particle and γ-ray excesses in cosmic structures

Contact Info

Product

Resources

About