Multi-wavelength studies

Profumo, Stefano; Ullio, Piero

doi:10.1017/cbo9780511770739.028

Cited by 23 publications

(22 citation statements)

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“…Based on this result, the diffusion term in the diffusion equation can be neglected and the injected spectrum of the electron and positron pairs is proportional to the source spectrum of dark matter annihilation dN e /dE [21]. By using the monochromatic approximation [22], the total synchrotron radiation energy flux of the electron and positron pairs produced by dark matter annihilation is given by [22,23]:…”

Section: Radio Observations Of M33mentioning

confidence: 99%

Constraining annihilating dark matter by radio data of M33

Chan

2017

Phys. Rev. D

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Recent studies of radio data put strong constraints on annihilation cross section for dark matter. In this article, we provide the first analysis of using M33 radio data in constraining annihilating dark matter. The resulting constraints of annihilation cross sections for some channels are more stringent than that obtained from 6 years of Fermi Large Area Telescope (Fermi-LAT) gamma-ray observations of the Milky Way dwarf spheroidal satellite galaxies. In particular, the conservative lower limits of dark matter mass annihilating via $e^+e^-$, $\mu^+\mu^-$and $\tau^+\tau^-$ channels are 190 GeV, 120 GeV and 70 GeV respectively with the thermal relic annihilation cross section. These results are in large tensions with some of the recent quantitative analyses of the AMS-02 and Fermi-LAT data of the Milky Way center.Comment: Accepted for publication in Phy. Rev.

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Section: Radio Observations Of M33mentioning

confidence: 99%

Constraining annihilating dark matter by radio data of M33

Chan

2017

Phys. Rev. D

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“…with direct detection data significantly improves the reconstruction [7]. One could cite several other examples of complementarity of different detection techniques, such as the combination of different targets in direct detection experiments [8][9][10][11], or multi-wavelength analyses in indirect detection experiments [12].…”

Section: Introductionmentioning

confidence: 99%

Astrophysical limitations to the identification of dark matter: Indirect neutrino signalsvis-à-visdirect detection recoil rates

Serpico

Bertone

2010

Phys. Rev. D

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A convincing identification of dark matter (DM) particles can probably be achieved only through a combined analysis of different detections strategies, which provides an effective way of removing degeneracies in the parameter space of DM models. In practice, however, this program is made complicated by the fact that different strategies depend on different physical quantities, or on the same quantities but in a different way, making the treatment of systematic errors rather tricky. We discuss here the uncertainties on the recoil rate in direct detection experiments and on the muon rate induced by neutrinos from dark matter annihilations in the Sun, and we show that, contrarily to the local DM density or overall cross section scale, irreducible astrophysical uncertainties affect the two rates in a different fashion, therefore limiting our ability to reconstruct the parameters of the dark matter particle. By varying within their respective errors astrophysical parameters such as the escape velocity and the velocity dispersion of dark matter particles, we show that the uncertainty on the relative strength of the neutrino and direct-detection signal is as large as a factor of two for typical values of the parameters, but can be even larger in some circumstances.PACS numbers: 95.35.+d, 14.60.Lm

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“…At high energy, the dominant energy loss processes are synchrotron and inverse Compton scattering, which create secondary radiation at radio frequencies as well as X-ray to gamma-ray energies, respectively (for a recent review of multi-wavelength emissions from dark matter annihilation see Ref. [42]). This secondary emission is a common denominator to any WIMP model.…”

Section: Introductionmentioning

confidence: 99%

Morphology of the Galactic dark matter synchrotron emission with self-consistent cosmic-ray diffusion models

2010

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A generic prediction in the paradigm of weakly interacting dark matter is the production of relativistic particles from dark matter pair-annihilation in regions of high dark matter density. Ultrarelativistic electrons and positrons produced in the center of the Galaxy by dark matter annihilation should produce a diffuse synchrotron emission. While the spectral shape of the synchrotron dark matter haze depends on the particle model (and secondarily on the galactic magnetic fields), the morphology of the haze depends primarily on (1) the dark matter density distribution, (2) the galactic magnetic field morphology, and (3) the diffusion model for high-energy cosmic-ray leptons.Interestingly, an unidentified excess of microwave radiation with characteristics similar to those predicted by dark matter models has been claimed to exist near the galactic center region in the data reported by the WMAP satellite, and dubbed the "WMAP haze". In this study, we carry out a self-consistent treatment of the variables enumerated above, enforcing constraints from the available data on cosmic rays, radio surveys and diffuse gamma rays. We outline and make predictions for the general morphology and spectral features of a "dark matter haze" and we compare them to the WMAP haze data. We also characterize and study the spectrum and spatial distribution of the inverse Compton emission resulting from the same population of energetic electrons and positrons.We point out that the spectrum and morphology of the radio emission at different frequencies is a powerful diagnostics to test whether a galactic synchrotron haze indeed originates from dark matter annihilation. *

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Multi-wavelength studies

Cited by 23 publications

References 0 publications

Constraining annihilating dark matter by radio data of M33

Constraining annihilating dark matter by radio data of M33

Astrophysical limitations to the identification of dark matter: Indirect neutrino signalsvis-à-visdirect detection recoil rates

Morphology of the Galactic dark matter synchrotron emission with self-consistent cosmic-ray diffusion models

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