When dark matter interacts with cosmic rays or interstellar matter: A morphological study

Carlson, Eric; Profumo, Stefano

doi:10.1103/physrevd.92.063003

Cited by 8 publications

(7 citation statements)

References 55 publications

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“…Merging galaxy clusters such as the Bullet Cluster can provide a powerful testing ground for galactic DM observation [57]. There are also proposals to consider a possibility of galactic DM interactions with cosmic rays and different kinds of interstellar matter [58]. In the case of multicomponent galactic DM sector with at least two DM species with different masses one can use the DM-to-DM decays as a new complementary tool for investigation of the DM properties [59].…”

Section: How Does One Want To Detect the Dm?mentioning

confidence: 99%

Is it possible to discover a dark matter particle with an accelerator?

Bednyakov

2015

Preprint

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The paper contains description of the main properties of the galactic dark matter (DM) particles, available approaches for detection of DM, main features of direct DM detection, ways to estimate prospects for the DM detection, the first collider search for a DM candidate within an Effective Field Theory, complete review of ATLAS results of the DM candidate search with LHC RUN I, and less complete review of "exotic" dark particle searches with other accelerators and not only.From these considerations it follows that one is unable to prove, especially modelindependently, a discovery of a DM particle with an accelerator, or collider. One can only obtain evidence on existence of a weakly interacting neutral particle, which could be, or could not be the DM candidate.The current LHC DM search program uses only the missing transverse energy signature. Non-observation of any excess above Standard Model expectations forces the LHC experiments to enter into the same fighting for the best exclusion curve, in which (almost) all direct and indirect DM search experiments permanently take place. But this fighting has very little (almost nothing) to do with a real possibility of discovering a DM particle. The true DM particles possess an exclusive galactic signature -annual modulation of a signal, which is accessible today only for direct DM detection experiments. There is no way for it with a collider, or accelerator.Therefore to prove the DM nature of a collider-discovered candidate one must find the candidate in a direct DM experiment and demonstrate the galactic signature for the candidate. Furthermore, being observed, the DM particle must be implemented into a modern theoretical framework. The best candidate is the supersymmetry, which looks today inevitable for coherent interpretation of all available DM data.

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Section: How Does One Want To Detect the Dm?mentioning

confidence: 99%

Is it possible to discover a dark matter particle with an accelerator?

Bednyakov

2015

Preprint

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“…For example, it is interesting to investigate boosted DM flux coming from the Galactic center which possesses high DM density and CR flux. One also expects that the morphology of signal resulted from the Galactic center is different from that originated from local interstellar [35]. Moreover, light DM with significant CR acceleration and heavy DM (m χ 10 MeV) with negligible CR acceleration could potentially produce degenerate signal; therefore, discrimination of such two kinds of scenarios in both model independent and model specific way is an intriguing issue [36].…”

mentioning

confidence: 99%

Exploring for sub-MeV Boosted Dark Matter from Xenon Electron Direct Detection

Cao,

Ding,

Xiang

2020

Preprint

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Direct detection experiments turn to lose sensitivity of searching for a sub-MeV light dark matter candidate due to the threshold of recoil energy. However, such light dark matter particles can be accelerated by energetic cosmic-rays such that they can be detected with existing detectors. We derive the constraints on the scattering of a boosted light dark matter and electron from the XENON100/1T experiment. We illustrate that the energy dependence of the cross section plays a crucial role in improving both the detection sensitivity and also the complementarity of direct detection and other experiments.

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“…The signal strength predicted in our model depends on a peculiar combination of the dark matter number density times the interstellar plasma number density, which falls in the class of signal morphology explored for example in Ref. [4]. The signal also depends on the kinetic energy of the plasma particles, and thus if the plasma is in thermal equilibrium, the plasma temperature is a key factor as to whether or not the excitation rate is significant.…”

Section: Introductionmentioning

confidence: 66%

“…[4]. The signal also depends on the kinetic energy of the plasma particles, and thus if the plasma is in thermal equilibrium, the plasma temperature is a key factor as to whether or not the excitation rate is significant.…”

Section: Introductionmentioning

confidence: 99%

Dark matter inelastic up-scattering with the interstellar plasma: A new source of x-ray lines, including at 3.5 keV

et al. 2016

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We explore the phenomenology of a class of models where the dark matter particle can inelastically up-scatter to a heavier excited state via off-diagonal dipolar interactions with the interstellar plasma (gas or free electrons). The heavier particle then rapidly decays back to the dark matter particle plus a quasi-monochromatic photon. For the process to occur at appreciable rates, the mass splitting between the heavier state and the dark matter must be comparable to, or smaller than, the kinetic energy of particles in the plasma. As a result, the predicted photon line falls in the soft X-ray range, or, potentially, at arbitrarily lower energies. We explore experimental constraints from cosmology and particle physics, and present accurate calculations of the dark matter thermal relic density and of the flux of monochromatic X-rays from thermal plasma excitation. We find that the model provides a natural explanation for the observed 3.5 keV line from clusters of galaxies and from the Galactic center, and is consistent with null detections of the line from dwarf galaxies. The unique line shape, which will be resolved by future observations with the Hitomi (formerly Astro-H) satellite, and the predicted unique morphology and target-temperature dependence will enable easy discrimination of this class of models versus other scenarios for the generation of the 3.5 keV line or of any other unidentified line across the electromagnetic spectrum.

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When dark matter interacts with cosmic rays or interstellar matter: A morphological study

Cited by 8 publications

References 55 publications

Is it possible to discover a dark matter particle with an accelerator?

Is it possible to discover a dark matter particle with an accelerator?

Exploring for sub-MeV Boosted Dark Matter from Xenon Electron Direct Detection

Dark matter inelastic up-scattering with the interstellar plasma: A new source of x-ray lines, including at 3.5 keV

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