Gamma ray constraints on Decaying Dark Matter

Cirelli, Marco; Panci, Paolo; Moulin, Emmanuel; Serpico, Pasquale D.; Viana, Aion

doi:10.1103/PhysRevD.86.083506

Article
Report number	CERN-PH-TH-2012-110 ; SACLAY-T12-034 ; IRFU-12-34 ; DIAS-2012-11 ; LAPTH-023-12 ; arXiv:1205.5283 ; SACLAY--T12-034 ; CP3-ORIGINS-2012-10 ; CERN-PH-TH-2012-110 ; SACLAY-T12-034 ; IRFU-12-34 ; CP3-ORIGINS-2012-10 ; DIAS-2012-11 ; LAPTH-023-12
Title	Gamma ray constraints on Decaying Dark Matter
Author(s)	Cirelli, Marco (CERN ; Saclay) ; Moulin, Emmanuel (Saclay) ; Panci, Paolo (Southern Denmark U., CP3-Origins) ; Serpico, Pasquale D. (Annecy, LAPTH ; CERN) ; Viana, Aion (Saclay)
Publication	2012
Imprint	25 May 2012
Number of pages	18
Note	Comments: 18 pages, 3 figures 18 pages, 3 figures. v2: constraint procedure slightly modified, conclusions unchanged; some references and some clarifications added; matches version published on PRD
In:	Phys. Rev. D 86 (2012) pp.083506
DOI	10.1103/PhysRevD.86.083506 10.1103/PhysRevD.86.109901
Subject category	Astrophysics and Astronomy
Abstract	We derive new bounds on decaying Dark Matter from the gamma ray measurements of (i) the isotropic residual (extragalactic) background by Fermi and (ii) the Fornax galaxy cluster by HESS. We find that those from (i) are among the most stringent constraints currently available, for a large range of DM masses and a variety of decay modes, excluding half-lives up to 10^26 to few 10^27 seconds. In particular, they rule out the interpretation in terms of decaying DM of the e^\pm spectral features in Pamela, Fermi and HESS, unless very conservative choices are adopted. We also discuss future prospects for CTA bounds from Fornax which, contrary to the present HESS constraints of (ii), may allow for an interesting improvement and may become better than those from the current or future extragalactic Fermi data.
Copyright/License	Preprint: © 2012-2025 CERN (License: CC-BY-3.0)

$\em An example of the signals in different channels from a decaying DM candidate that fits the charged CR anomalies: we show the positron fraction (upper left), all leptons (upper right), antiproton (lower left) and isotropic gamma ray (lower right) spectra for the best fit candidate DM $\to \mu^+\mu^-$, namely $M_{\rm DM} = 3760$ GeV, $\tau_{\rm dec} = 1.6 \ 10^{26}$ sec (marked by a white cross in fig.s~\ref{fig:exclusionexample} and \ref{fig:exclusion}). The `\,\PAMELA\ 2008' datapoints are reported for completeness, but we use only the more recent `\,\PAMELA\ 2010' in the fits (see text for details). In each panel, the DM contributions are dashed and the astrophysical background is shaded gray. In the lower right panel, the dotted (dashed) lines refer to the flux neglecting (including) extragalactic absorption, see Sec.~\ref{isotropic}.$ $\em An example of the signals in different channels from a decaying DM candidate that fits the charged CR anomalies: we show the positron fraction (upper left), all leptons (upper right), antiproton (lower left) and isotropic gamma ray (lower right) spectra for the best fit candidate DM $\to \mu^+\mu^-$, namely $M_{\rm DM} = 3760$ GeV, $\tau_{\rm dec} = 1.6 \ 10^{26}$ sec (marked by a white cross in fig.s~\ref{fig:exclusionexample} and \ref{fig:exclusion}). The `\,\PAMELA\ 2008' datapoints are reported for completeness, but we use only the more recent `\,\PAMELA\ 2010' in the fits (see text for details). In each panel, the DM contributions are dashed and the astrophysical background is shaded gray. In the lower right panel, the dotted (dashed) lines refer to the flux neglecting (including) extragalactic absorption, see Sec.~\ref{isotropic}.$ $\em An example of the signals in different channels from a decaying DM candidate that fits the charged CR anomalies: we show the positron fraction (upper left), all leptons (upper right), antiproton (lower left) and isotropic gamma ray (lower right) spectra for the best fit candidate DM $\to \mu^+\mu^-$, namely $M_{\rm DM} = 3760$ GeV, $\tau_{\rm dec} = 1.6 \ 10^{26}$ sec (marked by a white cross in fig.s~\ref{fig:exclusionexample} and \ref{fig:exclusion}). The `\,\PAMELA\ 2008' datapoints are reported for completeness, but we use only the more recent `\,\PAMELA\ 2010' in the fits (see text for details). In each panel, the DM contributions are dashed and the astrophysical background is shaded gray. In the lower right panel, the dotted (dashed) lines refer to the flux neglecting (including) extragalactic absorption, see Sec.~\ref{isotropic}.$ Show more plots

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ჩანაწერი შექმნილია 2012-05-25, ბოლოს შესწორებულია 2018-08-11

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