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X-ray lines and self-interacting dark matter.

Mambrini Y, Toma T - Eur Phys J C Part Fields (2015)

Bottom Line: We study the correlation between a monochromatic signal from annihilating dark matter and its self-interacting cross section.We apply our argument to a complex scalar dark sector, where the pseudo-scalar plays the role of a warm dark matter candidate while the scalar mediates its interaction with the Standard Model.We also propose a way to distinguish such models by future direct detection techniques.

View Article: PubMed Central - PubMed

Affiliation: Laboratoire de Physique Théorique, Université de Paris-Sud 11, CNRS-UMR 8627, 91405 Orsay Cedex, France.

ABSTRACT

We study the correlation between a monochromatic signal from annihilating dark matter and its self-interacting cross section. We apply our argument to a complex scalar dark sector, where the pseudo-scalar plays the role of a warm dark matter candidate while the scalar mediates its interaction with the Standard Model. We combine the recent observation of the cluster Abell 3827 for self-interacting dark matter and the constraints on the annihilation cross section for monochromatic X-ray lines. We also confront our model to a set of recent experimental analyses and find that such an extension can naturally produce a monochromatic keV signal corresponding to recent observations of Perseus or Andromeda, while in the meantime it predicts a self-interacting cross section of the order of [Formula: see text], as recently claimed in the observation of the cluster Abell 3827. We also propose a way to distinguish such models by future direct detection techniques.

No MeSH data available.


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Feynman diagrams for dark matter annihilation into two photons. The second diagram can be generated by higher dimensional operators (see the text for details)
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Fig2: Feynman diagrams for dark matter annihilation into two photons. The second diagram can be generated by higher dimensional operators (see the text for details)

Mentions: The presence of coupling generates naturally the production of monochromatic photons from the s-channel annihilation of the dark matter candidate a as depicted on the left of Fig. 2. The annihilation cross section for is given by [36]5\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\begin{aligned} \sigma {v}_{\gamma \gamma }=\frac{\lambda m_a^2m_s^2}{\pi \Lambda ^2(m_s^2-4m_a^2)^2}. \end{aligned}$$\end{document}σvγγ=λma2ms2πΛ2(ms2-4ma2)2.For , the above cross sections, Eqs. (3) and (5), can be simplified to6\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\begin{aligned} \frac{\sigma _{aa}}{m_a}\approx \frac{\lambda ^2 m_a}{32\pi m_s^4},\quad \sigma {v}_{\gamma \gamma }\approx \frac{\lambda m_a^2}{\pi \Lambda ^2m_s^2}. \end{aligned}$$\end{document}σaama≈λ2ma32πms4,σvγγ≈λma2πΛ2ms2.By eliminating in both expressions, it becomes possible for each energy being equivalent to the dark matter mass since dark matter is almost at rest, to express uniquely as a function of and ,7\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\begin{aligned} \sigma v_{\gamma \gamma }= & {} \frac{4 \sqrt{2} E_\gamma ^{3/2}}{\Lambda ^2 \sqrt{\pi }} \sqrt{\frac{\sigma _{aa}}{m_a}}\nonumber \\\simeq & {} 1.3 \times 10^{-33} \left( \frac{100~\mathrm {TeV}}{\Lambda } \right) ^2 \left( \frac{E_\gamma }{3~\mathrm {keV}}\right) ^{3/2}\nonumber \\&\times \sqrt{\frac{\sigma _{aa}/m_a}{1~\mathrm {cm^2 /g}}} ~~ \mathrm {cm^3/s} . \end{aligned}$$\end{document}σvγγ=42Eγ3/2Λ2πσaama≃1.3×10-33100TeVΛ2Eγ3keV3/2×σaa/ma1cm2/gcm3/s.This is one of the main results of our work. It is indeed surprising that, asking for a reasonable value for the self-interacting cross section of the order of , one obtains naturally the annihilation cross section of the order of for a monochromatic keV signal, which corresponds exactly to the magnitude of the signals observed by XMM Newton [33–35] in the Perseus cluster.5 On the other hand, strong limits obtained from the non-observation of a monochromatic line by observatories such as HEAO-1 INTEGRAL, COMPTEL, EGRET, and FERMI restrict severely the lower bound on the scale in the rest of the parameter space, as we will analyze in the following section.


X-ray lines and self-interacting dark matter.

Mambrini Y, Toma T - Eur Phys J C Part Fields (2015)

Feynman diagrams for dark matter annihilation into two photons. The second diagram can be generated by higher dimensional operators (see the text for details)
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Related In: Results  -  Collection

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Fig2: Feynman diagrams for dark matter annihilation into two photons. The second diagram can be generated by higher dimensional operators (see the text for details)
Mentions: The presence of coupling generates naturally the production of monochromatic photons from the s-channel annihilation of the dark matter candidate a as depicted on the left of Fig. 2. The annihilation cross section for is given by [36]5\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\begin{aligned} \sigma {v}_{\gamma \gamma }=\frac{\lambda m_a^2m_s^2}{\pi \Lambda ^2(m_s^2-4m_a^2)^2}. \end{aligned}$$\end{document}σvγγ=λma2ms2πΛ2(ms2-4ma2)2.For , the above cross sections, Eqs. (3) and (5), can be simplified to6\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\begin{aligned} \frac{\sigma _{aa}}{m_a}\approx \frac{\lambda ^2 m_a}{32\pi m_s^4},\quad \sigma {v}_{\gamma \gamma }\approx \frac{\lambda m_a^2}{\pi \Lambda ^2m_s^2}. \end{aligned}$$\end{document}σaama≈λ2ma32πms4,σvγγ≈λma2πΛ2ms2.By eliminating in both expressions, it becomes possible for each energy being equivalent to the dark matter mass since dark matter is almost at rest, to express uniquely as a function of and ,7\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\begin{aligned} \sigma v_{\gamma \gamma }= & {} \frac{4 \sqrt{2} E_\gamma ^{3/2}}{\Lambda ^2 \sqrt{\pi }} \sqrt{\frac{\sigma _{aa}}{m_a}}\nonumber \\\simeq & {} 1.3 \times 10^{-33} \left( \frac{100~\mathrm {TeV}}{\Lambda } \right) ^2 \left( \frac{E_\gamma }{3~\mathrm {keV}}\right) ^{3/2}\nonumber \\&\times \sqrt{\frac{\sigma _{aa}/m_a}{1~\mathrm {cm^2 /g}}} ~~ \mathrm {cm^3/s} . \end{aligned}$$\end{document}σvγγ=42Eγ3/2Λ2πσaama≃1.3×10-33100TeVΛ2Eγ3keV3/2×σaa/ma1cm2/gcm3/s.This is one of the main results of our work. It is indeed surprising that, asking for a reasonable value for the self-interacting cross section of the order of , one obtains naturally the annihilation cross section of the order of for a monochromatic keV signal, which corresponds exactly to the magnitude of the signals observed by XMM Newton [33–35] in the Perseus cluster.5 On the other hand, strong limits obtained from the non-observation of a monochromatic line by observatories such as HEAO-1 INTEGRAL, COMPTEL, EGRET, and FERMI restrict severely the lower bound on the scale in the rest of the parameter space, as we will analyze in the following section.

Bottom Line: We study the correlation between a monochromatic signal from annihilating dark matter and its self-interacting cross section.We apply our argument to a complex scalar dark sector, where the pseudo-scalar plays the role of a warm dark matter candidate while the scalar mediates its interaction with the Standard Model.We also propose a way to distinguish such models by future direct detection techniques.

View Article: PubMed Central - PubMed

Affiliation: Laboratoire de Physique Théorique, Université de Paris-Sud 11, CNRS-UMR 8627, 91405 Orsay Cedex, France.

ABSTRACT

We study the correlation between a monochromatic signal from annihilating dark matter and its self-interacting cross section. We apply our argument to a complex scalar dark sector, where the pseudo-scalar plays the role of a warm dark matter candidate while the scalar mediates its interaction with the Standard Model. We combine the recent observation of the cluster Abell 3827 for self-interacting dark matter and the constraints on the annihilation cross section for monochromatic X-ray lines. We also confront our model to a set of recent experimental analyses and find that such an extension can naturally produce a monochromatic keV signal corresponding to recent observations of Perseus or Andromeda, while in the meantime it predicts a self-interacting cross section of the order of [Formula: see text], as recently claimed in the observation of the cluster Abell 3827. We also propose a way to distinguish such models by future direct detection techniques.

No MeSH data available.


Related in: MedlinePlus