Extragalactic gamma-ray background radiation from dark matter annihilation

Zavala, Jesús; Springel, Volker; Boylan-Kolchin, Michael

doi:10.1111/j.1365-2966.2010.16482.x

Cited by 59 publications

(128 citation statements)

References 117 publications

(189 reference statements)

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“…The procedure we follow to construct the simulated sky maps of the contribution of dark matter annihilation to the X-ray and gamma-ray extragalactic background radiation is essentially an extension of the one discussed in [36]. For a detailed description of the map-making technique we used, we hence refer the reader to section 5.1 of that paper.…”

Section: Extragalactic Cdmabmentioning

confidence: 99%

“…It is then possible to construct simulated sky-maps of the background radiation that give a more complete description of the signal. Such an approach was developed in [36] to analyze the extragalactic gamma-ray radiation produced in situ by annihilation using the state-of-the-art Millennium II simulation [37]. In this paper, we extend this approach to include the contribution from CMB photons scattered by the electrons and positrons produced during annihilation.…”

Section: Introductionmentioning

confidence: 99%

“…This in situ contribution to the CDMAB has been studied in detail before by different authors. In this work we follow the analysis of [36], extending their results to lower energies as described below.…”

Section: A In Situ Photonsmentioning

confidence: 99%

“…(1), the local annihilation rate depends on the square of the local density of dark matter. For the computation of the cosmological background from an N-body simulation, it is more reliable to use analytically integrated quantities over whole dark matter halos (based on scaling laws tested with extremely high-resolution simulations of MW-like halos [42]) instead of trying to use individual simulation particles directly, which are subject to stronger resolution effects and numerical noise [36]. Using this method, each pixel in our sky maps receives contributions of all intervening resolved halos and subhalos along its corresponding past light cone.…”

Section: Extragalactic Cdmabmentioning

confidence: 99%

“…Using this method, each pixel in our sky maps receives contributions of all intervening resolved halos and subhalos along its corresponding past light cone. Additionally, we add the expected contribution of unresolved structures down to the damping scale limit of WIMPs (10 −6 M ⊙ , see sections 5.2-5.4 of [36]). Since we are exploring the case with Sommerfeld FIG.…”

Section: Extragalactic Cdmabmentioning

confidence: 99%

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Cosmic X-ray and gamma-ray background from dark matter annihilation

et al. 2011

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The extragalactic background light (EBL) observed at multiple wavelengths is a promising tool to probe the nature of dark matter. This radiation might contain a significant contribution from gamma-rays produced promptly by dark matter particle annihilation in the many halos and subhalos within our past-light cone. Additionally, the electrons and positrons produced in the annihilation give energy to the cosmic microwave photons to populate the EBL with X-rays and gamma-rays.To study these signals, we create full-sky maps of the expected radiation from both of these contributions using the high-resolution Millennium-II simulation of cosmic structure formation. Our method also accounts for a possible enhancement of the annihilation rate by a Sommerfeld mechanism due to a Yukawa interaction between the dark matter particles prior to annihilation. We use upper limits on the contributions of unknown sources to the EBL to constrain the intrinsic properties of dark matter using a model-independent approach that can be employed as a template to test different particle physics models. These upper limits are based on observational measurements spanning eight orders of magnitude in energy (from soft X-rays measured by the CHANDRA satellite to gamma-rays measured by the Fermi satellite), and on expectations for the contributions from non-blazar active galactic nuclei, blazars and star forming galaxies. To exemplify this approach, we analyze a set of benchmark Sommerfeld-enhanced models that give the correct abundance of dark matter, satisfy constraints from the cosmic microwave background, and fit the cosmic ray spectra measured by PAMELA and Fermi without any contribution from local substructure. We find that these models are in conflict with the EBL constraints unless the contribution of unresolved substructure is small and the dark matter annihilation signal dominates the EBL. We conclude that provided the collisionless cold dark matter paradigm is accurate, even for conservative estimates of the contribution from unresolved substructure and astrophysical backgrounds, the EBL is at least as sensitive a probe of these types of scenarios as the cosmic microwave background. More generally, our results disfavor an explanation of the positron excess measured by the PAMELA satellite based only on dark matter annihilation in the smooth Galactic dark matter halo.PACS numbers: 95.35.+d,95.85.Nv,95.85.Pw

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Section: Extragalactic Cdmabmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: A In Situ Photonsmentioning

confidence: 99%

Section: Extragalactic Cdmabmentioning

confidence: 99%

Section: Extragalactic Cdmabmentioning

confidence: 99%

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Cosmic X-ray and gamma-ray background from dark matter annihilation

et al. 2011

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Large-scale dark matter simulations

Angulo

Hahn

2022

Living Rev Comput Astrophys

111

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We review the field of collisionless numerical simulations for the large-scale structure of the Universe. We start by providing the main set of equations solved by these simulations and their connection with General Relativity. We then recap the relevant numerical approaches: discretization of the phase-space distribution (focusing on N-body but including alternatives, e.g., Lagrangian submanifold and Schrödinger–Poisson) and the respective techniques for their time evolution and force calculation (direct summation, mesh techniques, and hierarchical tree methods). We pay attention to the creation of initial conditions and the connection with Lagrangian Perturbation Theory. We then discuss the possible alternatives in terms of the micro-physical properties of dark matter (e.g., neutralinos, warm dark matter, QCD axions, Bose–Einstein condensates, and primordial black holes), and extensions to account for multiple fluids (baryons and neutrinos), primordial non-Gaussianity and modified gravity. We continue by discussing challenges involved in achieving highly accurate predictions. A key aspect of cosmological simulations is the connection to cosmological observables, we discuss various techniques in this regard: structure finding, galaxy formation and baryonic modelling, the creation of emulators and light-cones, and the role of machine learning. We finalise with a recount of state-of-the-art large-scale simulations and conclude with an outlook for the next decade.

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Numerical simulations of the dark universe: State of the art and the next decade

Kuhlen

Vogelsberger

Angulo

2012

Physics of the Dark Universe

198

174

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We present a review of the current state of the art of cosmological dark matter simulations, with particular emphasis on the implications for dark matter detection efforts and studies of dark energy. This review is intended both for particle physicists, who may find the cosmological simulation literature opaque or confusing, and for astro-physicists, who may not be familiar with the role of simulations for observational and experimental probes of dark matter and dark energy. Our work is complementary to the contribution by M. Baldi in this issue, which focuses on the treatment of dark energy and cosmic acceleration in dedicated N-body simulations.Truly massive dark matter-only simulations are being conducted on national supercomputing centers, employing from several billion to over half a trillion particles to simulate the formation and evolution of cosmologically representative volumes (cosmic scale) or to zoom in on individual halos (cluster and galactic scale). These simulations cost millions of core-hours, require tens to hundreds of terabytes of memory, and use up to petabytes of disk storage. Predictions from such simulations touch on almost every aspect of dark matter and dark energy studies, and we give a comprehensive overview of this connection. We also discuss the limitations of the cold and collisionless DM-only approach, and describe in some detail efforts to include different particle physics as well as baryonic physics in cosmological galaxy formation simulations, including a discussion of recent results highlighting how the distribution of dark matter in halos may be altered. We end with an outlook for the next decade, presenting our view of how the field can be expected to progress.

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Extragalactic gamma-ray background radiation from dark matter annihilation

Cited by 59 publications

References 117 publications

Cosmic X-ray and gamma-ray background from dark matter annihilation

Cosmic X-ray and gamma-ray background from dark matter annihilation

Large-scale dark matter simulations

Numerical simulations of the dark universe: State of the art and the next decade

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