Observation of the new emission line at ~3.5 keV in X-ray spectra of galaxies and galaxy clusters

Iakubovskyi, Dmytro

doi:10.17721/2227-1481.6.3-15

Cited by 27 publications

(28 citation statements)

References 169 publications

(265 reference statements)

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“…The detection of an unidentified line was reported recently in the stacked spectrum of galaxy clusters [190], in the individual spectra of nearby galaxy clusters [190,191,622] (see also [612]), in the Andromeda galaxy [191], and in the Galactic Center region [608][609][610], see also [623] for a recent review. The position of the line is E = 3.55 keV with an uncertainty in position ∼ 0.05 keV.…”

Section: 5 Kev Linementioning

confidence: 88%

A White Paper on keV sterile neutrino Dark Matter

Adhikari

Agostini

et al. 2017

J. Cosmol. Astropart. Phys.

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372

316

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Abstract. We present a comprehensive review of keV-scale sterile neutrino Dark Matter, collecting views and insights from all disciplines involved -cosmology, astrophysics, nuclear, and particle physics -in each case viewed from both theoretical and experimental/observational perspectives. After reviewing the role of active neutrinos in particle physics, astrophysics, and cosmology, we focus on sterile neutrinos in the context of the Dark Matter puzzle. Here, we first review the physics motivation for sterile neutrino Dark Matter, based on challenges and tensions in purely cold Dark Matter scenarios. We then round out the discussion by critically summarizing all known constraints on sterile neutrino Dark Matter arising from astrophysical observations, laboratory experiments, and theoretical considerations. In this context, we provide a balanced discourse on the possibly positive signal from X-ray observations. Another focus of the paper concerns the construction of particle physics models, aiming to explain how sterile neutrinos of keV-scale masses could arise in concrete settings beyond the Standard Model of elementary particle physics. The paper ends with an extensive review of current and future astrophysical and laboratory searches, highlighting new ideas and their experimental challenges, as well as future perspectives for the discovery of sterile neutrinos.

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Section: 5 Kev Linementioning

confidence: 88%

A White Paper on keV sterile neutrino Dark Matter

Adhikari

Agostini

et al. 2017

J. Cosmol. Astropart. Phys.

Self Cite

372

316

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“…4, we find that 7 keV axino DM with entropy dilution factor Δ ¼ 4.7 fits the strongest lower bound from the Ly-α forest data, m WDM ¼ 5.3 keV, very well. 5 It means that we need only a mild entropy dilution factor, Δ > 4.7, to evade the Ly-α forest constraints.…”

Section: Ly-α Forest Constraintsmentioning

confidence: 99%

“…While there are reports of null detection, e.g., in dwarf spheroidal galaxies [4], the decaying dark matter (DM) explanation of the 3.5 keV line excess is yet to be excluded (see Ref. [5] for a thorough review).…”

Section: Introductionmentioning

confidence: 99%

Colder freeze-in axinos decaying into photons

et al. 2018

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We point out that 7 keV axino dark matter (DM) in the R-parity violating (RPV) supersymmetric (SUSY) Dine-Fischler-Srednicki-Zhitnitsky axion model can simultaneously reproduce the 3.5 keV x-ray line excess and evade stringent constraints from the Ly-α forest data. Peccei-Quinn symmetry breaking naturally generates both the TeV-scale μ term and the MeV-scale RPV term. The RPV term introduces a tiny axinoneutrino mixing and provides axino DM as a variant of the sterile neutrino DM explaining the 3.5 keV x-ray line excess. Axinos are produced by freeze-in processes via the μ term. The resultant phase space distribution tends to be colder than the Fermi-Dirac distribution. The inherent entropy production from late-time saxion decay makes axinos even colder than those without saxion decay. The resultant axino DM takes the correct relic density and is compatible even with the latest and strongest constraint from the Ly-α forest data.

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“…There have also been null-detection reports[13][14][15][16][17][18][19][20][21] and claims that the DM interpretation fails to pass consistency checks from line profiles[22,23]. We note that some of the null-detection reports are just not sensitive enough to exclude the DM interpretation (see Refs [24,25]. for summaries) and the failure claims are refuted[26][27][28][29][30].…”

mentioning

confidence: 92%

Constraining FIMP from the structure formation of the Universe: analytic mapping from m_WDM

Kamada

Yanagi

2019

J. Cosmol. Astropart. Phys.

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A feebly interacting massive particle (FIMP), contrasting with a weakly interacting massive particle (WIMP), is an intriguing dark matter (DM) candidate. Light (keV-scale) FIMP DM is of particular interest: its radiative decay leaves a line signal in x-ray spectra; and it is warm dark matter (WDM) and alters the galactic-scale structure formation of the Universe from that with WIMP DM. Once a possible x-ray line is reported (e.g., 3.5 keV line and 7 keV FIMP DM is inferred), one has to check whether or not this FIMP DM is compatible with the structure formation. Here is an issue: the structure formation constraint on WDM is often reported in terms of the so-called thermal WDM mass m WDM , which cannot be directly applied to FIMP parameters. In this paper, we introduce a benchmark FIMP model that represents well a broad class of FIMP models. A big advantage of this benchmark is that we can derive the analytic formula of the non-thermal phase space distribution of FIMPs produced from freezein processes. By further deriving a certain "warmness" quantity, we can analytically map m WDM to FIMP parameters. Our analytic map indicates that 7 keV FIMP DM, without entropy production or a degenerate spectrum, is in tension with the latest Lyman-α forest data. Our analytic map will be very useful for future updates of observational constraints and reports of x-ray lines. It is also very easy to incorporate our analytic formula into a Boltzmann solver so that a linear matter power spectrum is readily accessible. Our benchmark model will facilitate FIMP searches and particle physics model-building. arXiv:1907.04558v1 [hep-ph]

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Observation of the new emission line at ~3.5 keV in X-ray spectra of galaxies and galaxy clusters

Cited by 27 publications

References 169 publications

A White Paper on keV sterile neutrino Dark Matter

A White Paper on keV sterile neutrino Dark Matter

Colder freeze-in axinos decaying into photons

Constraining FIMP from the structure formation of the Universe: analytic mapping from m_WDM

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Observation of the new emission line at ~3.5 keV in X-ray spectra of galaxies and galaxy clusters

Cited by 27 publications

References 169 publications

A White Paper on keV sterile neutrino Dark Matter

A White Paper on keV sterile neutrino Dark Matter

Colder freeze-in axinos decaying into photons

Constraining FIMP from the structure formation of the Universe: analytic mapping from mWDM

Contact Info

Product

Resources

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Constraining FIMP from the structure formation of the Universe: analytic mapping from m_WDM