Constraints on the presence of a 3.5 keV dark matter emission line from<i>Chandra</i>observations of the Galactic centre

Riemer-Sørensen, Signe

doi:10.1051/0004-6361/201527278

Cited by 56 publications

(41 citation statements)

References 94 publications

(170 reference statements)

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“…Such a scenario is relevant, for example, as a dark matter interpretation of a spectral feature at E ≃ 3.55 keV observed in x-ray observations from several dark matter dominated sources [24,25]. While non-dark-matter explanations of this observation have been suggested [49][50][51], the origin of the 3.5 keV line as dark matter decay has not been conclusively excluded [52].…”

Section: Other Constraintsmentioning

confidence: 98%

Observational constraints on decoupled hidden sectors

et al. 2016

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We consider an extension of the Standard Model with a singlet sector consisting of a real (pseudo)scalar and a Dirac fermion coupled with the Standard Model only via the scalar portal. We assume that the portal coupling is weak enough for the singlet sector not to thermalize with the Standard Model allowing the production of singlet particles via the freeze-in mechanism. If the singlet sector interacts with itself sufficiently strongly, it may thermalize within itself, resulting in dark matter abundance determined by the freeze-out mechanism operating within the singlet sector. We investigate this scenario in detail. In particular, we show that requiring the absence of inflationary isocurvature fluctuations provides lower bounds on the magnitude of the dark sector self-interactions and in parts of the parameter space favors sufficiently large self-couplings, supported also by the features observed in the small-scale structure formation.

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Section: Other Constraintsmentioning

confidence: 98%

Observational constraints on decoupled hidden sectors

et al. 2016

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“…Instead of interpolating, we track the positions and velocities of subhalos between snapshots by integrating their orbits in the po-tential of the halo, which we assume to be static over this time and, for simplicity, axisymmetric. We model the potential and integrate the orbits using the publicly available codes GALPY and PYNBODY (Bovy 2015;Pontzen et al 2013). This method accurately reproduces the orbits of subhalos around the host halo, even in situations where the cubic spline method is most prone to failure.…”

Section: Orbitsmentioning

confidence: 99%

Subhalo destruction in the Apostle and Auriga simulations

Richings

Frenk

Jenkins

et al. 2019

Monthly Notices of the Royal Astronomical Society

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N-body simulations make unambiguous predictions for the abundance of substructures within dark matter halos. However, the inclusion of baryons in the simulations changes the picture because processes associated with the presence of a large galaxy in the halo can destroy subhalos and substantially alter the mass function and velocity distribution of subhalos. We compare the effect of galaxy formation on subhalo populations in two state-of-the-art sets of hydrodynamical ΛCDM simulations of Milky Way mass halos, APOSTLE and AURIGA. We introduce a new method for tracking the orbits of subhalos between simulation snapshots that gives accurate results down to a few kiloparsecs from the centre of the halo. Relative to a dark matter-only simulation, the abundance of subhalos in APOSTLE is reduced by 50% near the centre and by 10% within r 200 . In AURIGA the corresponding numbers are 80% and 40%. The velocity distributions of subhalos are also affected by the presence of the galaxy, much more so in AURIGA than in APOSTLE . The differences on subhalo properties in the two simulations can be traced back to the mass of the central galaxies, which in AURIGA are typically twice as massive as those in APOSTLE . We show that some of the results from previous studies are inaccurate due to systematic errors in the modelling of subhalo orbits near the centre of halos.

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“…Recently, some researches claimed detection of emission lines due to annihilation of sterile neutrinos near the Galactic center region [17,18,19,20]. Since significance of the detection is not large, further observations are encouraged to constrain physical parameters of dark matter particles.…”

Section: Franco Giovannellimentioning

confidence: 99%