Constraints on 3.55 keV line emission from stacked observations of dwarf spheroidal galaxies

By Denys Malyshev, Andrii Y. Neronov, D. Eckert. 2014

154 citations recorded by the source corpus.

Several recent works have reported the detection of an unidentified x-ray line at 3.55 keV, which could possibly be attributed to the decay of dark matter (DM) particles in the halos of galaxy clusters and in the M31 galaxy. We analyze all publicly available XMM-Newton satellite data of dwarf spheroidal galaxies to test the possible DM origin of the line. Dwarf spheroidal galaxies have high mass-to-light ratios, and their interstellar medium is not a source of diffuse x-ray emission; thus, they are expected to provide the cleanest DM decay line signal. Our analysis shows no evidence for the presence of the line in the stacked spectra of the dwarf galaxies. It excludes the sterile neutrino DM decay origin of the 3.5 keV line reported by Bulbul et al. (2014) at the level of $4.1\ensuremath{\sigma}$ under standard assumptions about the Galactic DM column density in the direction of selected dwarf galaxies and at the level of $3.2\ensuremath{\sigma}$ assuming minimal Galactic DM column density. Our analysis is still consistent with the estimate of sterile neutrino DM parameters by Boyarsky et al. (2014) because of its larger uncertainty. However, the central value of their estimate of the mixing angle is inconsistent with our dwarf spheroidals data at the $3.4\ensuremath{\sigma}$ ($2.5\ensuremath{\sigma}$) level assuming the mean (minimal) Galactic DM column density. As a byproduct of our analysis, we provide updated upper limits to the mixing angle of sterile neutrino DM in the mass range between 2 and 20 keV.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/334299dc0d49eb43f141fe6de77fb77b839e9ef7

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Citations in the corpus

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Sterile neutrinos in cosmology (2017, background): “omprises all of the dark matter, is shown. Among the most stringent constraints at low energies and masses are constraints from X-ray observations M31 Horiuchi et al. [134], as well as stacked dwarfs [204]. Also shown are constraints from the diuse X-ray background [197], and individual clusters \Co”