THE X-RAY LINE FEATURE AT 3.5 KeV IN GALAXY CLUSTER SPECTRA

• Published in: The Astrophysical journal 2015-08, Vol.809 (1), p.1-7
• Main Authors: Phillips, K. J. H., Sylwester, B., Sylwester, J.
• Format: Article
• Language: English
• Subjects: Abundance; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; CHLORINE IONS; Galactic clusters; galaxies: clusters: general; galaxies: individual (M31); GALAXY CLUSTERS; GAMMA RADIATION; KEV RANGE; MULTICHARGED IONS; Neutrinos; NONLUMINOUS MATTER; Potassium; POTASSIUM IONS; RESOLUTION; SOLAR FLARES; Spectral lines; STELLAR CORONAE; SUN; Sun: abundances; Sun: X-rays, gamma rays; X RADIATION; X-RAY GALAXIES; X-RAY SPECTRA; X-rays; X-rays: galaxies: clusters; XMM (spacecraft)
• ISSN: 0004-637X; 1538-4357; 1538-4357
• DOI: 10.1088/0004-637X/809/1/50

ABSTRACT Recent work by Bulbul et al. and Boyarsky et al. has suggested that a line feature at ∼3.5 keV in the X-ray spectra of galaxy clusters and individual galaxies seen with XMM-Newton is due to the decay of sterile neutrinos, a dark matter candidate. This identification has been criticized by Jeltema & Profumo on the grounds that model spectra suggest that atomic transitions in helium-like potassium (K xviii) and chlorine (Cl xvi) are more likely to be the emitters. Here it is pointed out that the K xviii lines have been observed in numerous solar flare spectra at high spectral resolution with the RESIK crystal spectrometer and also appear in Chandra HETG spectra of the coronally active star Gem. In addition, the solar flare spectra at least indicate a mean coronal potassium abundance, which is a factor between 9 and 11 higher than the solar photospheric abundance. This fact, together with the low statistical quality of the XMM-Newton spectra, completely account for the ∼3.5 keV feature and there is therefore no need to invoke a sterile neutrino interpretation of the observed line feature at ∼3.5 keV.