Lovell, Mark R. and Iakubovskyi, Dmytro and Barnes, David and Bose, Sownak and Frenk, Carlos S. and Theuns, Tom and Hellwing, Wojciech A. (2019) 'Simulating the dark matter decay signal from the Perseus Galaxy Cluster.', The astrophysical journal., 875 (2). L24.
the C-EAGLE simulations of galaxy clusters to predict the flux, width, and shape of a dark matter decay line, paying particular attention to the unexplained 3.55keV line detected in the spectra of some galaxies and clusters, and the upcoming XRISM X-ray observatory mission. We show that the line width in C-EAGLE clusters similar to Perseus is typically [600–800]km s-1, and therefore narrower than the amplitude of the velocity dispersion of galaxies in the cluster. Halos that are significantly disturbed can, however, exhibit galaxy velocity dispersions higher than 1000km s-1, and in this case will show a large difference between the line profiles of on- and offcenter observations. We show that the line profile is likely to be slightly asymmetric, but still well approximated by a Gaussian at the 10% level, and that the halo asymmetry can lead to fluxes that vary by a factor of two. In summary, we predict that, if the previously reported 3.55keV line detections do originate from dark matter decay, the XRISM mission will detect a line with a roughly Gaussian profile at a rest-frame energy of 3.55keV, with a width >600 km s-1and flux approximately in the range [4–9] ´ 10-8 counts s-1 cm-2.
|Full text:||(VoR) Version of Record|
Download PDF (1001Kb)
|Publisher Web site:||https://doi.org/10.3847/2041-8213/ab13ac|
|Publisher statement:||© 2019. The American Astronomical Society. All rights reserved.|
|Date accepted:||26 March 2019|
|Date deposited:||09 May 2019|
|Date of first online publication:||19 April 2019|
|Date first made open access:||09 May 2019|
Save or Share this output
|Look up in GoogleScholar|