2013/05/31 by Matteo Bianconi, Stefano Ettori, S. Ettori +1
Physics and Astronomy · #Amplitude #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Cluster (spacecraft) #Flattening #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy cluster #Galaxy formation and evolution #Galaxy rotation curve #Geometry #Gravitational potential #Intracluster medium #Optics #Physics #Rotation (mathematics) #Spectral line #Stellar, planetary, and galactic studies #Surface brightness #astro-ph.CO
paper · pdf · doi:10.1093/mnras/stt1112
11 pages, 12 figures, MNRAS in press. Corrected figures. Matches published version
arxiv created 2013/07/14 · openalex publication_date 2013/07/24 · arxiv updated 2015/06/16 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We study simple models of massive galaxy clusters in which the intracluster medium (ICM) rotates differentially in equilibrium in the cluster gravitational potential. We obtain the X-ray surface-brightness maps, evaluating the isophote flattening due to the gas rotation. Using a set of different rotation laws, we put constraint on the amplitude of the rotation velocity, finding that rotation curves with peak velocity up to ̃600 km/s are consistent with the ellipticity profiles of observed clusters. We convolve each of our models with the instrument response of the X-ray Calorimeter Spectrometer on board the ASTRO-H to calculate the simulated X-ray spectra at different distance from the X-ray centre. We demonstrate that such an instrument will allow us to measure rotation of the ICM in massive clusters, even with rotation velocities as low as ̃100 km/s.