2001/07/17 by R. W. Schmidt, S. W. Allen, A. C. Fabian · 9 citations
Physics and Astronomy · #Abell 2744 #Astronomy and Astrophysical Research #Cluster (spacecraft) #Cooling flow #Dark matter #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy cluster #RADIUS #Radiative cooling #Scientific Research and Discoveries #Substructure #astro-ph
paper · pdf · doi:10.1046/j.1365-8711.2001.04809.x
published as Mon.Not.Roy.Astron.Soc.327:1057,2001 · 15 pages, 15 figures, accepted by MNRAS
arxiv created 2001/07/17 · openalex publication_date 2001/11/11 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We present the analysis of 30-ks of Chandra observations of the galaxy cluster Abell 1835. Overall, the X-ray image shows a relaxed morphology, although we detect substructure in the inner 30-kpc radius. Spectral analysis shows a steep drop in the X-ray gas temperature from ∼12-keV in the outer regions of the cluster to ∼4-keV in the core. The Chandra data provide tight constraints on the gravitational potential of the cluster which can be parametrized by a Navarro, Frenk & White model. The X-ray data allow us to measure the X-ray gas mass fraction as a function of radius, leading to a determination of the cosmic matter density of . The projected mass within a radius of ∼150-kpc implied by the presence of gravitationally lensed arcs in the cluster is in good agreement with the mass models preferred by the Chandra data. We find a radiative cooling time of the X-ray gas in the centre of Abell 1835 of about . Cooling-flow model fits to the Chandra spectrum and a deprojection analysis of the Chandra image both indicate the presence of a young cooling flow (∼ with an integrated mass deposition rate of within a radius of 30-kpc. We discuss the implications of our results in the light of recent Reflection Grating Spectrograph (RGS) observations of Abell 1835 with XMM-Newton.