Open AccessChandra observations of the galaxy cluster Abell 1835
Author(s) -
Schmidt R.W.,
Allen S.W.,
Fabian A.C.
Publication year - 2001
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2001.04809.x
Subject(s) - physics , astrophysics , abell 2744 , radius , cooling flow , galaxy , radiative cooling , galaxy cluster , substructure , astronomy , cluster (spacecraft) , dark matter , gravitational potential , type cd galaxy , computer security , structural engineering , computer science , engineering , programming language
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 .