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The distribution of dark matter in the A2256 clusterUsing spatially resolved X-ray spectroscopy, it was determined that the X-ray emitting gas in the rich cluster A2256 is nearly isothermal to a radius of at least 0.76/h Mpc, or about three core radii. These data can be used to measure the distribution of the dark matter in the cluster. It was found that the total mass interior to 0.76/h Mpc and 1.5/h Mpc is (0.5 +/- 0.1 and 1.0 +/- 0.5) x 10(exp 15)/h of the solar mass respectively where the errors encompass the full range allowed by all models used. Thus, the mass appropriate to the region where spectral information was obtained is well determined, but the uncertainties become large upon extrapolating beyond that region. It is shown that the galaxy orbits are midly anisotropic which may cause the beta discrepancy in this cluster.
Document ID
19940017106
Document Type
Preprint (Draft being sent to journal)
Authors
Henry, J. Patrick (Hawaii Univ. Honolulu., United States)
Briel, Ulrich G. (Max-Planck-Inst. fuer Physik und Astrophysik Garching, Germany)
Nulsen, Paul E. J. (Wollongong Univ. Australia)
Date Acquired
September 6, 2013
Publication Date
January 1, 1993
Subject Category
ASTRONOMY
Report/Patent Number
NAS 1.26:194699
MPE-PREPRINT-242
NASA-CR-194699
Funding Number(s)
CONTRACT_GRANT: NAG5-1789
CONTRACT_GRANT: NATO-CRG-910415
Distribution Limits
Public
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