Friday, May 06, 2005


Ostriker et al. present a simple polytropic model for the ICM.

Nulsen et al. find a Mach 1.65 shock in the X-ray image of the cluster around Her A.

Nevaleinen et al. describe XMM EPIC background modelling.

Page et al. suggest that it may be possible to use observations of minor planets in the outer Solar System to test the Pioneer Effect.

Matheson and Safi-Harb put together all the Chandra data on G21.5-0.9.

Begelmann & Nath invoke a feedback model to explain the MBH-bulge sigma relation.

Angulo et al. argue that a survey of clusters at z~1 looking for baryon fluctuations can determine dark energy w to better than 10% without requiring knowledge of the cluster mass.

Jenet et al. show that radio observations of 40 pulsars with a timing accuracy of 100 nano-seconds could detect the effects of the stochastic gravitational wave background from merging BHs. This would take 5-20 years of observations depending on the actual background.

Fabian et al. analyze six XMM observations of 1H0419-577 and argue that the lowest flux state is dominated by emission from within a few gravitational radii of the BH, which must be in an extreme Kerr state.

Keywords: ICM, XMM, Gravity, BH, SNR

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