Wednesday, February 23, 2005


Bryan & Voit use numerical simulations of cluster formation to argue that much of the ICM cools at high redshifts hence any heating mechanism to provide the extra entropy must operate at high redshifts as well.

Ballantyne & Fabian analyze XMM-Newton observations of the BLRG 4C+74.26 and find evidence for a relativistic Fe line extending into the ISCO for a maximally rotating BH.

Sesana et al. compute the expected GW signal from coalescing MBHs and predict ~90 events above S/N=5 in a three-year LISA mission.

Keywords: Clusters, AGN, Gravitational Waves

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