An X-ray Galaxy Cluster Survey for Investigations of Dark Energy
Haiman, Z. · Allen, S. · Bahcall, N. · Bautz, M. · Boehringer, H. · Borgani, S. · Bryan, G. · Cabrera, B. · Canizares, C. · Citterio, O. · Evrard, A. · Finoguenov, A. · Griffiths, R. · Hasinger, G. · Henry, P. · Jahoda, K. · Jernigan, G. · Kahn, S. · Lamb, D. · Majumdar, S. · Mohr, J. · Molendi, S. · Mushotzky, R. · Pareschi, G. · Peterson, J. · Petre, R. · Predehl, P. · Rasmussen, A. · Ricker, G. · Ricker, P. · Rosati, P. · Sanderson, A. · Stanford, A. · Voit, M. · Wang, S. · White, N. · White, S.
Original · EN
The amount and nature of dark energy (DE) can be tightly constrained by measuring the spatial correlation features and evolution of a sample of 100,000 galaxy clusters over the redshift range 0<z < 1.5. Such an X-ray survey will discover all collapsed structures with mass above 3.5e14 solar masss at redshifts z<2 (i.e. the full range where such objects are expected) in the high Galactic latitude sky. Above this mass threshold the tight correlations between X-ray observables and mass allow direct interpretation of the data. We describe the constraints on Dark Energy that can be inferred from such a survey, using powerful self-calibration techniques to relate the X-ray observables (luminosity and temperature) to the underlying mass.
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