Self-Calibration of Cluster Dark Energy Studies: Observable-Mass Distribution

Details Self-Calibration of Cluster Dark Energy Studies: Observable-Mass Distribution Self-Calibration of Cluster Dark Energy Studies: Observable-Mass Distribution

2005-03-16

arxiv.org/abs/astro-ph/0503363v1

Phys.Rev.D72:043006,2005

Astronomy and Astrophysics

Astrophysics

6 pages, 6 figures, submitted to PRD

Scientific paper

10.1103/PhysRevD.72.043006

The exponential sensitivity of cluster number counts to the properties of the dark energy implies a comparable sensitivity to not only the mean but also the actual_distribution_ of an observable mass proxy given the true cluster mass. For example a 25% scatter in mass can provide a ~50% change in the number counts at z~2 for the upcoming SPT survey. Uncertainty in the scatter of this amount would degrade dark energy constraints to uninteresting levels. Given the shape of the actual mass function, the properties of the distribution may be internally monitored by the shape of the_observable_ mass function. An arbitrary evolution of the scatter of a mass-independent Gaussian distribution may be self-calibrated to allow a measurement of the dark energy equation of state of Delta w ~0.1. External constraints on the mass_variance_ of the distribution that are more accurate than Delta var < 0.01 at z~1 can further improve constraints by up to a factor of 2. More generally, cluster counts and their sample variance measured as a function of the observable provide internal consistency checks on the assumed form of the observable-mass distribution that will protect against misinterpretation of the dark energy constraints.

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