The possibility of determining the value of the Hubble constant using observations of galaxy clusters in X-ray and microwave wavelengths through the Sunyaev Zel'dovich (SZ) effect has long been known. Previous measurements have been plagued by relatively large errors in the observational data and severe biases induced, for example, by cluster triaxiality and clumpiness. The advent of Planck allows us to map the Compton parameter y, that is, the amplitude of the SZ effect, with unprecedented accuracy at intermediate cluster-centric radii, which in turn allows performing a detailed spatially resolved comparison with X-ray measurements. Given such higher quality observational data, we developed a Bayesian approach that combines informed priors on the physics of the intracluster medium obtained from hydrodynamical simulations of massive clusters with measurement uncertainties. We applied our method to a sample of 61 galaxy clusters with redshifts up to z? < ? 0.5 observed with Planck and XMM-Newton and find H0? =? 67? ±? 3 km s -1 Mpc -1 © ESO 2019.
Kozmanyan, A., Bourdin, H., Mazzotta, P., Rasia, E., Sereno, M. (2019). Deriving the Hubble constant using Planck and XMM-Newton observations of galaxy clusters. ASTRONOMY & ASTROPHYSICS, 621 [10.1051/0004-6361/201833879].
Deriving the Hubble constant using Planck and XMM-Newton observations of galaxy clusters
Bourdin, H;Mazzotta, P;
2019-01-01
Abstract
The possibility of determining the value of the Hubble constant using observations of galaxy clusters in X-ray and microwave wavelengths through the Sunyaev Zel'dovich (SZ) effect has long been known. Previous measurements have been plagued by relatively large errors in the observational data and severe biases induced, for example, by cluster triaxiality and clumpiness. The advent of Planck allows us to map the Compton parameter y, that is, the amplitude of the SZ effect, with unprecedented accuracy at intermediate cluster-centric radii, which in turn allows performing a detailed spatially resolved comparison with X-ray measurements. Given such higher quality observational data, we developed a Bayesian approach that combines informed priors on the physics of the intracluster medium obtained from hydrodynamical simulations of massive clusters with measurement uncertainties. We applied our method to a sample of 61 galaxy clusters with redshifts up to z? < ? 0.5 observed with Planck and XMM-Newton and find H0? =? 67? ±? 3 km s -1 Mpc -1 © ESO 2019.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
