Abstract
In this proceeding I summarise the current status of cosmological constraints obtained from current SZ data, focusing on the Planck thermal SZ power spectrum and cluster counts. I discuss the consistency between Planck SZ data and other SZ cluster or galaxy surveys as well as the apparent discrepancy between SZ and CMB for the amplitude of matter clustering σ8. Finally I discuss forecasted constraints on massive neutrinos and the X-ray mass bias in the context of future SZ power spectrum measurements.
Highlights
The thermal Sunyaev Zeldovich power spectrum and galaxy cluster counts detected via the SZ effect are competitive probes of cosmology
The amplitude of the thermal Sunyaev Zeldovich (tSZ) power spectrum is set by the electron pressure profile projected along the line-of-sight and integrated over the halo mass function at all redshift, with heavier clusters contributing more to the largescale power while the abundance of less massive clusters determines the amplitude at small scales
(68%CL) and the probability distribution for the neutrino mass extends towards slightly larger neutrino masses, namely Σmν < 0.37 eV (95%CL) with cluster counts and Σmν < 0.39 eV (95%CL) with SZ power spectrum compared to Σmν < 0.35 eV (95%CL) with CMB alone, it does not peak at any particular value
Summary
The thermal Sunyaev Zeldovich (tSZ) power spectrum and galaxy cluster counts detected via the SZ effect are competitive probes of cosmology. The Planck Collaboration obtained the first all-sky map of the Compton parameter y and its associated power spectrum up to multipole ≈ 103 [7]. Along with the y-map power spectrum, the Planck Collaboration delivered a catalogue of 438 clusters with signal-to-noise ξ > 6 and their associated redshift measured by other X-ray or optical observations [8]. The Planck Collaboration uses X-ray data from the XMM-Newton survey to obtain a universal pressure profile. [9] and reference therein) To account for this X-ray mass bias, one can use a rescaled mass M/B with B ≈ 1.25 in the calculations of the pressure profile and cluster signal-to-noise, where M is the ‘true mass’ that enters the halo mass function. When considering models with massive neutrinos, one should compute the Halo Mass Function (HMF) with the baryon and CDM density instead of the total matter density and with the baryon and CDM transfer functions instead of the total matter transfer functions, see [13] and reference therein
Sign-in/Register to view highlights & summary 
Published Version (
Free)
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call