Optical-SZE Scaling Relations for DES Optically Selected Clusters within the SPT-SZ Survey

Article, Preprint English OPEN
Saro, A. ; Bocquet, S. ; Mohr, J. ; Rozo, E. ; Benson, B. A. ; Dodelson, S. ; Rykoff, E. S. ; Bleem, L. ; Abbott, T. M. C. ; Abdalla, F. B. ; Allen, S. ; Annis, J. ; Benoit-Levy, A. ; Brooks, D. ; Burke, D. L. ; Capasso, R. ; Rosell, A. Carnero ; Kind, M. Carrasco ; Carretero, J. ; Chiu, I. ; Crawford, T. M. ; Cunha, C. E. ; D'Andrea, C. B. ; da Costa, L. N. ; Desai, S. ; Dietrich, J. P. ; Evrard, A. E. ; Neto, A. Fausti ; Flaugher, B. ; Fosalba, P. ... view all 71 authors (2016)
  • Publisher: Wiley
  • Related identifiers: doi: 10.1093/mnras/stx594
  • Subject: QB | astro-ph.CO | RCUK | uploaded-in-3-months-elsewhere | STFC | Methods: observational; methods: statistical; galaxies: abundances; galaxies: clusters: general; large-scale structure of Universe | Astrophysics - Cosmology and Nongalactic Astrophysics
    arxiv: Astrophysics::Cosmology and Extragalactic Astrophysics

We study the Sunyaev-Zel'dovich effect (SZE) signature in South Pole Telescope (SPT) data for an ensemble of 719 optically identified galaxy clusters selected from 124.6 deg$^2$ of the Dark Energy Survey (DES) science verification data, detecting a stacked SZE signal down to richness $\lambda\sim20$. The SZE signature is measured using matched-filtered maps of the 2500 deg$^2$ SPT-SZ survey at the positions of the DES clusters, and the degeneracy between SZE observable and matched-filter size is broken by adopting as priors SZE and optical mass-observable relations that are either calibrated using SPT selected clusters or through the Arnaud et al. (2010, A10) X-ray analysis. We measure the SPT signal to noise $\zeta$-$\lambda$, relation and two integrated Compton-$y$ $Y_\textrm{500}$-$\lambda$ relations for the DES-selected clusters and compare these to model expectations accounting for the SZE-optical center offset distribution. For clusters with $\lambda > 80$, the two SPT calibrated scaling relations are consistent with the measurements, while for the A10-calibrated relation the measured SZE signal is smaller by a factor of $0.61 \pm 0.12$ compared to the prediction. For clusters at $20 < \lambda < 80$, the measured SZE signal is smaller by a factor of $\sim$0.20-0.80 (between 2.3 and 10~$\sigma$ significance) compared to the prediction, with the SPT calibrated scaling relations and larger $\lambda$ clusters showing generally better agreement. We quantify the required corrections to achieve consistency, showing that there is a richness dependent bias that can be explained by some combination of contamination of the observables and biases in the estimated masses. We discuss possible physical effects, as contamination from line-of-sight projections or from point sources, larger offsets in the SZE-optical centering or larger scatter in the $\lambda$-mass relation at lower richnesses.
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