Optical-SZE Scaling Relations for DES Optically Selected Clusters within the SPT-SZ Survey
Creators: name: Saro, A.
name: Bocquet, S.
name: Mohr, J.
name: Rozo, E.
name: Benson, B. A.
name: Dodelson, S.
name: Rykoff, E. S.
name: Bleem, L.
name: Abbott, T. M. C.
name: Abdalla, F. B.
name: Allen, S.
name: Annis, J.
name: Benoit-Levy, A.
name: Brooks, D.
name: Burke, D. L.
name: Capasso, R.
name: Rosell, A. Carnero
name: Kind, M. Carrasco
name: Carretero, J.
name: Chiu, I.
name: Crawford, T. M.
name: Cunha, C. E.
name: D'Andrea, C. B.
name: da Costa, L. N.
name: Desai, S.
name: Dietrich, J. P.
name: Evrard, A. E.
name: Neto, A. Fausti
name: Flaugher, B.
name: Fosalba, P.
name: Frieman, J.
name: Gangkofner, C.
name: Gaztanaga, E.
name: Gerdes, D. W.
name: Giannantonio, T.
name: Grandis, S.
name: Gruen, D.
name: Gruendl, R. A.
name: Gupta, N.
name: Gutierrez, G.
name: Holzapfel, W. L.
name: James, D. J.
name: Kuehn, K.
name: Kuropatkin, N.
name: Lima, M.
name: Marshall, J. L.
name: McDonald, M.
name: Melchior, P.
name: Menanteau, F.
name: Miquel, R.
name: Ogando, R.
name: Plazas, A. A.
name: Rapetti, D.
name: Reichardt, C. L.
name: Reil, K.
name: Romer, A. K.
name: Sanchez, E.
name: Scarpine, V.
name: Schubnell, M.
name: Sevilla-Noarbe, I.
name: Smith, R. C.
name: Soares-Santos, M.
name: Soergel, B.
name: Strazzullo, V.
name: Suchyta, E.
name: Swanson, M. E. C.
name: Tarle, G.
name: Thomas, D.
name: Vikram, V.
name: Walker, A. R.
name: Zenteno, A.
Publisher: name: arXiv
Year: 2016
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: 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 $λ\sim20$. 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 $ζ$-$λ$, relation and two integrated Compton-$y$ $Y_\textrm{500}$-$λ$ relations for the DES-selected clusters and compare these to model expectations accounting for the SZE-optical center offset distribution. For clusters with $λ&gt; 80$, 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 $20 &lt; λ&lt; 80$, the measured SZE signal is smaller by a factor of $\sim$0.20-0.80 (between 2.3 and 10~$σ$ significance) compared to the prediction, with the SPT calibrated scaling relations and larger $λ$ 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 $λ$-mass relation at lower richnesses.