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13 Dec 2019 • Bleem L. E. • Bocquet S. • Stalder B. • Gladders M. D. • Ade P. A. R. • Allen S. W. • Anderson A. J. • Annis J. • Ashby M. L. N. • Austermann J. E. • Avila S. • Avva J. S. • Bayliss M. • Beall J. A. • Bechtol K. • Bender A. N. • Benson B. A. • Bertin E. • Bianchini F. • Blake C. • Brodwin M. • Brooks D. • Buckley-Geer E. • Burke D. L. • Carlstrom J. E. • Rosell A. Carnero • Kind M. Carrasco • Carretero J. • Chang C. L. • Chiang H. C. • Citron R. • Moran C. Corbett • Costanzi M. • Crawford T. M. • Crites A. T. • da Costa L. N. • de Haan T. • De Vicente J. • Desai S. • Diehl H. T. • Dietrich J. P. • Dobbs M. A. • Eifler T. F. • Everett W. • Flaugher B. • Floyd B. • Frieman J. • Gallicchio J. • García-Bellido J. • George E. M. • Gerdes D. W. • Gilbert A. • Gruen D. • Gruendl R. A. • Gschwend J. • Gupta N. • Gutierrez G. • Halverson N. W. • Harrington N. • Henning J. W. • Heymans C. • Holder G. P. • Hollowood D. L. • Holzapfel W. L. • Honscheid K. • Hrubes J. D. • Huang N. • Hubmayr J. • Irwin K. D. • James D. J. • Jeltema T. • Joudaki S. • Khullar G. • Klein M. • Knox L. • Kuropatkin N. • Lee A. T. • Li D. • Lidman C. • Lowitz A. • MacCrann N. • Mahler G. • Maia M. A. G. • Marshall J. L. • McDonald M. • McMahon J. J. • Melchior P. • Menanteau F. • Meyer S. S. • Miquel R. • Mocanu L. M. • Mohr J. J. • Montgomery J. • Nadolski A. • Natoli T. • Nibarger J. P. • Noble G. • Novosad V. • Padin S. • Palmese A. • Parkinson D. • Patil S. • Paz-Chinchón F. • Plazas A. A. • Pryke C. • Ramachandra N. S. • Reichardt C. L. • González J. D. Remolina • Romer A. K. • Roodman A. • Ruhl J. E. • Rykoff E. S. • Saliwanchik B. R. • Sanchez E. • Saro A. • Sayre J. T. • Schaffer K. K. • Schrabback T. • Serrano S. • Sharon K. • Sievers C. • Smecher G. • Smith M. • Soares-Santos M. • Stark A. A. • Story K. T. • Suchyta E. • Tarle G. • Tucker C. • Vanderlinde K. • Veach T. • Vieira J. D. • Wang G. • Weller J. • Whitehorn N. • Wu W. L. K. • Yefremenko V. • Zhang Y.
We describe the observations and resultant galaxy cluster catalog from the 2770 deg$^2$ SPTpol Extended Cluster Survey (SPT-ECS). Clusters are identified via the Sunyaev-Zel'dovich (SZ) effect, and confirmed with a combination of archival and targeted follow-up data, making particular use of data from the Dark Energy Survey (DES)... With incomplete followup we have confirmed as clusters 244 of 266 candidates at a detection significance $\xi \ge 5$ and an additional 204 systems at $4<\xi<5$. The confirmed sample has a median mass of $M_{500c} \sim {4.4 \times 10^{14} M_\odot h_{70}^{-1}}$, a median redshift of $z=0.49$, and we have identified 44 strong gravitational lenses in the sample thus far. Radio data are used to characterize contamination to the SZ signal; the median contamination for confirmed clusters is predicted to be $\sim$1% of the SZ signal at the $\xi>4$ threshold, and $<4\%$ of clusters have a predicted contamination $>10\% $ of their measured SZ flux. We associate SZ-selected clusters, from both SPT-ECS and the SPT-SZ survey, with clusters from the DES redMaPPer sample, and find an offset distribution between the SZ center and central galaxy in general agreement with previous work, though with a larger fraction of clusters with significant offsets. Adopting a fixed Planck-like cosmology, we measure the optical richness-to-SZ-mass ($\lambda-M$) relation and find it to be 28% shallower than that from a weak-lensing analysis of the DES data---a difference significant at the 4 $\sigma$ level---with the relations intersecting at $\lambda=60$ . The SPT-ECS cluster sample will be particularly useful for studying the evolution of massive clusters and, in combination with DES lensing observations and the SPT-SZ cluster sample, will be an important component of future cosmological analyses. (read more)
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