The SPTpol Extended Cluster Survey

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.

ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES（2020）

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摘要

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 follow-up we have confirmed as clusters 244 of 266 candidates at a detection significance xi >= 5 and an additional 204 systems at 4 xi 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 similar to 1% of the SZ signal at the xi > 4 threshold, and 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 we 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-SZ mass ( 更多

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