CMB/kSZ and Compton-y Maps from 2500 deg2of SPT-SZ and Planck Survey Data

L. E. Bleem, T. M. Crawford, B. Ansarinejad, B. A. Benson, S. Bocquet, J. E. Carlstrom, C. L. Chang, R. Chown, A. T. Crites, T. De Haan, M. A. Dobbs, W. B. Everett, E. M. George, R. Gualtieri, N. W. Halverson, G. P. Holder, W. L. Holzapfel, J. D. Hrubes, L. Knox, A. T. LeeD. Luong-Van, D. P. Marrone, J. J. McMahon, S. S. Meyer, M. Millea, L. M. Mocanu, J. J. Mohr, T. Natoli, Y. Omori, S. Padin, C. Pryke, S. Raghunathan, C. L. Reichardt, J. E. Ruhl, K. K. Schaffer, E. Shirokoff, Z. Staniszewski, A. A. Stark, J. D. Vieira, R. Williamson

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4 Scopus citations

Abstract

We present component-separated maps of the primary cosmic microwave background/kinematic Sunyaev-Zel'dovich (SZ) amplitude and the thermal SZ Compton-y parameter, created using data from the South Pole Telescope (SPT) and the Planck satellite. These maps, which cover the a1/42500 deg2 of the southern sky imaged by the SPT-SZ survey, represent a significant improvement over previous such products available in this region by virtue of their higher angular resolution ( 1.′25 for our highest-resolution Compton-y maps) and lower noise at small angular scales. In this work we detail the construction of these maps using linear combination techniques, including our method for limiting the correlation of our lowest-noise Compton-y map products with the cosmic infrared background. We perform a range of validation tests on these data products to test our sky modeling and combination algorithms, and we find good performance in all of these tests. Recognizing the potential utility of these data products for a wide range of astrophysical and cosmological analyses, including studies of the gas properties of galaxies, groups, and clusters, we make these products publicly available at http://pole.uchicago.edu/public/data/sptsz_ymap and on the NASA/LAMBDA website.

Original languageEnglish (US)
Article number36
JournalAstrophysical Journal, Supplement Series
Volume258
Issue number2
DOIs
StatePublished - Feb 1 2022

Bibliographical note

Funding Information:
We thank the anonymous referee for the insightful comments on this manuscript. The South Pole Telescope program is supported by the National Science Foundation (NSF) through grants PLR-1248097 and OPP-1852617. Partial support is also provided by the NSF Physics Frontier Center grant PHY- 1125897 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation through grant GBMF#947 to the University of Chicago. Argonne National Laboratory’s work was supported by the US Department of Energy, Office of Science, Office of High Energy Physics, under contract DE-AC02-06CH11357. Work at Fermi National Accelerator Laboratory, a DOE-OS, HEP User Facility managed by the Fermi Research Alliance, LLC, was supported under contract No. DE-AC02-07CH11359. The Melbourne authors acknowledge support from the Australian Research Council’s Discovery Projects scheme (DP200101068). The McGill authors acknowledge funding from the Natural Sciences and Engineering Research Council of Canada, Canadian Institute for Advanced Research, and the Fonds de recherche du Québec Nature et technologies. The CU Boulder group acknowledges support from NSF AST-0956135. The Munich group acknowledges the support by the ORIGINS Cluster (funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy—EXC-2094—390783311), the Max-Planck-Gesellschaft Faculty Fellowship Program, and the Ludwig-Maximilians-Universität München. J.V. acknowledges support from the Sloan Foundation. This research made use of APLpy, an open-source plotting package for Python (Robitaille & Bressert ; Robitaille ).

Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.

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