CMB/kSZ and Compton-$y$ Maps from 2500 square degrees of SPT-SZ and Planck Survey Data. (arXiv:2102.05033v2 [astro-ph.CO] UPDATED)

CMB/kSZ and Compton-$y$ Maps from 2500 square degrees of SPT-SZ and Planck Survey Data. (arXiv:2102.05033v2 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Bleem_L/0/1/0/all/0/1">L. E. Bleem</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crawford_T/0/1/0/all/0/1">T. M. Crawford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ansarinejad_B/0/1/0/all/0/1">B. Ansarinejad</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benson_B/0/1/0/all/0/1">B. A. Benson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bocquet_S/0/1/0/all/0/1">S. Bocquet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carlstrom_J/0/1/0/all/0/1">J. E. Carlstrom</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chang_C/0/1/0/all/0/1">C. L. Chang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chown_R/0/1/0/all/0/1">R. Chown</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crites_A/0/1/0/all/0/1">A. T. Crites</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haan_T/0/1/0/all/0/1">T. de Haan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dobbs_M/0/1/0/all/0/1">M. A. Dobbs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Everett_W/0/1/0/all/0/1">W. B. Everett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+George_E/0/1/0/all/0/1">E. M. George</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gualtieri_R/0/1/0/all/0/1">R. Gualtieri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Halverson_N/0/1/0/all/0/1">N. W. Halverson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holder_G/0/1/0/all/0/1">G. P. Holder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holzapfel_W/0/1/0/all/0/1">W. L. Holzapfel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hrubes_J/0/1/0/all/0/1">J. D. Hrubes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Knox_L/0/1/0/all/0/1">L. Knox</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_A/0/1/0/all/0/1">A. T. Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Luong_Van_D/0/1/0/all/0/1">D. Luong-Van</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marrone_D/0/1/0/all/0/1">D. P. Marrone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McMahon_J/0/1/0/all/0/1">J. J. McMahon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meyer_S/0/1/0/all/0/1">S. S. Meyer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Millea_M/0/1/0/all/0/1">M. Millea</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mocanu_L/0/1/0/all/0/1">L. M. Mocanu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mohr_J/0/1/0/all/0/1">J. J. Mohr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Natoli_T/0/1/0/all/0/1">T. Natoli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Omori_Y/0/1/0/all/0/1">Y. Omori</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Padin_S/0/1/0/all/0/1">S. Padin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pryke_C/0/1/0/all/0/1">C. Pryke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Raghunathan_S/0/1/0/all/0/1">S. Raghunathan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reichardt_C/0/1/0/all/0/1">C. L. Reichardt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruhl_J/0/1/0/all/0/1">J. E. Ruhl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schaffer_K/0/1/0/all/0/1">K. K. Schaffer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shirokoff_E/0/1/0/all/0/1">E. Shirokoff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Staniszewski_Z/0/1/0/all/0/1">Z. Staniszewski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stark_A/0/1/0/all/0/1">A. A. Stark</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vieira_J/0/1/0/all/0/1">J. D. Vieira</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Williamson_R/0/1/0/all/0/1">R. Williamson</a>

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 $sim$2500 square degrees
of the Southern sky imaged by the SPT-SZ survey, represent a significant
improvement over previous such products available in this region by virtue of
their higher angular resolution (1.25 arcminutes for our highest resolution
Compton-$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 this http URL and on the
NASA/LAMBDA website.

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