A High-resolution SZ View of the Warm-Hot Universe. (arXiv:1903.02595v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Mroczkowski_T/0/1/0/all/0/1">Tony Mroczkowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nagai_D/0/1/0/all/0/1">Daisuke Nagai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andreani_P/0/1/0/all/0/1">Paola Andreani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arnaud_M/0/1/0/all/0/1">Monique Arnaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bartlett_J/0/1/0/all/0/1">James Bartlett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Battaglia_N/0/1/0/all/0/1">Nicholas Battaglia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Basu_K/0/1/0/all/0/1">Kaustuv Basu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bulbul_E/0/1/0/all/0/1">Esra Bulbul</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chluba_J/0/1/0/all/0/1">Jens Chluba</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Churazov_E/0/1/0/all/0/1">Eugene Churazov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cicone_C/0/1/0/all/0/1">Claudia Cicone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crites_A/0/1/0/all/0/1">Abigail Crites</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DeNigris_N/0/1/0/all/0/1">Nat DeNigris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Devlin_M/0/1/0/all/0/1">Mark Devlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mascolo_L/0/1/0/all/0/1">Luca Di Mascolo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dicker_S/0/1/0/all/0/1">Simon Dicker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaspari_M/0/1/0/all/0/1">Massimo Gaspari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Golwala_S/0/1/0/all/0/1">Sunil Golwala</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guglielmetti_F/0/1/0/all/0/1">Fabrizia Guglielmetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hill_J/0/1/0/all/0/1">J. Colin Hill</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klaassen_P/0/1/0/all/0/1">Pamela Klaassen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kitayama_T/0/1/0/all/0/1">Tetsu Kitayama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kneissl_R/0/1/0/all/0/1">R&#xfc;diger Kneissl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kohno_K/0/1/0/all/0/1">Kotaro Kohno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Komatsu_E/0/1/0/all/0/1">Eiichiro Komatsu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lacy_M/0/1/0/all/0/1">Mark Lacy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mason_B/0/1/0/all/0/1">Brian Mason</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nyland_K/0/1/0/all/0/1">Kristina Nyland</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Romero_C/0/1/0/all/0/1">Charles Romero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sayers_J/0/1/0/all/0/1">Jack Sayers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sehgal_N/0/1/0/all/0/1">Neelima Sehgal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Simon_S/0/1/0/all/0/1">Sara Simon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sunyaev_R/0/1/0/all/0/1">Rashid Sunyaev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilson_G/0/1/0/all/0/1">Grant Wilson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zemcov_M/0/1/0/all/0/1">Michael Zemcov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+ZuHone_J/0/1/0/all/0/1">John ZuHone</a>

The Sunyaev-Zeldovich (SZ) effect was first predicted nearly five decades
ago, but has only recently become a mature tool for performing high resolution
studies of the warm and hot ionized gas in and between galaxies, groups, and
clusters. Galaxy groups and clusters are powerful probes of cosmology, and they
also serve as hosts for roughly half of the galaxies in the Universe. In this
white paper, we outline the advances in our understanding of thermodynamic and
kinematic properties of the warm-hot universe that can come in the next decade
through spatially and spectrally resolved measurements of the SZ effects. Many
of these advances will be enabled through new/upcoming millimeter/submillimeter
(mm/submm) instrumentation on existing facilities, but truly transformative
advances will require construction of new facilities with larger fields of view
and broad spectral coverage of the mm/submm bands.

The Sunyaev-Zeldovich (SZ) effect was first predicted nearly five decades
ago, but has only recently become a mature tool for performing high resolution
studies of the warm and hot ionized gas in and between galaxies, groups, and
clusters. Galaxy groups and clusters are powerful probes of cosmology, and they
also serve as hosts for roughly half of the galaxies in the Universe. In this
white paper, we outline the advances in our understanding of thermodynamic and
kinematic properties of the warm-hot universe that can come in the next decade
through spatially and spectrally resolved measurements of the SZ effects. Many
of these advances will be enabled through new/upcoming millimeter/submillimeter
(mm/submm) instrumentation on existing facilities, but truly transformative
advances will require construction of new facilities with larger fields of view
and broad spectral coverage of the mm/submm bands.

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