The Atacama Cosmology Telescope: A Catalog of > 4000 Sunyaev-Zel’dovich Galaxy Clusters. (arXiv:2009.11043v2 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Hilton_M/0/1/0/all/0/1">M. Hilton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sifon_C/0/1/0/all/0/1">C. Sif&#xf3;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Naess_S/0/1/0/all/0/1">S. Naess</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Madhavacheril_M/0/1/0/all/0/1">M. Madhavacheril</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oguri_M/0/1/0/all/0/1">M. Oguri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rozo_E/0/1/0/all/0/1">E. Rozo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rykoff_E/0/1/0/all/0/1">E. Rykoff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abbott_T/0/1/0/all/0/1">T. M. C. Abbott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adhikari_S/0/1/0/all/0/1">S. Adhikari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aguena_M/0/1/0/all/0/1">M. Aguena</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aiola_S/0/1/0/all/0/1">S. Aiola</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allam_S/0/1/0/all/0/1">S. Allam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amodeo_S/0/1/0/all/0/1">S. Amodeo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amon_A/0/1/0/all/0/1">A. Amon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Annis_J/0/1/0/all/0/1">J. Annis</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:+Aros_Bunster_C/0/1/0/all/0/1">C. Aros-Bunster</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Austermann_J/0/1/0/all/0/1">J. E. Austermann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avila_S/0/1/0/all/0/1">S. Avila</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bacon_D/0/1/0/all/0/1">D. Bacon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Battaglia_N/0/1/0/all/0/1">N. Battaglia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beall_J/0/1/0/all/0/1">J. A. Beall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Becker_D/0/1/0/all/0/1">D. T. Becker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernstein_G/0/1/0/all/0/1">G. M. Bernstein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertin_E/0/1/0/all/0/1">E. Bertin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhandarkar_T/0/1/0/all/0/1">T. Bhandarkar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhargava_S/0/1/0/all/0/1">S. Bhargava</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bond_J/0/1/0/all/0/1">J. R. Bond</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brooks_D/0/1/0/all/0/1">D. Brooks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burke_D/0/1/0/all/0/1">D. L. Burke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calabrese_E/0/1/0/all/0/1">E. Calabrese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carretero_J/0/1/0/all/0/1">J. Carretero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choi_S/0/1/0/all/0/1">S. K. Choi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choi_A/0/1/0/all/0/1">A. Choi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Conselice_C/0/1/0/all/0/1">C. Conselice</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Costa_L/0/1/0/all/0/1">L. N. da Costa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Costanzi_M/0/1/0/all/0/1">M. Costanzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crichton_D/0/1/0/all/0/1">D. Crichton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crowley_K/0/1/0/all/0/1">K. T. Crowley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunner_R/0/1/0/all/0/1">R. D&#xfc;nner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Denison_E/0/1/0/all/0/1">E. V. Denison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Devlin_M/0/1/0/all/0/1">M. J. Devlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dicker_S/0/1/0/all/0/1">S. R. Dicker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diehl_H/0/1/0/all/0/1">H. T. Diehl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dietrich_J/0/1/0/all/0/1">J. P. Dietrich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doel_P/0/1/0/all/0/1">P. Doel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duff_S/0/1/0/all/0/1">S. M. Duff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duivenvoorden_A/0/1/0/all/0/1">A. J. Duivenvoorden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunkley_J/0/1/0/all/0/1">J. Dunkley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Everett_S/0/1/0/all/0/1">S. Everett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferraro_S/0/1/0/all/0/1">S. Ferraro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferrero_I/0/1/0/all/0/1">I. Ferrero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferte_A/0/1/0/all/0/1">A. Fert&#xe9;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Flaugher_B/0/1/0/all/0/1">B. Flaugher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frieman_J/0/1/0/all/0/1">J. Frieman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gallardo_P/0/1/0/all/0/1">P. A. Gallardo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_Bellido_J/0/1/0/all/0/1">J. Garc&#xed;a-Bellido</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaztanaga_E/0/1/0/all/0/1">E. Gaztanaga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gerdes_D/0/1/0/all/0/1">D. W. Gerdes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Giles_P/0/1/0/all/0/1">P. Giles</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Golec_J/0/1/0/all/0/1">J. E. Golec</a>, et al. (88 additional authors not shown)

We present a catalog of 4195 optically confirmed Sunyaev-Zel’dovich (SZ)
selected galaxy clusters detected with signal-to-noise > 4 in 13,211 deg$^2$ of
sky surveyed by the Atacama Cosmology Telescope (ACT). Cluster candidates were
selected by applying a multi-frequency matched filter to 98 and 150 GHz maps
constructed from ACT observations obtained from 2008-2018, and confirmed using
deep, wide-area optical surveys. The clusters span the redshift range 0.04 < z
< 1.91 (median z = 0.52). The catalog contains 222 z > 1 clusters, and a total
of 868 systems are new discoveries. Assuming an SZ-signal vs. mass scaling
relation calibrated from X-ray observations, the sample has a 90% completeness
mass limit of M500c > 3.8 x 10$^{14}$ MSun, evaluated at z = 0.5, for clusters
detected at signal-to-noise ratio > 5 in maps filtered at an angular scale of
2.4′. The survey has a large overlap with deep optical weak-lensing surveys
that are being used to calibrate the SZ-signal mass-scaling relation, such as
the Dark Energy Survey (4566 deg$^2$), the Hyper Suprime-Cam Subaru Strategic
Program (469 deg$^2$), and the Kilo Degree Survey (825 deg$^2$). We highlight
some noteworthy objects in the sample, including potentially projected systems;
clusters with strong lensing features; clusters with active central galaxies or
star formation; and systems of multiple clusters that may be physically
associated. The cluster catalog will be a useful resource for future
cosmological analyses, and studying the evolution of the intracluster medium
and galaxies in massive clusters over the past 10 Gyr.

We present a catalog of 4195 optically confirmed Sunyaev-Zel’dovich (SZ)
selected galaxy clusters detected with signal-to-noise > 4 in 13,211 deg$^2$ of
sky surveyed by the Atacama Cosmology Telescope (ACT). Cluster candidates were
selected by applying a multi-frequency matched filter to 98 and 150 GHz maps
constructed from ACT observations obtained from 2008-2018, and confirmed using
deep, wide-area optical surveys. The clusters span the redshift range 0.04 < z
< 1.91 (median z = 0.52). The catalog contains 222 z > 1 clusters, and a total
of 868 systems are new discoveries. Assuming an SZ-signal vs. mass scaling
relation calibrated from X-ray observations, the sample has a 90% completeness
mass limit of M500c > 3.8 x 10$^{14}$ MSun, evaluated at z = 0.5, for clusters
detected at signal-to-noise ratio > 5 in maps filtered at an angular scale of
2.4′. The survey has a large overlap with deep optical weak-lensing surveys
that are being used to calibrate the SZ-signal mass-scaling relation, such as
the Dark Energy Survey (4566 deg$^2$), the Hyper Suprime-Cam Subaru Strategic
Program (469 deg$^2$), and the Kilo Degree Survey (825 deg$^2$). We highlight
some noteworthy objects in the sample, including potentially projected systems;
clusters with strong lensing features; clusters with active central galaxies or
star formation; and systems of multiple clusters that may be physically
associated. The cluster catalog will be a useful resource for future
cosmological analyses, and studying the evolution of the intracluster medium
and galaxies in massive clusters over the past 10 Gyr.

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