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Support for ACT was provided through the U.S. National Science Foundation through awards AST-0408698, AST-0965625, and AST-1440226 for the ACT project, as well as awards PHY-0355328, PHY-0855887, and PHY-1214379.Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation (CFI) award to UBC. ACT operated in the Parque Astronomico Atacama in northern Chile under the auspices of the Agencia Nacional de Investigacion y Desarrollo (ANID). The development of multichroic detectors and lenses was supported by NASA grant Nos. NNX13AE56G and NNX14AB58G. Detector research at NIST was supported by the NIST Innovations in Measurement Science program. Computing for ACT was performed using the Princeton Research Computing resources at Princeton University, the National Energy Research Scientific Computing Center (NERSC), and the Niagara supercomputer at the SciNet HPC Consortium. SciNet is funded by the CFI under the auspices of Compute Canada, the Government of Ontario, the Ontario Research Fund-Research Excellence, and the University of Toronto. We thank the Republic of Chile for hosting ACT in the northern Atacama, and the local indigenous Licanantay communities, whom we follow in observing and learning from the night sky. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmo-logical Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundacao Carlos Chagas Filho de Amparoa Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerioda Ciencia, Tecnologia e Inovacao, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the DES. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai (IEEC/CSIC),the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster Universe, the University of Michigan, NSF NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at NSF CTIO at NSFNOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grantsPID2021-123012, PID2021-128989 PID2022-141079, SEV-2016-0588, CEX2020-001058-M, and CEX2020-001007-S, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. We acknowledge support from the Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) do e-Universo (CNPq grant No. 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. Canadian coauthors acknowledge support from the Natural Sciences and Engineering Research Council of Canada. Websky computations were performed on the SciNet super-computer at the SciNet HPC Consortium. SciNet is funded by the Canada Foundation for Innovation; the Government of Ontario; Ontario Research Fund-Research Excellence; and the University of Toronto. IFAE is partially funded by the CERCA program of theGeneralitat de Catalunya. R.H. acknowledges support from CIFAR, the Azrieli and Alfred. P. Sloan foundations. GAM is part of Fermi Research Alliance, LLC under contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. E.C. acknowledges support from the European Research Council (ERC) under the European Union's Horizon 2020research and innovation program(grant agreement No. 849169).C.H.T. received support from the United States Department of Energy, Office of High Energy Physics under award No.DE-SC-0011726.The Flatiron Institute is supported by the Simons Foundation. C.S. acknowledges support from the Agencia Nacional de Investigacion y Desarrollo (ANID) through Basal project FB210003.This work received support from the U.S. Department of Energy under contract No. DE-AC02-76SF00515 at SLAC National Accelerator Laboratory. This research used computing resources at SLAC National Accelerator Laboratory and at the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility located at Lawrence Berkeley National Laboratory, operated under contract No. DE-AC02-05CH11231.

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Superclustering with the Atacama Cosmology Telescope and Dark Energy Survey. II. Anisotropic Large-scale Coherence in Hot Gas, Galaxies, and Dark Matter

Publicated to:ASTROPHYSICAL JOURNAL 982 (2): 186- - 2025-04-01 982(2), DOI: 10.3847/1538-4357/adb622

Authors: Lokken, M; van Engelen, A; Aguena, M; Allam, S S; Anbajagane, D; Bacon, D; Baxter, E; Blazek, J; Bocquet, S; Bond, J R; Brooks, D; Calabrese, E; Rosell, A Carnero; Carretero, J; Costanzi, M; da Costa, L N; Coulton, W R; De Vicente, J; Desai, S; Doel, P; Doux, C; Duivenvoorden, A J; Dunkley, J; Huang, Z; Everett, S; Ferrero, I; Frieman, J; Garcia-Bellido, J; Gatti, M; Gaztanaga, E; Giannini, G; Gluscevic, Vera; Gruen, D; Gruendl, R A; Guan, Y; Gutierrez, G; Hinton, S R; Hlozek, R; Hollowood, D L; Honscheid, K; James, D J; Kuehn, K; Lahav, O; Lee, S; Li, Z; Madhavacheril, M; Marques, G A; Marshall, J L; Mena-Fernandez, J; Menanteau, F; Miquel, R; Myles, J; Niemack, M D; Pandey, S; Pereira, M E S; Pieres, A; Malagon, A A Plazas; Porredon, A; Rodriguez-Monroy, M; Roodman, A; Samuroff, S; Sanchez, E; Cid, D Sanchez; Santiago, B; Schubnell, M; Sevilla-Noarbe, I; Sifon, C; Smith, M; Staggs, S T; Suchyta, E; Swanson, M E C; Tarle, G; To, C-H; Weaverdyck, N; Wiseman, P; Wollack, E J

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Abstract

Statistics that capture the directional dependence of the baryon distribution in the cosmic web enable unique tests of cosmology and astrophysical feedback. We use constrained oriented stacking of thermal Sunyaev-Zel'dovich (tSZ) maps to measure the anisotropic distribution of hot gas 2.5-40 Mpc away from galaxy clusters embedded in massive filaments and superclusters. The cluster selection and orientation (at a scale of similar to 15 Mpc) use Dark Energy Survey (DES) Year 3 data, while expanded tSZ maps from the Atacama Cosmology Telescope Data Release 6 enable a similar to 3x more significant measurement of the extended gas compared to the technique's proof-of-concept. Decomposing stacks into cosine multipoles of order m, we detect a dipole (m = 1) and quadrupole (m = 2) at 8 sigma-10 sigma, as well as evidence for m = 4 signal at up to 6 sigma, indicating sensitivity to late-time non-Gaussianity. We compare to Cardinal simulations with spherical gas models pasted onto dark matter halos. The fiducial tSZ data can discriminate between two models that deplete pressure differently in low-mass halos (mimicking astrophysical feedback), preferring higher average pressure in extended structures. However, uncertainty in the amount of cosmic infrared background contamination reduces the constraining power. Additionally, we apply the technique to DES galaxy density and weak lensing to study for the first time their oriented relationships with tSZ. In the tSZ-to-lensing relation, averaged on 7.5 Mpc (transverse) scales, we observe dependence on redshift but not shape or radial distance. Thus, on large scales, the superclustering of gas pressure, galaxies, and total matter is coherent in shape and extent.

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