@article{94be360980df44c499f02d239bd53640,
title = "Cross-correlation of Dark Energy Survey Year 3 lensing data with ACT and Planck thermal Sunyaev-Zel'dovich effect observations. II. Modeling and constraints on halo pressure profiles",
abstract = "Hot, ionized gas leaves an imprint on the cosmic microwave background via the thermal Sunyaev-Zel'dovich (tSZ) effect. The cross-correlation of gravitational lensing (which traces the projected mass) with the tSZ effect (which traces the projected gas pressure) is a powerful probe of the thermal state of ionized baryons throughout the Universe and is sensitive to effects such as baryonic feedback. In a companion paper (Gatti et al. Phys. Rev. D 105, 123525 (2022)PRVDAQ2470-0010), we present tomographic measurements and validation tests of the cross-correlation between Galaxy shear measurements from the first three years of observations of the Dark Energy Survey and tSZ measurements from a combination of Atacama Cosmology Telescope and Planck observations. In this work, we use the same measurements to constrain models for the pressure profiles of halos across a wide range of halo mass and redshift. We find evidence for reduced pressure in low-mass halos, consistent with predictions for the effects of feedback from active Galactic nuclei. We infer the hydrostatic mass bias (BM500c/MSZ) from our measurements, finding B=1.8±0.1 when adopting the Planck-preferred cosmological parameters. We additionally find that our measurements are consistent with a nonzero redshift evolution of B, with the correct sign and sufficient magnitude to explain the mass bias necessary to reconcile cluster count measurements with the Planck-preferred cosmology. Our analysis introduces a model for the impact of intrinsic alignments (IAs) of galaxy shapes on the shear-tSZ correlation. We show that IA can have a significant impact on these correlations at current noise levels.",
author = "{(DES and ACT Collaboration)} and S. Pandey and M. Gatti and E. Baxter and Hill, {J. C.} and X. Fang and C. Doux and G. Giannini and M. Raveri and J. Derose and H. Huang and E. Moser and N. Battaglia and A. Alarcon and A. Amon and M. Becker and A. Campos and C. Chang and R. Chen and A. Choi and K. Eckert and J. Elvin-Poole and S. Everett and A. Ferte and I. Harrison and N. Maccrann and J. McCullough and J. Myles and {Navarro Alsina}, A. and J. Prat and Rollins, {R. P.} and C. Sanchez and T. Shin and M. Troxel and I. Tutusaus and B. Yin and M. Aguena and S. Allam and F. Andrade-Oliveira and Bernstein, {G. M.} and E. Bertin and B. Bolliet and Bond, {J. R.} and D. Brooks and E. Calabrese and {Carnero Rosell}, A. and {Carrasco Kind}, M. and J. Dunkley and P. Melchior and L. Page and D. Spergel",
note = "Funding Information: This paper has gone through internal review by the DES and ACT Collaborations. S. P. is supported in part by the U.S. Department of Energy Award No. DE-SC0007901 and NASA ATP Grant No. NNH17ZDA001N. E. S. is supported by DOE Award No. DE-AC02-98CH10886. K. M. acknowledges support from the National Research Foundation of South Africa. Z. X. is supported by the Gordon and Betty Moore Foundation. J. P. H. acknowledges funding for SZ cluster studies from NSF AAG No. AST-1615657. A. D. H. acknowledges support from the Sutton Family Chair in Science, Christianity, and Cultures. C. S. acknowledges support from the Agencia Nacional de Investigaci{\'o}n y Desarrollo (ANID) under FONDECYT Grant No. 11191125. Funding for the DES Projects has been provided by the U.S. Department of Energy, U.S. National Science Foundation, Ministry of Science and Education of Spain, Science and Technology Facilities Council of the United Kingdom, Higher Education Funding Council for England, National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, Kavli Institute of Cosmological Physics at the University of Chicago, Center for Cosmology and Astro-Particle Physics at The Ohio State University, Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Funda{\c c}{\~a}o Carlos Chagas Filho de Amparo {\`a} Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cient{\'i}fico e Tecnol{\'o}gic and the Minist{\'e}rio da Ci{\^e}ncia, Tecnologia e Inova{\c c}{\~a}o, Deutsche Forschungsgemeinschaft, and the collaborating institutions in the Dark Energy Survey. The collaborating institutions are Argonne National Laboratory, University of California at Santa Cruz, University of Cambridge, Centro de Investigaciones Energ{\'e}ticas, Medioambientales y Tecnol{\'o}gicas-Madrid, University of Chicago, University College London, the DES-Brazil Consortium, University of Edinburgh, Eidgen{\"o}ssische Technische Hochschule (ETH) Z{\"u}rich, Fermi National Accelerator Laboratory, University of Illinois at Urbana-Champaign, Institut de Ci{\`e}ncies de l{\textquoteright}Espai (IEEC/CSIC), Institut de F{\'i}sica d{\textquoteright}Altes Energies, Lawrence Berkeley National Laboratory, Ludwig-Maximilians Universit{\"a}t M{\"u}nchen and the associated Excellence Cluster Universe, University of Michigan, National Optical Astronomy Observatory, University of Nottingham, The Ohio State University, University of Pennsylvania, University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF{\textquoteright}s NOIRLab (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 Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under Grants No. AYA2015-71825, No. ESP2015-66861, No. FPA2015-68048, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union{\textquoteright}s Seventh Framework Program (FP7/2007-2013) including ERC Grant Agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ci{\^e}ncia e Tecnologia (INCT) e-Universe (CNPq Grant No. 465376/2014-2). This manuscript has been coauthored by employees 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. Support for ACT was through the U.S. National Science Foundation through Grants No. AST-0408698, No. AST-0965625, and No. AST-1440226 for the ACT project, as well as Grants No. PHY-0355328, No. PHY-0855887, and No. PHY-1214379. Funding was also provided by Princeton University, the University of Pennsylvania, and a Canada Foundation for Innovation (CFI) award to UBC. ACT operates in the Parque Astron{\textquoteright}omico Atacama in northern Chile under the auspices of the Agencia Nacional de Investigaci{\textquoteright}on y Desarrollo (ANID). The development of multichroic detectors and lenses was supported by NASA Grants No. NNX13AE56G and No. NNX14AB58G. Detector research at N. I. S. T. was supported by the NIST Innovations in Measurement Science program. Publisher Copyright: {\textcopyright} 2022 American Physical Society.",
year = "2022",
month = jun,
day = "15",
doi = "10.1103/PhysRevD.105.123526",
language = "English (US)",
volume = "105",
journal = "Physical Review D",
issn = "2470-0010",
publisher = "American Physical Society",
number = "12",
}