Weak lensing combined with the kinetic Sunyaev–Zel’dovich effect: a study of baryonic feedback

L. Bigwood; A. Amon; A. Schneider; J. Salcido; I. G. McCarthy; C. Preston; D. Sanchez; D. Sijacki; E. Schaan; S. Ferraro; N. Battaglia; A. Chen; S. Dodelson; A. Roodman; A. Pieres; A. Ferté; A. Alarcon; A. Drlica-Wagner; A. Choi; A. Navarro-Alsina; A. Campos; A. J. Ross; A. Carnero Rosell; B. Yin; B. Yanny; C. Sánchez; C. Chang; C. Davis; C. Doux; D. Gruen; E. S. Rykoff; E. M. Huff; E. Sheldon; F. Tarsitano; F. Andrade-Oliveira; G. M. Bernstein; G. Giannini; H. T. Diehl; H. Huang; I. Harrison; I. Sevilla-Noarbe; I. Tutusaus; J. Elvin-Poole; J. McCullough; J. Zuntz; J. Blazek; J. DeRose; J. Cordero; J. Prat; J. Myles; K. Eckert; K. Bechtol; K. Herner; L. F. Secco; M. Gatti; M. Raveri; M. Carrasco Kind; M. R. Becker; M. A. Troxel; M. Jarvis; N. MacCrann; O. Friedrich; O. Alves; P. F. Leget; R. Chen; R. P. Rollins; R. H. Wechsler; R. A. Gruendl; R. Cawthon; S. Allam; S. L. Bridle; S. Pandey; S. Everett; T. Shin; W. G. Hartley; X. Fang; Y. Zhang; M. Aguena; J. Annis; D. Bacon; E. Bertin; S. Bocquet; D. Brooks; J. Carretero; F. J. Castander; L. N. da Costa; M. E.S. Pereira; J. De Vicente; S. Desai; P. Doel; I. Ferrero; B. Flaugher; J. Frieman; J. García-Bellido; E. Gaztanaga; G. Gutierrez; S. R. Hinton; D. L. Hollowood; K. Honscheid; D. Huterer; D. J. James; K. Kuehn; O. Lahav; S. Lee; J. L. Marshall; J. Mena-Fernández; R. Miquel; J. Muir; M. Paterno; A. A.Plazas Malagón; A. Porredon; A. K. Romer; S. Samuroff; E. Sanchez; D. Sanchez Cid; M. Smith; M. Soares-Santos; E. Suchyta; M. E.C. Swanson; G. Tarle; C. To; N. Weaverdyck; J. Weller; P. Wiseman; M. Yamamoto

doi:10.1093/mnras/stae2100

Weak lensing combined with the kinetic Sunyaev–Zel’dovich effect: a study of baryonic feedback

L. Bigwood, A. Amon, A. Schneider, J. Salcido, I. G. McCarthy, C. Preston, D. Sanchez, D. Sijacki, E. Schaan, S. Ferraro, N. Battaglia, A. Chen, S. Dodelson, A. Roodman, A. Pieres, A. Ferté, A. Alarcon, A. Drlica-Wagner, A. Choi, A. Navarro-AlsinaA. Campos, A. J. Ross, A. Carnero Rosell, B. Yin, B. Yanny, C. Sánchez, C. Chang, C. Davis, C. Doux, D. Gruen, E. S. Rykoff, E. M. Huff, E. Sheldon, F. Tarsitano, F. Andrade-Oliveira, G. M. Bernstein, G. Giannini, H. T. Diehl, H. Huang, I. Harrison, I. Sevilla-Noarbe, I. Tutusaus, J. Elvin-Poole, J. McCullough, J. Zuntz, J. Blazek, J. DeRose, J. Cordero, J. Prat, J. Myles, K. Eckert, K. Bechtol, K. Herner, L. F. Secco, M. Gatti, M. Raveri, M. Carrasco Kind, M. R. Becker, M. A. Troxel, M. Jarvis, N. MacCrann, O. Friedrich, O. Alves, P. F. Leget, R. Chen, R. P. Rollins, R. H. Wechsler, R. A. Gruendl, R. Cawthon, S. Allam, S. L. Bridle, S. Pandey, S. Everett, T. Shin, W. G. Hartley, X. Fang, Y. Zhang, M. Aguena, J. Annis, D. Bacon, E. Bertin, S. Bocquet, D. Brooks, J. Carretero, F. J. Castander, L. N. da Costa, M. E.S. Pereira, J. De Vicente, S. Desai, P. Doel, I. Ferrero, B. Flaugher, J. Frieman, J. García-Bellido, E. Gaztanaga, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. Huterer, D. J. James, K. Kuehn, O. Lahav, S. Lee, J. L. Marshall, J. Mena-Fernández, R. Miquel, J. Muir, M. Paterno, A. A.Plazas Malagón, A. Porredon, A. K. Romer, S. Samuroff, E. Sanchez, D. Sanchez Cid, M. Smith, M. Soares-Santos, E. Suchyta, M. E.C. Swanson, G. Tarle, C. To, N. Weaverdyck, J. Weller, P. Wiseman, M. Yamamoto

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Abstract

Extracting precise cosmology from weak lensing surveys requires modelling the non-linear matter power spectrum, which is suppressed at small scales due to baryonic feedback processes. However, hydrodynamical galaxy formation simulations make widely varying predictions for the amplitude and extent of this effect. We use measurements of Dark Energy Survey Year 3 weak lensing (WL) and Atacama Cosmology Telescope DR5 kinematic Sunyaev–Zel’dovich (kSZ) to jointly constrain cosmological and astrophysical baryonic feedback parameters using a flexible analytical model, ‘baryonification’. First, using WL only, we compare the S₈ constraints using baryonification to a simulation-calibrated halo model, a simulation-based emulator model, and the approach of discarding WL measurements on small angular scales. We find that model flexibility can shift the value of S₈ and degrade the uncertainty. The kSZ provides additional constraints on the astrophysical parameters, with the joint WL + kSZ analysis constraining S₈ = 0.823⁺₋₀⁰₀₂₀⁰¹⁹. We measure the suppression of the non-linear matter power spectrum using WL + kSZ and constrain a mean feedback scenario that is more extreme than the predictions from most hydrodynamical simulations. We constrain the baryon fractions and the gas mass fractions and find them to be generally lower than inferred from X-ray observations and simulation predictions. We conclude that the WL + kSZ measurements provide a new and complementary benchmark for building a coherent picture of the impact of gas around galaxies across observations.

Original language	English
Pages (from-to)	655-682
Number of pages	28
Journal	Monthly Notices of the Royal Astronomical Society
Volume	534
Issue number	1
DOIs	https://doi.org/10.1093/mnras/stae2100
State	Published - Oct 1 2024

Funding

This project has used public archival data from the DES. 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 Cosmological 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, Funda\u00E7\u00E3o Carlos Chagas Filho de Amparo \u00E0 Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cient\u00EDfico e Tecnol\u00F3gico and the Minist\u00E9rio da Ci\u00EAncia, Tecnologia e Inova\u00E7\u00E3o, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. LB is supported by a Science and Technology Facilities Council studentship. AA was supported by a Kavli Fellowship for part of the duration of this work. JS and IGM were supported by an European Research Council (ERC) Consolidator Grant under the European Union\u2019s Horizon 2020 research and innovation programme (grant agreement no. 769130). The author\u2019s contributions are as follows. LB and AA performed the analysis and wrote the bulk of the manuscript. The additional core authors of AA, JS, and IGM contributed BCEmu and SP(k) code and continuous insight. CP and DS assisted in the early stages, including the mock analysis. DSi provided useful discussions and detailed comments on the manuscript. ES, SF, and NB provided the ACT kSZ data set. The paper has gone through internal review by the DES collaboration, with A. Chen and S. Dodelson serving as excellent internal reviewers. The remaining authors have made contributions to the DES instrumentation, data collection, data processing, and calibration, in addition to other code and validation tests. This project has used public archival data from the DES. 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 Cosmological 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, Funda\u00E7\u00E3o Carlos Chagas Filho de Amparo \u00E0 Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cient\u00EDfico e Tecnol\u00F3gico and the Minist\u00E9rio da Ci\u00EAncia, Tecnologia e Inova\u00E7\u00E3o, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energ\u00E9ticas, Medioambientales y Tecnol\u00F3gicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgen\u00F6ssische Technische Hochschule (ETH) Z\u00FCrich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ci\u00E8ncies de l\u2019Espai (IEEC/CSIC), the Institut de F\u00EDsica d\u2019Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universit\u00E4t M\u00FCnchen 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 Cerro Tololo Inter-American Observatory at NSF 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 grant nos AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE 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\u2019s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ci\u00EAncia e Tecnologia (INCT) do e-Universo (CNPq grant 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. 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 grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE 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\u2019s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ci\u00EAncia e Tecnologia (INCT) do e-Universo (CNPq grant 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. LB is supported by a Science and Technology Facilities Council studentship. AA was supported by a Kavli Fellowship for part of the duration of this work. JS and IGM were supported by an European Research Council (ERC) Consolidator Grant under the European Union\u2019s Horizon 2020 research and innovation programme (grant agreement no. 769130). Based in part on observations at NSF Cerro Tololo Inter-American Observatory at NSF 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.

Funders	Funder number
Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University
University of Illinois at Urbana-Champaign
Institut de Ciències de l’Espai
Brazilian Instituto Nacional de Ciência e Tecnologia
University of Nottingham
University of Sussex
High Energy Physics
Science and Technology Facilities Council
University of Edinburgh
Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro
Seventh Framework Programme
Ohio State University
Stanford University
University of Chicago
Generalitat de Catalunya
Higher Education Funding Council for England
Financiadora de Estudos e Projetos
Ministry of Education and Science of Ukraine
Eidgenössische Technische Hochschule Zürich
University of California, Santa Cruz
Deutsche Forschungsgemeinschaft
Neurosciences Foundation
European Commission
Instituto Nacional de Ciência e Tecnologia para Excitotoxicidade e Neuroproteção
SLAC National Accelerator Laboratory
U.S. Department of Energy
Lawrence Berkeley National Laboratory
Fermilab
Collaborating Institutions are Argonne National Laboratory
University College London
University of Portsmouth
Science and Technology Facilities Council of the United Kingdom
Ministério da Ciência, Tecnologia e Inovação
Office of Science
National Centre for Supercomputing Applications
European Regional Development Fund
University of Michigan
Institut de Física d'Altes Energies
University of Pennsylvania
Collaborating Institutions in the Dark Energy Survey
Ludwig-Maximilians-Universität München
European Research Council	240672, 306478, 291329
European Research Council
Texas A and M University	2012B-0001
Texas A and M University
National Science Foundation	AST-1138766, AST-1536171
National Science Foundation
Horizon 2020 Framework Programme	769130
Horizon 2020 Framework Programme
Conselho Nacional de Desenvolvimento Científico e Tecnológico	465376/2014-2
Conselho Nacional de Desenvolvimento Científico e Tecnológico
Ministerio de Ciencia e Innovación	SEV-2016-0588, SEV-2016-0597, MDM-2015-0509, PGC2018-094773, PGC2018-102021, ESP2017-89838
Ministerio de Ciencia e Innovación
Fermi Research Alliance, LLC	DE-AC02-07CH11359

Keywords

cosmology: observations
gravitational lensing: weak
large-scale structure of Universe

Access to Document

10.1093/mnras/stae2100

Cite this

Bigwood, L., Amon, A., Schneider, A., Salcido, J., McCarthy, I. G., Preston, C., Sanchez, D., Sijacki, D., Schaan, E., Ferraro, S., Battaglia, N., Chen, A., Dodelson, S., Roodman, A., Pieres, A., Ferté, A., Alarcon, A., Drlica-Wagner, A., Choi, A., ... Yamamoto, M. (2024). Weak lensing combined with the kinetic Sunyaev–Zel’dovich effect: a study of baryonic feedback. Monthly Notices of the Royal Astronomical Society, 534(1), 655-682. https://doi.org/10.1093/mnras/stae2100

@article{cfe11b751186448bb48c90c1191ce292,

title = "Weak lensing combined with the kinetic Sunyaev–Zel{\textquoteright}dovich effect: a study of baryonic feedback",

abstract = "Extracting precise cosmology from weak lensing surveys requires modelling the non-linear matter power spectrum, which is suppressed at small scales due to baryonic feedback processes. However, hydrodynamical galaxy formation simulations make widely varying predictions for the amplitude and extent of this effect. We use measurements of Dark Energy Survey Year 3 weak lensing (WL) and Atacama Cosmology Telescope DR5 kinematic Sunyaev–Zel{\textquoteright}dovich (kSZ) to jointly constrain cosmological and astrophysical baryonic feedback parameters using a flexible analytical model, {\textquoteleft}baryonification{\textquoteright}. First, using WL only, we compare the S8 constraints using baryonification to a simulation-calibrated halo model, a simulation-based emulator model, and the approach of discarding WL measurements on small angular scales. We find that model flexibility can shift the value of S8 and degrade the uncertainty. The kSZ provides additional constraints on the astrophysical parameters, with the joint WL + kSZ analysis constraining S8 = 0.823+−00020019. We measure the suppression of the non-linear matter power spectrum using WL + kSZ and constrain a mean feedback scenario that is more extreme than the predictions from most hydrodynamical simulations. We constrain the baryon fractions and the gas mass fractions and find them to be generally lower than inferred from X-ray observations and simulation predictions. We conclude that the WL + kSZ measurements provide a new and complementary benchmark for building a coherent picture of the impact of gas around galaxies across observations.",

keywords = "cosmology: observations, gravitational lensing: weak, large-scale structure of Universe",

author = "L. Bigwood and A. Amon and A. Schneider and J. Salcido and McCarthy, {I. G.} and C. Preston and D. Sanchez and D. Sijacki and E. Schaan and S. Ferraro and N. Battaglia and A. Chen and S. Dodelson and A. Roodman and A. Pieres and A. Fert{\'e} and A. Alarcon and A. Drlica-Wagner and A. Choi and A. Navarro-Alsina and A. Campos and Ross, {A. J.} and Rosell, {A. Carnero} and B. Yin and B. Yanny and C. S{\'a}nchez and C. Chang and C. Davis and C. Doux and D. Gruen and Rykoff, {E. S.} and Huff, {E. M.} and E. Sheldon and F. Tarsitano and F. Andrade-Oliveira and Bernstein, {G. M.} and G. Giannini and Diehl, {H. T.} and H. Huang and I. Harrison and I. Sevilla-Noarbe and I. Tutusaus and J. Elvin-Poole and J. McCullough and J. Zuntz and J. Blazek and J. DeRose and J. Cordero and J. Prat and J. Myles and K. Eckert and K. Bechtol and K. Herner and Secco, {L. F.} and M. Gatti and M. Raveri and {Carrasco Kind}, M. and Becker, {M. R.} and Troxel, {M. A.} and M. Jarvis and N. MacCrann and O. Friedrich and O. Alves and Leget, {P. F.} and R. Chen and Rollins, {R. P.} and Wechsler, {R. H.} and Gruendl, {R. A.} and R. Cawthon and S. Allam and Bridle, {S. L.} and S. Pandey and S. Everett and T. Shin and Hartley, {W. G.} and X. Fang and Y. Zhang and M. Aguena and J. Annis and D. Bacon and E. Bertin and S. Bocquet and D. Brooks and J. Carretero and Castander, {F. J.} and {da Costa}, {L. N.} and Pereira, {M. E.S.} and {De Vicente}, J. and S. Desai and P. Doel and I. Ferrero and B. Flaugher and J. Frieman and J. Garc{\'i}a-Bellido and E. Gaztanaga and G. Gutierrez and Hinton, {S. R.} and Hollowood, {D. L.} and K. Honscheid and D. Huterer and James, {D. J.} and K. Kuehn and O. Lahav and S. Lee and Marshall, {J. L.} and J. Mena-Fern{\'a}ndez and R. Miquel and J. Muir and M. Paterno and Malag{\'o}n, {A. A.Plazas} and A. Porredon and Romer, {A. K.} and S. Samuroff and E. Sanchez and {Sanchez Cid}, D. and M. Smith and M. Soares-Santos and E. Suchyta and Swanson, {M. E.C.} and G. Tarle and C. To and N. Weaverdyck and J. Weller and P. Wiseman and M. Yamamoto",

note = "Publisher Copyright: {\textcopyright} 2024 The Author(s).",

year = "2024",

month = oct,

day = "1",

doi = "10.1093/mnras/stae2100",

language = "English",

volume = "534",

pages = "655--682",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "1",

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Bigwood, L, Amon, A, Schneider, A, Salcido, J, McCarthy, IG, Preston, C, Sanchez, D, Sijacki, D, Schaan, E, Ferraro, S, Battaglia, N, Chen, A, Dodelson, S, Roodman, A, Pieres, A, Ferté, A, Alarcon, A, Drlica-Wagner, A, Choi, A, Navarro-Alsina, A, Campos, A, Ross, AJ, Rosell, AC, Yin, B, Yanny, B, Sánchez, C, Chang, C, Davis, C, Doux, C, Gruen, D, Rykoff, ES, Huff, EM, Sheldon, E, Tarsitano, F, Andrade-Oliveira, F, Bernstein, GM, Giannini, G, Diehl, HT, Huang, H, Harrison, I, Sevilla-Noarbe, I, Tutusaus, I, Elvin-Poole, J, McCullough, J, Zuntz, J, Blazek, J, DeRose, J, Cordero, J, Prat, J, Myles, J, Eckert, K, Bechtol, K, Herner, K, Secco, LF, Gatti, M, Raveri, M, Carrasco Kind, M, Becker, MR, Troxel, MA, Jarvis, M, MacCrann, N, Friedrich, O, Alves, O, Leget, PF, Chen, R, Rollins, RP, Wechsler, RH, Gruendl, RA, Cawthon, R, Allam, S, Bridle, SL, Pandey, S, Everett, S, Shin, T, Hartley, WG, Fang, X, Zhang, Y, Aguena, M, Annis, J, Bacon, D, Bertin, E, Bocquet, S, Brooks, D, Carretero, J, Castander, FJ, da Costa, LN, Pereira, MES, De Vicente, J, Desai, S, Doel, P, Ferrero, I, Flaugher, B, Frieman, J, García-Bellido, J, Gaztanaga, E, Gutierrez, G, Hinton, SR, Hollowood, DL, Honscheid, K, Huterer, D, James, DJ, Kuehn, K, Lahav, O, Lee, S, Marshall, JL, Mena-Fernández, J, Miquel, R, Muir, J, Paterno, M, Malagón, AAP, Porredon, A, Romer, AK, Samuroff, S, Sanchez, E, Sanchez Cid, D, Smith, M, Soares-Santos, M, Suchyta, E, Swanson, MEC, Tarle, G, To, C, Weaverdyck, N, Weller, J, Wiseman, P & Yamamoto, M 2024, 'Weak lensing combined with the kinetic Sunyaev–Zel’dovich effect: a study of baryonic feedback', Monthly Notices of the Royal Astronomical Society, vol. 534, no. 1, pp. 655-682. https://doi.org/10.1093/mnras/stae2100

TY - JOUR

T1 - Weak lensing combined with the kinetic Sunyaev–Zel’dovich effect

T2 - a study of baryonic feedback

AU - Bigwood, L.

AU - Amon, A.

AU - Schneider, A.

AU - Salcido, J.

AU - McCarthy, I. G.

AU - Preston, C.

AU - Sanchez, D.

AU - Sijacki, D.

AU - Schaan, E.

AU - Ferraro, S.

AU - Battaglia, N.

AU - Chen, A.

AU - Dodelson, S.

AU - Roodman, A.

AU - Pieres, A.

AU - Ferté, A.

AU - Alarcon, A.

AU - Drlica-Wagner, A.

AU - Choi, A.

AU - Navarro-Alsina, A.

AU - Campos, A.

AU - Ross, A. J.

AU - Rosell, A. Carnero

AU - Yin, B.

AU - Yanny, B.

AU - Sánchez, C.

AU - Chang, C.

AU - Davis, C.

AU - Doux, C.

AU - Gruen, D.

AU - Rykoff, E. S.

AU - Huff, E. M.

AU - Sheldon, E.

AU - Tarsitano, F.

AU - Andrade-Oliveira, F.

AU - Bernstein, G. M.

AU - Giannini, G.

AU - Diehl, H. T.

AU - Huang, H.

AU - Harrison, I.

AU - Sevilla-Noarbe, I.

AU - Tutusaus, I.

AU - Elvin-Poole, J.

AU - McCullough, J.

AU - Zuntz, J.

AU - Blazek, J.

AU - DeRose, J.

AU - Cordero, J.

AU - Prat, J.

AU - Myles, J.

AU - Eckert, K.

AU - Bechtol, K.

AU - Herner, K.

AU - Secco, L. F.

AU - Gatti, M.

AU - Raveri, M.

AU - Carrasco Kind, M.

AU - Becker, M. R.

AU - Troxel, M. A.

AU - Jarvis, M.

AU - MacCrann, N.

AU - Friedrich, O.

AU - Alves, O.

AU - Leget, P. F.

AU - Chen, R.

AU - Rollins, R. P.

AU - Wechsler, R. H.

AU - Gruendl, R. A.

AU - Cawthon, R.

AU - Allam, S.

AU - Bridle, S. L.

AU - Pandey, S.

AU - Everett, S.

AU - Shin, T.

AU - Hartley, W. G.

AU - Fang, X.

AU - Zhang, Y.

AU - Aguena, M.

AU - Annis, J.

AU - Bacon, D.

AU - Bertin, E.

AU - Bocquet, S.

AU - Brooks, D.

AU - Carretero, J.

AU - Castander, F. J.

AU - da Costa, L. N.

AU - Pereira, M. E.S.

AU - De Vicente, J.

AU - Desai, S.

AU - Doel, P.

AU - Ferrero, I.

AU - Flaugher, B.

AU - Frieman, J.

AU - García-Bellido, J.

AU - Gaztanaga, E.

AU - Gutierrez, G.

AU - Hinton, S. R.

AU - Hollowood, D. L.

AU - Honscheid, K.

AU - Huterer, D.

AU - James, D. J.

AU - Kuehn, K.

AU - Lahav, O.

AU - Lee, S.

AU - Marshall, J. L.

AU - Mena-Fernández, J.

AU - Miquel, R.

AU - Muir, J.

AU - Paterno, M.

AU - Malagón, A. A.Plazas

AU - Porredon, A.

AU - Romer, A. K.

AU - Samuroff, S.

AU - Sanchez, E.

AU - Sanchez Cid, D.

AU - Smith, M.

AU - Soares-Santos, M.

AU - Suchyta, E.

AU - Swanson, M. E.C.

AU - Tarle, G.

AU - To, C.

AU - Weaverdyck, N.

AU - Weller, J.

AU - Wiseman, P.

AU - Yamamoto, M.

PY - 2024/10/1

Y1 - 2024/10/1

N2 - Extracting precise cosmology from weak lensing surveys requires modelling the non-linear matter power spectrum, which is suppressed at small scales due to baryonic feedback processes. However, hydrodynamical galaxy formation simulations make widely varying predictions for the amplitude and extent of this effect. We use measurements of Dark Energy Survey Year 3 weak lensing (WL) and Atacama Cosmology Telescope DR5 kinematic Sunyaev–Zel’dovich (kSZ) to jointly constrain cosmological and astrophysical baryonic feedback parameters using a flexible analytical model, ‘baryonification’. First, using WL only, we compare the S8 constraints using baryonification to a simulation-calibrated halo model, a simulation-based emulator model, and the approach of discarding WL measurements on small angular scales. We find that model flexibility can shift the value of S8 and degrade the uncertainty. The kSZ provides additional constraints on the astrophysical parameters, with the joint WL + kSZ analysis constraining S8 = 0.823+−00020019. We measure the suppression of the non-linear matter power spectrum using WL + kSZ and constrain a mean feedback scenario that is more extreme than the predictions from most hydrodynamical simulations. We constrain the baryon fractions and the gas mass fractions and find them to be generally lower than inferred from X-ray observations and simulation predictions. We conclude that the WL + kSZ measurements provide a new and complementary benchmark for building a coherent picture of the impact of gas around galaxies across observations.

AB - Extracting precise cosmology from weak lensing surveys requires modelling the non-linear matter power spectrum, which is suppressed at small scales due to baryonic feedback processes. However, hydrodynamical galaxy formation simulations make widely varying predictions for the amplitude and extent of this effect. We use measurements of Dark Energy Survey Year 3 weak lensing (WL) and Atacama Cosmology Telescope DR5 kinematic Sunyaev–Zel’dovich (kSZ) to jointly constrain cosmological and astrophysical baryonic feedback parameters using a flexible analytical model, ‘baryonification’. First, using WL only, we compare the S8 constraints using baryonification to a simulation-calibrated halo model, a simulation-based emulator model, and the approach of discarding WL measurements on small angular scales. We find that model flexibility can shift the value of S8 and degrade the uncertainty. The kSZ provides additional constraints on the astrophysical parameters, with the joint WL + kSZ analysis constraining S8 = 0.823+−00020019. We measure the suppression of the non-linear matter power spectrum using WL + kSZ and constrain a mean feedback scenario that is more extreme than the predictions from most hydrodynamical simulations. We constrain the baryon fractions and the gas mass fractions and find them to be generally lower than inferred from X-ray observations and simulation predictions. We conclude that the WL + kSZ measurements provide a new and complementary benchmark for building a coherent picture of the impact of gas around galaxies across observations.

KW - cosmology: observations

KW - gravitational lensing: weak

KW - large-scale structure of Universe

UR - http://www.scopus.com/inward/record.url?scp=85205220352&partnerID=8YFLogxK

U2 - 10.1093/mnras/stae2100

DO - 10.1093/mnras/stae2100

M3 - Article

AN - SCOPUS:85205220352

SN - 0035-8711

VL - 534

SP - 655

EP - 682

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 1

ER -

Weak lensing combined with the kinetic Sunyaev–Zel’dovich effect: a study of baryonic feedback

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