Constraints on the redshift evolution of astrophysical feedback with Sunyaev-Zel'dovich effect cross-correlations

(DES Collaboration)

doi:10.1103/PhysRevD.100.063519

Constraints on the redshift evolution of astrophysical feedback with Sunyaev-Zel'dovich effect cross-correlations

(DES Collaboration)

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Abstract

An understanding of astrophysical feedback is important for constraining models of galaxy formation and for extracting cosmological information from current and future weak lensing surveys. The thermal Sunyaev-Zel'dovich effect, quantified via the Compton-y parameter, is a powerful tool for studying feedback, because it directly probes the pressure of the hot, ionized gas residing in dark matter halos. Cross-correlations between galaxies and maps of Compton-y obtained from cosmic microwave background surveys are sensitive to the redshift evolution of the gas pressure, and its dependence on halo mass. In this work, we use galaxies identified in year one data from the Dark Energy Survey and Compton-y maps constructed from Planck observations. We find highly significant (roughly 12σ) detections of galaxy-y cross-correlation in multiple redshift bins. By jointly fitting these measurements as well as measurements of galaxy clustering, we constrain the halo bias-weighted, gas pressure of the Universe as a function of redshift between 0.15?z?0.75. We compare these measurements to predictions from hydrodynamical simulations, allowing us to constrain the amount of thermal energy in the halo gas relative to that resulting from gravitational collapse.

Original language	English
Article number	63519
Journal	Physical Review D
Volume	100
Issue number	6
DOIs	https://doi.org/10.1103/PhysRevD.100.063519
State	Published - Sep 16 2019

Funding

We thank the Websky group for making their simulations publicly available, and for providing support for their use. We thank Mathieu Remazeilles for assistance in understanding the Planck maps. We also thank Nicholas Battaglia for valuable discussions regarding pressure profile models and the formalism of the paper. S. P., E. B., Z. X., and J. O. S. are partially supported by the U.S. National Science Foundation through Grant No. AST-1440226 for the ACT project. S. P. and E. B. are also partially supported by the U.S. Department of Energy Grant No. DE-SC0007901. 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, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, 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 Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, 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 Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated 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’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 Ciência e Tecnologia (INCT) e-Universe (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. The U.S. Government retains and the publisher, by accepting the article for publication, acknowledges that the U.S. Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. S.P., E.B., Z.X., and J.O.S. are partially supported by the U.S. National Science Foundation through Grant No. AST-1440226 for the ACT project.

Funders	Funder number
Brazilian Instituto Nacional de Ciência e Tecnologia
Collaborating Institutions in the Dark Energy Survey
Fermi Research Alliance, LLC	DE-AC02-07CH11359
INCT
Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University
National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign
Science and Technology Facilities Council of the United Kingdom
U.S. National Science Foundation
National Science Foundation	AST-1138766, AST-1440226, AST-1536171
U.S. Department of Energy	DE-SC0007901
Office of Science
High Energy Physics
Ohio State University
University of Chicago
Seventh Framework Programme	1138766, 240672, 1440226, 306478, 291329
Higher Education Funding Council for England
Engineering Research Centers
European Commission
European Research Council
Deutsche Forschungsgemeinschaft
Generalitat de Catalunya
Ministerio de Economía y Competitividad	SEV-2016-0588, SEV-2016-0597, ESP2015-66861, MDM-2015-0509, FPA2015-68048, AYA2015-71825
Ministério da Ciência, Tecnologia e Inovação
Conselho Nacional de Desenvolvimento Científico e Tecnológico	465376/2014-2
Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro
Financiadora de Estudos e Projetos
Ministry of Education and Science of Ukraine
European Regional Development Fund

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10.1103/PhysRevD.100.063519

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@article{26913aa8201d44459816cccf75184193,

title = "Constraints on the redshift evolution of astrophysical feedback with Sunyaev-Zel'dovich effect cross-correlations",

abstract = "An understanding of astrophysical feedback is important for constraining models of galaxy formation and for extracting cosmological information from current and future weak lensing surveys. The thermal Sunyaev-Zel'dovich effect, quantified via the Compton-y parameter, is a powerful tool for studying feedback, because it directly probes the pressure of the hot, ionized gas residing in dark matter halos. Cross-correlations between galaxies and maps of Compton-y obtained from cosmic microwave background surveys are sensitive to the redshift evolution of the gas pressure, and its dependence on halo mass. In this work, we use galaxies identified in year one data from the Dark Energy Survey and Compton-y maps constructed from Planck observations. We find highly significant (roughly 12σ) detections of galaxy-y cross-correlation in multiple redshift bins. By jointly fitting these measurements as well as measurements of galaxy clustering, we constrain the halo bias-weighted, gas pressure of the Universe as a function of redshift between 0.15?z?0.75. We compare these measurements to predictions from hydrodynamical simulations, allowing us to constrain the amount of thermal energy in the halo gas relative to that resulting from gravitational collapse.",

author = "{(DES Collaboration)} and S. Pandey and Baxter, {E. J.} and Z. Xu and J. Orlowski-Scherer and N. Zhu and A. Lidz and J. Aguirre and J. Derose and M. Devlin and Hill, {J. C.} and B. Jain and Sheth, {R. K.} and S. Avila and E. Bertin and D. Brooks and E. Buckley-Geer and {Carnero Rosell}, A. and {Carrasco Kind}, M. and J. Carretero and Castander, {F. J.} and R. Cawthon and {Da Costa}, {L. N.} and {De Vicente}, J. and S. Desai and Diehl, {H. T.} and Dietrich, {J. P.} and P. Doel and Evrard, {A. E.} and B. Flaugher and P. Fosalba and J. Frieman and J. Garc{\'i}a-Bellido and Gerdes, {D. W.} and T. Giannantonio and Gruendl, {R. A.} and J. Gschwend and Hartley, {W. G.} and Hollowood, {D. L.} and James, {D. J.} and E. Krause and K. Kuehn and N. Kuropatkin and Maia, {M. A.G.} and Marshall, {J. L.} and P. Melchior and F. Menanteau and R. Miquel and Plazas, {A. A.} and A. Roodman and E. Suchyta",

note = "Publisher Copyright: {\textcopyright} 2019 American Physical Society.",

year = "2019",

month = sep,

day = "16",

doi = "10.1103/PhysRevD.100.063519",

language = "English",

volume = "100",

journal = "Physical Review D",

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T1 - Constraints on the redshift evolution of astrophysical feedback with Sunyaev-Zel'dovich effect cross-correlations

AU - (DES Collaboration)

AU - Pandey, S.

AU - Baxter, E. J.

AU - Xu, Z.

AU - Orlowski-Scherer, J.

AU - Zhu, N.

AU - Lidz, A.

AU - Aguirre, J.

AU - Derose, J.

AU - Devlin, M.

AU - Hill, J. C.

AU - Jain, B.

AU - Sheth, R. K.

AU - Avila, S.

AU - Bertin, E.

AU - Brooks, D.

AU - Buckley-Geer, E.

AU - Carnero Rosell, A.

AU - Carrasco Kind, M.

AU - Carretero, J.

AU - Castander, F. J.

AU - Cawthon, R.

AU - Da Costa, L. N.

AU - De Vicente, J.

AU - Desai, S.

AU - Diehl, H. T.

AU - Dietrich, J. P.

AU - Doel, P.

AU - Evrard, A. E.

AU - Flaugher, B.

AU - Fosalba, P.

AU - Frieman, J.

AU - García-Bellido, J.

AU - Gerdes, D. W.

AU - Giannantonio, T.

AU - Gruendl, R. A.

AU - Gschwend, J.

AU - Hartley, W. G.

AU - Hollowood, D. L.

AU - James, D. J.

AU - Krause, E.

AU - Kuehn, K.

AU - Kuropatkin, N.

AU - Maia, M. A.G.

AU - Marshall, J. L.

AU - Melchior, P.

AU - Menanteau, F.

AU - Miquel, R.

AU - Plazas, A. A.

AU - Roodman, A.

AU - Suchyta, E.

PY - 2019/9/16

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N2 - An understanding of astrophysical feedback is important for constraining models of galaxy formation and for extracting cosmological information from current and future weak lensing surveys. The thermal Sunyaev-Zel'dovich effect, quantified via the Compton-y parameter, is a powerful tool for studying feedback, because it directly probes the pressure of the hot, ionized gas residing in dark matter halos. Cross-correlations between galaxies and maps of Compton-y obtained from cosmic microwave background surveys are sensitive to the redshift evolution of the gas pressure, and its dependence on halo mass. In this work, we use galaxies identified in year one data from the Dark Energy Survey and Compton-y maps constructed from Planck observations. We find highly significant (roughly 12σ) detections of galaxy-y cross-correlation in multiple redshift bins. By jointly fitting these measurements as well as measurements of galaxy clustering, we constrain the halo bias-weighted, gas pressure of the Universe as a function of redshift between 0.15?z?0.75. We compare these measurements to predictions from hydrodynamical simulations, allowing us to constrain the amount of thermal energy in the halo gas relative to that resulting from gravitational collapse.

AB - An understanding of astrophysical feedback is important for constraining models of galaxy formation and for extracting cosmological information from current and future weak lensing surveys. The thermal Sunyaev-Zel'dovich effect, quantified via the Compton-y parameter, is a powerful tool for studying feedback, because it directly probes the pressure of the hot, ionized gas residing in dark matter halos. Cross-correlations between galaxies and maps of Compton-y obtained from cosmic microwave background surveys are sensitive to the redshift evolution of the gas pressure, and its dependence on halo mass. In this work, we use galaxies identified in year one data from the Dark Energy Survey and Compton-y maps constructed from Planck observations. We find highly significant (roughly 12σ) detections of galaxy-y cross-correlation in multiple redshift bins. By jointly fitting these measurements as well as measurements of galaxy clustering, we constrain the halo bias-weighted, gas pressure of the Universe as a function of redshift between 0.15?z?0.75. We compare these measurements to predictions from hydrodynamical simulations, allowing us to constrain the amount of thermal energy in the halo gas relative to that resulting from gravitational collapse.

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JO - Physical Review D

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Constraints on the redshift evolution of astrophysical feedback with Sunyaev-Zel'dovich effect cross-correlations

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