Dark energy survey year 1 results: The relationship between mass and light around cosmic voids

DES Collaboration

doi:10.1093/mnras/stz2805

Dark energy survey year 1 results: The relationship between mass and light around cosmic voids

DES Collaboration

Workflow Systems

Research output: Contribution to journal › Article › peer-review

36 Scopus citations

Abstract

What are the mass and galaxy profiles of cosmic voids? In this paper, we use two methods to extract voids in the Dark Energy Survey (DES) Year 1 redMaGiC galaxy sample to address this question. We use either 2D slices in projection, or the 3D distribution of galaxies based on photometric redshifts to identify voids. For the mass profile, we measure the tangential shear profiles of background galaxies to infer the excess surface mass density. The signal-to-noise ratio for our lensing measurement ranges between 10.7 and 14.0 for the two void samples. We infer their 3D density profiles by fitting models based on N-body simulations and find good agreement for void radii in the range 15-85 Mpc. Comparison with their galaxy profiles then allows us to test the relation between mass and light at the 10 per cent level, the most stringent test to date. We find very similar shapes for the two profiles, consistent with a linear relationship between mass and light both within and outside the void radius. We validate our analysis with the help of simulated mock catalogues and estimate the impact of photometric redshift uncertainties on the measurement. Our methodology can be used for cosmological applications, including tests of gravity with voids. This is especially promising when the lensing profiles are combined with spectroscopic measurements of void dynamics via redshift-space distortions.

Original language	English
Pages (from-to)	3573-3587
Number of pages	15
Journal	Monthly Notices of the Royal Astronomical Society
Volume	490
Issue number	3
DOIs	https://doi.org/10.1093/mnras/stz2805
State	Published - Dec 1 2019

Funding

This paper has gone through internal review by the DES collaboration. We are grateful to Arka Banerjee, Elena Massara, Alice Pisani, and Ravi Sheth for helpful discussions. NH and GP acknowledge support from the DFG cluster of excellence 'Origins' and the Trans-Regional Collaborative Research Center TRR 33 'The Dark Universe' of the DFG. YF and BJ are supported in part by the U.S. Department of Energy grant DE-SC0007901. This work has made use of CosmoHub, see Carretero et al. (2017). CosmoHub has been developed by the Port d'Informaci\u00F3 Cient\u00EDfica (PIC), maintained through a collaboration of the Institut de F\u00EDsica d'Altes Energies (IFAE) and the Centro de Investigaciones Energ\u00E9ticas, Medioambientales y Tecnol\u00F3gicas (CIEMAT), and was partially funded by the 'Plan Estatal de Investigaci\u00F3n Cient\u00EDfica y T\u00E9cnica y de Innovaci\u00F3n' program of the Spanish government. 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 DES. 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'Espai (IEEC/CSIC), the Institut de F\u00EDsica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universit\u00E4t M\u00FCnchen 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 grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, 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's 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) e-Universe (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 United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, worldwide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. This paper has gone through internal review by the DES collaboration. We are grateful to Arka Banerjee, Elena Massara, Alice Pisani, and Ravi Sheth for helpful discussions. NH and GP acknowledge support from the DFG cluster of excellence \u2018Origins\u2019 and the Trans-Regional Collaborative Research Center TRR 33 \u2018The Dark Universe\u2019 of the DFG. YF and BJ are supported in part by the U.S. Department of Energy grant DE-SC0007901. The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-66861, FPA2015-68048, 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) e-Universe (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 United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, worldwide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes.

Funders	Funder number
Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University
University of Illinois at Urbana-Champaign
United States Government
Spanish National Plan for Scientific and Technical Research and Innovation
Brazilian Instituto Nacional de Ciência e Tecnologia
University of Nottingham
University of Sussex
High Energy Physics
Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas
University of Edinburgh
Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro
Ohio State University
Stanford University
University of Chicago
Engineering Research Centers
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
European Commission
Instituto Nacional de Ciência e Tecnologia para Excitotoxicidade e Neuroproteção
SLAC National Accelerator Laboratory
Lawrence Berkeley National Laboratory
Fermilab
Seventh Framework Programme
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 Research Council
European Regional Development Fund
University of Michigan
Institut de Física d'Altes Energies
University of Pennsylvania
Ludwig-Maximilians-Universität München
Texas A and M University
Institut de Ciències de l'Espai
U.S. Department of Energy	DE-SC0007901
National Science Foundation	1138766, AST-1536171
Ministerio de Economía y Competitividad	SEV-2016-0588, SEV-2016-0597, ESP2015-66861, MDM-2015-0509, FPA2015-68048, AYA2015-71825
Seventh Framework Programme	1138766, 240672, 306478, 291329
Fermi Research Alliance, LLC	DE-AC02-07CH11359
Conselho Nacional de Desenvolvimento Científico e Tecnológico	465376/2014-2

Keywords

Cosmology: observations
Gravitational lensing: weak
Large-scale structure of Universe

Access to Document

10.1093/mnras/stz2805

Cite this

@article{ff8b5352001f4257b512c8119ba77a41,

title = "Dark energy survey year 1 results: The relationship between mass and light around cosmic voids",

abstract = "What are the mass and galaxy profiles of cosmic voids? In this paper, we use two methods to extract voids in the Dark Energy Survey (DES) Year 1 redMaGiC galaxy sample to address this question. We use either 2D slices in projection, or the 3D distribution of galaxies based on photometric redshifts to identify voids. For the mass profile, we measure the tangential shear profiles of background galaxies to infer the excess surface mass density. The signal-to-noise ratio for our lensing measurement ranges between 10.7 and 14.0 for the two void samples. We infer their 3D density profiles by fitting models based on N-body simulations and find good agreement for void radii in the range 15-85 Mpc. Comparison with their galaxy profiles then allows us to test the relation between mass and light at the 10 per cent level, the most stringent test to date. We find very similar shapes for the two profiles, consistent with a linear relationship between mass and light both within and outside the void radius. We validate our analysis with the help of simulated mock catalogues and estimate the impact of photometric redshift uncertainties on the measurement. Our methodology can be used for cosmological applications, including tests of gravity with voids. This is especially promising when the lensing profiles are combined with spectroscopic measurements of void dynamics via redshift-space distortions.",

keywords = "Cosmology: observations, Gravitational lensing: weak, Large-scale structure of Universe",

author = "{DES Collaboration} and Y. Fang and N. Hamaus and B. Jain and S. Pandey and G. Pollina and C. S{\'a}nchez and A. Kov{\'a}cs and C. Chang and J. Carretero and Castander, {F. J.} and A. Choi and M. Crocce and J. DeRose and P. Fosalba and M. Gatti and E. Gazta{\~n}aga and D. Gruen and Hartley, {W. G.} and B. Hoyle and N. MacCrann and J. Prat and Rau, {M. M.} and Rykoff, {E. S.} and S. Samuroff and E. Sheldon and Troxel, {M. A.} and P. Vielzeuf and J. Zuntz and J. Annis and S. Avila and E. Bertin and D. Brooks and Burke, {D. L.} and {Carnero Rosell}, A. and {Carrasco Kind}, M. 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 S. Everett and Evrard, {A. E.} and B. Flaugher and J. Frieman and J. Garc{\'i}a-Bellido and Gerdes, {D. W.} and Gruendl, {R. A.} and E. Suchyta",

note = "Publisher Copyright: {\textcopyright} 2019 The Author(s)",

year = "2019",

month = dec,

day = "1",

doi = "10.1093/mnras/stz2805",

language = "English",

volume = "490",

pages = "3573--3587",

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

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

}

TY - JOUR

T1 - Dark energy survey year 1 results

T2 - The relationship between mass and light around cosmic voids

AU - DES Collaboration

AU - Fang, Y.

AU - Hamaus, N.

AU - Jain, B.

AU - Pandey, S.

AU - Pollina, G.

AU - Sánchez, C.

AU - Kovács, A.

AU - Chang, C.

AU - Carretero, J.

AU - Castander, F. J.

AU - Choi, A.

AU - Crocce, M.

AU - DeRose, J.

AU - Fosalba, P.

AU - Gatti, M.

AU - Gaztañaga, E.

AU - Gruen, D.

AU - Hartley, W. G.

AU - Hoyle, B.

AU - MacCrann, N.

AU - Prat, J.

AU - Rau, M. M.

AU - Rykoff, E. S.

AU - Samuroff, S.

AU - Sheldon, E.

AU - Troxel, M. A.

AU - Vielzeuf, P.

AU - Zuntz, J.

AU - Annis, J.

AU - Avila, S.

AU - Bertin, E.

AU - Brooks, D.

AU - Burke, D. L.

AU - Carnero Rosell, A.

AU - Carrasco Kind, M.

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 - Everett, S.

AU - Evrard, A. E.

AU - Flaugher, B.

AU - Frieman, J.

AU - García-Bellido, J.

AU - Gerdes, D. W.

AU - Gruendl, R. A.

AU - Suchyta, E.

PY - 2019/12/1

Y1 - 2019/12/1

N2 - What are the mass and galaxy profiles of cosmic voids? In this paper, we use two methods to extract voids in the Dark Energy Survey (DES) Year 1 redMaGiC galaxy sample to address this question. We use either 2D slices in projection, or the 3D distribution of galaxies based on photometric redshifts to identify voids. For the mass profile, we measure the tangential shear profiles of background galaxies to infer the excess surface mass density. The signal-to-noise ratio for our lensing measurement ranges between 10.7 and 14.0 for the two void samples. We infer their 3D density profiles by fitting models based on N-body simulations and find good agreement for void radii in the range 15-85 Mpc. Comparison with their galaxy profiles then allows us to test the relation between mass and light at the 10 per cent level, the most stringent test to date. We find very similar shapes for the two profiles, consistent with a linear relationship between mass and light both within and outside the void radius. We validate our analysis with the help of simulated mock catalogues and estimate the impact of photometric redshift uncertainties on the measurement. Our methodology can be used for cosmological applications, including tests of gravity with voids. This is especially promising when the lensing profiles are combined with spectroscopic measurements of void dynamics via redshift-space distortions.

AB - What are the mass and galaxy profiles of cosmic voids? In this paper, we use two methods to extract voids in the Dark Energy Survey (DES) Year 1 redMaGiC galaxy sample to address this question. We use either 2D slices in projection, or the 3D distribution of galaxies based on photometric redshifts to identify voids. For the mass profile, we measure the tangential shear profiles of background galaxies to infer the excess surface mass density. The signal-to-noise ratio for our lensing measurement ranges between 10.7 and 14.0 for the two void samples. We infer their 3D density profiles by fitting models based on N-body simulations and find good agreement for void radii in the range 15-85 Mpc. Comparison with their galaxy profiles then allows us to test the relation between mass and light at the 10 per cent level, the most stringent test to date. We find very similar shapes for the two profiles, consistent with a linear relationship between mass and light both within and outside the void radius. We validate our analysis with the help of simulated mock catalogues and estimate the impact of photometric redshift uncertainties on the measurement. Our methodology can be used for cosmological applications, including tests of gravity with voids. This is especially promising when the lensing profiles are combined with spectroscopic measurements of void dynamics via redshift-space distortions.

KW - Cosmology: observations

KW - Gravitational lensing: weak

KW - Large-scale structure of Universe

UR - http://www.scopus.com/inward/record.url?scp=85079677795&partnerID=8YFLogxK

U2 - 10.1093/mnras/stz2805

DO - 10.1093/mnras/stz2805

M3 - Article

AN - SCOPUS:85079677795

SN - 0035-8711

VL - 490

SP - 3573

EP - 3587

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

Dark energy survey year 1 results: The relationship between mass and light around cosmic voids

Abstract

Funding

Keywords

Access to Document

Other files and links

Fingerprint

Cite this