SPT clusters with DES and HST weak lensing. II. Cosmological constraints from the abundance of massive halos

Bocquet, S. [Ludwig-Maximilians-Universität] (ORCID:000000024900805X); Grandis, S. [Universität Innsbruck; Ludwig-Maximilians-Universität] (ORCID:0000000245778217); Bleem, L. E. [Argonne National Laboratory; University of Chicago] (ORCID:0000000176655079); Klein, M. [Ludwig-Maximilians-Universität] (ORCID:0000000282484488); Mohr, J. J. [Ludwig-Maximilians-Universität; Max Planck Institute for Extraterrestrial Physics] (ORCID:0000000268752087); Schrabback, T. [Universität Innsbruck; Argelander-Institut für Astronomie] (ORCID:0000000269877834); Abbott, T. M. C. [NSF’s National Optical-Infrared Astronomy Research Laboratory]; Ade, P. A. R. [Cardiff University]; Aguena, M. [Laboratório Interinstitucional de e-Astronomia—LIneA]; Alarcon, A. [Argonne National Laboratory]; Allam, S. [Fermi National Accelerator Laboratory]; Allen, S. W. [Stanford University; Stanford University; SLAC National Accelerator Laboratory]; Alves, O. [University of Michigan]; Amon, A. [University of Cambridge; University of Cambridge]; Anderson, A. J. [Fermi National Accelerator Laboratory]; Annis, J. [Fermi National Accelerator Laboratory]; Ansarinejad, B. [University of Melbourne]; Austermann, J. E. [NIST Quantum Devices Group; University of Colorado]; Avila, S. [Barcelona Institute of Science and Technology]; Bacon, D. [University of Portsmouth]; Bayliss, M. [University of Cincinnati]; Beall, J. A. [NIST Quantum Devices Group]; Bechtol, K. [University of Wisconsin-Madison]; Becker, M. R. [Argonne National Laboratory]; Bender, A. N. [Argonne National Laboratory; University of Chicago; University of Chicago]; Benson, B. A. [University of Chicago; University of Chicago; Fermi National Accelerator Laboratory]; Bernstein, G. M. [University of Pennsylvania]; Bhargava, S. [University of Sussex]; Bianchini, F. [Stanford University; Stanford University; SLAC National Accelerator Laboratory]; Brodwin, M. [University of Missouri]; Brooks, D. [University College London]; Bryant, L. [University of Chicago]; Campos, A. [Carnegie Mellon University]; Canning, R. E. A. [University of Portsmouth]; Carlstrom, J. E. [University of Chicago; University of Chicago; University of Chicago; Argonne National Laboratory; University of Chicago]; Carnero Rosell, A. [Instituto de Astrofisica de Canarias; Laboratório Interinstitucional de e-Astronomia—LIneA; Universidad de La Laguna]; Carrasco Kind, M. [National Center for Supercomputing Applications; University of Illinois Urbana-Champaign]; Carretero, J. [Barcelona Institute of Science and Technology]; Castander, F. J. [Institut d’Estudis Espacials de Catalunya (IEEC); Institute of Space Sciences (ICE, CSIC)]; Cawthon, R. [William Jewell College]; Chang, C. L. [University of Chicago; Argonne National Laboratory; University of Chicago]; Chang, C. [University of Chicago; University of Chicago]; Chaubal, P. [University of Melbourne]; Chen, R. [Duke University Durham]; Chiang, H. C. [McGill University; University of KwaZulu-Natal]; Choi, A. [NASA Goddard Space Flight Center]; Chou, T-L. [University of Chicago; University of Chicago]; Citron, R. [University of Chicago]; Corbett Moran, C. [California Institute of Technology]; Cordero, J. [University of Manchester]; Costanzi, M. [University of Trieste; INAF-Osservatorio Astronomico di Trieste; Institute for Fundamental Physics of the Universe]; Crawford, T. M. [University of Chicago; University of Chicago]; Crites, A. T. [Cornell University]; da Costa, L. N. [Laboratório Interinstitucional de e-Astronomia—LIneA]; Pereira, M. E. S. [Universität Hamburg]; Davis, C. [Stanford University]; Davis, T. M. [University of Queensland]; DeRose, J. [Lawrence Berkeley National Laboratory]; Desai, S. [IIT Hyderabad]; de Haan, T. [High Energy Accelerator Research Organization (KEK); High Energy Accelerator Research Organization (KEK)]; Diehl, H. T. [Fermi National Accelerator Laboratory]; Dobbs, M. A. [McGill University; Canadian Institute for Advanced Research]; Dodelson, S. [Carnegie Mellon University; Carnegie Mellon University]; Doux, C. [University of Pennsylvania; Université Grenoble Alpes]; Drlica-Wagner, A. [University of Chicago; Fermi National Accelerator Laboratory; University of Chicago]; Eckert, K. [University of Pennsylvania]; Elvin-Poole, J. [University of Waterloo]; Everett, S. [California Institute of Technology]; Everett, W. [University of Colorado]; Ferrero, I. [Institute of Theoretical Astrophysics]; Ferté, A. [SLAC National Accelerator Laboratory]; Flores, A. M. [Stanford University; Stanford University]; Frieman, J. [Fermi National Accelerator Laboratory; University of Chicago]; Gallicchio, J. [University of Chicago; Harvey Mudd College]; García-Bellido, J. [Universidad Autonoma de Madrid]; Gatti, M. [University of Pennsylvania]; George, E. M. [European Southern Observatory]; Giannini, G. [Barcelona Institute of Science and Technology; University of Chicago]; Gladders, M. D. [University of Chicago; University of Chicago]; Gruen, D. [Ludwig-Maximilians-Universität]; Gruendl, R. A. [National Center for Supercomputing Applications; University of Illinois Urbana-Champaign]; Gupta, N. [CSIRO Space and Astronomy]; Gutierrez, G. [Fermi National Accelerator Laboratory]; Halverson, N. W. [University of Colorado; University of Colorado]; Harrison, I. [Cardiff University]; Hartley, W. G. [University of Geneva]; Herner, K. [Fermi National Accelerator Laboratory]; Hinton, S. R. [University of Queensland]; Holder, G. P. [University of Illinois Urbana-Champaign; University of Illinois Urbana-Champaign; Canadian Institute for Advanced Research]; Hollowood, D. L. [Santa Cruz Institute for Particle Physics]; Holzapfel, W. L. [University of California]; Honscheid, K. [The Ohio State University; The Ohio State University]; Hrubes, J. D. [University of Chicago]; Huang, N. [University of California]; Hubmayr, J. [NIST Quantum Devices Group]; Huff, E. M. [California Institute of Technology]; Huterer, D. [University of Michigan]; Irwin, K. D. [SLAC National Accelerator Laboratory; Stanford University]; James, D. J. [Center for Astrophysics | Harvard & Smithsonian]; Jarvis, M. [University of Pennsylvania]

doi:10.1103/physrevd.110.083510

DOE OSTI · 2920381

SPT clusters with DES and HST weak lensing. II. Cosmological constraints from the abundance of massive halos

View original source ↗Read source document ↗Export metadata ↓

Abstract

We present cosmological constraints from the abundance of galaxy clusters selected via the thermal Sunyaev-Zel’dovich (SZ) effect in South Pole Telescope (SPT) data with a simultaneous mass calibration using weak gravitational lensing data from the Dark Energy Survey (DES) and the Hubble Space Telescope (HST). The cluster sample is constructed from the combined SPT-SZ, SPTpol ECS, and SPTpol 500d surveys, and comprises 1,005 confirmed clusters in the redshift range 0.25–1.78 over a total sky area of 5200 deg 2 . We use DES Year 3 weak-lensing data for 688 clusters with redshifts 𝑧 < 0.95 and HST weak-lensing data for 39 clusters with 0.6 < 𝑧 < 1.7. The weak-lensing measurements enable robust mass measurements of sample clusters and allow us to empirically constrain the SZ observable-mass relation without having to make strong assumptions about, e.g., the hydrodynamical state of the clusters. For a flat Λ⁢ CDM cosmology, and marginalizing over the sum of massive neutrinos, we measure Ω m = 0.286 ± 0.032, 𝜎 8 = 0.817 ± 0.026, and the parameter combination 𝜎 8 ⁢(Ω m /0.3) 0.25 = 0.805 ± 0.016. Our measurement of 𝑆 8 ≡ 𝜎 8 ⁢$\sqrt{Ω_{m}/0.3}$ = 0.795 ± 0.029 and the constraint from Planck CMB anisotropies (2018 TT, TE, EE+lowE) differ by 1.1⁢𝜎. In combination with that Planck dataset, we place a 95% upper limit on the sum of neutrino masses ∑𝑚 𝜈 < 0.18 eV. When additionally allowing the dark energy equation of state parameter 𝑤 to vary, we obtain 𝑤 = −1.45 ± 0.31 from our cluster-based analysis. In combination with Planck data, we measure 𝑤 =−1.3⁢4$^{+0.22}_{−0.15}$, or a 2.2⁢𝜎 difference with a cosmological constant. We use the cluster abundance to measure 𝜎8 in five redshift bins between 0.25 and 1.8, and we find the results to be consistent with structure growth as predicted by the Λ⁢ CDM model fit to Planck primary CMB data.

Explore related subjects

79 ASTRONOMY AND ASTROPHYSICS cosmological parameters dark energy galaxy clusters large-scale structure of the universe

Keep this discovery

BibTeX RIS

Bocquet, S. [Ludwig-Maximilians-Universität] (ORCID:000000024900805X), Grandis, S. [Universität Innsbruck; Ludwig-Maximilians-Universität] (ORCID:0000000245778217), Bleem, L. E. [Argonne National Laboratory; University of Chicago] (ORCID:0000000176655079), Klein, M. [Ludwig-Maximilians-Universität] (ORCID:0000000282484488), Mohr, J. J. [Ludwig-Maximilians-Universität; Max Planck Institute for Extraterrestrial Physics] (ORCID:0000000268752087), Schrabback, T. [Universität Innsbruck; Argelander-Institut für Astronomie] (ORCID:0000000269877834), Abbott, T. M. C. [NSF’s National Optical-Infrared Astronomy Research Laboratory], Ade, P. A. R. [Cardiff University], Aguena, M. [Laboratório Interinstitucional de e-Astronomia—LIneA], Alarcon, A. [Argonne National Laboratory], Allam, S. [Fermi National Accelerator Laboratory], Allen, S. W. [Stanford University; Stanford University; SLAC National Accelerator Laboratory], Alves, O. [University of Michigan], Amon, A. [University of Cambridge; University of Cambridge], Anderson, A. J. [Fermi National Accelerator Laboratory], Annis, J. [Fermi National Accelerator Laboratory], Ansarinejad, B. [University of Melbourne], Austermann, J. E. [NIST Quantum Devices Group; University of Colorado], Avila, S. [Barcelona Institute of Science and Technology], Bacon, D. [University of Portsmouth], Bayliss, M. [University of Cincinnati], Beall, J. A. [NIST Quantum Devices Group], Bechtol, K. [University of Wisconsin-Madison], Becker, M. R. [Argonne National Laboratory], Bender, A. N. [Argonne National Laboratory; University of Chicago; University of Chicago], Benson, B. A. [University of Chicago; University of Chicago; Fermi National Accelerator Laboratory], Bernstein, G. M. [University of Pennsylvania], Bhargava, S. [University of Sussex], Bianchini, F. [Stanford University; Stanford University; SLAC National Accelerator Laboratory], Brodwin, M. [University of Missouri], Brooks, D. [University College London], Bryant, L. [University of Chicago], Campos, A. [Carnegie Mellon University], Canning, R. E. A. [University of Portsmouth], Carlstrom, J. E. [University of Chicago; University of Chicago; University of Chicago; Argonne National Laboratory; University of Chicago], Carnero Rosell, A. [Instituto de Astrofisica de Canarias; Laboratório Interinstitucional de e-Astronomia—LIneA; Universidad de La Laguna], Carrasco Kind, M. [National Center for Supercomputing Applications; University of Illinois Urbana-Champaign], Carretero, J. [Barcelona Institute of Science and Technology], Castander, F. J. [Institut d’Estudis Espacials de Catalunya (IEEC); Institute of Space Sciences (ICE, CSIC)], Cawthon, R. [William Jewell College], Chang, C. L. [University of Chicago; Argonne National Laboratory; University of Chicago], Chang, C. [University of Chicago; University of Chicago], Chaubal, P. [University of Melbourne], Chen, R. [Duke University Durham], Chiang, H. C. [McGill University; University of KwaZulu-Natal], Choi, A. [NASA Goddard Space Flight Center], Chou, T-L. [University of Chicago; University of Chicago], Citron, R. [University of Chicago], Corbett Moran, C. [California Institute of Technology], Cordero, J. [University of Manchester], Costanzi, M. [University of Trieste; INAF-Osservatorio Astronomico di Trieste; Institute for Fundamental Physics of the Universe], Crawford, T. M. [University of Chicago; University of Chicago], Crites, A. T. [Cornell University], da Costa, L. N. [Laboratório Interinstitucional de e-Astronomia—LIneA], Pereira, M. E. S. [Universität Hamburg], Davis, C. [Stanford University], Davis, T. M. [University of Queensland], DeRose, J. [Lawrence Berkeley National Laboratory], Desai, S. [IIT Hyderabad], de Haan, T. [High Energy Accelerator Research Organization (KEK); High Energy Accelerator Research Organization (KEK)], Diehl, H. T. [Fermi National Accelerator Laboratory], Dobbs, M. A. [McGill University; Canadian Institute for Advanced Research], Dodelson, S. [Carnegie Mellon University; Carnegie Mellon University], Doux, C. [University of Pennsylvania; Université Grenoble Alpes], Drlica-Wagner, A. [University of Chicago; Fermi National Accelerator Laboratory; University of Chicago], Eckert, K. [University of Pennsylvania], Elvin-Poole, J. [University of Waterloo], Everett, S. [California Institute of Technology], Everett, W. [University of Colorado], Ferrero, I. [Institute of Theoretical Astrophysics], Ferté, A. [SLAC National Accelerator Laboratory], Flores, A. M. [Stanford University; Stanford University], Frieman, J. [Fermi National Accelerator Laboratory; University of Chicago], Gallicchio, J. [University of Chicago; Harvey Mudd College], García-Bellido, J. [Universidad Autonoma de Madrid], Gatti, M. [University of Pennsylvania], George, E. M. [European Southern Observatory], Giannini, G. [Barcelona Institute of Science and Technology; University of Chicago], Gladders, M. D. [University of Chicago; University of Chicago], Gruen, D. [Ludwig-Maximilians-Universität], Gruendl, R. A. [National Center for Supercomputing Applications; University of Illinois Urbana-Champaign], Gupta, N. [CSIRO Space and Astronomy], Gutierrez, G. [Fermi National Accelerator Laboratory], Halverson, N. W. [University of Colorado; University of Colorado], Harrison, I. [Cardiff University], Hartley, W. G. [University of Geneva], Herner, K. [Fermi National Accelerator Laboratory], Hinton, S. R. [University of Queensland], Holder, G. P. [University of Illinois Urbana-Champaign; University of Illinois Urbana-Champaign; Canadian Institute for Advanced Research], Hollowood, D. L. [Santa Cruz Institute for Particle Physics], Holzapfel, W. L. [University of California], Honscheid, K. [The Ohio State University; The Ohio State University], Hrubes, J. D. [University of Chicago], Huang, N. [University of California], Hubmayr, J. [NIST Quantum Devices Group], Huff, E. M. [California Institute of Technology], Huterer, D. [University of Michigan], Irwin, K. D. [SLAC National Accelerator Laboratory; Stanford University], James, D. J. [Center for Astrophysics | Harvard & Smithsonian], Jarvis, M. [University of Pennsylvania]. 2024-10-03. SPT clusters with DES and HST weak lensing. II. Cosmological constraints from the abundance of massive halos. https://doi.org/10.1103/physrevd.110.083510

Cite the original work for its findings. Save a collection to share your selection of sources.

Discover connections

79 ASTRONOMY AND ASTROPHYSICS subject Cosmological parameters subject dark energy subject galaxy clusters subject large-scale structure of the universe subject

Connections use source metadata and explicit phrase matches, not verified experimental comparisons.

KEEP EXPLORING

Related discoveries

DOE OSTI2024

Dark energy survey year 3 results: likelihood-free, simulation-based w CDM inference with neural compression of weak-lensing map statistics

We present simulation-based cosmological wcold dark matter (wCDM) inference using dark energy survey year 3 weak-lensing maps, via neural data compression of weak-lensing map summary statistics: power spectra, peak counts, and direct map-level compression/inference with convolutional neural networks (CNN). Using simulation-based inference, also known as likelihood-free or implicit inference, we use forward-modelled mock data to estimate posterior probability distributions of unknown parameters. This approach allows all statistical assumptions and uncertainties to be propagated through the forward-modelled mock data; these include sky masks, non-Gaussian shape noise, shape measurement bias, source galaxy clustering, photometric redshift uncertainty, intrinsic galaxy alignments, non-Gaussian density fields, neutrinos, and non-linear summary statistics. We include a series of tests to validate our inference results. This paper also describes the Gower Street simulation suite: 791 full-sky pkdgrav3 dark matter simulations, with cosmological model parameters sampled with a mixed active-learning strategy, from which we construct over 3000 mock dark energy survey lensing data sets. For wCDM inference, for which we allow –1 < w < –$\frac{1}{3}$⁠, our most constraining result uses power spectra combined with map-level (CNN) inference. Using gravitational lensing data only, this map-level combination gives Ω m = 0.283$^{+0.020}_{–0.027}$⁠, S 8 = 0.804$^{+0.025}_{–0.017⁠}$, and w < –0.80 (with a 68 per cent credible interval); compared to the power spectrum inference, this is more than a factor of two improvement in dark energy parameter (Ω⁠ DE , w⁠) precision.

79 ASTRONOMY AND ASTROPHYSICS↗

DOE OSTI2026

The Dark Energy Survey supernova program: a reanalysis of cosmology results and evidence for evolving dark energy with an updated Type Ia supernova calibration

We present improved cosmological constraints from a re-analysis of the Dark Energy Survey (DES) 5-year sample of Type Ia supernovae (DES-SN5YR). This re-analysis includes an improved photometric cross-calibration, recent white dwarf observations to cross-calibrate between DES and low-redshift surveys, retraining the salt3 light-curve model and fixing a numerical approximation in the host-galaxy colour law. Our fully recalibrated sample, which we call DES-Dovekie, comprises ~1600 likely Type Ia SNe from DES and ~200 low-redshift SNe from other surveys. With DES-Dovekie, we obtain Ω m = 0.330 ± 0.015 in flat Lambda-cold dark matter (⁠ΛCDM) which changes Ω m by –0.022 compared to DES-SN5YR. Combining DES-Dovekie with cosmic microwave background data from Planck, Atacama Cosmology Telescope, and South Pole Telescope and the DESI DR2 measurements in a flat CDM cosmology, we find ω 0 = –0.803 ± 0.054 and ω a = –0.72 ± 0.21⁠. Our results hold a significance of 3.2σ, reduced from 4.2σ for DES-SN5YR, to reject the null hypothesis that the data are compatible with the cosmological constant. This significance is equivalent to a Bayesian model preference odds of approximately 5:1 in favour of the flat ω 0 ω a CDM model. Using generally accepted thresholds for model preference, our updated data exhibits only a weak preference for evolving dark energy.

dark energy↗

DOE OSTI2025

Evidence for large baryonic feedback at low and intermediate redshifts from kinematic Sunyaev-Zel’dovich observations with ACT and DESI photometric galaxies

Recent advances in cosmological observations have provided an unprecedented opportunity to investigate the distribution of baryons relative to the underlying matter. In this work, we show that the gas is more extended than the dark matter, and the amount of baryonic feedback at $z \lesssim 1$ disfavors low-feedback models such as that of state-of-the-art hydrodynamical simulation IllustrisTNG compared with high-feedback models such as that of the original Illustris simulation. This has important implications for bridging the gap between theory and observations and understanding galaxy formation and evolution. Furthermore, a better grasp of the baryon-dark matter link is critical to future cosmological analyses, which are currently impeded by our limited knowledge of baryonic feedback. Here, we measure the kinematic Sunyaev-Zel'dovich (kSZ) effect from the Atacama Cosmology Telescope (ACT), stacked on the luminous red galaxy (LRG) sample of the Dark Energy Spectroscopic Instrument (DESI) imaging survey. This is the first analysis to use photometric redshifts for reconstructing galaxy velocities. Due to the large number of galaxies comprising the DESI imaging survey, this is the highest signal-to-noise stacked kSZ measurement to date: we detect the signal at 13$σ$, finding strong evidence that the gas is more spread out than the dark matter, as well as a preference for larger feedback compared to some commonly used state-of-the-art hydrodynamical simulations. Here, our work opens up the possibility of recalibrating large hydrodynamical simulations using the kSZ effect. In addition, our findings highlight the importance of properly accounting for baryonic feedback with future surveys such as LSST through direct probes such as the kSZ, and shed light on long-standing enigmas in astrophysics, such as the “missing baryon” problem.

79 ASTRONOMY AND ASTROPHYSICS↗