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Predicted future fate of COSMOS galaxy protoclusters over 11 Gyr with constrained simulations

Nature Astronomy volume 6, pages 857–865 (2022)Cite this article

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Abstract

Cosmological simulations are crucial tools in studying the Universe, but they typically do not directly match real observed structures. Constrained cosmological simulations, on the other hand, are designed to match the observed distribution of galaxies. Here we present constrained simulations based on spectroscopic surveys at a redshift of z ≈ 2.3, corresponding to an epoch of nearly 11 Gyr ago. This allows us to ‘fast-forward’ the simulation to our present day and study the evolution of observed cosmic structures self-consistently. We confirm that several previously reported protoclusters will evolve into massive galaxy clusters by our present epoch, including the ‘Hyperion’ structure that we predict will collapse into a giant filamentary supercluster spanning 100 Mpc. We also discover previously unknown protoclusters with lower final masses than are typically detectable by other methods that nearly double the number of known protoclusters within this volume. Constrained simulations, applied to future high-redshift datasets, represent a unique opportunity for studying early structure formation and matching galaxy properties between high and low redshifts.

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Fig. 1: Matter density field of the COSMOS volume in the observed redshift range of 2.00 ≤ zobs ≤ 2.52 from 1 realization out of 50 constrained simulations.
Fig. 2: Two examples of massive Mvir ≥ 2 × 1014 h−1 M⊙ halos in our constrained simulations.
Fig. 3: 3D visualizations of the Hyperion supercluster filament for 4 realizations at z = 0.
Fig. 4: Protocluster density map from all 50 COSTCO realizations.

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Data availability

The data products generated for this study are available at https://zenodo.org/record/6425013.

Code availability

Analysis codes used for this study are available at https://github.com/gmetin/COSTCO.

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Acknowledgements

The authors thank P. Behroozi and D. Potter for their support with Rockstar and PKDGRAV3, respectively. M.A. thanks T. Nishimichi, M. Takada and V. Vardanyan for useful discussions. M.A. was supported by JSPS Kakenhi Grant JP21K13911. K.-G.L. acknowledges support from JSPS Kakenhi Grants JP18H05868 and JP19K14755. C.D.V. acknowledges support from the Spanish Ministry of Science and Innovation (MICIU/FEDER) through research grants PGC2018-094975-C22 and RYC-2015-18078. This research is based on observations undertaken at the European Southern Observatory Very Large Telescope under Large Program 175.A-0839 and has been supported by the Swiss National Science Foundation. Some of the material presented in this paper is based upon work supported by the National Science Foundation under Grant No. 1908422. This work was made possible by the World Premier International Research Center Initiative (WPI), MEXT, Japan.

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Authors and Affiliations

  1. Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, Kashiwa, Japan

    Metin Ata & Khee-Gan Lee

  2. Instituto de Astrofísica de Canarias, La Laguna, Spain

    Claudio Dalla Vecchia & Francisco-Shu Kitaura

  3. Departamento de Astrofísica, Universidad de La Laguna, La Laguna, Spain

    Claudio Dalla Vecchia & Francisco-Shu Kitaura

  4. INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Bologna, Italy

    Olga Cucciati

  5. Gemini Observatory, NSF’s NOIRLab, Hilo, HI, USA

    Brian C. Lemaux

  6. Department of Physics and Astronomy, University of California, Davis, CA, USA

    Brian C. Lemaux

  7. Institute for Advanced Research, Nagoya University, Nagoya, Japan

    Daichi Kashino

  8. Max Planck Institute for Astronomy, Heidelberg, Germany

    Thomas Müller

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Contributions

M.A. calculated the selection functions, initial conditions, simulations and halo catalogues and conducted the full analysis. M.A. and K.-G.L. conceptualized the analysis and wrote the paper. C.D.V. helped perform the simulations. F.-S.K. provided expertise about density field reconstructions. O.C., B.C.L. and D.K. provided the (partly) proprietary data and relevant literature. T.M. provided the visualizations. All authors reviewed the manuscript.

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Correspondence to Metin Ata.

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Nature Astronomy thanks Jorge Zavala and Miguel Aragón-Calvo for their contribution to the peer review of this work.

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Supplementary Figs. 1–5.

Supplementary Video 1

Summarizing video of the simulations, including two zoom-ins. Music credit: REDproductions/Pixabay.

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Ata, M., Lee, KG., Vecchia, C.D. et al. Predicted future fate of COSMOS galaxy protoclusters over 11 Gyr with constrained simulations. Nat Astron 6, 857–865 (2022). https://doi.org/10.1038/s41550-022-01693-0

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