LARgE Survey – II. The dark matter haloes and the progenitors and descendants of ultramassive passive galaxies at cosmic noon
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- Gurpreet Kaur Cheema
- Institute for Computational Astrophysics and Department of Astronomy and Physics, Saint Mary’s University, 923 Robie Street, Halifax NS B3H 3C 3, Canada
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- Marcin Sawicki
- Institute for Computational Astrophysics and Department of Astronomy and Physics, Saint Mary’s University, 923 Robie Street, Halifax NS B3H 3C 3, Canada
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- Liz Arcila-Osejo
- Institute for Computational Astrophysics and Department of Astronomy and Physics, Saint Mary’s University, 923 Robie Street, Halifax NS B3H 3C 3, Canada
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- Anneya Golob
- Institute for Computational Astrophysics and Department of Astronomy and Physics, Saint Mary’s University, 923 Robie Street, Halifax NS B3H 3C 3, Canada
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- Thibaud Moutard
- Institute for Computational Astrophysics and Department of Astronomy and Physics, Saint Mary’s University, 923 Robie Street, Halifax NS B3H 3C 3, Canada
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- Stéphane Arnouts
- Laboratoire d’Astrophysique de Marseille, 38 rue Frederic Joliot Curie, Université Aix-Marseille, Marseille F-13388, France
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- Jean Coupon
- Astronomy Department, University of Geneva, Chemin d’Ecogia 16, CH-1290 Versoix, Switzerland
抄録
<jats:title>ABSTRACT</jats:title> <jats:p>We use a 27.6 deg2 survey to measure the clustering of gzKs-selected quiescent galaxies at z ∼ 1.6, focusing on ultramassive quiescent galaxies. We find that z ∼ 1.6 Ultra-Massive Passively Evolving Galaxies (UMPEGs), which have Ks(AB) < 19.75 (stellar masses of M⋆$\gtrsim10^{11.4}\,\mathrm{ M}_{\odot }$ and mean <M⋆> = 1011.5 M⊙), cluster more strongly than any other known galaxy population at high redshift. Comparing their correlation length, r0 = 29.77 ± 2.75h−1Mpc, with the clustering of dark matter (DM) haloes in the Millennium XXL N-body simulation suggests that these z ∼ 1.6 UMPEGs reside in DM haloes of mass Mh ∼ 1014.1h−1M⊙. Such very massive z ∼ 1.6 haloes are associated with the ancestors of z ∼ 0 massive galaxy clusters such as the Virgo and Coma clusters. Given their extreme stellar masses and lack of companions with comparable mass, we surmise that these UMPEGs could be the already-quenched central massive galaxies of their (proto)clusters. We conclude that with only a modest amount of further growth in their stellar mass, z ∼ 1.6 UMPEGs could be the progenitors of some of the massive central galaxies of present-day massive galaxy clusters observed to be already very massive and quiescent near the peak epoch of the cosmic star formation.</jats:p>
収録刊行物
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- Monthly Notices of the Royal Astronomical Society
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Monthly Notices of the Royal Astronomical Society 494 (1), 804-818, 2020-02-28
Oxford University Press (OUP)