Cosmic Vine: A z = 3.44 large-scale structure hosting massive quiescent galaxies
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Cosmic Vine : A z = 3.44 large-scale structure hosting massive quiescent galaxies. / Jin, Shuowen; Sillassen, Nikolaj B.; Magdis, Georgios E.; Brinch, Malte; Shuntov, Marko; Brammer, Gabriel; Gobat, Raphael; Valentino, Francesco; Carnall, Adam C.; Lee, Minju; Vijayan, Aswin P.; Gillman, Steven; Kokorev, Vasily; Le Bail, Aurélien; Greve, Thomas R.; Gullberg, Bitten; Gould, Katriona M.L.; Toft, Sune.
I: Astronomy & Astrophysics, Bind 683, L4, 29.02.2024.Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt
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TY - JOUR
T1 - Cosmic Vine
T2 - A z = 3.44 large-scale structure hosting massive quiescent galaxies
AU - Jin, Shuowen
AU - Sillassen, Nikolaj B.
AU - Magdis, Georgios E.
AU - Brinch, Malte
AU - Shuntov, Marko
AU - Brammer, Gabriel
AU - Gobat, Raphael
AU - Valentino, Francesco
AU - Carnall, Adam C.
AU - Lee, Minju
AU - Vijayan, Aswin P.
AU - Gillman, Steven
AU - Kokorev, Vasily
AU - Le Bail, Aurélien
AU - Greve, Thomas R.
AU - Gullberg, Bitten
AU - Gould, Katriona M.L.
AU - Toft, Sune
N1 - Publisher Copyright: © The Authors 2024.
PY - 2024/2/29
Y1 - 2024/2/29
N2 - We report the discovery of a large-scale structure at z = 3.44 revealed by JWST data in the Extended Groth Strip (EGS) field. This structure, called the Cosmic Vine, consists of 20 galaxies with spectroscopic redshifts at 3.43 < z < 3.45 and six galaxy overdensities (4−7σ) with consistent photometric redshifts, making up a vine-like structure extending over a ∼4 × 0.2 pMpc2 area. The two most massive galaxies (M∗ ≈ 1010.9 M ) of the Cosmic Vine are found to be quiescent with bulge-dominated morphologies (B/T > 70%). Comparisons with simulations suggest that the Cosmic Vine would form a cluster with halo mass Mhalo > 1014M at z = 0, and the two massive galaxies are likely forming the brightest cluster galaxies (BCGs). The results unambiguously reveal that massive quiescent galaxies can form in growing large-scale structures at z > 3, thus disfavoring the environmental quenching mechanisms that require a virialized cluster core. Instead, as suggested by the interacting and bulge-dominated morphologies, the two galaxies are likely quenched by merger-triggered starburst or active galactic nucleus (AGN) feedback before falling into a cluster core. Moreover, we found that the observed specific star formation rates of massive quiescent galaxies in z > 3 dense environments are one to two orders of magnitude lower than that of the BCGs in the TNG300 simulation. This discrepancy potentially poses a challenge to the models of massive cluster galaxy formation. Future studies comparing a large sample with dedicated cluster simulations are required to solve the problem.
AB - We report the discovery of a large-scale structure at z = 3.44 revealed by JWST data in the Extended Groth Strip (EGS) field. This structure, called the Cosmic Vine, consists of 20 galaxies with spectroscopic redshifts at 3.43 < z < 3.45 and six galaxy overdensities (4−7σ) with consistent photometric redshifts, making up a vine-like structure extending over a ∼4 × 0.2 pMpc2 area. The two most massive galaxies (M∗ ≈ 1010.9 M ) of the Cosmic Vine are found to be quiescent with bulge-dominated morphologies (B/T > 70%). Comparisons with simulations suggest that the Cosmic Vine would form a cluster with halo mass Mhalo > 1014M at z = 0, and the two massive galaxies are likely forming the brightest cluster galaxies (BCGs). The results unambiguously reveal that massive quiescent galaxies can form in growing large-scale structures at z > 3, thus disfavoring the environmental quenching mechanisms that require a virialized cluster core. Instead, as suggested by the interacting and bulge-dominated morphologies, the two galaxies are likely quenched by merger-triggered starburst or active galactic nucleus (AGN) feedback before falling into a cluster core. Moreover, we found that the observed specific star formation rates of massive quiescent galaxies in z > 3 dense environments are one to two orders of magnitude lower than that of the BCGs in the TNG300 simulation. This discrepancy potentially poses a challenge to the models of massive cluster galaxy formation. Future studies comparing a large sample with dedicated cluster simulations are required to solve the problem.
KW - galaxies: clusters: general
KW - galaxies: evolution
KW - galaxies: formation
KW - galaxies: high-redshift
KW - galaxies: structure
U2 - 10.1051/0004-6361/202348540
DO - 10.1051/0004-6361/202348540
M3 - Journal article
AN - SCOPUS:85186589599
VL - 683
JO - Astronomy & Astrophysics
JF - Astronomy & Astrophysics
SN - 0004-6361
M1 - L4
ER -
ID: 389364994