Bimodal morphologies of massive galaxies at the core of a protocluster at z = 3.09 and the strong size growth of a brightest cluster galaxy

Kubo, Mariko; Yamada, Tōru; Ichikawa, Takashi; Kajisawa, Masaru; Matsuda, Yoshihisa; Tanaka, Ichi; Umehata, Hideki

doi:10.1093/mnras/stx920

Cited by 18 publications

(34 citation statements)

References 118 publications

(168 reference statements)

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“…Its spectroscopic redshift is limited to z spec = 2.7 or 3.0-3.15 by detecting the 4000 Å break (Kubo et al 2015). We took a high-resolution K′-band image of the target by using the adaptive optics AO188 and infrared camera and spectrograph (IRCS) on the Subaru telescope, and found that its effective radius (r eff ) is 1.01 ± 0.04 kpc (Kubo et al 2017). Uniquely, it is likely in an extremely dense group of massive galaxies and SMGs identified by follow-up NIR spectroscopic observations of a 1.1 mm source found with ASTE/AzTEC (Kubo et al 2016;hereafter AzTEC14 group).…”

Section: Targetmentioning

confidence: 99%

“…The spectroscopic confirmation of ADF22-QG1 in the AzTEC14 group and newly confirmed [O III] emitters, which are possible evidence of interactions between ADF22-QG1 and K15d, further support such an early BCG assembly scenario via multiple mergers. We discussed the size and stellar mass growths of ADF22-QG1 via mergers based on the observed sizes and stellar masses of the AzTEC14 group members in Kubo et al (2017). Assuming no further stellar mass and size growth in each group member, and that all mergers are dry, the size and stellar mass of ADF22-QG1 can increase by 3-4 times and double via mergers of all the group members, respectively.…”

Section: 3mentioning

confidence: 99%

“…The environmental differences of the galaxy population at z ∼ 4 have been shown statistically by using the deep and wide optical survey of the Hyper Suprime-Cam Subaru Strategic Program survey (Toshikawa et al 2018;Kubo et al 2019;Ito et al 2020). However, morphologies of only a small number of massive quiescent galaxies have been studied (see Zirm et al 2008and Kubo et al 2017, and also Strazzullo et al 2013and Mei et al 2015 including mature clusters at z ∼ 2), and the detailed spectral characteristics of massive quiescent galaxies have not yet been characterized in protoclusters.…”

Section: Introductionmentioning

confidence: 99%

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A Massive Quiescent Galaxy Confirmed in a Protocluster at z = 3.09

Kubo

Umehata

Matsuda

et al. 2021

ApJ

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We report a massive quiescent galaxy at = -+ z 3.0922 spec 0.004 0.008 spectroscopically confirmed at a protocluster in the SSA22 field by detecting the Balmer and Ca II absorption features with the multi-object spectrometer for infrared exploration on the Keck I telescope. This is the most distant quiescent galaxy confirmed in a protocluster to date. We fit the optical to mid-infrared photometry and spectrum simultaneously with spectral energy distribution (SED) models of parametric and nonparametric star formation histories (SFHs). Both models fit the observed SED well and confirm that this object is a massive quiescent galaxy with a stellar mass of = -+  M M log 11.26 0.04 0.03 ( )  and -+ 11.54 0.00 0.03 , and a star formation rate of SFR/M e yr −1 < 0.3 and = -+0.01 0.01 0.03 for parametric and nonparametric models, respectively. The SFH from the former modeling is described as an instantaneous starburst whereas that of the latter modeling is longer-lived, but both models agree with a sudden quenching of the star formation at ∼0.6 Gyr ago. This massive quiescent galaxy is confirmed in an extremely dense group of galaxies predicted as a progenitor of a brightest cluster galaxy formed via multiple mergers in cosmological numerical simulations. We discover three new plausible [O III]λ5007 emitters at 3.0791 z spec 3.0833 serendipitously detected around the target. Two of them just between the target and its nearest massive galaxy are possible evidence of their interactions. They suggest the future great size and stellar mass evolution of this massive quiescent galaxy via mergers.Unified Astronomy Thesaurus concepts: Galaxy evolution (594); Galaxy environments (2029); Giant elliptical galaxies (651); Protoclusters (1297)

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Section: Targetmentioning

confidence: 99%

Section: 3mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A Massive Quiescent Galaxy Confirmed in a Protocluster at z = 3.09

Kubo

Umehata

Matsuda

et al. 2021

ApJ

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“…Mihos & Hernquist 1996;Teyssier et al 2010;Bournaud et al 2015). So far, many studies have investigated the environmental dependence of mass and size evolution in high-z clusters (Papovich et al 2012;Lani et al 2013;Gobat et al 2013;Newman et al 2014;Belli et al 2014;Tran et al 2017;Kubo et al 2017), however, the conclusion is still controversial, especially in rich systems of star-forming galaxies like USS 1558. The existing F160W image in USS 1558 taken by HST ( Fig.…”

Section: Mass-size Distributionmentioning

confidence: 99%

MAHALO Deep Cluster Survey I. Accelerated and enhanced galaxy formation in the densest regions of a protocluster at z = 2.5

Shimakawa

Kodama

Hayashi

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We carried out deep Hα narrowband imaging with 10 hours net integrations towards the young protocluster, USS1558−003 at z = 2.53 with the Subaru Telescope. This system is composed of four dense groups with massive local overdensities, traced by 107 Hα emitters (HAEs) with stellar masses and dust-corrected star formation rates down to 1 × 10 8 M and 3 M yr −1 , respectively. We have investigated the environmental dependence of various physical properties within the protocluster by comparing distributions of HAEs in higher and lower densities with a standard Kolmogorov-Smirnov test. At 97% confidence level, we find enhanced star formation across the star-forming main sequence of HAEs living in the most extreme 'supergroup', corresponding to the top quartile of overdensities. Furthermore, we derive distribution functions of Hα luminosity and stellar mass in group and intergroup regions, approximately corresponding to 30 times and 8 times higher densities than the general field. As a consequence, we identify 0.7 and 0.9 dex higher cutoffs in Hα luminosity and stellar mass functions in the dense groups, respectively. On the other hand, HAEs in the intergroup environment of the protocluster show similar distribution functions to those of field galaxies despite residing in significant overdensities. In the early phase of cluster formation, as inferred from our results, the densest parts in the protocluster have had an accelerated formation of massive galaxies. We expect that these eventually grow and transform into early-type galaxies at the bright end of the red sequence as seen in present-day rich clusters of galaxies.

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“…Our present work lays out an effective strategy to unveil the evolutionary pathways of MGs by exploiting the increased statistics of MGs that will become available from future observations. Data for MGs are in fact at present quite sparse and uncertain at 1 (e.g., Kawinwanichakĳ et al 2020), and effective radii have been measured for only a handful of MGs at 2 (e.g., Kubo et al 2017;Patel et al 2017;Faisst et al 2017;Mowla et al 2018;Stockmann et al 2020;Lustig et al 2021).…”

Section: Introductionmentioning

confidence: 99%

The evolution of compact massive quiescent and star-forming galaxies derived from the Re–Rh and Mstar–Mh relations

Zanisi

Shankar

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The mean size ( effective radius Re) of Massive Galaxies (MGs, Mstar > 1011.2M⊙) is observed to increase steadily with cosmic time. It is still unclear whether this trend originates from the size growth of individual galaxies (via, e.g., mergers and/or AGN feedback) or from the inclusion of larger galaxies entering the selection at later epochs (progenitor bias). We here build a data-driven, flexible theoretical framework to probe the structural evolution of MGs. We assign galaxies to dark matter haloes via stellar mass-halo mass (SMHM) relations with varying high-mass slopes and scatters σSMHM in stellar mass at fixed halo mass, and assign sizes to galaxies using an empirically-motivated, constant and linear relationship between Re and the host dark matter halo radius Rh. We find that: 1) the fast mean size growth of MGs is well reproduced independently of the shape of the input SMHM relation; 2) the numbers of compact MGs grow steadily until z ≳ 2 and fall off at lower redshifts, suggesting a lesser role of progenitor bias at later epochs; 3) a time-independent scatter σSMHM is consistent with a scenario in which compact starforming MGs transition into quiescent MGs in a few 108yr with a negligible structural evolution during the compact phase, while a scatter increasing at high redshift implies significant size growth during the starforming phase. A robust measurement of the size function of MGs at high redshift can set strong constraints on the scatter of the SMHM relation and, by extension, on models of galaxy evolution.

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Bimodal morphologies of massive galaxies at the core of a protocluster at z = 3.09 and the strong size growth of a brightest cluster galaxy

Cited by 18 publications

References 118 publications

A Massive Quiescent Galaxy Confirmed in a Protocluster at z = 3.09

A Massive Quiescent Galaxy Confirmed in a Protocluster at z = 3.09

MAHALO Deep Cluster Survey I. Accelerated and enhanced galaxy formation in the densest regions of a protocluster at z = 2.5

The evolution of compact massive quiescent and star-forming galaxies derived from the Re–Rh and Mstar–Mh relations

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