Massive quiescent galaxies at $z\sim3$: a comparison of selection, stellar population and structural properties with simulation predictions

Lustig, P.; Strazzullo, V.; Remus, Rhea-Silvia; D’Eugenio, Chiara; Daddi, E.; Burkert, Andreas; Lucia, G. De; Delvecchio, I.; Dolag, K.; Fontanot, Fabio; Gobat, R.; Mohr, J. J.; Onodera, Makoto; Pannella, M.; Pillepich, Annalisa; Renzini, A.

doi:10.48550/arxiv.2201.09068

Cited by 6 publications

(5 citation statements)

References 140 publications

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“…Deep near-infrared photometric surveys of the last decade have suggested larger numbers of massive galaxies at high redshifts than predicted by cosmological galaxy simulations (e.g., Muzzin et al 2013a;Straatman et al 2014;Sherman et al 2019;Marsan et al 2022). More recent simulations have better agreement with observations, but the discrepancy is still a factor of a few to 10 at the highest masses (though see Donnari et al 2021;Lustig et al 2022). In the last several years, spectroscopic confirmation of a handful of galaxies with stellar masses of *  ( ) M M log > 11 and at redshifts of z > 3 have shown that such galaxies do indeed exist in nonnegligible numbers (Marsan et al 2015(Marsan et al , 2017Glazebrook et al 2017;Schreiber et al 2018a;Tanaka et al 2019;Forrest et al 2020aForrest et al , 2020bValentino et al 2020), but a robust measurement of the number density of such galaxies is still lacking.…”

Section: Introductionmentioning

confidence: 85%

MAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3*

Forrest

Wilson

Muzzin

et al. 2022

ApJ

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In this work, we publish stellar velocity dispersions, sizes, and dynamical masses for eight ultramassive galaxies (UMGs; log ( M * / M ⊙ ) > 11), z ≳ 3) from the Massive Ancient Galaxies At z > 3 NEar-infrared (MAGAZ3NE) Survey, more than doubling the number of such galaxies with velocity dispersion measurements at this epoch. Using the deep Keck/MOSFIRE and Keck/NIRES spectroscopy of these objects in the H and K bandpasses, we obtain large velocity dispersions of ∼400 km s−1 for most of the objects, which are some of the highest stellar velocity dispersions measured and ∼40% larger than those measured for galaxies of similar mass at z ∼ 1.7. The sizes of these objects are also smaller by a factor of 1.5–3 compared to this same z ∼ 1.7 sample. We combine these large velocity dispersions and small sizes to obtain dynamical masses. The dynamical masses are similar to the stellar masses of these galaxies, consistent with a Chabrier initial mass function (IMF). Considered alongside previous studies of massive quiescent galaxies across 0.2 < z < 4.0, there is evidence for an evolution in the relation between the dynamical mass–stellar mass ratio and velocity dispersion as a function of redshift. This implies an IMF with fewer low-mass stars (e.g., Chabrier IMF) for massive quiescent galaxies at higher redshifts in conflict with the bottom-heavy IMF (e.g., Salpeter IMF) found in their likely z ∼ 0 descendants, though a number of alternative explanations such as a different dynamical structure or significant rotation are not ruled out. Similar to data at lower redshifts, we see evidence for an increase of IMF normalization with velocity dispersion, though the z ≳ 3 trend is steeper than that for z ∼ 0.2 early-type galaxies and offset to lower dynamical-to-stellar mass ratios.

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Section: Introductionmentioning

confidence: 85%

MAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3*

Forrest

Wilson

Muzzin

et al. 2022

ApJ

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“…Although many studies have been conducted to determine the physical properties and quenching processes of ancient quiescent galaxies (e.g., van Dokkum et al 2015;Park et al 2021;Zhang et al 2022;Lustig et al 2022), TNG provides a means to address a cosmological enigma yet to be resolved in this field, namely the lives and quenching mechanisms of the very first quiescent galaxies in our Universe. The most massive galaxies in the Universe today host maximally old stars (e.g., Thomas et al 2010;McDermid et al 2015), suggesting that they are relics of very early star formation and the early truncation thereof.…”

Section: Introductionmentioning

confidence: 99%

The first quiescent galaxies in TNG300

Hartley

Nelson

Suess

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We identify the first quiescent galaxies in TNG300, the largest volume of the IllustrisTNG cosmological simulation suite, and explore their quenching processes and time evolution to z = 0. We find that the first quiescent galaxies with stellar masses M* > 3 × 1010M⊙ and specific star formation rates sSFR <10−11yr−1 emerge at z ∼ 4.2 in TNG300. Suppression of star formation in these galaxies begins with a thermal mode of AGN feedback at z ∼ 6, and a kinetic feedback mode acts in each galaxy by z ∼ 4.7 to complete the quenching process, which occurs on a time-scale of ∼0.35 Gyr. Surprisingly, we find that the majority of these galaxies are not the main progenitors of their z = 0 descendants; instead, four of the five galaxies fall into more massive galaxies in subsequent mergers at a range of redshifts 2.5 < z < 0.2. By z = 0, these descendants are the centres of galaxy clusters with average stellar masses of 8 × 1011M⊙. We make predictions for the first quenched galaxies to be located by the James Webb Space Telescope (JWST).

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“…As shown in previous studies, the galaxy physics implemented in the Magneticum simulations leads to successfully reproducing basic galaxy properties like the stellar mass-function (Naab & Ostriker 2017;Lustig et al 2022), the environmental impact of galaxy clusters on galaxy properties (Lotz et al 2019) and the appearance of post-starburst galaxies (Lotz et al 2021) as well as the associated AGN population at various redshifts (Hirschmann et al 2014;Steinborn et al 2016;Biffi et al 2018a). At cluster scale, the Magneticum simulations has demonstrated to reproduce the observable X-ray luminosityrelation (Biffi et al 2013), the pressure profile of the ICM (Gupta et al 2017) and the chemical composition (Dolag et al 2017;Biffi et al 2018b) of the ICM, the high concentration observed in fossil groups (Ragagnin et al 2019), as well as the gas properties in between galaxy clusters (Biffi et al 2021).…”

Section: Cosmological Simulations: Magneticummentioning

confidence: 58%

Mapping ‘out-of-the-box’ the properties of the baryons in massive halos

Angelinelli

Ettori

Dolag

et al. 2022

A&A

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We study the distributions of the baryons in massive halos (Mvir > 1013 h−1 M⊙) in the Magneticum suite of smoothed particle hydrodynamical cosmological simulations, out to the unprecedented radial extent of 10R500, c. We confirm that, under the action of non-gravitational physical phenomena, the baryon mass fraction is lower in the inner regions (< R500, c) of increasingly less massive halos, and rises moving outwards, with values that span from 51% (87%) of the cosmological value in the regions around R500, c to 95% (100%) at 10R500, c in the systems with the lowest (highest; Mvir ∼ 5 × 1014 h−1 M⊙) masses. The galaxy groups almost match the gas (and baryon) fraction measured in the most massive halos only at very large radii (r > 6R500, c), where the baryon depletion factor Ybar = fbar/(Ωb/Ωm) approaches the value of unity, expected for ‘closed-box’ systems. We find that both the radial and mass dependence of the baryon, gas, and hot depletion factors are predictable and follow a simple functional form. The star mass fraction is higher in less massive systems, decreases systematically with increasing radii, and reaches a constant value of Ystar ≈ 0.09, where the gas metallicity is also constant, regardless of the host halo mass, as a result of the early (z > 2) enrichment process.

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Massive quiescent galaxies at $z\sim3$: a comparison of selection, stellar population and structural properties with simulation predictions

Cited by 6 publications

References 140 publications

MAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3*

MAGAZ3NE: High Stellar Velocity Dispersions for Ultramassive Quiescent Galaxies at z ≳ 3*

The first quiescent galaxies in TNG300

Mapping ‘out-of-the-box’ the properties of the baryons in massive halos

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