Investigating the growing population of massive quiescent galaxies at cosmic noon

Sherman, Sydney; Jogee, Shardha; Florez, Jonathan; Stevans, Matthew L.; Kawinwanichakij, Lalitwadee; Wold, Isak; Finkelstein, Steven L.; Papovich, Casey; Ciardullo, Robin; Grönwall, C.; Cora, S. A.; Hough, Tomás; Vega-Martínez, Cristian A

doi:10.1093/mnras/staa3167

Cited by 26 publications

(60 citation statements)

References 138 publications

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“…1 reveals that Illustris-1 galaxies are typically thicker and thus less susceptible to bar instability. In general, the TNG galaxies agree better with observational properties (Nelson et al 2018), except for overquenching (Angthopo et al 2020;Sherman et al 2020), which is most probably due to too strong kinetic feedback from active galactic nuclei, combined with high thresholds for the seed black hole mass and halo mass. This may be of concern in the case of galaxies of our class C, which may rid themselves of the gas too efficiently and form bars too easily.…”

Section: Discussionmentioning

confidence: 62%

Bar-like galaxies in IllustrisTNG

Lokas

2021

Preprint

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We study a sample of bar-like galaxies in the Illustris TNG100 simulation, in which almost the whole stellar component is in the form of a prolate spheroid. The sample is different from the late-type barred galaxies studied before. In addition to the requirement of a high enough stellar mass and resolution, the 277 galaxies were selected based on the single condition of a low enough ratio of the intermediate to long axis of the stellar component. We followed the mass and shape evolution of the galaxies as well as their interactions with other objects and divided them into three classes based on the origin of the bar and the subsequent history. In galaxies of class A (comprising 28% of the sample), the bar was induced by an interaction with a larger object, most often a cluster or group central galaxy, and the galaxies were heavily stripped of dark matter and gas. In classes B and C (27% and 45% of the sample, respectively) the bars were induced by a merger or a passing satellite, or they were formed by disk instability. Class B galaxies were then partially stripped of mass, while those of class C evolved without strong interactions, thus retaining their dark matter and gas in the outskirts. We illustrate the properties of the different classes with three representative examples of individual galaxies. In spite of the different evolutionary histories, the bars are remarkably similar in strength, length, and formation times. The gas fraction in the baryonic component within two stellar half-mass radii at the time of bar formation is always below 0.4 and usually very low, which confirms in the cosmological context the validity of this threshold, which has previously been identified in controlled simulations. Observational counterparts of these objects can be found among early-type fast rotators, S0 galaxies, or red spirals with bars.

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Section: Discussionmentioning

confidence: 62%

Bar-like galaxies in IllustrisTNG

Lokas

2021

Preprint

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“…An often used SFR threshold for defining quiescence is 1 dex below the main sequence (see e.g., Morselli et al 2019;Donnari et al 2019;Sherman et al 2020) which we show for measurements in an aperture of 30 kpc in Figure 1 together with the Franx et al (2008) criterion sSFR < 0.3 × 𝐻 (𝑡) (see also Lotz et al 2021, in particular on a study in Magneticum), that is log(sSFR × yr) ≈ −10.0 at 𝑧 = 2.75. As the figure shows, in M3 the MS-based quiescence threshold is 0.3 dex lower than the Franx et al (2008) sSFR threshold over the full mass range.…”

Section: Selection Of Quiescent Galaxies In Simulationsmentioning

confidence: 52%

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

Lustig¹,

Strazzullo²,

Remus³

et al. 2022

Preprint

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We study stellar population and structural properties of massive log(𝑀 ★ /𝑀 ) > 11 galaxies at 𝑧 ≈ 2.7 in the Magneticum (box 3) and IllustrisTNG (TNG100, TNG300) hydrodynamical simulations. We find stellar mass functions broadly consistent with observations, with no scarcity of massive, quiescent galaxies at 𝑧 ≈ 2.7, but with a higher quiescent galaxy fraction at high masses in IllustrisTNG. Average ages of simulated quiescent galaxies are between ≈ 0.8 and 1.0 Gyr, older by a factor ≈ 2 than observed in spectroscopically-confirmed quiescent galaxies at similar redshift. Besides being potentially indicative of issues with star-formation recipes in simulations, this discrepancy might also be partly explained by limitations in the estimation of observed ages. We investigate the purity of simulated UVJ rest-frame color-selected massive quiescent samples with photometric uncertainties typical of deep surveys (e.g., COSMOS). We find evidence for significant contamination (up to 60 percent) by dusty star-forming galaxies in the UVJ region that is typically populated by older quiescent sources. Furthermore, simulations suggest that the completeness of UVJ-selected quiescent samples at this redshift may be reduced by ≈ 30 percent due to a high fraction of young quiescent galaxies not entering the UVJ quiescent region. Massive, quiescent galaxies in simulations have on average lower angular momenta and higher projected axis ratios and concentrations than star-forming counterparts. Average sizes of simulated quiescent galaxies are relatively close to observed ones, and broadly consistent within the uncertainties. The average size ratio of quiescent and star-forming galaxies in the probed mass range is formally consistent with observations, although this result is partly affected by poor statistics.

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“…This fraction is consistent with the results of B19, who found that their emission-line sample only contained ∼ 30% of the galaxies with photometric redshifts between 1.90 < z < 2.35 in the 3D-HST catalog. While a subset of the photometric redshift sample is quiescent, the data of Sherman et al (2020) show that the quiescent fraction is not sufficient to explain the discrepancy. The B19 analysis also found strong trends with rest-frame near-IR continuum magnitude and dust content, where the fraction of emission-line galaxies fell to zero at bright magnitudes and large A V values.…”

Section: Calibrating the Sfr Relationmentioning

confidence: 94%

The $z \sim 2$ $\rm{[O\ III]}$ Luminosity Function of Grism-selected Emission-line Galaxies

Bowman,

Ciardullo,

Zeimann

et al. 2021

Preprint

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Upcoming missions such as Euclid and the Nancy Grace Roman Space Telescope (Roman) will use emission-line selected galaxies to address a variety of questions in cosmology and galaxy evolution in the z > 1 universe. The optimal observing strategy for these programs relies upon knowing the number of galaxies that will be found and the bias of the galaxy population. Here we measure the [O III] λ5007 luminosity function for a vetted sample of 1951 m J+JH+H < 26 galaxies with unambiguous redshifts between 1.90 < z < 2.35, which were selected using HST/WFC3 G141 grism frames made available by the 3D-Hubble Space Telescope program. These systems are directly analogous to the galaxies that will be identified by the Euclid and Roman missions, which will utilize grism spectroscopy to find [O III] λ5007-emitting galaxies at 0.8 ∼ < z ∼ < 2.7 and 1.7 ∼ < z ∼ < 2.8, respectively. We interpret our results in the context of the expected number counts for these upcoming missions. Finally, we combine our dust-corrected [O III] luminosities with rest-frame ultraviolet star formation rates to present the first estimate of the SFR density associated with 1.90 < z < 2.35 [O III]-emitting galaxies. We find that these grism-selected galaxies contain roughly half of the total star formation activity at z ∼ 2.

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Investigating the growing population of massive quiescent galaxies at cosmic noon

Cited by 26 publications

References 138 publications

Bar-like galaxies in IllustrisTNG

Bar-like galaxies in IllustrisTNG

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

The $z \sim 2$ $\rm{[O\ III]}$ Luminosity Function of Grism-selected Emission-line Galaxies

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