On the formation of massive quiescent galaxies with diverse morphologies in the TNG50 simulation

Park, Minjung; Tacchella, Sandro; Nelson, Erica J.; Hernquist, Lars; Weinberger, Rainer; Diemer, Benedikt; Nelson, Dylan; Pillepich, Annalisa; Marinacci, Federico; Vogelsberger, Mark

doi:10.48550/arxiv.2112.07679

Cited by 7 publications

(7 citation statements)

References 104 publications

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“…Excitingly, the potential disconnect between quenching and morphological transformation as well as the large variety of mergerdriven kinematic changes in galaxies suggested here appear in line with predictions from large hydro-dynamical cosmological simulations such as EAGLE (e.g., Lagos et al 2018Lagos et al , 2022 IllustrisTNG (e.g., Tacchella et al 2019;Park et al 2021). However, it is important to note that some of these findings may be affected by spurious collisional heating (Ludlow et al 2021) and next generation/higher resolution runs are needed to fully confirm these scenarios and allow us to perform a quantitative comparison between observations and simulations (see also van de Sande et al 2019).…”

Section: Discussionsupporting

confidence: 83%

The physical connection between central stellar surface density and stellar spin in SAMI and MaNGA nearby galaxies

Cortese,

Fraser-McKelvie,

Woo

et al. 2022

Preprint

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The stellar surface density within the inner 1 kpc (Σ 1 ) has become a popular tool for understanding the growth of galaxies and its connection with the quenching of star formation. The emerging picture suggests that building a central dense core is a necessary condition for quenching. However, it is not clear whether changes in Σ 1 trace changes in stellar kinematics and the growth of dispersion-dominated bulges. In this paper, we combine imaging from the Sloan Digital Sky Survey with stellar kinematics from the Sydney-AAO Multi-object Integral-field unit (SAMI) and Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) surveys to quantify the correlation between Σ 1 and the proxy for stellar spin parameter within one effective radius (𝜆 𝑟 𝑒 ) for 1599 nearby galaxies. We show that, on the star-forming main sequence and at fixed stellar mass, changes in Σ 1 are mirrored by changes in 𝜆 𝑟 𝑒 . While forming stars, main sequence galaxies remain rotationally-dominated systems, with their Σ 1 increasing but their stellar spin staying either constant or slightly increasing. The picture changes below the main sequence, where Σ 1 and 𝜆 𝑟 𝑒 are no longer correlated. Passive systems show a narrower range of Σ 1 , but a wider range of 𝜆 𝑟 𝑒 compared to star-forming galaxies. Our results indicate that, from a structural point of view, passive galaxies are a more heterogeneous population than star-forming systems, and may have followed a variety of evolutionary paths. This also suggests that, if dispersion-dominated bulges still grow significantly at 𝑧 ∼0, this generally takes place during, or after, the quenching phase.

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Section: Discussionsupporting

confidence: 83%

The physical connection between central stellar surface density and stellar spin in SAMI and MaNGA nearby galaxies

Cortese,

Fraser-McKelvie,

Woo

et al. 2022

Preprint

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“…Interestingly, these major mergers did not quench the star formation of those galaxies (sSFR decreased significantly only after t max , see Figure 9). This is consistent with the results of Weinberger et al (2018); Park et al (2021) that major merger event is not a main cause of quenching in the TNG simulation.…”

Section: The Evolution History Of Morphology and Mergersupporting

confidence: 92%

Quenching of Massive Disk Galaxies in the IllustrisTNG Simulation

Xu,

Luo,

Kang

et al. 2022

Preprint

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A rare population of massive disk galaxies have been found to invade the red sequence dominated by early-type galaxies. These red/quenched massive disk galaxies have recently gained great interest into their formation and origins. The usually proposed quenching mechanisms, such as bar quenching and environment quenching, seem not suitable for those bulge-less quenched disks in low-density environment. In this paper, we use the TNG300 simulation to investigate the formation of massive quenched central disk galaxies. It is found that these galaxies contain less gas and harbor giant supermassive black holes(SMBHs) (above 10 8 M ) than their star forming counterparts. By tracing their formation history, we found that quenched disk galaxies formed early and preserved disk morphology for cosmological time scales. They have experienced less than one major merger on average and it is mainly mini-mergers (mass ratio <1/10) that contribute to the growth of their SMBHs. In the IllustrisTNG simulation the black hole feedback mode switches from thermal to kinetic feedback when the black hole mass is more massive than ∼ 10 8 M , which is more efficient to eject gas outside of the galaxy and to suppress further cooling of hot gaseous halo. We conclude that kinetic AGN feedback in massive red/quenched disk galaxy is the dominant quenching mechanism.

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“…Even though such galaxies are mainly lenticulars in the EFIGI sample (as we show in Figs. 12, 13 and 14), our observations are not in agreement with the evolutionary trajectories seen in Park et al (2021). We emphasize that understanding their results in light of ours can be prejudiced by their choice in definition for the two splits describing galaxies : star-forming and quiescent as well as disk and elliptical.…”

Section: Evolution Pathways Of Lenticulars In Numerical Simulationscontrasting

confidence: 71%

Aging of galaxies along the morphological sequence, marked by bulge growth and disk quenching

Quilley

Lapparent

2022

A&A

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Aims. We revisit the color bimodality of galaxies using the extensive EFIGI morphological classification of nearby galaxies. Methods. The galaxy profiles from the Sloan Digital Sky Survey (SDSS) gri images were decomposed as a bulge and a disk by controlled profile modeling with the Euclid SourceXtractor++ software. The spectral energy distributions from our resulting gri SDSS photometry complemented with Galaxy Evolution Explorer (GALEX) NUV photometry were fitted with the ZPEG software and PEGASE.2 templates in order to estimate the stellar masses and specific star formation rates (sSFR) of whole galaxies as well as their bulge and disk components. Results. The absolute NUV − r color versus stellar mass diagram shows a continuous relationship between the present sSFR of galaxies and their stellar mass, which spans all morphological types of the Hubble sequence monotonously. Irregular galaxies to intermediate-type Sab spirals make up the "Blue Cloud" across 4 orders of magnitude in stellar mass but a narrow range of sSFR. This mass build-up of spiral galaxies requires major mergers, in agreement with their frequently perturbed isophotes. At high mass, the Blue Cloud leads to the "Green Plain," dominated by S0a and Sa early-type spirals. It was formerly called the "Green Valley," due to its low density, but we rename it because of its wide stretch and nearly flat density over ∼ 2 magnitudes in NUV − r color (hence sSFR), despite a limited range of stellar mass (1 order of magnitude). The Green Plain links up the "Red Sequence," containing all lenticular and elliptical galaxies with a 2 order of magnitude mass interval, and systematically higher masses for the ellipticals. We confirm that the Green Plain cannot be studied using u − r optical colors because it is overlayed by the Red Sequence, hence NUV data are necessary. Galaxies across the Green Plain undergo a marked growth by a factor 2 to 3 in their bulge-to-total mass ratio and a systematic profile change from pseudo to classical bulges, as well as a significant reddening due to star formation fading in their disks. The Green Plain is also characterized by a maximum stellar mass of 10 11.7 M ⊙ beyond which only elliptical galaxies exist, hence supporting the scenario of ellipticals partly forming by major mergers of massive disk galaxies. Conclusions. The EFIGI attributes indicate that dynamical processes (spiral arms and isophote distortions) contribute to the scatter of the Main Sequence of star-forming galaxies (Blue Cloud), via the enhancement of star formation (flocculence, HII regions). The significant bulge growth across the Green Plain confirms that it is a transition region, and excludes a predominantly quick transit due to rapid quenching. The high frequency of bars for all spirals as well as the stronger spiral arms and flocculence in the knee of the Green Plain suggest that internal dynamics, likely triggered by flybys or (mainly minor) mergers, may be the key to the bulge growth of massive disk galaxies, which is a marker of the aging of galaxie...

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On the formation of massive quiescent galaxies with diverse morphologies in the TNG50 simulation

Cited by 7 publications

References 104 publications

The physical connection between central stellar surface density and stellar spin in SAMI and MaNGA nearby galaxies

The physical connection between central stellar surface density and stellar spin in SAMI and MaNGA nearby galaxies

Quenching of Massive Disk Galaxies in the IllustrisTNG Simulation

Aging of galaxies along the morphological sequence, marked by bulge growth and disk quenching

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