Nearly all Massive Quiescent Disk Galaxies Have a Surprisingly Large Atomic Gas Reservoir

Zhang, Chengpeng; Peng, Yingjie; Ho, Luis C.; Maiolino, R.; Dekel, Avishai; Guo, Qi; Mannucci, F.; Li, Di; Yuan, Feng; Renzini, A.; Dou, Jing; Guo, Kaihua; Man, Zhongyi; Li, Qiong

doi:10.3847/2041-8213/ab4ae4

Cited by 62 publications

(51 citation statements)

References 61 publications

(71 reference statements)

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“…Figure 6 shows that even quenched galaxies with relatively large sizes are not fully reproduced by simulations. In particular, at star 10 11 , some of the larger galaxies where star formation has been halted belong to the population of quenched disks (e.g., Zhang et al 2019). Furthermore, as shown in Figure 12, TNG quenched disks are still in worse agreement with SDSS than star-forming disk, the Δ of quenched disks being twice as lower than that of star forming disks.…”

Section: Quenching May Affect the Small-scale Morphology By Modifying The Underlying Gas Distributionmentioning

confidence: 95%

A deep learning approach to test the small-scale galaxy morphology and its relationship with star formation activity in hydrodynamical simulations

Zanisi

Huertas-Company

Lanusse

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Hydrodynamical simulations of galaxy formation and evolution attempt to fully model the physics that shapes galaxies. The agreement between the morphology of simulated and real galaxies, and the way the morphological types are distributed across galaxy scaling relations are important probes of our knowledge of galaxy formation physics. Here, we propose an unsupervised deep learning approach to perform a stringent test of the fine morphological structure of galaxies coming from the Illustris and IllustrisTNG (TNG100 and TNG50) simulations against observations from a subsample of the Sloan Digital Sky Survey. Our framework is based on PixelCNN, an autoregressive model for image generation with an explicit likelihood. We adopt a strategy that combines the output of two PixelCNN networks in a metric that isolates the small-scale morphological details of galaxies from the sky background. We are able to quantitatively identify the improvements of IllustrisTNG, particularly in the high-resolution TNG50 run, over the original Illustris. However, we find that the fine details of galaxy structure are still different between observed and simulated galaxies. This difference is mostly driven by small, more spheroidal, and quenched galaxies that are globally less accurate regardless of resolution and which have experienced little improvement between the three simulations explored. We speculate that this disagreement, that is less severe for quenched discy galaxies, may stem from a still too coarse numerical resolution, which struggles to properly capture the inner, dense regions of quenched spheroidal galaxies.

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Section: Quenching May Affect the Small-scale Morphology By Modifying The Underlying Gas Distributionmentioning

confidence: 95%

A deep learning approach to test the small-scale galaxy morphology and its relationship with star formation activity in hydrodynamical simulations

Zanisi

Huertas-Company

Lanusse

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…The tidal force and/or gas ram pressure in such intermediate density environments could be strong enough to destroy the cold gas reservoir, but still too weak to affect the disk structures. Statistical studies of nearby massive red disks (10 10.5 -10 11.0 M ⊙ ) show larger bulge/total mass ratios than their blue counterparts [35,36]. Various quenching mechanisms have been theoretically proposed to quench a massive galaxy without AGN feedback such as halo quenching [5] and angularmomentum quenching [37], which should be investigated further.…”

Section: Discussionmentioning

confidence: 98%

A giant central red disk galaxy at redshift z = 0.76: Challenge to theories of galaxy formation

Liu

Jing

et al. 2021

Sci. China Phys. Mech. Astron.

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We report a giant red central disk galaxy in the XMM-LSS north region. The region is covered with a rich variety of multi-band photometric and spectroscopic observations. Using the photometric data of the Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) and spectroscopic observation of the baryon oscillation spectroscopic survey (BOSS), we find that the galaxy has a stellar mass of ∼10 11.6 M ⊙ . The galaxy has a red color and has an old stellar population, and thus its star formation has stopped. With the photometric image data of the Hyper Suprime-Cam (HSC) Subaru Strategic Program, we demonstrate that its luminosity profile is perfectly described by a Sérsic form with n=1.22 consistent with that of a disk. We also analyze its environment based on the VIMOS Public Extragalactic Redshift Survey (VIPERS) photometric catalog, and find that its close neighbors are all less massive, indicating that our observed galaxy is sitting at the center of its dark matter host halo. Existence of such a giant red central disk galaxy seriously challenges the current standard paradigm of galaxy formation, as there is no known physical mechanism to explain the quenching of its star formation. This conclusion is supported by state-of-the-art hydrodynamical simulations of galaxy formation.

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“…By assuming a molecular gas to dust mass ratio, δ, of 100 37 , we can thereby infer M H2 from M dust . In principle M dust could trace both neutral and molecular hydrogen, and quiescent galaxies at z~0 are known to harbor non-negligible neutral gas reservoirs 38 . Local studies show that the neutral hydrogen contribution varies widely 19,39 .…”

Section: Methodsmentioning

confidence: 99%

Exhausted gas reservoirs drive massive galaxy quenching in the early universe

Whitaker¹,

Williams²,

Mowla³

et al. 2020

Preprint

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When the Universe was merely three billion years old, about half of massive galaxies had already formed the bulk of their stars and new star formation plummeted [1]. How galaxies quench at such early times remains a puzzle, as their dark matter halos contain large gas reservoirs [2-4]. This gas should cool efficiently, sustaining star formation over long periods [5,6]. Here we present sensitive 1.3mm wavelength observations of cold dust in six quenched galaxies in the redshift range z=1.6 to z=3.2 with stellar masses ranging from 2.5x1010M⊙ to 5x1011M⊙, which are magnified by foreground galaxy clusters. Even with factors of up to 30 in magnification, four of the six galaxies are undetected at this wavelength. We show that these quenched galaxies have extremely little dust at early times, and by proxy very little cold molecular gas. The median dust mass is <0.01% of the stellar mass (molecular gas mass <1%), more than two orders of magnitude less than star-forming galaxies at this epoch [4]. The implication is that most early galaxies shut off star formation because their reservoir of molecular gas was rapidly depleted or removed, and is not being replenished.

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Nearly all Massive Quiescent Disk Galaxies Have a Surprisingly Large Atomic Gas Reservoir

Cited by 62 publications

References 61 publications

A deep learning approach to test the small-scale galaxy morphology and its relationship with star formation activity in hydrodynamical simulations

A deep learning approach to test the small-scale galaxy morphology and its relationship with star formation activity in hydrodynamical simulations

A giant central red disk galaxy at redshift z = 0.76: Challenge to theories of galaxy formation

Exhausted gas reservoirs drive massive galaxy quenching in the early universe

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