Galaxy And Mass Assembly (GAMA): properties and evolution of red spiral galaxies

Mahajan, Smriti; Gupta, Kriti Kamal; Rana, Rahul; Brown, M. J. I.; Phillipps, Steven; Bland-Hawthorn, Joss; Bremer, M. N.; Brough, Sarah; Holwerda, Benne W.; Hopkins, A. M.; Loveday, Jon; Pimbblet, Kevin A.; Wang, Lingyu

doi:10.1093/mnras/stz2993

Cited by 21 publications

(10 citation statements)

References 68 publications

(99 reference statements)

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“…While star-forming disk galaxies and quenched spheroidal galaxies are typically observed, the star-forming bulge-dominated and quenched disk galaxies are much less abundant. The quenched disk galaxies or red spiral galaxies have raised lots of interests recently (see e.g., Masters et al 2010;Cortese 2012;Tojeiro et al 2013;Schawinski et al 2014;Bremer et al 2018;Hao et al 2019;Guo et al 2020b;Luo et al 2020a;Mahajan et al 2020;Zhou et al 2020).…”

Section: Dependence On Morphologymentioning

confidence: 99%

Star Formation and Quenching of Central Galaxies from Stacked HI Measurements

Guo,

Jones,

Wang

et al. 2021

Preprint

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We quantitatively investigate the dependence of central galaxy Hi mass (M HI ) on the stellar mass (M * ), halo mass (M h ), star formation rate (SFR), and central stellar surface density within 1 kpc (Σ 1 ), taking advantage of the Hi spectra stacking technique using both the Arecibo Fast Legacy ALFA Survey and the Sloan Digital Sky Survey. We find that the shapes of M HI -M h and M HI -M * relations are remarkably similar for both star-forming and quenched galaxies, with massive quenched galaxies having constantly lower Hi masses of around 0.6 dex. This similarity strongly suggests that neither halo mass nor stellar mass is the direct cause of quenching, but rather the depletion of Hi reservoir. While the Hi reservoir for low-mass galaxies of M * < 10 10.5 M strongly increases with M h , more massive galaxies show no significant dependence of M HI with M h , indicating the effect of halo to determine the smooth cold gas accretion. We find that the star formation and quenching of central galaxies are directly regulated by the available Hi reservoir, with an average relation of SFR ∝ M 2.75 HI /M 0.40 * , implying a quasi-steady state of star formation. We further confirm that galaxies are depleted of their Hi reservoir once they drop off the star-formation main sequence and there is a very tight and consistent correlation between M HI and Σ 1 in this phase, with M HI ∝ Σ −2 1 . This result is in consistent with the compaction-triggered quenching scenario, with galaxies going through three evolutionary phases of cold gas accretion, compaction and post-compaction, and quenching.

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Section: Dependence On Morphologymentioning

confidence: 99%

Star Formation and Quenching of Central Galaxies from Stacked HI Measurements

Guo,

Jones,

Wang

et al. 2021

Preprint

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“…It is interesting to point out that a few studies of red spiral galaxies have appeared recently in the literature. Red disks with smaller mass (∼ 10 10.0 M ⊙ ) are found at intermediate local densities such as the infall regions of clusters [33,34]. 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.…”

Section: Discussionmentioning

confidence: 99%

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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“…Most red disks preferentially reside in intermediate/high density regions and they also show distinct sign of bars (e.g. Masters et al 2010;Hao et al 2019;Mahajan et al 2020;Zhou et al 2021).…”

Section: Amongmentioning

confidence: 99%

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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Galaxy And Mass Assembly (GAMA): properties and evolution of red spiral galaxies

Cited by 21 publications

References 68 publications

Star Formation and Quenching of Central Galaxies from Stacked HI Measurements

Star Formation and Quenching of Central Galaxies from Stacked HI Measurements

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

Quenching of Massive Disk Galaxies in the IllustrisTNG Simulation

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