Galaxy zoo: stronger bars facilitate quenching in star-forming galaxies

Géron, Tobias; Smethurst, Rebecca; Lintott, Chris; Kruk, Sandor; Masters, Karen L.; Simmons, Brooke; Stark, David V.

doi:10.1093/mnras/stab2064

Cited by 38 publications

(26 citation statements)

References 122 publications

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“…Many studies have explored the properties of barred and unbarred galaxies in the local Universe, and there is growing evidence that bars are more likely to be found in disc galaxies that are red, massive and gas-poor than those that are in blue, low-mass, and gas-rich (e.g., Masters et al 2011Masters et al , 2012Cheung et al 2013;Gavazzi et al 2015;Consolandi 2016;Géron et al 2021). We present the properties of the barred and unbarred galaxies at stacked high redshifts 𝑧 = [2, 4] and redshifts 𝑧 = 1, 0.5, 0 in subsection 4.1.…”

Section: Properties Of Barred and Unbarred Galaxiesmentioning

confidence: 99%

The evolution of the barred galaxy population in the TNG50 simulation

Rosas-Guevara,

Bonoli,

Dotti

et al. 2021

Preprint

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We use the magnetic-hydrodynamical simulation TNG50 to study the evolution of barred massive disc galaxies. Massive spirals are already present as early as 𝑧 = 4, and stable bars start developing at these early epochs. Bars grow longer and stronger with time, with their size increasing at a pace similar to that of the disc scale lengths. The bar fraction mildly evolves with redshift for galaxies with 𝑀 * 10 10 M , being above ∼ 40% at 0.5 < 𝑧 < 3 and ∼ 30% at 𝑧 = 0. However, the bar fraction decreases significantly with increasing redshift when bars above a certain physical size or angular resolution limit are considered, reconciling the theoretical predictions with observational findings. We find that barred galaxies have an older stellar population, lower gas fractions, and less star formation compared to unbarred galaxies with the same stellar mass. Indeed, the discs of barred galaxies generally assembled earlier and faster than the discs of unbarred galaxies. When looking at the host haloes of these galaxies, barred galaxies are generally in haloes with larger concentrations and smaller spin parameters. The inner regions of barred galaxies are more baryon-dominated than those of unbarred galaxies, but with similar global stellar mass fractions. Our findings suggest that the bar population could be used as a potential tracer of the buildup of disc galaxies and their host haloes. We also release a catalogue of barred galaxies in TNG50 at 6 redshifts between 𝑧 = 4 and 𝑧 = 0, with their corresponding properties.

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Section: Properties Of Barred and Unbarred Galaxiesmentioning

confidence: 99%

The evolution of the barred galaxy population in the TNG50 simulation

Rosas-Guevara,

Bonoli,

Dotti

et al. 2021

Preprint

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“…In particular, stronger bars tend to have more enhanced central star formation (Zhou et al 2015;Lin et al 2017;Chown et al 2019), due to stronger effect in strong bars than in weak bars (Regan & Teuben 2004). Barred galaxies may have shorter depletion timescales measured for the whole galaxy (e.g., Géron et al 2021). Still, spatially resolved study finds no remarkable differences in the Kennicutt-Schmidt law in the central regions of barred and unbarred galaxies (Díaz-García et al 2021).…”

Section: Introductionmentioning

confidence: 91%

Strong spiral arms drive secular growth of pseudo bulges in disk galaxies

Yu,

Xu,

et al. 2022

Preprint

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Spiral-driven instabilities may drive gas inflow to enhance central star formation in disk galaxies. We investigate this hypothesis using the Sloan Digital Sky Survey (SDSS) in a sample of 2779 nearby unbarred star-forming main-sequence spiral galaxies. The strength of spiral arms is quantified by their average Fourier amplitude relative to the axisymmetric disk. The star formation properties in the central 1-3 kpc region were derived from the SDSS spectra. We show that galaxies with stronger spiral arms not only tend to have more intense central specific star formation rate (sSFR), larger Balmer absorption line index, and lower 4000-Å break strength, but also have enhanced central sSFR relative to sSFR measured for the whole galaxy. This link is independent of redshift, stellar mass, surface density, and concentration. There is a lack of evidence for strong spiral arms being associated with a significant fraction of starburst or post-starburst galaxies, implying that the spiral-induced central star formation is likely continuous rather than bursty. We also show that stronger spiral arms tend to have an increasing fraction of pseudo bulges, a relatively unchanged fraction of star-forming classical bulges, and a decreasing fraction of quenched classical bulges. Moreover, the concentration of galaxies hosting pseudo bulges mildly increases with stronger spiral arms, implying that spirals help pseudo bulges grow. The connection between spirals and the bulge type is partly attributed to the suppression of spirals by classical bulges and partly to the enhanced central star formation driven by spirals. We explain our results in a picture where spiral arms transport cold gas inward to trigger continuous central star formation, which facilitates the build-up of pseudo bulges. Spiral arms thus play a role in the secular evolution of disk galaxies.

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“…High-mass barred S0s have lower star formation rates compared to unbarred S0s, while the reverse is true for low-mass S0s. Lower star formation rates in barred galaxies is consistent with bar-driven quenching and gas removal (Spinoso et al 2017;Fraser-McKelvie et al 2020;Géron et al 2021), but further analysis is required to investigate these mechanisms in detail. Across all types and mass ranges in Table 1, barred galaxies have higher corotation parameters 𝜅 co,rot , with values higher in spirals than for S0s, consistent with more energetic corotation.…”

Section: Properties Of Barred Galaxiesmentioning

confidence: 97%

“…Bars are important drivers of galaxy evolution (Cheung et al 2013;Conselice 2014). They affect many key galaxy processes including the distribution of angular momentum (Weinberg 1985;Athanassoula 2005), secular evolution (Kormendy & Kennicutt 2004;Sheth et al 2005;Sellwood 2014), interactions with the stellar disc and surrounding dark matter halo (Athanassoula 2002;Valenzuela & Klypin 2003), gas dynamics and metallicities (Bournaud & Combes 2002;Berentzen et al 2007;Fanali et al 2015;Fraser-McKelvie et al 2019), star formation, especially in the centres of galaxies (Ellison et al 2011;Lin et al 2020), AGN activity (Alonso et al 2014;Galloway et al 2015) and quenching (Masters et al 2012;Kruk et al 2018;Fraser-McKelvie et al 2020;Géron et al 2021).…”

Section: Introductionmentioning

confidence: 99%

The evolution of barred galaxies in the EAGLE simulations

Cavanagh,

Bekki,

Groves

et al. 2021

Preprint

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We study the morphologies of 3,964 galaxies and their progenitors with 𝑀 ★ > 10 10 𝑀 in the reference EAGLE hydrodynamical simulation from redshifts 𝑧 = 1 to 𝑧 = 0, concentrating on the redshift evolution of the bar fraction. We apply two convolutional neural networks (CNNs) to classify 35,082 synthetic g-band images across 10 snapshots in redshift. We identify galaxies as either barred or unbarred, while also classifying each sample into one of four morphological types: elliptical (E), lenticular (S0), spiral (Sp), and irregular/miscellaneous (IrrM). We find that the bar fraction is roughly constant between 𝑧 = 0.0 to 𝑧 = 0.5 (32% to 33%), before exhibiting a general decline to 26% out to 𝑧 = 1. The bar fraction is highest in spiral galaxies, from 49% at 𝑧 = 0 to 39% at 𝑧 = 1. The bar fraction in S0s is lower, ranging from 22% to 18%, with similar values for the miscellaneous category. Under 5% of ellipticals were classified as barred. We find that the bar fraction is highest in low mass galaxies (𝑀 ★ ≤ 10 10.5 𝑀 ). Through tracking the evolution of galaxies across each snapshot, we find that some barred galaxies undergo episodes of bar creation, destruction and regeneration, with a mean bar lifetime of 2.24 Gyr. We further find that incidences of bar destruction are more commonly linked to major merging, while minor merging and accretion is linked to both bar creation and destruction.

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Galaxy zoo: stronger bars facilitate quenching in star-forming galaxies

Cited by 38 publications

References 122 publications

The evolution of the barred galaxy population in the TNG50 simulation

The evolution of the barred galaxy population in the TNG50 simulation

Strong spiral arms drive secular growth of pseudo bulges in disk galaxies

The evolution of barred galaxies in the EAGLE simulations

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