The impact of gas inflows on star formation rates and metallicities in barred galaxies

Ellison, Sara L.; Nair, Preethi; Patton, David R.; Scudder, Jillian M.; Mendel, J. Trevor; Simard, Luc

doi:10.1111/j.1365-2966.2011.19195.x

Cited by 174 publications

(230 citation statements)

References 84 publications

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“…By comparing barred and unbarred galaxies with the same global stellar mass, Ellison et al (2011) found an enhancement in central SFR for barred galaxies with global M * > 10 10 M⊙, with no corresponding enhancement in central metallicity. These authors suggested a possible explanation based on the simulations of Combes & Elmegreen (1993).…”

Section: Central Propertiesmentioning

confidence: 90%

“…This work is particularly motivated by the observational result of Ellison et al (2011) that the SFRs of barred galaxies are enhanced only for galaxies with log(M * /M⊙) > 10, where M * is the stellar mass. In contrast, the metallicity enhancement measured by Ellison et al (2011) is seen at all stellar masses.…”

Section: Introductionmentioning

confidence: 99%

“…The disparity between the central metallicity and the SFR was believed to be due to a fast, starburst-like formation episode in lowmass galaxies while high-mass galaxies retained a high SFR through their evolution. In order to provide a theoretical comparison with the results of Ellison et al (2011), we simulate isolated barred and unbarred galaxies of various stellar masses between log M * = 9.6 and 10.4 and study the variation as a function of mass of the SFR and gas flows along the bar of both barred and unbarred galaxies. We present our simulation code and our suite of simulations in Section 2.…”

Section: Introductionmentioning

confidence: 99%

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The mass dependence of star formation histories in barred spiral galaxies

Carles¹,

Martel²,

Ellison³

et al. 2016

Mon. Not. R. Astron. Soc.

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We performed a series of 29 gasdynamical simulations of disc galaxies, barred and unbarred, with various stellar masses, to study the impact of the bar on star formation history. Unbarred galaxies evolve very smoothly, with a star formation rate (SFR) that varies by at most a factor of three over a period of 2 Gyr. The evolution of barred galaxies is much more irregular, especially at high stellar masses. In these galaxies, the bar drives a substantial amount of gas toward the centre, resulting in a high SFR, and producing a starburst in the most massive galaxies. Most of the gas is converted into stars, and gas exhaustion leads to a rapid drop of star formation after the starburst. In massive barred galaxies (stellar mass M * > 2 × 10 10 M ⊙ ) the large amount of gas funnelled toward the centre is completely consumed by the starburst, while in lower-mass barred galaxies it is only partially consumed. Gas concentration is thus higher in lower-mass barred galaxies than it is in higher-mass ones. Even though unbarred galaxies funnelled less gas toward their centre, the lower SFR allows this gas to accumulate. At late times, the star formation efficiency is higher in barred galaxies than unbarred ones, enabling these galaxies to maintain a higher SFR with a smaller gas supply. Several properties, such as the global SFR, central SFR, or central gas concentration, vary monotonically with time for unbarred galaxies, but not for barred galaxies. Therefore one must be careful when comparing barred and unbarred galaxies that share one observational property, since these galaxies might be at very different stages of their respective evolution.

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Section: Central Propertiesmentioning

confidence: 90%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The mass dependence of star formation histories in barred spiral galaxies

Carles¹,

Martel²,

Ellison³

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Ellison et al 2011), we study in this subsection the dependence of the relative frequencies of SNe types on the presence of bars in spiral host galaxies. Table 12 shows the distribution of the number ratios of SN types after separating the hosts into unbarred and barred types.…”

Section: Dependence Of Relative Frequencies Of Sne Types On Host Barrmentioning

confidence: 99%

“…In this respect, the presence of bars can play an important role in the star formation of galaxies (e.g. Ellison et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Supernovae and their host galaxies – II. The relative frequencies of supernovae types in spirals

Hakobyan¹,

Nazaryan²,

Adibekyan³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present an analysis of the relative frequencies of different supernova (SN) types in spirals with various morphologies and in barred or unbarred galaxies. We use a well-defined and homogeneous sample of spiral host galaxies of 692 SNe from the Sloan Digital Sky Survey in different stages of galaxy-galaxy interaction and activity classes of nucleus. We propose that the underlying mechanisms shaping the number ratios of SNe types can be interpreted within the framework of interaction-induced star formation, in addition to the known relations between morphologies and stellar populations. We find a strong trend in behaviour of the N Ia /N CC ratio depending on host morphology, such that early spirals include more Type Ia SNe. The N Ibc /N II ratio is higher in a broad bin of early-type hosts. The N Ia /N CC ratio is nearly constant when changing from normal, perturbed to interacting galaxies, then declines in merging galaxies, whereas it jumps to the highest value in post-merging/remnant galaxies. In contrast, the N Ibc /N II ratio jumps to the highest value in merging galaxies and slightly declines in post-merging/remnant subsample. The interpretation is that the star formation rates and morphologies of galaxies, which are strongly affected in the final stages of interaction, have an impact on the number ratios of SNe types. The N Ia /N CC (N Ibc /N II ) ratio increases (decreases) from star-forming to active galactic nuclei (AGN) classes of galaxies. These variations are consistent with the scenario of an interaction-triggered starburst evolving into AGN during the later stages of interaction, accompanied with the change of star formation and transformation of the galaxy morphology into an earlier type.

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Stellar Populations of Bulges at Low Redshift

Sánchez‐Blázquez

2016

Astrophysics and Space Science Library

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The impact of gas inflows on star formation rates and metallicities in barred galaxies

Cited by 174 publications

References 84 publications

The mass dependence of star formation histories in barred spiral galaxies

The mass dependence of star formation histories in barred spiral galaxies

Supernovae and their host galaxies – II. The relative frequencies of supernovae types in spirals

Stellar Populations of Bulges at Low Redshift

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