Evolution of the Bar Fraction in COSMOS: Quantifying the Assembly of the Hubble Sequence

Sheth, Kartik; Elmegreen, D. M.; Elmegreen, Bruce G.; Capak, P.; Abraham, Roberto; Athanassoula, E.; Ellis, Richard S.; Mobasher, Bahram; Salvato, M.; Schinnerer, E.; Scoville, N. Z.; Spalsbury, L.; Strubbe, Linda E.; Carollo, M.; Rich, R. Michael; West, Andrew A.

doi:10.1086/524980

Cited by 389 publications

(509 citation statements)

References 91 publications

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“…Recent results suggest indeed that the fraction of barred spirals declines with redshift (Sheth et al 2008;Masters et al 2011;Melvin et al 2013).…”

Section: Introductionmentioning

confidence: 94%

Fractal basins of escape and the formation of spiral arms in a galactic potential with a bar

Ernst¹,

Peters²

2014

Monthly Notices of the Royal Astronomical Society

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We investigate the dynamics in the close vicinity of and within the critical area in a 2D effective galactic potential with a bar of Zotos. We have calculated Poincaré surfaces of section and the basins of escape. In both the Poincaré surfaces of section and the basins of escape we find numerical evidence for the existence of a separatrix which hinders orbits from escaping out of the bar region. We present numerical evidence for the similarity between spiral arms of barred spiral galaxies and tidal tails of star clusters.

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“…Recent results suggest indeed that the fraction of barred spirals declines with redshift (Sheth et al 2008;Masters et al 2011;Melvin et al 2013).…”

Section: Introductionmentioning

confidence: 94%

Fractal basins of escape and the formation of spiral arms in a galactic potential with a bar

Ernst¹,

Peters²

2014

Monthly Notices of the Royal Astronomical Society

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“…However, since the strongest change in morphology occurs in correspondence of the Balmer break (i.e. Cassata et al 2005;Sheth et al 2003Sheth et al , 2008, the strongest bias is introduced when optical rest-frame morphologies (4000 Å < λ < 10 000 Å) are compared with UV ones (λ < 4000 Å). In our case, the i-band maps the rest-frame r-band at z = 0.2, the V-band at z = 0.6 and the B-band at z = 1, therefore galaxies are observed redwards the Balmer break confidently up to z ∼ 0.8.…”

Section: The Morphological Classificationmentioning

confidence: 99%

The zCOSMOS redshift survey: the role of environment and stellar mass in shaping the rise of the morphology-density relation from z ~ 1

Tasca

Kneib²,

Iovino

et al. 2009

A&A

152

146

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Context. For more than two decades we have known that galaxy morphological segregation is present in the Local Universe. It is important to see how this relation evolves with cosmic time. Aims. To investigate how galaxy assembly took place with cosmic time, we explore the evolution of the morphology-density relation up to redshift z ∼ 1 using about 10 000 galaxies drawn from the zCOSMOS Galaxy Redshift Survey. Taking advantage of accurate HST/ACS morphologies from the COSMOS survey, of the well-characterised zCOSMOS 3D environment, and of a large sample of galaxies with spectroscopic redshift, we want to study here the evolution of the morphology-density relation up to z ∼ 1 and its dependence on galaxy luminosity and stellar mass. The multi-wavelength coverage of the field also allows a first study of the galaxy morphological segregation dependence on colour. We further attempt to disentangle between processes that occurred early in the history of the Universe or late in the life of galaxies. Methods. The zCOSMOS field benefits of high-resolution imaging in the F814W filter from the Advanced Camera for Survey (ACS). We use standard morphology classifiers, optimised for being robust against band-shifting and surface brightness dimming, and a new, objective, and automated method to convert morphological parameters into early, spiral, and irregular types. We use about 10 000 galaxies down to I AB = 22.5 with a spectroscopic sampling rate of 33% to characterise the environment of galaxies up to z ∼ 1 from the 100 kpc scales of galaxy groups up to the 100 Mpc scales of the cosmic web. The evolution of the morphology-density relation in different environments is then studied for luminosity and stellar-mass selected, volume-limited samples of galaxies. The trends are described and related to the various physical processes that could play a relevant role in the build-up of the morphology-density relation. Results. We confirm that the morphological segregation is present up to z ∼ 1 for luminosity-selected, volume-limited samples. The behaviour of the morphology-density relation gets flatter at fixed masses expecially above 10 10.6 M . We suggest the existence of a critical mass above which the physical processes governing galaxy stellar mass also determine the shaping of the galaxy more than its environment. We finally show that at a fixed morphology there is still a residual variation in galaxy colours with density. Conclusions. The observed evolution with redshift of the morphology-density relation offers an opportunity to trace the effect of nature and nurture as a function of environment. Even though it is based mainly on a biased view, the environmental dependence of the morphological evolution for luminosity-selected, volume-limited samples seems to indicate that nurture is in play. On the other hand, the lack of evolution observed for earlytype and spiral galaxies that are more massive than 10 10.8 M independents of the environment indicates that nature has imprinted these properties early in the life of...

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“…Their presence is quite ubiquitous, with recent observational data consistently establishing a bar fraction somewhere between 30% and 60% in the local universe (Knapen et al 2000;Martnez & Muriel 2011;Masters et al 2011;Lee et al 2012) and a slightly lesser value at higher redshift (Elmegreen et al 2004;Sheth et al 2008;Simmons et al 2014). Bars create a strong torque on the galaxy (Lynden-Bell 1979; leading to a redistribution of the gaseous and stellar component (Gadotti & dos Anjos 2001;Grand et al 2015) and a transport of angular momentum from the inner to the outer regions of the galaxy ( Seidel et al 2015).…”

Section: Introductionmentioning

confidence: 99%

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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Evolution of the Bar Fraction in COSMOS: Quantifying the Assembly of the Hubble Sequence

Cited by 389 publications

References 91 publications

Fractal basins of escape and the formation of spiral arms in a galactic potential with a bar

Fractal basins of escape and the formation of spiral arms in a galactic potential with a bar

The zCOSMOS redshift survey: the role of environment and stellar mass in shaping the rise of the morphology-density relation from z ~ 1

The mass dependence of star formation histories in barred spiral galaxies

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